QuantumSpacetime Phenomenology
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Abstract
I review the current status of phenomenological programs inspired by quantumspacetime research. I stress in particular the significance of results establishing that certain data analyses provide sensitivity to effects introduced genuinely at the Planck scale. My main focus is on phenomenological programs that affect the directions taken by studies of quantumspacetime theories.
Keywords
quantum spacetime loop quantum gravity spacetime noncommutativity1 Introduction and Preliminaries
1.1 The “QuantumGravity problem” as seen by a phenomenologist
Our present description of the fundamental laws of Nature is based on two disconnected pieces: “quantum mechanics” and “general relativity”. On the quantummechanics side our most significant successes were obtained applying relativistic quantum field theory, which turns out to be the appropriate formalization of (special) relativistic quantum mechanics. This theory neglects gravitational effects and is formulated in a flat/Minkowskian spacetime background. Interesting results (but, so far, with little experimental support) can be obtained by reformulating this theory in certain curved spacetime backgrounds, but there is no rigorous generalization allowing for the dynamics of gravitational fields. The only known way for having a manageable formulation of some gravitational effects within quantum field theory is to adopt the perspective of effective field theory [144, 276], which allows Lagrangians that are not renormalizable. At leading order, this effective theory just gives us back Einstein’s general relativity (GR), but beyond leading order it predicts corrections proportional to powers of \({E^2}/E_p^2\), where E is the characteristic energy scale of the process under consideration (typically, the centerofmass energy for a scattering experiment) and E_{ p } is the Planck scale (E_{ p } ∼ 10^{28} eV). The effectivefieldtheory description evidently breaks down at energies E on the order of the Planck scale, leaving unanswered [144, 276] most of the core issues concerning the interplay between gravity and quantum mechanics. Most importantly, the experiments that have formed our trust in quantum mechanics are nearly exclusively experiments in which gravitational effects are negligible at the presentlyachievable levels of experimental sensitivity (some of the rare instances where the outcome of a quantummechanical measurement is affected by gravitational effects, such as the one reported in Ref. [428], will be discussed later in this review).
On the gravity side our present description is based on GR. This is a classicalmechanics theory that neglects all quantum properties of particles. Our trust in GR has emerged in experimental studies and observations in which gravitational interactions cannot be neglected, such as the motion of planets around the Sun. Planets are “composed” of a huge number of fundamental particles, and the additive nature of energy (playing in such contexts roughly the role of “gravitational charge”) is such that the energy of a planet is very large, in spite of the fact that each composing fundamental particle carries only a small amount of energy. As a result, for planets gravitational interactions dominate over other interactions. Moreover, a planet satisfies the conditions under which quantum theory is in the classical limit: in the description of the orbits of the planets the quantum properties of the composing particles can be safely neglected.
GR and relativistic quantum mechanics do have some “shared tools”, such as the notion of spacetime, but they handle these entities in profoundly different manners. The differences are indeed so profound that it might be natural to expect only one or the other language to be successful, but instead they have both been extremely successful. This is possible because of the type of experiments in which they have been tested so far, with two sharply separated classes of experiments, allowing complementary approximations.
While somewhat puzzling from a philosopher’s perspective, all this would not on its own amount to a scientific problem. In the experiments we are presently able to perform and at the level of sensitivities we are presently able to achieve there is no problem. But a scientific problem, which may well deserve to be called a “quantumgravity problem”, is found if we consider, for example, the structure of the scattering experiments done in particlephysics laboratories. There are no surprises in the analysis of processes with an “in” state with two particles each with an energy of 10^{12} eV. Relativistic quantum mechanics makes definite predictions for the (distributions/probabilities of) results of this type of measurement procedure, and our experiments fully confirm the validity of these predictions. We are presently unable to redo the same experiments having as “in state” two particles with energy of 10^{30} eV (i.e., energy higher than the Planck scale), but, nonetheless, if one factors out gravity, relativistic quantum mechanics makes a definite prediction for these conceivable (but presently undoable) experiments. However, for collisions of particles of 10^{30} eV energy, the gravitational interactions predicted by GR are very strong and gravity should not be negligible. On the other hand, the quantum properties predicted for the particles by relativistic quantum mechanics (for example the fuzziness of their trajectories) cannot be neglected, contrary to the “desires” of the classical mechanics of our present description of gravity. One could naively attempt to apply both theories simultaneously, but it is well established that such attempts do not produce anything meaningful (for example by encountering uncontrollable divergences). As mentioned above, a framework where these issues can be raised in very precise manner is the one of effective quantum field theory, and the break down of the effective quantum field theory of gravitation at the Planck scale signals the challenges that are here concerning me.
This “transPlanckian collisions” picture is one (not necessarily the best, but a sufficiently clear) way to introduce a quantumgravity problem. But is the conceivable measurement procedure I just discussed truly sufficient to introduce a scientific problem? One ingredient appears to be missing: the measurement procedure is conceivable but presently we are unable to perform it. Moreover, one could argue that mankind might never be able to perform the measurement procedure I just discussed. There appears to be no need to elaborate predictions for the outcomes of that measurement procedure. However, it is easy to see that the measurement procedure I just discussed contains the elements of a true scientific problem. One relevant point can be made considering the experimental/observational evidence we are gathering about the “early Universe”. This evidence strongly supports the idea that in the early Universe particles with energies comparable to the Planck energy scale E_{ p } were abundant, and that these particles played a key role in those early stages of evolution of the Universe. This does not provide us with opportunities for “good experiments” (controlled repeatable experiments), but it does represent a context in which proposals for the quantumgravity/Planckscale realm could be tested. Different scenarios for the physical theory that applies in the quantumgravity realm could be compared on the basis of their description of the early Universe. The detailed analysis of a given physical theory for the quantumgravity realm could allow us to establish some characteristic predictions for the early Universe and for some manifestations in our observations (cosmology) of those early stages of evolution of the Universe. The theory would be testable on the basis of those predictions for our present observations. Therefore, these earlyUniverse considerations provide an opportunity for comparison between the predictions of a quantumgravity theory and measurement results. And it might not be necessary to resort to cosmology: the fact that (in setting up the quantumgravity problem) we have established some objective limitations of our present theories implies that some qualitatively new effects will be predicted by the theory that applies to the quantumgravity realm. These effects should dominate in that realm (in particular, they will profoundly affect the results of measurements done on particles with Planckscale energy), but they should always be present. For processes involving particles with energy E much smaller than E_{ p } the implications of a typical quantumgravity theory will be rather marginal but not altogether absent. The magnitude of the associated effects should be suppressed by some small overall coefficients, probably given by powers of the ratio E/E_{ p }; small but different from zero.
Therefore, we do have a genuine “quantumgravity problem”, and this problem has been studied for more than 70 years [508]. Unfortunately, most of this research has been conducted assuming that no guidance could be obtained from experiments. But, if there is to be a “science” of the quantumgravity problem, this problem must be treated just like any other scientific problem, seeking desperately the guidance of experimental facts, and letting those facts take the lead in the development of new concepts. Clearly, physicists must hope this also works for the quantumgravity problem, or else abandon it to the appetites of philosophers.
It is unfortunately true that there is a certain level of risk that experiments might never give us any clear lead toward quantum gravity, especially if we are correct in expecting that the magnitude of the characteristic effects of the new theory should be set by the tiny Planck length (ℓ_{ p } ≡ 1/Ep ∼ 10^{−35} m, the inverse of the huge Planck scale in natural units). But even if the new effects were really so small we could still try to uncover experimentally some manifestations of quantum gravity. This is hard, and there is no guarantee of success, but we must try. As I shall stress again in later parts of this first section, let me note here that some degree of optimism could be inspired by considering, for example, the prediction of proton decay within certain modern grand unified theories of particle physics. The decay probability for a proton in those theories is really very small, suppressed by the fourth power of the ratio between the mass of the proton and the grand unification scale (a scale that is only some three orders of magnitude smaller than the Planck scale), but meaningful tests of scenarios for proton decay in grand unified theories have been devised.
While the possibility of a “quantum gravity phenomenology” [52] could be considered, on the basis of these arguments, even in the early days of quantumgravity research, a sizable effort has finally matured only since the second half of the 1990s. In particular, only over this recent period do we have the first cases of phenomenological programs that truly affect the directions taken by more formal work in quantum gravity. And, especially in relation to this healthy twoway crossinfluence between formal theory and phenomenology, a prominent role has been played by proposals testing features that could be manifestations of spacetime quantization. The expectation that the fundamental description of spacetime should not be given by a classical geometry is shared by a large majority of quantumgravity researchers. And, as a result, the phenomenology inspired by this expectation has had influence on a sizable part of the recent quantumgravity literature. My goal here is primarily the one of reviewing the main results and proposals produced by this emerging area of phenomenology centered on the possibility of spacetime quantization.
1.2 Quantum spacetime vs quantum black hole and graviton exchange
The notion of “quantumgravity research” can have a different meaning for different researchers. This is due both to the many sides of the quantumgravity problem and the fact that most researchers arrive to the study of quantum gravity from earlier interests in other areas of physics research. Because of its nature the quantumgravity problem has a different appearance, for example, to a particle physicist and to a relativist.
In particular, this affects the perception of the implications of the “double role” of gravitational fields: unlike all other fields studied in fundamental physics the gravitational field is not just used to describe “gravitational interactions” but also characterizes the structure of spacetime itself. The structure of Einstein’s theory of gravitational phenomena tells us both of the geometry of spacetime, which should be described in terms of smooth Riemannian manifolds, and of the implications of Einstein’s equations for dynamics. But in most approaches these two sides of gravity are not handled on the same footing. Particularly from the perspective of a particle physicist it makes sense to focus on contexts amenable to treatment assuming some given Riemannianmanifold spacetime background and “gravitons” as mediators of “perturbative gravitational interactions”. Other researchers, typically not coming from a particlephysics background, are instead primarily interested in speculations for how to replace Riemannian manifolds in the description of the structure of spacetime, and contemplating a regime describing perturbative gravitational interactions is not one of their main concerns.
Because of my objectives, it is appropriate for me to locate early on in this review the quantumspacetime issues within the broader spectrum of quantumgravity research.
1.2.1 The quantumblackhole regime
We do expect that there is a regime of physics where quantum gravity does not simply amount to small corrections to our currently adopted theories, but rather our current theories should be there completely inapplicable. An example of this is the class of hypothetical situations discussed in my opening remarks: if we consider a collision with impact parameter on the order of the Planck length between two particles, which exchange in the collision an energy on the order of the Planck scale, then our current theories do not even give us a reliable first approximation of the outcome.
If M ∼ ℏ/ℓ_{ p } (rest energy on the order of the Planck scale), the Compton and Schwarzschild radii are of the same order of magnitude and quantum mechanics cannot ignore gravitation but at the same time gravitation cannot ignore quantum mechanics. Evidently we can get nowhere attempting to investigate this issue by just combining^{2} somehow the Standard Model of particle physics and the generalrelativistic classical description of gravitational phenomena.
Another context of similar conceptual content can be imagined if we take for granted (which we can do only as working assumptions) the existence of Hawking radiation. We could then start with an isolated macroscopic black hole and attempt to describe its whole future evolution. As long as the black hole remains macroscopic, but loses weight through Hawking radiation, we can imagine to be able to devise a reliable first approximation. But when the black hole reaches Plancklength size (and Planckscale rest energy) we are again left without any even approximate answers.
The description of these types of “quantumblackhole regimes” (description that I shall use rather generically, including for example the regime characteristic of the very early Universe) is evidently an example of cases such that we could only have a satisfactory picture by understanding how both of the two roles of the gravitational fields need to be revised (how spacetime structure should be then described and how the gravitationalinteraction aspects of gravitation should be then described).
Providing a description of such a quantumblackhole regime is probably the most fascinating challenge for quantumgravity research, but evidently it is not a promising avenue for actually discovering quantumgravity effects experimentally. As I shall mention, somewhat incidentally in a few points of this review, this expectation would change if, surprisingly, gravitation turns out to be much stronger than we presently expect, so that at least in some contexts its strength is not characterized by the Planck scale. But this review adopts the conservative view that quantumgravity effects are at least roughly as small as we expect, and, therefore, characterized roughly by the Planck scale. And if that is the case, it is hard to even imagine a future in which we gain access to a quantumblackhole regime.
A key assumption of this review is that quantum gravity will manifest itself experimentally in the shape of small corrections to contexts, which we are able to describe in first approximation within our current theories.
1.2.2 The gravitonexchange regime
For particle physicists (and, therefore, for at least part of the legitimate overall perspective on the quantumgravity problem) the most natural opportunities in which quantum gravity could introduce small corrections are in contexts involving the gravitationalinteraction aspects of quantum gravity.
Rather than attempting to give general definitions let me offer a clear example. These are studies of longrange corrections to the Newtonian limit of gravitation, where gravity does look like a Newtonforce interaction. By focusing on longrange features one stays far from the trouble zone mentioned in the previous Section 1.2.1. But there are still issues of considerable interest, at least conceptually, that quantum gravity should address in that regime. It is natural to expect that the description of gravity in terms of a Newtonforce interaction would also show traces of the new laws that quantum gravity will bring about.
This illustrates the sort of effects one may look for within schemes centered on a background Minkowski spacetime and properties of the graviton. In this specific case the effect is unmanageably small,^{3} but in principle one could look for other effects of this sort that might be observably large in some applications.
1.2.3 The quantumspacetime regime
Having given some examples of the ways in which quantum gravity might change our description of gravitational interactions, let me now turn to the complementary type of issues that are in focus when one studies the idea of spacetime quantization.
The nature of the quantumgravity problem tells us in many ways that the ultimate description of spacetime structure is not going to be in terms of a smooth classical geometry. We do not have at present enough information to deduce how our formalization of spacetime should change, but it must change. The collection of arguments in support of this expectation (see, e.g., Refs. [406, 532, 269, 44, 332, 442, 211, 20, 432, 50, 249, 489]) is impressive and relies both on aspects of the quantumgravity problem and on analyses of proposed approaches to the solution of the quantumgravity problem.
Surely, some very dramatic manifestations of spacetime quantization should be expected in what I labeled as the quantumblackhole regime. But, as already stressed above, it is hard to even imagine managing to derive evidence of spacetime quantization from experimental access to that regime. It is easy to see that our best chance for uncovering nonclassical properties of spacetime is to focus on the implications of spacetime quantization for the “Minkowski limit” (or perhaps the “de Sitter limit”) of quantum gravity. Our data on contexts we presently describe as involving particle propagation in a background Minkowski spacetime is abundant and of high quality. If the fundamental formalization of spacetime is not in terms of a smooth classical geometry then we should find some traces of spacetime quantization also in those wellstudied contexts. The effects are likely to be very small, but the quality of the data available to us in this quantumspacetime regime is very high, occasionally high enough to probe spacetime structure with Planckscale sensitivity.
This is the main theme of my review. I do not elaborate further on it here since it will take full shape in the following.
1.2.4 Aside on the classicalgravity regime
It is an interesting aspect of how the quantumgravity community is fragmented to observe that it is sometimes difficult to explain to a relativist how gravitonexchange studies could be seen as part of quantumgravity research and it is difficult to explain to particle physicists how studies of particles not interacting gravitationally in a quantumspacetime can play a role in quantumgravity research. I hope this Section proves useful in this respect.
Let me also discuss one more aspect of the interplay between quantum mechanics and gravitation that is of interest from a quantumgravity perspective, even though at first sight it does not look like quantum gravity at all. These are studies of quantum mechanics in a curved background spacetime, without assuming spacetime is quantized and without including any gravitonlike contribution to the interactions. No aspect of gravity is quantized in such studies, but they concern a regime that must be present as a limiting case of quantum gravity, and, therefore, by studying this regime we are establishing constraints on how quantum gravity might look.
On the conceptual side perhaps the most significant example of how quantum mechanics in curved spacetime backgrounds can provide important hints toward quantum gravity is provided by studies of blackhole thermodynamics. And it is a regime of physics where we do have some experimental access mainly through studies of the quantum properties of particles in cases when the geometry of spacetime near the surface of the Earth (essentially gravity of Earth, the acceleration g) does matter. I shall mention a couple of these experimental studies in the next Section 1.3.
While my focus here is on quantumspacetime studies, it will occasionally be useful for me to adopt the perspective of quantum mechanics in curved classical background spacetimes.
1.3 20th century quant umgravity phenomenology
In order to fully expose the change of perspective, which matured over the last decade, it is useful to first discuss briefly some earlier analyses that made contact with experiments/observations and are relevant for the understanding of the interplay between GR and quantum mechanics.
Some of the works produced by Chandrasekhar in the 1930s already fit this criterion. In particular, the renowned Chandrasekhar limit [164, 165], which describes the maximum mass of a whitedwarf star, was obtained introducing some quantummechanical properties of particles (essentially Pauli’s exclusion principle) within an analysis of gravitational phenomena.
A fully rigorous derivation of the Chandrasekhar limit would require quantum gravity, but not all of it: it would suffice to master one special limit of quantum gravity, the “classicalgravity limit”, in which one takes into account the quantum properties of matter fields (particles) in the presence of rather strong spacetime curvature (treated, however, classically). By testing experimentally the Chandrasekharlimit formula, one is, therefore, to some extent probing (the classicalgravity limit of) quantum gravity.
The COW experiments exploit the fact that the Earth’s gravitational potential puts together the contributions of a very large number of particles (all the particles composing the Earth) and, as a result, in spite of its perparticle weakness, the overall gravitational field is large enough to introduce observable effects.
Valuable reading material relevant for these COW experiments can be found in Refs. [484, 252, 14]. While the basic message is that a gravityimproved Schrödinger equation of the form (1) is indeed essentially applicable, some interesting discussions have been generated by these COW experiments, particularly as a result of the data reported by one such experiment [369] (data whose reliability is still being debated), which some authors have interpreted as a possible manifestation of a violation of the equivalence principle.
In the same category of studies relevant for the classicalgravity limit of quantum gravity I should mention some proposals put forward mainly by Anandan (see, e.g., Ref. [77, 76]), already in the mid 1980s, and some very recent remarkable studies that test how the gravitational field affects the structure of quantum states, such as the study reported in Ref. [428] that I shall discuss in some detail later in this review.
Evidently, the study of the classical limit provides only a limited window on quantum gravity, and surely cannot provide any insight on the possibility of shortdistance spacetime quantization, on which I shall focus here.
A list of early examples of studies raising at least the issue that spacetime structure might one day be probed with Planckscale sensitivity should start with the arguments reported by Mead in 1965 [407]. There, Mead contemplated the broadening of spectral lines possibly resulting from adopting the Planck length as the value of the minimum possible uncertainty in position measurements. Then, in works published in the 1980s and early 1990s, there were a few phenomenological studies, adopting the Planck scale as target and focusing essentially on the possibility that quantummechanical coherence might be spoiled by quantumgravity effects. One example is provided by the studies of Planckscaleinduced CPTsymmetry violation and violations of ordinary quantum mechanics reported in Refs. [219, 220] and references therein (also see, for aspects concerning mainly the CPTsymmetry aspects, Refs. [298, 108]), which are particularly relevant for the analysis of data [13] on the neutralkaon system. A quantization of spacetime is encoded in the noncriticalstringtheory formalism adopted in Refs. [219, 220], but only to the extent that one can view as such the novel description of time there adopted. A similar characterization applies to the studies reported in Refs. [452, 453, 454], which considered violations of ordinary quantum mechanics of a type describable in terms of the “primarystatediffusion” formalism, with results that could be relevant for atom interferometry. Also in Refs. [452, 453, 454] the main quantumspacetime feature is found in the description of time.
From a broader quantumgravityproblem perspective I should also mention the possibility of violations of CPT and Lorentz symmetry within string theory analyzed in Refs. [347, 345]. These studies, like most phenomelogyrelevant studies inspired by string theory (see related comments later in this review), do not involve any spacetime quantization and do not necessarily imply that the magnitude of the effects is set by a Planckian scale. But they should nonetheless be prominently listed among the early proposals assuming that some of the theories used in quantumgravity research might be testable with currentlyavailable experimental techniques.
1.4 Genuine Planckscale sensitivity and the dawn of quantumspacetime phenomenology
The rather isolated proposals that composed “20thcentury quantumgravity phenomenology” were already rather significant. In particular, some of these studies, perhaps most notably the ones in Ref. [220] and Ref. [454], were providing first preliminary evidence of the fact that it might be possible to investigate experimentally the structure of spacetime at the Planck scale, which is expected to be the main key to the understanding of the quantumgravity realm, and should involve spacetime quantization. But, in spite of their objective significance, these studies did not manage to have an impact on the overall development of quantumgravity research. For example, all mainstream quantumgravity reviews up to the mid 1990s still only mentioned the “experiments issue” in the form of some brief folkloristic statements, such as “the only way to test Planck scale effects is to build a particle accelerator all around our galaxy”.
The fact that up to the mid 1990s the possibility of a quantumspacetime phenomenology was mostly ignored, resulted in large part from a common phenomenon of “human inertia” that affects some scientific communities, but some role was also played by a meaningful technical observation: the studies available up to that point relied on models with the magnitude of the effect set by a free dimensionless parameter, and at best the sensitivity of the experiment was at a level such that one could argue setting the value of the dimensionless parameter as a ratio between the Planck length and one of the characteristic length scales of the relevant physical context. It is true that this kind of dimensionalanalysis reasoning does not amount to really establishing that the relevant candidate quantumgravity effect is being probed with Planckscale sensitivity, and this resulted in a perception that such studies, while deserving some interest, could not be described objectively as probes of the quantumgravity realm. For some theorists a certain level of uneasiness also originated from the fact that the formalisms adopted in studies such as the ones in Ref. [220] and Ref. [454] involved rather virulent departures from quantum mechanics.
Still, it did turn out that those earlier attempts to investigate the quantumgravity problem experimentally were setting the stage for a wider acceptance of quantumspacetime phenomenology. The situation started to evolve rather rapidly when in the span of just a few years, between 1997 and 2000, several analyses were produced describing different physical contexts in which effects introduced genuinely at the Planck sale could be tested. It started with some analyses of observations of gammaray bursts at subMeV energies [66, 247, 491], then came some analyses of large laserlight interferometers [51, 54, 53, 433], quickly followed by the first discussions of Planck scale effects relevant for the analysis of ultrahighenergy cosmic rays [327, 38, 73] and the first analyses relevant for observations of TeV gamma rays from blazars [38, 73, 463] (also see Ref. [331, 119]).
In particular, the fact that some of these analyses (as I discuss in detail later) considered Planckscale effects amounting to departures from classical Lorentz symmetry played a key role in their ability to have an impact on a significant portion of the overall quantumgravityresearch effort. Classical Lorentz symmetry is a manifestation of the smooth (classical) lightcone structure of Minkowski spacetime, and it has long been understood that by introducing new “quantum features” (e.g., discreteness or noncommutativity of the spacetime coordinates) in spacetime structure, as some aspects of the “quantumgravity problem” might invite us to do, Lorentz symmetry may be affected. And the idea of having some departure from Lorentz symmetry does not necessarily require violations of ordinary quantum mechanics. Moreover, by offering an opportunity to test quantumgravity theories at a pure kinematical level, these “Lorentzsymmetrytest proposals” provided a path toward testability that appeared to be accessible even to the most ambitious theories that are being considered as candidates for the solution of the quantum gravity problem. Some of these theories are so complex that one cannot expect (at least not through the work of only a few generations of physicists) to extract all of their physical predictions, but the kinematics of the “Minkowski limit” may well be within our reach. An example of this type is provided by Loop Quantum Gravity (LQG) [476, 96, 502, 524, 93], where one is presently unable to even formulate many desirable physics questions, but at least some (however tentative) progress has been made [247, 33, 523, 75, 128] in the exploration of the kinematics of the Minkowski limit.
From a purephenomenology perspective, the late1990s transition is particularly significant, as I shall discuss in greater detail later, in as much as it marks a sharp transition toward falsifiability. Some of the late1990s phenomenology proposals concern effects that one can imagine honestly deriving in a given quantumgravity theory. Instead the effects described in studies such as the ones reported in Ref. [220] and Ref. [454] were not really derived from proposed models but rather they were inspired by some paths toward the solution of the quantumgravity problem (the relevant formalisms were not really manageable to the point of allowing a rigorous derivation of the nature and size of the effects under study, but some intuition for the nature and size of the effects was developed combining our limited understanding of the formalisms and some heuristics). Such a line of reasoning is certainly valuable, and can inspire some meaningful “new physics” experimental searches, but if the results of the experiments are negative the theoretical ideas that motivated them are not falsified: when the link from theory to experiments is weak (contaminated by heuristic arguments) it is not possible to follow the link in the opposite direction (use negative experimental results to falsify the theory). Through further developments of the work that started in the late 1990s we are now getting close to taking quantumspacetime phenomenology from the mere realm of searches of quantumspacetime effects (which are striking if they are successful but have limited impact if they fail) to the one of “falsification tests” of some theoretical ideas. This is a point that I am planning to convey strongly with some key parts of this review, together with another sign of maturity of this phenomenology: the ability to discriminate between different (but similar) Planckscale physics scenarios. In order for a phenomenology to even get started one must find some instances in which the newphysics effects can be distinguished from the effects predicted by current theories, but a more mature phenomenology should also be able to discriminate between similar (but somewhat different) newphysics scenarios.
Together with some (however slow) progress toward establishing the ability to falsify models and discriminate between models, the phenomenology work of this past decade has also shown that the handful of examples of “Planckscale sensitivities” that generated excitement between 1997 and 2000 were not a “onetime lucky streak”: the list of examples of experimental/observational contexts in which sensitivity to some effects introduced genuinely at the Planck scale is established (or found to be realistically within reach) has continued to grow at a steady pace, as the content of this review will indicate, and the number of research groups joining the quantumspacetimephenomenology effort is also growing rapidly. And it is not uncommon for recent quantumgravity reviews [91, 475, 501, 151], even when the primary focus is on developments on the mathematics side, to discuss in some detail (and acknowledge the significance of) the work done in quantumgravity phenomenology.
1.5 A simple example of genuine Planckscale sensitivity
So far, my preliminary description of quantumspacetime phenomenology has a rather abstract character. It may be useful to now provide a simple example of analysis that illustrates some of the concepts I have discussed and renders more explicit the fact that some of the sensitivity levels now available experimentally do correspond to effects introduced genuinely at the Planck scale.
I should stress that the idea of a rigidlattice description of spacetime is not really one of the most advanced for quantumgravity research (but see the recent related study in Ref. [114]). Moreover, while it is easy to describe a free particle on such a lattice, the more realistic case of interacting fields is very different, and its implications for the form of the onshell relation are expected to be significantly more complex than assumed in Eq. (2). In particular, if described within effective field theory, the implications for interacting theories of such a lattice description of spacetime include departures from specialrelativistic onshellness for which there is no Planckscale suppression, and are therefore unacceptable. This is due to loop corrections, through a mechanism of the type discussed in Refs. [455, 182, 515, 190] (on which I shall return later), and assumes one is naturally unwilling to contemplate extreme finetuning. I feel it is nonetheless very significant that the, however, unrealistic case of a free particle propagating in a lattice with Planckscale lattice spacing leads to features of the type shown in Eq. (2). It shows that features of the type shown in Eq. (2) have magnitude set by nothing else but a feature of Planckscale magnitude introduced in spacetime structure. So, in spite of the idealizations involved, the smallness of the effects discussed in this Section is plausibly representative of the type of magnitude that quantumspacetime effects could have, even though any realistic model of the Standard Model of particle physics in a quantum spacetime, should evidently remove those idealizations.
One finds that in most contexts corrections to the energymomentum relation of the type in Eq. (2) are completely negligible. For example, for the analysis of centerofmass collisions between particles of energy ∼ 1 TeV (such as the ones studied at the LHC) these correction terms affect the analysis at the level of 1 part in 10^{32}. However (at least if such a modified dispersion relation is part of a framework with standard laws of energymomentum conservation), one easily finds [327, 38, 463, 73] significant implications for the cosmicray spectrum. In particular, one can consider the “GZK cutoff” (named after GreisenZatsepinKuzmin), which is a key expected feature of the cosmicray spectrum, and is essentially given by the threshold energy for cosmicray protons to produce pions in collisions with cosmic microwave background radiation (CMBR) photons. In the evaluation of the threshold energy for p + γ_{cmbr} → p + π, the \(1/E_p^2\) correction terms of (2) can be very significant. As I shall discuss in greater detail in Section 3.5, whereas the classicalspacetime prediction for the GZK cutoff is around 5·10^{19} eV, a much higher value of the cutoff is naturally obtained [327, 38, 463, 73] in frameworks with the structure of Eq. (2). The Planckscale correction terms in Eq. (2) turn into corresponding correction terms for the thresholdenergy formula, and the significance of these corrections can be roughly estimated with \(\eta {E^4}/(\epsilon E_p^2)\), where E is the energy of the cosmicray proton and ϵ is the energy of the CMBR photon, to be compared to m^{2}/16_{ ∊ }, where m here is the proton mass, which roughly gives the GZK scale. Adopting the “typical quantumgravity estimate”^{6} η ∼ 1 it turns out that in the GZK regime the ratio E/m is large enough to compensate for the smallness of the ratio E/E_{ p }, so that a term of the type \({E^4}/(\epsilon E_p^2)\) is not negligible with respect to m^{2}/∊. This observation is one of the core ingredients of the quantumspacetime phenomenology that has been done [327, 38, 463, 73] analyzing GZKscale cosmic rays. Another key ingredient of those analyses is the quality of cosmicray data, which has improved very significantly over these last few years, especially as a result of observations performed at the Pierre Auger Observatory.
Let me here use this cosmicray context also as an opportunity to discuss explicitly a first example of the type of “amplifier” that is inevitably needed in quantumgravity phenomenology. It is easy to figure out [52, 73] that the large ordinaryphysics number that acts as amplifier of the Planckscale effect in this case is provided by the ratio between a cosmicray proton ultrahigh energy, which can be of order 10^{20} eV, and the mass (rest energy) of the proton. This is clearly shown by the comparison I made between an estimate of Planckscale corrections of order \({E^4}/(\epsilon E_p^2)\) and an estimate of the uncorrected result of order m^{2}/e. Evidently, E/m is the amplifier of the Planckscale corrections, which also implies that these Planckscale modifications of the photopionproduction threshold formula go very quickly from being significant to being completely negligible, as the proton energy is decreased. A cosmicray proton with energy E on the order of 10^{20} eV is so highly boosted that E/m_{ p } ∼ 10^{11}, and this leads to \({E^4}/(\epsilon E_p^2) \sim {m^2}/\epsilon\) in my estimates, but at acceleratoraccessible proton energies (and proton boosts with respect to its rest frame) the correction is completely negligible. According to traditional quantumgravity arguments, which focus only on the role played by the ratio E/E_{ p }, one should assume that this analysis could be successful only when E/E_{ p } ∼ 1; clearly instead this analysis is successful already at energies of order 10^{20} eV (i.e., some 8 orders of magnitude below the Planck scale). And this is not surprising since the relevant Planckscale effect is an effect of Lorentz symmetry violation, so that large boosts (i.e., in this context, large values of E/m_{ p }) can act as powerful amplifiers of the effect, even when the energies are not Planckian.
1.6 Focusing on a neighborhood of the Planck scale
There are a strikingly large number of arguments pointing to the Planck scale as the characteristic scale of quantumgravity effects. Although clearly these arguments are not all independent, their overall weight must certainly be judged as substantial. I shall not review them here since they can easily be found in several quantumgravity reviews, and there are even some dedicated review papers (see, e.g., Ref. [249]). Faithful to the perspective of this review, I do want to stress one argument in favor of the Planck scale as the quantumgravity/quantumspacetime scale, which is often overlooked, but is in my opinion particularly significant, especially since it is based (however indirectly) on experimental facts. These are the wellknown experimental facts pointing to a unification of the coupling “constants” of the electroweak forces and of the strong force. While gravity usually is not involved in arguments that provide support for unification of the nongravitational couplings, it is striking from a quantumgravity perspective that, even just using the little information we presently have (mostly at scales below the TeV scale), our present best extrapolation of the available data on the running of these coupling constants rather robustly indicates that there will indeed be a unification and that this unification will occur at a scale that is not very far from the Planck scale. In spite of the fact that we are not in a position to exclude that it is just a quantitative accident, this correspondence between (otherwise completely unrelated) scales must presently be treated as the clearest hint of new physics that is available to us.
Even setting aside this couplingunification argument, there are other compelling reasons for attributing to the Planck scale the role of characteristic sale of quantumgravity effects. In particular, if one adopts the perspective of the effectivequantumfieldtheory description of gravitational phenomena the case for the Planck scale can be made rather precisely. A particularly compelling argument in this respect is found in Ref. [276] which focuses on the loss of unitarity within the effectivequantumfieldtheory description of gravitational phenomena. Unitarity has been a successful criterion for determining the scale at which other effective quantum field theories break down, such as the Fermi theory of weak interactions. And it does turn out that the scale at which unitarity is violated for the effectivequantumfieldtheory description of gravitational phenomena is within an order of magnitude of the Planck scale [276].
But it appears legitimate to consider alternatives to such estimates. For example, some authors (see, e.g., Ref. [146]) consider it to be likely that the “effective Newton constant” is also affected by some sort of renormalizationgroup running, and, if this is the case, then the prospects of all these arguments would change significantly. For the length scale of spacetime quantization, ℓ_{QST}, naively assumed to be given by \(\sqrt {{G_N}(\infty)}\), where G_{ N } (∞) is the measured value of the Newton constant (characteristic of gravity at large distances), any running of gravity would imply an estimate^{7} of the type \({\ell _{{\rm{QST}}}} \sim \sqrt {{G_N}({\ell _{{\rm{QST}}}})}\).
In relation to estimates of the scale of spacetime quantization these considerations should invite us to consider the Planck length, ∼ 10^{−35} m only as a crude, very preliminary estimate. Throughout this review I shall tentatively take into account this issue by assuming that the scale where nonclassical properties of spacetime emerge should be somewhere between ∼ 10^{−32} m and ∼ 10^{−38} m, hoping that three orders of magnitude of prudence from above and below should suffice.
It is striking that these considerations also allow one to be more optimistic with respect to the (already intrinsically appealing [473]) hypothesis of a single stage of unification of all forces, possibly even at distance scales as “large” as (10^{26} eV)^{−1} ≃ 10^{−33} m. And I find that, in relation to this issue, the recent (mini)burst of interest in the role of gravity in unification is particularly exciting. A convincing case is being built concerning the possibility that gravity might affect the running of the StandardModel coupling constants, and this too could have significant effects for the estimate of the unification scale (see, e.g., Refs. [473, 529] and references therein). And in turn there is a rather robust argument (see, e.g., Refs. [146, 147] and references therein) suggesting that the other fields might significantly affect the strength of gravity.
My personal perspective on the overall balance of this limited insight that is available to us is summarized by the attitude I adopted for this review in relation to the expectations for the value of the quantumspacetime scale. Unsurprisingly, I give top priority for this to the only (and however faint) indication we have from experiments: the values measured for coupling constants at presently accessible “ultralarge” distance scales appear to be arranged in such a way as to produce a unification of nongravitational forces at a much smaller length scale, which happens to be not distant from where we would naively expect gravity to come into the picture. This in some sense tells us that our naive estimate of where gravity becomes “strong” (and spacetime turns nonclassical) cannot be too far off the mark. But at the same time imposes upon us at least a certain level of prudence: we cannot assume that the quantumspacetime scale is exactly the Planck length, but we have some encouragement for assuming that it is within a few orders of magnitude of the Planck length.
In closing this long aside on the quantumgravity/quantumspacetime scale, let me stress that even prudently assuming a few orders of uncertainty above and below the Planck length is not necessarily safe. It is in my opinion the most natural working assumption in light of the information presently available to us, but we should be fully aware of the fact that our naive estimates might be off by more than a few orders of magnitude. Following the line of reasoning adopted here this would take the shape of a solution for \({\ell _{{\rm{QST}}}} \sim \sqrt {{G_N}({\ell _{{\rm{QST}}}})}\) that unexpectedly turned out to be wildly different form the Planck length. The outlook of the analysis of the unification of forces appears to discourage such speculations, but we must be open to the possibility that the story here summarized in Figure 1 might just be a cruel numerical accident (more on this toward the end of this review, when I briefly consider the “large extra dimensions” scenario).
1.7 Characteristics of the experiments
Having commented on the first “ingredient” for the search of experiments relevant for quantum spacetime and quantum gravity, which is the estimate of the characteristic scale of this new physics, let me next comment on a few other ingredients, starting with some intuition for the type of quantumspacetime effects that one might plausibly look for, and what that requires.
As stressed earlier in this section, we cannot place much hope of experimental breakthroughs in the full quantumblackhole regime. Our best chances are for studies of contexts amenable to a description in terms of the properties of particles in a background quantum spacetime. And, as also already stressed, these effects will be minute, with magnitude governed by some power of the ratio between the Planck length and the wavelength of the particles involved.
The presence of these suppression factors on the one hand reduces sharply our chances of actually discovering quantumspacetime effects, but on the other hand simplifies the problem of figuring out what are the most promising experimental contexts, since these experimental contexts must enjoy very special properties that would not easily go unnoticed. For laboratory experiments, even an optimistic estimate of these suppression factors leads to a suppression of order 10^{−16}, which one obtains by assuming (probably already using some optimism) that at least some quantumgravity effects are only linearly suppressed by the Planck length and taking as particle wavelength the shorter wavelengths we are able to produce (∼ 10^{−19} m). In astrophysics (which, however, limits one to “observations” rather than “experiments”) particles of shorter wavelength are being studied, but even for the highest energy cosmic rays, with energy of ∼ 10^{20} eV and, therefore, wavelengths of ∼ 10^{−27} m, a suppression of the type L_{ p }/λ would take values of order 10^{−8}. It is mostly as a result of this type of consideration that traditional quantumgravity reviews considered the possibility of experimental studies with unmitigated pessimism. However, the presence of these large suppression factors surely cannot suffice for drawing any conclusions. Even just looking within the subject of particle physics we know that certain types of small effects can be studied, as illustrated by the example of the remarkable limits obtained on proton instability. The prediction of proton decay within certain grand unified theories of particle physics is really a small effect, suppressed by the fourth power of the ratio between the mass of the proton and grandunification scale, which is only three orders of magnitude smaller than the Planck scale. In spite of this horrifying suppression, of order [m_{proton}/E_{GUT}]^{4} ∼ 10^{−64}, with a simple idea we have managed to acquire full sensitivity to the new effect: the proton lifetime predicted by grand unified theories is of order 10^{39} s and quite a few generations of physicists should invest their entire lifetimes staring at a single proton before its decay, but by managing to keep under observation a large number of protons (think for example of a situation in which 10^{33} protons are monitored) our sensitivity to proton decay is dramatically increased. In that context the number of protons is the (ordinaryphysics) dimensionless quantity that works as “amplifier” of the newphysics effect.
Outside of particle physics more success stories of this type are easily found: think for example of the Brownianmotion studies conducted a century ago. Within the 1905 Einstein description one uses Brownianmotion measurements on macroscopic scales as evidence for the atomic structure of matter. For the Brownianmotion case the needed amplifier is provided by the fact that a very large number of microscopic processes intervenes in each single macroscopic effect that is being measured.
It is hard but clearly not impossible to find experimental contexts in which there is effectively a large amplification of some small effects of interest. And this is the strategy that is adopted [52] in the attempts to gain access to the Planckscale realm.
1.8 Paradigm change and test theories of not everything
Something else that characterizes the work attitude of the community, whose results I am here reviewing, is the expectation that the solution of the quantumgravity problem will require a significant change of theory paradigm. Members of this community find in the structure of the quantumgravity problem sufficient elements for expecting that the transition from our current theories to a successful theory of quantum gravity should be no less (probably more) significant then the transition from classical mechanics to quantum mechanics, the prototypical example of a change of theory paradigm.
This marks a strong difference in intuition and methodology with respect to other areas of quantumgravity research, which do not assume the need of a paradigm change. If the string theory program turned out to be successful then quantum gravity should take the shape of just one more (particularly complex but nonetheless consequential) step in the exploitation of the current theory paradigm, the one that took us all the way from QED to the Standard Model of particle physics.
This difference of intuitions even affects the nature of the sort of questions the different communities ask. The expectation of those not preparing for a change of theory paradigm is that one day some brilliant mind will wake up with the correct full quantumgravity theory, with a single big conceptual jump. What is expected is a single big conceptual step leading to a theory that describes potentially everything we know so far.^{8} Something of the sort of the discovery of QCD: a full theory even though some of its answers to our questions are not immediately manifest once the theory is written out (see, e.g., confinement).
The expectation of those who are instead preparing for a change of theory paradigm is that we will get to a mature formulation of quantum gravity only at the end of a multistep journey, with each step being of rather humble nature. The model here of is the phase of the “old quantum theory”. The change of theory paradigm in going from classical mechanics to quantum mechanics was of such magnitude that we could not possibly get it right in one single jump. Imagine someone, however brilliant, looking at blackbody radiation and proposing a solution based on observables described as selfadjoint operators on Hilbert spaces and all that. Planck’s description of blackbody radiation was very far from being a full formalization of quantum mechanics, and was even internally unsatisfactory, with a very limited class of contexts and regimes where it could be applied. It was a theory of very few things, but it was a necessary step toward quantum mechanics. A similar role in the gradual emergence of quantum mechanics was played by other theories of limited scope, such as Einstein’s description of the photoelectric effect, Bohr’s description of atoms, and the successful proposal by de Broglie that waveparticle duality should be applied also to matter.
So, while those not preparing for a change of paradigm look for theories of everything, we are looking for theories of very few things, like Planck, Einstein, Bohr, de Broglie and other great contributors to the ultimate advent of quantum mechanics. Let me here add that even when exploiting a successful theory paradigm, often the next level of exploitation still requires us taking some clumsy steps based on theories of few things. Consider Fermi’s description of weak interactions in terms of fourfermionvertex processes. Fermi’s theory can be applied to a limited class of phenomena and only in a relatively narrow regime, and it is even a theory that is not satisfactory from the perspective of internal logical consistency. Yet Fermi’s theory was an important and necessary step toward richer and more satisfactory descriptions of weak interactions.
The difference in methodologies is also connected with some practical considerations, connected with the fact that the formalisms presently being considered as solutions for the quantumgravity problem are so complex that very little is understood of their truly physical implications. Some theories of few things can even be inspired by a given theory of everything: since it is de facto impossible to compare to data present full candidates for quantum gravity one ends up comparing to data the predictions of an associated “test theory”, a model that is inspired by some features we do understand (usually not more than qualitatively or semiquantitatively) of the original theory, but casts them within a simple framework that is well suited for comparison to experiments (but for which there is no actual guarantee of full compatibility with the original theory).
So, in the eyes of some workers these test theories of few things are needed to bridge the gap between the experimental data and our present understanding of the relevant formalisms. In the eyes of others the test theories of few things are just attempts to bridge the gap between the experimental data available to us and our limited understanding of the quantumgravity problem.
Essentially in working in quantumspacetime phenomenology one must first develop some intuition for some candidate quantumspacetime effects. And this can come either from analyzing the structure of the formalisms that are being considered in the search of a solution to the quantumgravity problem or from analyzing the structure of the quantumgravity problem. Once a class of effects is deemed of interest some test theories of these candidate effects must be developed so that they can be used as guidance for experimental searches.
From the perspective of a phenomenologist, some carefully tailored test theories can also be valuable as some sort of common language to be used in assessing the progresses made in improving the sensitivity of experiments, a language that must be suitable both for experimentalists and for those working on the development of quantumgravity theories.
The possibility to contemplate such “quantumgravity theories of not everything” is facilitated by the fact that the “quantumgravity problem” can be described in terms of several “subproblems”, each challenging us perhaps as much as some full open problems of other areas of physics. To mention just a few of these “subproblems” let me notice that: (i) it appears likely that the solution of this problem requires a nonclassical description of spacetime geometry, (ii) quantum gravity might have to be profoundly different (from an “informationtheory perspective”) from previous fundamentalphysics theories, as suggested by certain analyses of the evolution of pure states in a blackhole background, (iii) the perturbative expansions that are often needed for the analysis of experimental data might require the development of new techniques, since it appears that the ones that rely on perturbative renormalizability might be unavailable, and (iv) we must find some way to reconcile generalrelativistic background independence with the apparent need of quantum mechanics to be formulated in a given background spacetime.
For each of these aspects of the quantumgravity problem we can, in principle, attempt to devise formalisms, intended as descriptions of those regimes of the quantumgravity realm that are dominantly characterized by the corresponding features.
1.9 Sensitivities rather than limits
In providing my description of the present status of quantumspacetime phenomenology, I shall adopt as my “default mode” that of characterizing the sensitivities that are within reach for certain classes of experiments/observations, with only a few cases where I discuss both sensitivities and available experimental limits. The analysis of sensitivities was the traditional exercise a decade ago, in the early days of modern quantumspacetime phenomenology, since the key objective then was to establish that sensitivity to effects introduced genuinely at the Planck scale is achievable. In light of the observation I already reported in Section 1.5 (and several other observations reported later in this review), the “case for existence” of quantumspacetime phenomenology is at this point well settled.
We are now entering a more mature phase in which we start having the first examples of candidate quantumspacetime effects for which the development of suitable test theories is approaching a level of maturity such that placing experimental bounds (“limits”) on the parameters of these test theories does deserve intrinsic interest. However, at the time of writing, the transition “from sensitivities to limits” is not yet complete. The cases where I will offer comments on available experimental limits are cases for which (in my opinion) this transition has been made satisfactorily. But in several areas of quantumspacetime phenomenology it is still common practice to discuss experimental bounds on the basis of a single littleunderstood experimental result (often a single observation in astrophysics) and most of the test theories are not yet developed to the point that we can attach much significance to placing limits on their parameters. This is a key issue, and throughout this review I will find opportunities to discuss in more detail my concerns and offer some remarks that are relevant for completing the needed transition “from sensitivities to limits”. I do plan to regularly update this review, and with each update readers should find the emphasis gradually going more and more from sensitivities to experimental limits.
1.10 Other limitations on the scope of this review
After having clarified that the “default mode” of this review provides descriptions of sensitivities (with occasional characterizations of experimental bounds), I should comment on the types of theory and phenomenology that are the main focus of this review. I have prepared other reviews on these and related topics [52, 62] with a broader perspective but much more limited depth. Here my main focus is to analyze and review in some detail the healthy interface between pure theory and phenomenology of quantum spacetime. I shall mostly describe the phenomenology proposals, but the selection of which proposals should be included is primarily based on their proven ability to motivate developments on the puretheory side and to react to (take into account adaptively of) the indications that then emerge from these puretheory studies. This will be the “default mode” of my selection of topics, with some exceptions allowed in cases where I find that there are promising opportunities for such a healthy interface to mature over the next few years.
The net result of these goals of the review produces a certain bias toward proposals for quantum spacetime, which originated from (or were inspired by) the study of LQG and/or the study of Planckscale spacetime noncommutativity. These are the two areas of puretheory research in which, so far, the desirable twoway interface has most concretely materialized: puretheory specialists have redirected part of their work toward the topics that phenomenologists have highlighted as most promising for phenomenology; and the work of quantumspacetime phenomenologists has been in turn influenced by the results then obtained on the puretheory side.
In addition to a relatively long list of proposals inspired by LQG and/or by Planckscale spacetime noncommutativity, I shall also comment on a few proposals inspired by other approaches to spacetime quantization (e.g., Causal Sets and Noncritical String Theory). From a broader quantumgravityproblem perspective one should also consider critical string theory, which actually remains the most studied candidate for quantum gravity. However, I focus here on quantumspacetime effects and effects whose natural characteristic scale is the Planck scale, whereas the phenomenology proposals so far inspired by the criticalstringtheory research program do not revolve around quantum properties of spacetime and often the characteristic scale of the effects is not naturally the Planck scale.
I shall observe in Section 2.1.1 that the analysis of critical string theory actually has provided encouragement for the idea that it could also be a model of spacetime quantization, but the relevant aspects of critical string theory are still poorly understood and have not produced phenomenological proposals of the sort I am here reviewing. I do believe that it is likely that in a notsodistant future some new opportunities for quantumspacetime phenomenology will arise from this avenue.
1.11 Schematic outline of this review
The main objective of the next Section 2 is to motivate a list of candidate quantumspacetime effects, on the basis of the structure of the quantumgravity problem and/or of results obtained in certain theories that are being considered as relevant to the understanding of the quantumgravity problem. The rest of this review attempts to describe the status of searches of these candidate quantumspacetime effects.
Choosing what structure to give to Sections 3, 4, 5 and 6 was the main challenge faced by my work on this review. The option that finally prevailed attempts to assign each phenomenological proposal to a certain area of quantumspacetime phenomenology. These should be viewed only as tentative assignments, or at least assignments based on a perception of what could be the primary targets of a given phenomenological proposal. And there are some visible limitations: some readers could legitimately argue that a certain subsection that I placed in one of the sections should instead find a more fitting setting in another section. Indeed, as I was working on this review, there were a few subsections that kept switching from one section to another. If used wisely, I feel that the structure I gave is still preferable to some of the alternatives that could have been considered. For example, even such a tentative structure of organization is probably going to be more easy to use than a long unstructured list of all the many phenomenological proposals I am considering. And the option of organizing phenomenological proposals on the basis of the theories that motivate them, rather than roughly on the basis of their primary area of relevance in phenomenology, would have been against the whole spirit of this review.
Section 3 focuses on effects that amount to Planckscale departures from Lorentz/Poincaré symmetry, which is the type of effects on which the most energetic quantumspacetime phenomenology effort has been so far directed. The content of Section 3 has some overlap with [395] that describes the status of modern tests of Lorentz symmetry, and, therefore, is in part also devoted to cases in which such tests are motivated by quantumspacetime research. However, my perspective will be rather different, focused on the quantumspacetimemotivated searches and also using the example of Lorentz/Poincarésymmetry tests to comment on the level of maturity reached by quantumspacetime phenomenology in relation to the falsification of (test) theories and to the discrimination between different but similar theories. And whereas from the broader viewpoint of probing the robustness of Lorentz symmetry one should consider as significant any proposal capable of improving the bounds established within a given parametrization of departures from Lorentz symmetry, I shall focus on the demands of Planckscale sensitivity, as required by the objectives of research on Planckscale quantization of spacetime, that is my main focus here.
In Section 4, I describe the status of other areas of quantumspacetime phenomenology in which the Planckscale also characterizes the onset of ultraviolet effects, but not of the types that require departures from Lorentz/Poincaré symmetry.
While the primary objectives of this review are the ultraviolet effects linked with the Planckscale structure of spacetime, in Section 5 I briefly consider the possibility of ultraviolet/infrared (UV/IR) mixing. In such UV/IRmixing scenarios the role of the Planck scale would be in governing the UV side, and possibly then combining with other scales when IR effects are considered.
Sections 3, 4, and 5 concern proposals of (only a few) controlled laboratory experiments and (several) observations in astrophysics. These are the contexts in which currently one finds more mature proposals, particularly concerning the robustness of claims of Planckscale sensitivity of some relevant data analyses. However, observations in cosmology should also provide some very valuable opportunities, and there are some “quantumspacetimecosmology” proposals, to which I devote Section 6, that can already be used to expose the great potential reach of this type of analyses.
While different proposals of quantumspacetime phenomenology often involve different formalizations and completely different experimental techniques, there is a common setup of all proposals described in Sections 3, 4, 5, and 6. This main strategy of quantumspacetime phenomenology is summarized in Section 7, also pondering what might be some of its limitations.
Section 8 offers some closing remarks.
2 QuantumGravity Theories, Quantum Spacetime, and Candidate Effects
Before getting to the main task of this review, which concerns phenomenology proposals, it is useful to summarize briefly the motivation for studying certain candidate quantumspacetime effects. The possible sources of motivation come either from analyses of the structure of the quantumgravity problem or from what is emerging in the development of some theories that have been proposed as candidate solutions of the quantumgravity problem. As already stressed, my main focus here is on effects that can be linked to spacetime quantization at (about) the Planck scale, and particularly the ones that were involved in the twoway interface that materialized over this last decade between phenomenologists and theorists working on the LQG approach and spacetime noncommutativity.
In the first part of this section, I offer a few comments on some of the approaches being pursued in the study of the quantumgravity problem, mostly focusing on whether or not they support a quantumspacetime picture and the role played by the Planck scale. This part focuses primarily on LQG and spacetime noncommutativity, but I also comment briefly on critical string theory and other approaches.
Then in the second part of this section I list some key candidates as phenomena that could characterize the quantumspacetime realm. This list is only very tentative but it seems to me we cannot do any better than this at the present time. Indeed, compiling a list of candidate quantumspacetime effects is not straightforward. Analogous situations in other areas of physics are usually such that there are a few new theories that have started to earn our trust by successfully describing some otherwise unexplained data, and then often we let those theories guide us toward new effects that should be looked for. The theories that are under consideration for the solution of the quantumgravity problem, and for a “quantum” (nonclassical) description of spacetime, cannot yet claim any success in the experimental realm. Moreover, even if nonetheless we wanted to use them as guidance for experiments, the complexity of these theories proves to be a formidable obstruction. In most cases, especially concerning testable predictions, the best we can presently do with these theories is analyze their general structure and use this as a source of intuition for the proposal of a few candidate effects. Similarly, when we motivate the search of certain quantumspacetime features on the basis of our present understanding of the quantumgravity problem we are in no way assured that they should still find support in future better insight on the nature of this problem, but it is the best we can do at the present time.
2.1 QuantumGravity Theories and Quantum Spacetime
2.1.1 Critical String Theory
The most studied approach to the quantumgravity problem is a version of string theory that adopts supersymmetry and works in a “critical” number of spacetime dimensions. If this mainstream perspective turned out to be correct it would be bad news for quantumspacetime phenomenologists, since the theory is formulated in classical Minkowski background spacetime. It would be bad news for phenomenology in general because (critical, supersymmetric) string theory is a particularly soft modification of current theories, and the new effects that can be accommodated by the theory are untestably small, if all the new features are indeed introduced (as traditionally assumed) at a string scale roughly given by the Planck scale.
String theory is the natural attempt from a particlephysics perspective, but other perspectives on the quantumgravity problem remain unimpressed, particularly considering that most results of string theory still only apply in a fixed background Minkowski spacetime. And it is interesting to notice how the most careful analyses performed even adopting a stringtheory perspective end up finding that the case for applicability to the quantumgravity problem is still rather weak (see, e.g., Ref. [257]).
This not withstanding there has been in recent years a more vigorous effort of development of a stringinspired phenomenology, with inspiration found in mechanisms that are, however, outside the traditional formulation of string theory. This stringinspired phenomenology does not involve spacetime quantization and often does not refer explicitly to the Planck scale, so I shall not discuss it in detail in this review (although there will be scattered opportunities, at points of this review, where it becomes indirectly relevant). The possibility that received the most attention in recent years is the one of “large” extra dimensions [80, 375, 552, 84, 85, 480]. The existence of extra dimensions can be conceived even outside string theory, but it is noteworthy that in string theory the criticality criterion actually requires extra dimensions. If the extra dimensions, as traditionally assumed, have finite size on the order of the Planck length, then one ends up having associated Planckscale effects for the lowenergy realm, where our experiments and observations take place. This would be a classic exercise for quantumgravity phenomenology but it appears that the Planckscale suppression of these extradimension effects is so strong that they really could not ever be seen/tested. The recent interest in the “large extra dimensions” scenario originates from the observation that dimensions of size much larger than the Planck length (but still microscopic), while not particularly natural from a stringtheory perspective, may well be allowed in string theory [80, 375, 552, 84, 85, 480]. And for some choices of number and sizes of extra dimensions a rich phenomenology is produced.
Most other phenomenological proposals inspired by string theory essentially make use of the fact that, at least as seen by a traditional particle physicist, string theory makes room for several new fields. The new effects are indeed of types that are naturally described by introducing new fields in a classical spacetime background, rather than quantumspacetime features, and the magnitude of these effects is not naturally governed by the Planck scale.^{9}
In spite of these profound differences there are some points of contact between the Planckscale quantumspacetime phenomenology, which I am here concerned with, and this string phenomenology. In a quantum spacetime it is necessary to reexamine the issue of spacetime symmetries, and certain specific scenarios for the fate of Lorentz symmetry come into focus. From a different perspective and in a technically different way one also finds reasons to scrutinize Lorentz symmetry in string phenomenology: it is plausible [347] that some stringtheory tensor fields (most likely some of the new fields introduced by the theory) could acquire a nonzero vacuum expectation value, in which case evidently one would have a “spontaneous breakdown” of Lorentz symmetry. I shall also comment on the possibility that spacetime quantization might affect the equivalence principle. Again, from a different perspective and in a technically different way, one also finds reasons to scrutinize the equivalence principle in string phenomenology. And again it is typically due to the extra fields introduced in string theory: most notably some scenarios involving the dilaton, a scalar partner to the graviton predicted by string theory, produce violations of the equivalence principle (see, e.g., Ref. [193]).
I should stress here, because of the scope of this review, that the idea of a quantum spacetime is not completely foreign to string theory. It is presently appearing at an undigested and/or indirect level of analysis, but it is plausible that future evolutions of the stringtheory program might have a primitive/fundamental role for spacetime quantization. So far the most studied connection with quantumspacetime ideas comes from a mechanism analogous to the emergence of noncommutativity of position coordinates in the Landau model (see, e.g., Ref. [101]) that is found to be applicable to the description of strings in the presence of a constant NeveuSchwarz twoform (“B_{ μν }”) field [213, 516]. It should be stressed that these cases of “emerging noncommutativity” (effective descriptions applicable only in certain specific regimes) do not amount to genuine nonclassicality of spacetime. Still, these recent stringtheory results do create a point of contact between research (and particularly phenomenology) on fundamental spacetime noncommutativity and string theory, with the peculiarity that from the stringtheory perspective one would not necessarily focus (and typically there is no focus) on the case of noncommutativity introduced at about the Planck scale, since it is instead given in terms of the free specification of the field B_{ μν }.
For the hope of a possible future reformulation of string theory in some way that would accommodate a primitive role for spacetime nonclassicality my impression is that the key opportunities should be seen in results suggesting that there are fundamental limitations for the localization of a spacetime event in string theory [532, 269, 44, 332]. The significance of these results on limitations of localizability in string theory probably has not been appreciated sufficiently. Only a few authors have emphasized the possible significance of these results [551], but I would argue that finding such limitations in a theory originally formulated in a classical spacetime background may well provide the starting point for reformulating the theory completely, perhaps codifying spacetime quantization at a primitive level.
2.1.2 Loop Quantum Gravity
The most studied theory framework providing a quantum description of spacetime is LQG [476, 96, 502, 524, 93]. The intuition of many phenomenologists who have looked at (or actually worked on) LQG is that this theory should predict quite a few testable effects, some of which may well be testable with existing technologies. However, the complexity of the formalism has proven so far to be unmanageable from the point of view of obtaining crisp physical predictions. Among the many challenges I should at least mention the much debated “classicallimit problem”, which obstructs the way toward a definite set of predictions for the quasiMinkowski (or quasideSitter, or quasiFRW) regime, which is where most of the opportunities for phenomenology can be found.
However, one may attempt to infer from the general structure of the theory motivation for the study of some candidate LQG effects. And, as I shall stress in several parts of this review, this type of attitude has generated a healthy interface between phenomenologists and LQG theorists. Most of the relevant proposals are ignited indeed by the quantum properties of spacetime in LQG, which appear to be primarily codified in a discretization of the area and volume observables [477, 95, 476] In particular, several studies (see later in this review) have argued that the type of discretization of spacetime observables usually attributed to LQG could be responsible^{10} for Planckscale departures from Lorentz symmetry.
In addition to a large effort focused on the fate of Lorentz symmetry, there has also been a rather large effort focused on earlyUniverse cosmology inspired by LQG. Among the appealing features of this cosmology work I should at least mention “singularity avoidance”. For the LQG approach, there might be no alternative to avoiding the bigbang singularity, since indeed, at least as presently understood, LQG describes spacetime has a fundamentally discrete structure governed by difference (rather than differential) equations. This discreteness is expected to become a dominant characteristic of the framework for processes involving comparably small (Planckian) length scales, and in particular it should inevitably give rise to a totally unconventional picture of the earliest stages of evolution of the Universe. Attempts at developing a setup for a quantitative description of these earlyUniverse features have been put forward in Refs. [125, 94, 126, 92] and references therein, but one must inevitably resort to rather drastic approximations, since a full LQG analysis is not possible at present.
For other areas of phenomenology discussed in this review the influence of LQG has been less direct, but it appears safe to assume that it will inevitably grow in the coming years. To give a particularly striking example, let me mention the many proposals here discussed that concern spacetime fuzziness. It is evident that LQG gives a fuzzy picture of spacetime (in the sense discussed more precisely in later parts of this review), and it would be of important guidance for the phenomenologists to have definite predictions for these features. Even just a semiheuristic derivation of such effects is beyond the reach of our present understanding of LQG, but it will come.
2.1.3 Approaches based on spacetime noncommutativity
The idea of having a nonclassical fundamental description of spacetime is central to the study of spacetime noncommutativity. The formalization that is most applied in the study of the quantumgravity/quantumspacetime problem is mainly based on the formalism of “quantumgroups” and essentially assumes that the quantum properties of spacetime should be at least to some extent analogous to the quantum properties of phase space in ordinary quantum mechanics. Ordinary quantum mechanics introduces some limitations for procedures intending to obtain a combined determination of both position and momentum, and this is formalized in terms of noncommutativity of the position and momentum observables. With spacetime noncommutativity one essentially assumes that spacetime coordinates should not commute [211, 391, 374, 384, 70, 98] among themselves, producing some limitations for the combined determination of more than one coordinate of a spacetime point/event. This has been the formalization of spacetime noncommutativity for which the twoway interface between theory and phenomenology, which is at center stage in this review, has been most significant.
Looking ahead at the future of quantumspacetime phenomenology, it appears legitimate to hope that another, perhaps even more compelling, candidate concept of noncommutative geometry, the one championed by Connes [185, 184], may provide guidance. At present the most studied applications of this notion of noncommutative geometry are focused on giving a fully geometric description of the standard model of particle physics, with the noncommutativity of geometry used to codify known properties of particle physics in geometric fashion, while keeping spacetime as a classical geometry.
Going back to the quantumgroupbased description of spacetime noncommutativity I should stress that, so far, the most significant developments have concerned attempts to describe the Minkowski limit of the quantumgravity problem, i.e., a noncommutative version of Minkowski spacetime (spacetimes that reproduce classical Minkowski spacetime in the limit in which the noncommutativity parameters are taken to 0). Some related work has also been directed toward quantum versions of de Sitter spacetime, but very little about spacetime dynamics and only at barely an exploratory level. This should change in the future. But at the present time this situation could be described by stating that most work on spacetime noncommutatvity is considering only one half of the quantumgravity problem, the quantumspacetime aspects (neglecting the gravity aspects). Because of the double role of the gravitational field, which in some ways is just like another (e.g., electromagnatic) field given in spacetime but it is also the field that describes the structure of spacetime, in quantumgravity research the idea that this classical field be replaced by a nonclassical one ends up amounting to two concepts: some sort of quantization of gravitational interactions (which might be mediated by a graviton) and some sort of quantization of spacetime structure. At present one might say that only within the LQG approach are we truly exploring both aspects of the problem. String theory, as long as it is formulated in a classical (background) spacetime, focuses in a sense on the quantization of the gravitational interaction, and sets aside (or will address in the future) the possible “quantization” of spacetime [551]. Spacetime noncommutativity is an avenue for exploring the implications of the other side, the quantization of spacetime geometry.
The description of (Minkowskilimit) spacetime in terms of (quantumgroupbased) spacetime noncommutativity has proven particularly valuable in providing intuition for the fate of (Minkowskilimit/Poincaré) spacetime symmetries at the Planck scale. Also parity transformations appear to be affected by at least some schemes of spacetime noncommutativity and this in turn provides motivation for testing CPT symmetry.
Unfortunately, spacetime fuzziness, which is the primary intuition that leads most researchers to noncommutativity, frustratingly remains only vaguely characterized in current research on noncommutative spacetimes; certainly not characterized with the sharpness needed for phenomenology.
2.1.4 Other proposals
I shall not attempt to review the overall status of quantumgravity research. The challenge of reviewing and offering a perspective on quantumspacetime phenomenology is already overwhelming. And according to the perspective of this phenomenological approach the central challenge of quantumgravity research is to find the first experimental manifestations of the quantumgravity realm. The different formalisms proposed for the study of the quantumgravity problem can be very valuable for this objective, but only in as much as they provide intuition for the type of new effects that might characterize the quantumgravity realm. In practice, at least for the next few decades, what will be compared to data will be simple test theories inspired by our understanding of the quantumgravity problem or by the intuition obtained in the study of formal theories of quantum gravity. The possibility of comparing a full quantumgravity theory directly to experiments appears to be for a still distant future, as a result of the complexity of these theories (which prevents us from deriving testable predictions).
I have invested a few pages on string theory, LQG and spacetime noncommutativity for different reasons. Providing some reasonably detailed comments on string theory was encouraged, in spite of the lack of a fundamental role for spacetime quantization, by its prominent role in the quantumgravity literature. And, as stressed above, LQG and spacetime noncommutativity are particularly relevant for this review because the scenarios of spacetime quantization these approaches consider/derive have been a particularly influential source of intuition for proposals in quantumspacetime phenomenology. Moreover, it is within the LQG and spacetimenoncommutativity communities that we have, so far, witnessed the most significant examples of the healthy twoway crossinfluence between formal theory and phenomenology.
I shall not offer comparably detailed comments on any other quantumgravity formalism, but there are a few that I should mention because of the significance of their role in quantumspacetime phenomenology. First of all let me mention the noncritical “Liouville string theory” approach championed by Ellis, Mavromatos and Nanopoulos [221, 223, 65, 399]. This is a variant of the stringtheory approach that (unlike the mainstream criticalstringtheory approach) adopts the choice of working in “noncritical” number of spacetime dimensions, and describes time in a novel way. As will be evident in several points of this review, Ellis, Mavromatos, Nanopoulos and collaborators have developed noncritical Liouville string theory from a perspective that admirably keeps phenomenology always at center stage, and this has been a key influence on several quantumspacetimephenomenology research lines.
Another approach for which there is by now a rather sizable research program aimed at phenomenological consequences is the one based on “discrete causal sets” [131, 470]. This is an approach of spacetime discretization that exploits the fact that a Lorentzian metric determines both a geometry and a causal structure and also determines the metric up to a conformal factor. One can then take the causal structure as primary, and start with a finite set of points with a causal ordering, recovering the conformal factor by counting points. Several opportunities for phenomenology are then produced by the discretization of spacetime.
Still, on the subject of approaches in which a role is played by spacetime discretization I should also bring to the attention of my readers the recent developments in the study of causal dynamical triangulations [45, 371, 46, 47, 372, 49]. Through causal dynamical triangulations one gives an explicit, nonperturbative and backgroundindependent, realization of the formal gravitational path integral on a given differential manifold. And some of the results obtained within this approach already provide elements of valuable intuition for quantumspacetime phenomenology, as exemplified by the results providing [48] first evidence for a scaledependent spectral dimension of spacetime, varying from four at large scales to two at scales on the order of the Planck length. These “running spectral dimensions” could have very significant applications in phenomenology, and early signs that this might indeed be the case can be found in the debate reported in Refs. [424, 505, 425] concerning the implication for primordial gravity waves.
Also particularly important for quantumspacetime phenomenology is the program of asymptoticallysafe quantum gravity. This is an attempt at the nonperturbative construction of a predictive quantum field theory of the metric tensor centered on the availability of a nonGaussian renormalizationgroup fixed point [544, 466, 212]. There are a few perspectives from which this asymptoticsafety program is influencing part of the research on quantumspacetime phenomenology. As an example of phenomenology work that was directly inspired by asymptotic safety, I should mention the expectation that quantumgravity effects might also be important in a largedistance regime [469], with possible relevance for phenomenology. I shall comment on this later in this review, also in relation to the idea of “UV/IR mixing” as a possibility that appears to be plausible even within other perspectives on quantum gravity and quantum spacetime. And there are significant indications (see, e.g., Ref. [468]) that ultimately the description of spacetime in a quantum gravity with asymptotic safety will be a quantumspacetime description. Also significant for quantumspacetime phenomenology is the whole idea of running gravitational couplings, which is central to asymptotic safety. As mentioned we tentatively assume that quantumspacetime effects originate at the Planck scale, but the Planck scale is computed in terms of (the IR value of) Newton’s constant and might give us a misleading intuition for the characteristic scales of spacetime quantization.
There are also some perspectives on the quantumgravity problem that at present I do not see as direct opportunities for quantumspacetime phenomenology, but certainly are playing the role of “intuition builders” for the phenomenologists, affecting the perception of the quantumgravity problem that guides some of the relevant research. Among these I should mention the rather large literature on the “emergent gravity paradigm” (see, e.g., Refs. [103, 538, 443, 513, 555, 499, 297]). This literature actually contains a variety of possible way through which gravity could be described not as a fundamental aspect of the laws of nature, but rather as an emergent feature. A simple analogy here is with pionmediated strong interactions, which emerge from the quantum chromodynamics of quarks and gluons at low energies.
And I should mention as another potential “intuition builder” for the phenomenologists a class of studies that in various ways place dissipation in connection with aspects of the quantumgravity problem (see, e.g., Refs. [518, 296]).
2.2 Candidate effects
From the viewpoint of phenomenologists, the theory proposals I briefly considered in Section 2.1.4 (all still lacking any experimental success) can only serve the purpose of inspiring some test theories suitable for comparison to data.
In this Section, I will briefly motivate a partial list of possible classes of effects that could characterize the quantumgravity/quantumspacetime realm. And indeed in compiling such a list, one ends up using both intuition based on the general structure of the quantumgravity problem and intuition based on what has been so far understood of theories that predict or assume spacetime quantization.
Both the analysis of the general structure of the quantumgravity problem and the analysis of proposed approaches to the solution of the quantumgravity problem provide a rather broad collection of intuitions for what might be the correct “quantization” of spacetime (see, e.g., Refs. [406, 532, 269, 44, 332, 442, 211, 20, 432, 50, 249, 489]), and in turn this variety of scenarios produces a rather broad collection of hypothesis concerning possible experimental manifestations of spacetime quantization.
2.2.1 Planckscale departures from classicalspacetime symmetries
From a quantumspacetime perspective it is natural to expect that some opportunities for phenomenology might come from tests of spacetime symmetries. It is relatively easy to test spacetime symmetries very sensitively, and it is natural to expect that introducing new (“quantum”) features in spacetime structure would affect the symmetries.
Let us consider in particular the Minkowski limit, the one described by the classical Minkowski spacetime in current theories: there is a duality onetoone relation between the classical Minkowski spacetime and the classical (Lie) algebra of Poincaré symmetry. Poincaré transformations are smooth arbitrarymagnitude classical transformations and it is, therefore, natural to subject them to scrutiny^{11} if the classical Minkowski spacetime is replaced by a quantized/discretized version.
The most active quantumspacetimephenomenology research area is indeed the one considering possible Planckscale departures from Poincaré/Lorentz symmetries. One possibility that has been considered in detail is the one of some symmetrybreaking mechanism affecting Poincaré/Lorentz symmetry. An alternative, which I advocated a few years ago [58, 55], is the one of a “spacetime quantization” that deforms but does not break some spacetime symmetries.
Besides the analysis of the general structure of the quantumgravity problem, encouragement for these Poincaré/Lorentzsymmetry studies is also found within some of the most popular proposals for spacetime quantization. As mentioned, according to the present understanding of LQG, the fundamental description of spacetime involves some intrinsic discretization [476, 502], and, although very little of robust is presently known about the Minkowski limit of the theory, several indirect arguments suggest that this discretization should induce departures from classical Poincaré symmetry. While most of the LQG literature on the fate of Poincaré symmetries argues for symmetry violation (see, e.g., Refs. [247, 33]), there are some candidate mechanisms (see, e.g., Refs. [75, 237, 503]) that appear to provide opportunities for a deformation of symmetries in LQG.
2.2.2 Planckscale departures from CPT symmetry
Arguments suggesting that CPT violation might arise in the quantumgravity realm have a long tradition [279, 445, 540, 446, 42, 222, 298, 345, 117] (and also see, e.g., the more recent Refs. [21, 423, 330]). And, in light of the scope of this review, I should stress that specifically the idea of spacetime quantization invites one to place CPT symmetry under scrutiny. Indeed, locality (in addition to unitarity and Lorentz invariance) is a crucial ingredient for ensuring CPT invariance, and a common feature of all the proposals for spacetime quantization is the presence of limitations to locality, at least intended as limitations to the localizability of a spacetime event.
Unfortunately, a proper analysis of CPT symmetry requires a level of understanding of the formalism that is often beyond our present reach in the study of formalizations of the concept of quantum spacetime. In LQG one should have a good control of the Minkowski (classical) limit, and of the description of charged particles in that limit, and this is still beyond what can presently be done within LQG.
Similar remarks apply to spacetime noncommutativity, although in that case some indirect arguments relevant for CPT symmetry can be meaningfully structured. For example, in Ref. [70] it is observed that certain spacetime noncommutativity scenarios appear to require a deformation of P (parity) transformations, which would result in a corresponding deformation of CPT transformations.
In the mentioned quantumspacetime picture based on noncritical Liouville string theory [221, 224], evidence of violations of CPT symmetry has been reported [220], and later in this review I shall comment on the exciting phenomenology that was inspired by these results.
2.2.3 Decoherence and modifications of the Heisenberg principle
It is well established that the availability of a classical spacetime background has been instrumental to the successful tests of quantum mechanics so far performed. The applicability of quantum mechanics to a broader class of contexts remains an open experimental question. If indeed spacetime is quantized there might be some associated departures from quantum mechanics. And this quantumspacetime intuition fits well with a rather popular intuition for the broader context of quantumgravity research, as discussed for example in Refs. [280, 361].
Some of the test theories used to model spacetime quantization have been found to provide motivation for departures from quantum mechanics in the form of “decoherence”, loss of quantum coherence [432, 50, 246]. A description of decoherence has been inspired by the mentioned noncritical Liouville string theory [221, 224], and is essentially the core feature of the formalism advocated by Percival and collaborators [452, 453, 454].
The possibility of modifications of the Heisenberg principle and of the de Broglie relation has also been much studied in accordance with the intuition that some aspects of quantum mechanics might need to be adapted to spacetime quantization. Although the details of the mechanism that produces such modifications vary significantly from one picture of spacetime quantization to another [322, 22, 122], one can develop an intuition of rather general applicability by noticing that the form of the de Broglie relation in ordinary quantum mechanics reflects the properties of the classical geometry of spacetime that is there assumed. More precisely, the de Broglie relation reflects the properties of the differential calculus on the spacetime manifold, since ordinary quantum mechanics describes the momentum observable in terms of a derivative operator (assuming the Heisenberg principle holds), which, acting on wave functions with wavelength λ, leads to the de Broglie relation p = h/λ. In a nonclassical (“quantum”) spacetime one must adopt new forms of differential calculus [500, 390], and as a result the description of the momentum observable and its relation to the wavelength of a wave must be reformulated [322, 22, 122, 63].
While the possibility of spacetime quantization provides a particularly direct logical line toward modifications of laws of quantum mechanics, one should consider such modifications as natural for the whole quantumgravity problem (even when studied without assuming spacetime quantization). For example, in string theory, assuming the availability of a classical spacetime background, one finds some evidence of modification of the Heisenberg principle (the “Generalized Uncertainty Principle” discussed, e.g., in Refs. [532, 269, 44, 332, 551]).
2.2.4 Distance fuzziness and spacetime foam
A description that is often used to give some intuition for the effects induced by spacetime quantization is Wheeler’s “spacetime foam”, even though it does not amount to an operative definition. Most authors see it as motivation to look for formalizations of spacetime in which the distance between two events cannot be sharply determined, and the metric is correspondingly fuzzy. As I shall discuss in Section 4, a few attempts to operatively characterize the concept of spacetime foam and to introduce corresponding test theories have been recently developed. And a rather rich phenomenology is maturing from these proposals, often centered both on spacetime fuzziness per se and associated decoherence.
Unfortunately, very little guidance can be obtained from the most studied quantumspacetime pictures. In LQG this type of experimentally tangible characterization of spacetime foam is not presently available. And remarkably even with spacetime noncommutativity, an idea that was mainly motivated by the spacetimefoam intuition of a nonclassical spacetime, we are presently unable to describe, for example, the fuzziness that would intervene in operating an interferometer with the type of crisp physical characterization needed for phenomenology.
2.2.5 Planckscale departures from the equivalence principle
The possibility of violations of the equivalence principle has not been extensively studied from a quantumspacetime perspective, in spite of the fact that spacetime quantization does provide some motivation for placing under scrutiny at least some implications of the equivalence principle. This is at least suggested by the observation that locality is a key ingredient of the present formulation of the equivalence principle: the equivalence principle ensures that (under appropriate conditions) two point particles would go on the same geodesic independent of their mass. But it is well established that this is not applicable to extended bodies, and presumably also not applicable to “delocalized point particles” (point particles whose position is affected by uncontrolled uncertainties). Presumably also the description of particles in a spacetime that is nonclassical (“quantized”), and, therefore, sets absolute limitations on the identification of a spacetime point, would require departures from some aspects of the equivalence principle.
Relatively few studies have been devoted to violations of the equivalence principle from a quantumspacetime perspective. Examples are the study reported in Ref. [149], which obtained violations of the equivalence principle from quantumspacetimeinduced decoherence, the study based on noncritical Liouville string theory reported in Ref. [227], and the study based on metric fluctuations reported in Ref. [263].
Also the broader quantumgravity literature (even without spacetime quantization) provides motivation for scrutinizing the equivalence principle. In particular, a strong phenomenology centered on violations of the equivalence principle was proposed in the stringtheoryinspired studies reported in Refs. [521, 195, 196, 194, 193, 192] and references therein, which actually provide a description of violations of the equivalence principle^{13} at a level that might soon be within our experimental reach.
Also relevant to this review is the possibility that violations of the equivalence principle might be a byproduct of violations of Lorentz symmetry. In particular, this is suggested by the analysis in Ref. [338], where the gravitational couplings of matter are studied in the presence of Lorentz violation.
3 QuantumSpacetime Phenomenology of UV Corrections to Lorentz Symmetry
The largest area of quantumspacetimephenomenology research concerns the fate of Lorentz (/Poincaré) symmetry at the Planck scale, focusing on the idea that the conjectured new effects might become manifest at low energies (the particle energies accessible to us, which are much below the Planck scale) in the form of “UV corrections”, correction terms with powers of energy in the numerator and powers of the Planck scale in the denominator.
Among the possible effects that might signal departures from Lorentz/Poincaré symmetry, the interest has been predominantly directed toward the study of the form of the energymomentum (dispersion) relation. This was due both to the (relative) robustness of associated theory results in quantumspacetime research and to the availability of very valuable opportunities of related data analyses. Indeed, as several examples in this section will show, over the last decade there were very significant improvements of the sensitivity of Lorentz and Poincarésymmetry tests.
Before discussing some actual phenomenologic al analyses, I find it appropriate to start this section with some preparatory work. This will include some comments on the “Minkowski limit of Quantum Gravity”, which I have already referred to but should be discussed a bit more carefully. And I shall also give a rather broad perspective on the quantumspacetime implications for the set up of test theories suitable for the study of the fate of Lorentz/Poincaré symmetry at the Planck scale.
3.1 Some relevant concepts
3.1.1 The Minkowski limit
In our current conceptual framework Poincaré symmetry emerges in situations that allow the adoption of a Minkowski metric throughout. These situations could be described as the “classical Minkowski limit”.
It is not inconceivable that quantum gravity might admit a limit in which one can assume throughout a (expectation value of the) metric of Minkowski type, but some Planckscale features of the fundamental description of spacetime (such as spacetime discreteness and/or spacetime noncommutativity) are still not completely negligible. This “nontrivial Minkowski limit” would be such that essentially the role of the Planck scale in the description of gravitational phenomena can be ignored (so that indeed one can make reference to a fixed Minkowski metric), but the possible role of the Planck scale in spacetime structure/kinematics is still significant. This intuition inspires the work on quantumMinkowski spacetimes, and the analysis of the symmetries of these quantum spacetimes.
It is not obvious that the correct quantum gravity should admit such a nontrivial Minkowski limit. With the little we presently know about the quantumgravity problem we must be open to the possibility that the Minkowski limit could actually be trivial, i.e., that whenever the role of the Planck scale in the description of gravitational phenomena can be neglected (and the metric is Minkowskian at least on average) one should also neglect the role of the Planck scale in spacetime structure. But the hypothesis of a nontrivial Minkowski limit is worth exploring: it is a plausible hypothesis and it would be extremely valuable for us if quantum gravity did admit such a limit, since it might open a wide range of opportunities for accessible experimental verification, as I shall stress in what follows.
When I mention a result on the theory side concerning the fate of Poincaré symmetry at the Planck scale clearly it must be the case that the authors have considered (or attempted to consider) the Minkowski limit of their preferred formalism.
3.1.2 Three perspectives on the fate of Lorentz symmetry at the Planck scale
It is fair to state that each quantumgravity research line can be connected with one of three perspectives on the problem: the particlephysics perspective, the GR perspective and the condensedmatter perspective.
From a particlephysics perspective it is natural to attempt to reproduce as much as possible the successes of the Standard Model of particle physics. One is tempted to see gravity simply as one more gauge interaction. From this particlephysics perspective a natural solution of the quantumgravity problem should have its core features described in terms of gravitonlike exchange in a background classical spacetime. Indeed this structure is found in string theory, the most developed among the quantumgravity approaches that originate from a particlephysics perspective.
The particlephysics perspective provides no a priori reasons to renounce Poincaré symmetry, since Minkowski classical spacetime is an admissible background spacetime, and in classical Minkowski there cannot be any a priori obstruction for classical Poincaré symmetry. Still, a breakdown of Lorentz symmetry, in the sense of spontaneous symmetry breaking, is possible, and this possibility has been studied extensively over the last few years, especially in string theory (see, e.g., Ref. [347, 213] and references therein).
Complementary to the particlephysics perspective is the GR perspective, whose core characteristic is the intuition that one should firmly reject the possibility of relying on a background spacetime [476, 502]. According to GR the evolution of particles and the structure of spacetime are selfconsistently connected: rather than specify a spacetime arena (a spacetime background) beforehand, the dynamical equations determine at once both the spacetime structure and the evolution of particles. Although less publicized, there is also growing awareness of the fact that, in addition to the concept of background independence, the development of GR relied heavily on the careful consideration of the inprinciple limitations that measurement procedures can encounter.^{14} In light of the various arguments suggesting that, whenever both quantum mechanics and GR are taken into account, there should be an inprinciple Planckscale limitation to the localization of a spacetime point (an event), the GR perspective invites one to renounce any direct reference to a classical spacetime [211, 20, 432, 50, 249]. Indeed, this requirement that spacetime be described as fundamentally nonclassical (“fundamentally quantum”), so that the measurability limitations be reflected by a corresponding measurabilitylimited formalization of spacetime, is another element of intuition that is guiding quantumgravity research from the GR perspective. This naturally leads one to consider discretized spacetimes, as in the LQG approach or noncommutative spacetimes.
Results obtained over the last few years indicate that this GR perspective naturally leads, through the emergence of spacetime discreteness and/or noncommutativity, to some departures from classical Poincaré symmetry. LQG and some other discretizedspacetime quantumgravity approaches appear to require a description of the familiar (classical, continuous) Poincaré symmetry as an approximate symmetry, with departures governed by the Planck scale. And in the study of noncommutative spacetimes some Planckscale departures from Poincaré symmetry appear to be inevitable.
The third possibility is a condensedmatter perspective on the quantumgravity problem (see, e.g., Refs. [537, 358, 166]), in which spacetime itself is seen as a sort of emerging criticalpoint entity. Condensedmatter theories are used to describe the degrees of freedom that are measured in the laboratory as collective excitations within a theoretical framework, whose primary description is given in terms of much different, and often practically inaccessible, fundamental degrees of freedom. Close to a critical point some symmetries arise for the collectiveexcitation theory, which do not carry the significance of fundamental symmetries, and are, in fact, lost as soon as the theory is probed away from the critical point. Notably, some familiar systems are known to exhibit specialrelativistic invariance in certain limits, even though, at a more fundamental level, they are described in terms of a nonrelativistic theory. So, from the condensedmatter perspective on the quantumgravity problem it is natural to see the familiar classical continuous Poincaré symmetry only as an approximate symmetry.
Further encouragement for the idea of an emerging spacetime (though not necessarily invoking the condensedmatter perspective) comes from the realization [304, 533, 444] that the Einstein equations can be viewed as an equation of state, so in some sense thermodynamics implies GR and the associated microscopic theory might not look much like gravity.
3.1.3 Aside on broken versus deformed spacetime symmetries
If the fate of Poincaré symmetry at the Planck scale is nontrivial, the simplest possibility is the one of broken Poincaré symmetry, in the same sense that other symmetries are broken in physics. As mentioned, an example of a suitable mechanism is provided by the possibility that a tensor field might have a vacuum expectation value [347].
An alternative possibility, that in recent years has attracted the interest of a growing number of researchers within the quantumspacetime and the quantumgravity communities, is the one of deformed (rather than broken) spacetime symmetries, in the sense of the “doublyspecialrelativity” (DSR) proposal I put forward a few years ago [58]. I have elsewhere [63] attempted to expose the compellingness of this possibility. Still, because of the purposes of this review, I must take into account that the development of phenomenologicallyviable DSR models is still in its infancy. In particular, several authors (see, e.g., Refs. [56, 493, 202, 292]) have highlighted the challenges for the description of spacetime and in particular spacetime locality that inevitably arise when contemplating a DSR scenario. I am confident that some of the most recent DSR studies, particularly those centered on the analysis of the “relative locality” [71, 504, 88, 67], contain the core ideas that in due time will allow us to fully establish a robust DSR picture of spacetime, but I nonetheless feel that we are still far from the possibility of developing a robust DSR phenomenology.
Interested readers have available a rather sizable DSR literature (see, e.g., Ref. [58, 55, 349, 140, 386, 387, 354, 388, 352, 353, 350, 26, 200, 493, 465, 291, 314, 366] and references therein), but for the purposes of this review I shall limit my consideration of DSR ideas on phenomenology to a single one of the (many) relevant issues, which is an observation that concerns the compatibility between modifications of the energymomentum dispersion relation and modifications of the law of conservation of energymomentum. My main task in this Section is to illustrate the differences (in relation to this compatibility issue) between the brokensymmetry hypothesis and the DSRdeformedsymmetry hypothesis.
The DSR scenario was proposed [58] as a sort of alternative perspective on the results on Planckscale departures from Lorentz symmetry that had been reported in numerous articles [66, 247, 327, 38, 73, 463, 33] between 1997 and 2000. These studies were advocating a Planckscale modification of the energymomentum dispersion relation, usually of the form \({E^2} = {p^2} + {m^2} + \eta L_p^n{p^2}{E^n} + O(L_p^{n + 1}{E^{n + 3}})\), on the basis of preliminary findings in the analysis of several formalisms in use for Planckscale physics. The complexity of the formalisms is such that very little else was known about their physical consequences, but the evidence of a modification of the dispersion relation was becoming robust. In all of the relevant papers it was assumed that such modifications of the dispersion relation would amount to a breakdown of Lorentz symmetry, with associated emergence of a preferred class of inertial observers (usually identified with the natural observer of the cosmic microwave background radiation).
However, it then turned out to be possible [58] to avoid this preferredframe expectation, following a line of analysis in many ways analogous to the one familiar from the developments that led to the emergence of special relativity (SR), now more than a century ago. In Galileian relativity there is no observerindependent scale, and in fact the energymomentum relation is written as E = p^{2}/(2m). As experimental evidence in favor of Maxwell’s equations started to grow, the fact that those equations involve a fundamental velocity scale appeared to require the introduction of a preferred class of inertial observers. But in the end we discovered that the situation was not demanding the introduction of a preferred frame, but rather a modification of the laws of transformation between inertial observers. Einstein’s SR introduced the first observerindependent relativistic scale (the velocity scale c), its dispersion relation takes the form E^{2} = c^{2}p^{2} + c^{4}m^{2} (in which c plays a crucial role in relation to dimensional analysis), and the presence of c in Maxwell’s equations is now understood as a manifestation of the necessity to deform the Galilei transformations.
It is plausible that we might be presently confronted with an analogous scenario. Research in quantum gravity is increasingly providing reasons for interest in Planckscale modifications of the dispersion relation, and, while it was customary to assume that this would amount to the introduction of a preferred class of inertial frames (a “quantumgravity ether”), the proper description of these new structures might require yet again a modification of the laws of transformation between inertial observers. The new transformation laws would have to be characterized by two scales (c and λ) rather than the single one (c) of ordinary SR.
This observation provides a general motivation for contemplating modifications of the law of energymomentum conservation in frameworks with modified dispersion relations. And I shall often test the potential impact on the phenomenology of introducing such modifications of the conservation of energymomentum by using as examples DSRinspired laws of the type (7), (8), (9), (10). I shall do this without necessarily advocating a DSR interpretation: knowing whether or not the outcome of tests of modifications of the dispersion relation depends on the possibility of also having a modification of the momentumconservation laws is of intrinsic interest, with or without the DSR intuition. But I must stress that when the relativistic symmetries are broken (rather than deformed in the DSR sense) there is no a priori reason to modify the law of energymomentum conservation, even when the dispersion relation is modified. Indeed most authors adopting modified dispersion relations within a brokensymmetry scenario keep the law of energymomentum conservation undeformed.
On the other hand the DSR research program has still not reached the maturity for providing a fully satisfactory interpretation of the nonlinearities in the conservation laws. For some time the main challenge came (in addition to the mentioned interpretational challenges connected with spacetime locality) from arguments suggesting that one might well replace a given nonlinear setup for a DSR model with one obtained by redefining nonlinearly the coordinatization of momentum space (see, e.g., Ref. [26]). When contemplating such changes of coordinatization of momentum space many interpretational challenges appeared to arise. In my opinion, also in this direction the recent DSR literature has made significant progress, by casting the nonlinearities for momentumspace properties in terms of geometric entities, such as the metric and the affine connection on momentum space (see, e.g., Ref. [67]). This novel geometric interpretation is offering several opportunities for addressing the interpretational challenges, but the process is still far from complete.
3.2 Preliminaries on test theories with modified dispersion relation
So far the main focus of Poincarésymmetry tests planned from a quantumspacetimephenomenology perspective has been on the form of the energymomentum dispersion relation. Indeed, certain analyses of formalisms provide encouragement for the possibility that the Minkowski limit of quantum gravity might indeed be characterized by modified dispersion relations. However, the complexity of the formalisms that motivate the study of Planckscale modifications of the dispersion relation is such that one has only partial information on the form of the correction terms and actually one does not even establish robustly the presence of modifications of the dispersion relation. Still, in some cases, most notably within some LQG studies and some studies of noncommutative spacetimes, the “theoretical evidence” in favor of modifications of the dispersion relations appears to be rather robust.
This is exactly the type of situation that I mentioned earlier in this review as part of a preliminary characterization of the peculiar type of test theories that must at present be used in quantumspacetime phenomenology. It is not possible to compare to data the predictions for departures from Poincaré symmetry of LQG and/or noncommutative geometry because these theories do not yet provide a sufficiently rich description of the structures needed for actually doing phenomenology with modified dispersion relations. What we can compare to data are some simple models inspired by the little we believe we understand of the relevant issues within the theories that provide motivation for this phenomenology.
And the development of such models requires a delicate balancing act. If we only provide them with the structures we do understand of the original theories they will be as sterile as the original theories. So, we must add some structure, make some assumptions, but do so with prudence, limiting as much as possible the risk of assuming properties that could turn out not to be verified once we understand the relevant formalisms better.
As this description should suggest, there has been a proliferation of models adopted by different authors, each reflecting a different intuition on what could or could not be assumed. Correspondingly, in order to make a serious overall assessment of the experimental limits so far established with quantumspacetime phenomenology of modified dispersion relations, one should consider a huge zoo of parameters. Even the parameters of the same parametrization of modifications of the dispersion relation when analyzed using different assumptions about other aspects of the model should really be treated as different/independent sets of parameters.
I shall be satisfied with considering some illustrative examples of models, chosen in such a way as to represent possibilities that are qualitatively very different, and representative of the breadth of possibilities that are under consideration. These examples of models will then be used in some relevant parts of this review as “language” for the description of the sensitivity to Planckscale effects that is within the reach of certain experimental analyses.
3.2.1 With or without standard quantum field theory?
Before describing actual test theories, I should at least discuss the most significant among the issues that must be considered in setting up any such test theory with modified dispersion relation. This concerns the choice of whether or not to assume that the test theory should be a standard lowenergy effective quantum field theory.
A significant portion of the quantumgravity and quantumspacetime community is rather skeptical of the results obtained using lowenergy effective field theory in analyses relevant to the Planckscale regime. One of the key reasons for this skepticism is the description given by effective field theory of the cosmological constant. The cosmological constant is the most significant experimental fact of evident gravitational relevance that could be within the reach of effective field theory. And current approaches to deriving the cosmological constant within effective field theory produce results, which are some 120 orders of magnitude greater than allowed by observations.^{15}
However, just like there are several researchers who are skeptical about any results obtained using lowenergy effective field theory in analyses relevant for the quantumgravity/quantumspacetime regime, there are also quite a few researchers who feel that it should be ok to assume a description in terms of effective field theory for all lowenergy (subPlanckian) manifestations of the quantumgravity/quantumspacetime regime.
Adopting a strict phenomenologist viewpoint, perhaps the most important observation is that for several of the effects discussed in this section on UV corrections to Lorentz symmetry, and for some of the effects discussed in later sections, studies based on effective quantum field theory can only be performed with a rather strongly “pragmatic” attitude. One would like to confine the new effects to unexplored highenergy regimes, by adjusting bare parameters accordingly, but, as I shall stress again later, quantum corrections produce [455, 182, 515, 190] effects that are nonetheless significant at accessible low energies, unless one allows for rather severe finetuning. On the other hand, we do not have enough clues concerning setups alternative to quantumfield theory that could be used. For example, as I discuss in detail later, some attempts are centered on densitymatrix formalisms that go beyond quantum mechanics, but those are (however legitimate) mere speculations at the present time. Nonetheless several of the phenomenologists involved, myself included, feel that in such a situation phenomenology cannot be stopped by the theory impasse, even at the risk of later discovering that the whole (or a sizable part of) the phenomenological effort was not on sound conceptual bases.
And the assumption of availability of an ordinary effective lowenergy quantumfieldtheory description has also been challenged by some perspectives on the LQG approach. For example, the arguments presented in Ref. [245] suggest that in several contexts in which one would naively expect a lowenergy field theory description LQG might instead require a densitymatrix description with features going beyond the reach of effective quantum field theory.
3.2.2 Other key features of test theories with modified dispersion relation
 (i)
is the modification of the dispersion relation “universal”? or should one instead allow different modification parameters for different particles?
 (ii)
in the presence of a modified dispersion relation between the energy E and the momentum p of a particle, should we still assume the validity of the relation υ = dE/dp between the speed of a particle and its dispersion relation?
 (iii)
in the presence of a modified dispersion relation, should we still assume the validity of the standard law of energymomentum conservation?
Unfortunately on these three key points, the quantumspacetime pictures that are providing motivation for the study of Planckscale modifications of the dispersion relation are not giving us much guidance yet.
For example, in LQG, while we do have some (however fragile and indirect) evidence that the dispersion relation should be modified, we do not yet have a clear indication concerning whether the law of energymomentum conservation should also be modified and we also cannot yet establish whether the relation υ = dE/dp should be preserved.
Similarly, in the analysis of noncommutative spacetimes we are close to establishing rather robustly the presence of modifications of the dispersion relation, but other aspects of the relevant theories have not yet been clarified. While most of the literature for canonical noncommutative spacetimes assumes [213, 397] that the law of energymomentum conservation should not be modified, most of the literature on κMinkowski spacetime argues in favor of a modification of the law of energymomentum conservation. There is also still no consensus on the relation between speed and dispersion, and particularly in the κMinkowski literature some departures from the υ = dE/dp relation are actively considered [336, 414, 199, 351]. And at least for canonical noncommutative spacetimes the possibility of a nonuniversal dispersion relation is considered extensively [213, 397].
Concerning the relation υ = dE/dp it may be useful to stress that it can be obtained assuming that a Hamiltonian description is still available, υ = dx/dt ∼ [x, H(p)], and that the Heisenberg uncertainty principle still holds exactly ([x,p] = 1 → x ∼ ∂/∂p). The possibility of modifications of the Hamiltonian description is an aspect of the debate on “Planckscale dynamics” that was in part discussed in Section 3.2.1. And concerning the Heisenberg uncertainty principle I have already mentioned some arguments that invite us to contemplate modifications.
3.2.3 A test theory for pure kinematics
With so many possible alternative ingredients to mix one can of produce a large variety of test theories. As mentioned, I intend to focus on some illustrative examples of test theories for my characterization of achievable experimental sensitivities.
My first example is a test theory of very limited scope, since it is conceived to only describe purekinematics effects. This will strongly restrict the class of experiments that can be analyzed in terms of this test theory, but the advantage is that the limits obtained on the parameters of this test theory will have rather wide applicability (they will apply to any quantumspacetime theory with that form of kinematics, independent of the description of dynamics).
Already in the first studies [66] that proposed a phenomenology based on (13) it was assumed that even at the Planck scale the familiar description of “group velocity”, obtained from the dispersion relation according to υ = dE/dp, would hold.
In the following, I will refer to this test theory as the “PKV0 test theory”, where “PK” reflects its “PureKinematics” nature, “V” reflects its “Lorentzsymmetry Violation” content, and “0” reflects the fact that it combines the dispersion relation (13) with what appears to be the most elementary set of assumptions concerning other key aspects of the physics: universality of the dispersion relation, υ = dE/dp, and the unmodified law of energymomentum conservation.
This rudimentary framework is a good starting point for exploring the relevant phenomenology. But one should also consider some of the possible variants. For example, the undeformed conservation of energymomentum is relativistically incompatible with the deformation of the dispersion relation (so, in particular, the PKV0 test theory requires a preferred frame). Modifications of the law of energymomentum conservation would be required in a DSR picture, and may be considered even in other scenarios.^{16}
Evidently, the universality of the effect can and should be challenged. And there are indeed (as I shall stress again later in this review) several proposals of test theories with different magnitudes of the effects for different particles [395, 308]. Let me just mention, in closing this section, a case that is particularly challenging for phenomenology: the case of the variant of the PKV0 test theory allowing for nonuniversality such that the effects are restricted only to photons [227, 74], thereby limiting significantly the class of observations/experiments that could test the scenario (see, however, Ref. [380]).
3.2.4 A test theory based on lowenergy effective field theory
The restriction to pure kinematics has the merit to allow us to establish constraints that are applicable to a relatively large class of quantumspacetime scenarios (different formulations of dynamics would still be subject to the relevant constraints), but it also severely restricts the type of experimental contexts that can be considered, since it is only in rare instances (and only to some extent) that one can qualify an analysis as purely kinematical. Therefore, the desire to be able to analyze a wider class of experimental contexts is, therefore, providing motivation for the development of test theories more ambitious than the PKV0 test theory, with at least some elements of dynamics. This is rather reasonable, as long as one proceeds with awareness of the fact that, in light of the situation on the theory side, for test theories adopting a given description of dynamics there is a risk that we may eventually find out that none of the quantumgravity approaches that are being pursued are reflected in the test theory.
In some investigations one might prefer to look at particularly meaningful portions of this large parameter space. For example, one might consider [62] the possibility that the deformation for all spin1/2 particles be characterized by only two parameters, the same two parameters for all particleantipartic le pairs (leaving open, however, some possible sign ambiguities to accommodate the possibility to choose between, for example, \(\eta _ + ^{({\rm{muon}})} = \eta _ + ^{({\rm{electron}})} =  \eta _  ^{({\rm{positron}})}\;{\rm{and}}\;\eta _ + ^{({\rm{muon}})} = \eta _ + ^{({\rm{positron}})} =  \eta _  ^{({\rm{electron}})}\). In the following I will refer to this test theory as the “FTV0 test theory”, where “FT” reflects its adoption of a “lowenergy effective Field Theory” description, “V” reflects its “Lorentzsymmetry Violation” content, and “0” reflects the “minimalistic” assumption of “universality for spin1/2 particles”.
3.2.5 More on “purekinematics” and “fieldtheorybased” phenomenology
Before starting my characterization of experimental sensitivities in terms of the parameters of some test theories I find it appropriate to add a few remarks warning about some difficulties that are inevitably encountered.
For the purekinematics test theories, some key difficulties originate from the fact that sometimes an effect due to the modification of dynamics can take a form that is not easily distinguished from a purekinematics effect. And other times one deals with an analysis of effects that appear to be exclusively sensitive to kinematics but then at the stage of converting experimental results into bounds on parameters some level of dependence on dynamics arises. An example of this latter possibility will be provided by my description of particledecay thresholds in test theories that violate Lorentz symmetry. The derivation of the equations that characterize the threshold requires only the knowledge of the laws of kinematics. And if, according to the kinematics of a given test theory, a certain particle at a certain energy cannot decay, then observation of the decay allows one to set robust purekinematics limits on the parameters. But if the test theory predicts that a certain particle at a certain energy can decay then by not finding such decays we are not in a position to truly establish purekinematics limits on the parameters of the test theory. If the decay is kinematically allowed but not seen, it is possible that the laws of dynamics prevent it from occurring (small decay amplitude).
By adopting a lowenergy quantum field theory this type of limitations is removed, but other issues must be taken into account, particularly in association with the fact that the FTV0 quantum field theory is not renormalizable. Quantumfieldtheorybased descriptions of Planckscale departures from Lorentz symmetry can only be developed with a rather strongly “pragmatic” attitude. In particular, for the FTV0 test theory, with its Planckscale suppressed effects at tree level, some authors (notably Refs. [455, 182, 515, 190]) have argued that the loop expansion could effectively generate additional terms of modification of the dispersion relation that are unsuppressed by the cutoff scale of the (nonrenormalizable) field theory. The parameters of the field theory can be finetuned to eliminate unwanted large effects, but the needed level of fine tuning is usually rather unpleasant. While certainly undesirable, this severe finetuning problem should not discourage us from considering the FTV0 test theory, at least not at this early stage of the development of the relevant phenomenology. Actually some of the most successful theories used in fundamental physics are affected by severe fine tuning. It is not uncommon to eventually discover that the fine tuning is only apparent, and some hidden symmetry is actually “naturally” setting up the hierarchy of parameters.
In particular, it is already established that supersymmetry can tame the finetuning issue [268, 130]. If one extends supersymmetric quantum electrodynamics by adding interactions with external vector and tensor backgrounds that violate Lorentz symmetry at the Planck scale, then exact supersymmetry requires that such interactions correspond to operators of dimension five or higher, so that no finetuning is needed in order to suppress the unwanted operators of dimension lower than five. Supersymmetry can only be an approximate symmetry of the physical world, and the effects of the scale of softsupersymmetrybreaking masses controls the renormalizationgroup evolution of dimension five Lorentzviolating operators and their mixing with dimension three Lorentzviolating operators [268, 130].
It has also been established [461] that if Lorentz violation occurs in the gravitational sector, then the violations of Lorentz symmetry induced on the matter sector do not require severe finetuning. In particular, this has been investigated by coupling the Standard Model of particle physics to a HořavaLifshitz description of gravitational phenomena.
The study of Planckscale departures from Lorentz symmetry may find some encouragement in perspectives based on renormalization theory, at least in as much as it has been shown [79, 78, 289, 507] that some field theories modified by Lorentzviolating terms are actually rather well behaved in the UV.
3.3 Photon stability
3.3.1 Photon stability and modified dispersion relations
The first example of Planckscale sensitivity that I discuss is the case of a process that is kinematically forbidden in the presence of exact Lorentz symmetry, but becomes kinematically allowed in the presence of certain departures from Lorentz symmetry. It has been established (see, e.g., Refs. [305, 59, 334, 115]) that when Lorentz symmetry is broken at the Planck scale, there can be significant implications for certain decay processes. At the qualitative level, the most significant novelty would be the possibility for massless particles to decay. And certain observations in astrophysics, which allow us to establish that photons of energies up to ∼ 10^{14} eV are stable, can then be used [305, 59, 334, 115] to set limits on schemes for departures from Lorentz symmetry.
The fact that for η = 0 Eq. (21) would require cos(θ) > 1 reflects the fact that, if Lorentz symmetry is preserved, the process γ → e^{+}e^{−} is kinematically forbidden. For η < 0 the process is still forbidden, but for positive η highenergy photons can decay into an electronpositron pair. In fact, for \({E_\gamma} \gg {(m_e^2{E_p}/\vert\eta \vert)^{1/3}}\) one finds that there is a region of phase space where cos(θ) < 1, i.e., there is a physical phase space available for the decay.
The energy scale \({(m_e^2{E_p})^{1/3}}\) ∼ 10^{13} eV is not too high for testing, since, as mentioned, in astrophysics we see photons of energies up to ∼ 10^{14} eV that are stable (they clearly travel safely some large astrophysical distances). The level of sensitivity that is within reach of these studies therefore goes at least down to values of (positive) η of order 1 and somewhat smaller than 1. This is what one describes as “Planckscale sensitivity” in the quantumspacetime phenomenology literature: having set the dimensionful deformation parameter to the Planckscale value, the coefficient of the term that can be tested is of order 1 or smaller. However, specifically for the case of the photonstability analysis it is rather challenging to transform this Planckscale sensitivity into actual experimental limits.
Within PKV0 kinematics, for n = 1 and positive η of order 1, it would have been natural to expect that photons with ∼ 10^{14} eV energy are unstable. But the fact that the decay of 10^{14} eV photons is allowed by PKV0 kinematics of does not guarantee that these photons should rapidly decay. It depends on the relevant probability amplitude, whose evaluation goes beyond the reach of kinematics. Still, it is likely that these observations are very significant for theories that are compatible with PKV0 kinematics. For a theory that is compatible with PKV0 kinematics (with positive η) this evidence of stability of photons imposes the identification of a dynamical mechanism that essentially prevents photon decay. If one finds no such mechanism, the theory is “ruled out” (or at least its parameters are severely constrained), but in principle one could look endlessy for such a mechanism. A balanced approach to this issue must take into account that quantumspacetime physics may well modify both kinematics and the strength (and nature) of interactions at a certain scale, and it might in principle do this in ways that cannot be accommodated within the confines of effective quantum field theory, but one should take notice of the fact that, even in some new (tobediscovered) framework outside effective quantum field theory, it is unlikely that there will be very large “conspiracies” between the modifications of kinematics and the modifications of the strength of interaction. In principle, models based on pure kinematics are immune from certain bounds on parameters that are also derived also using descriptions of the interactions, and it is conceivable that in the correct theory the actual bound would be somewhat shifted from the value derived within effective quantum field theory. But in order to contemplate large differences in the bounds one would need to advocate very large and ad hoc modifications of the strength of interactions, large enough to compensate for the often dramatic implications of the modifications of kinematics. The challenge then is to find satisfactory criteria for confining speculations about variations of the strengths of interaction only within a certain plausible range. To my knowledge this has not yet been attempted, but it deserves high priority.
A completely analogous calculation can be done within the FTV0 test theory, and there one can easily arrive at the conclusion [377] that the FTV0 description of dynamics should not significantly suppress the photondecay process. However, as mentioned, consistency with the effectivefieldtheory setup requires that the two polarizations of the photon acquire oppositesign modifications of the dispersion relation. We observe in astrophysics some photons of energies up to ∼ 10^{14} eV that are stable over large distances, but as far as we know those photons could be all rightcircular polarized (or all leftcircular polarized). This evidence of stability of photons, therefore, is only applicable to the portion of the FTV0 parameter space in which both polarizations should be unstable (a subset of the region with η_{+} > η_{ γ } and η_{−} > η_{ γ }).
3.3.2 Photon stability and modified energymomentum conservation
If the modification of the dispersion relation and the modification of the law of energymomentum conservation are not matched exactly to get this result, then one can have the possibility of photon decay, but in some cases it can be further suppressed (in addition to the Planckscale suppression) by the partial compensation between the two modifications.
The fact that the matching between modification of the dispersion relation and modification of the law of energymomentum conservation that produces a stable photon is obtained using a DSRinspired setup is not surprising [63]. The relativistic properties of the framework are clearly at stake in this derivation. A thresholdenergy requirement for particle decay (such as the \({E_\gamma} \gg {(m_e^2{E_p}/\vert\eta \vert)^{1/3}}\) mentioned above) cannot be introduced as an observerindependent law, and is therefore incompatible with any relativistic (even DSRrelativistic) formulation of the laws of physics. In fact, different observers assign different values to the energy of a particle and, therefore, in the presence of a thresholdenergy requirement for particle decay a given particle should be allowed to decay, according to some observers while being totally stable for others.
3.4 Pairproduction threshold anomalies and gammaray observations
Another opportunity to investigate quantumspacetimeinspired Planckscale departures from Lorentz symmetry is provided by certain types of energy thresholds for particleproduction processes that are relevant in astrophysics. This is a very powerful tool for quantumspacetime phenomenology [327, 38, 73, 463, 512, 364, 307, 494], and, in fact, at the beginning of this review, I chose the evaluation of the threshold energy for photopion production, p + γ_{CMBER} → p + π, as the basis for illustrating how the sensitivity levels that are within our reach can be placed in rather natural connection with effects introduced at the Planck scale.
I discuss the photopion production threshold analysis in more detail in Section 3.5. Here, I consider instead the electronpositron pair production process, γγ → e^{+}e^{−}.
3.4.1 Modified dispersion relations and γγ → e^{+}e^{−}
The threshold for γγ → e^{+}e^{−} is relevant for studies of the opacity of our Universe to photons. In particular, according to the conventional (classicalspacetime) description, the IR diffuse extragalactic background should give rise to the strong absorption of “TeV photons” (here understood as photons with energy 1 TeV < E < 30 TeV), but this prediction must be reassessed in the presence of violations of Lorentz symmetry.
This provides an opportunity for a purekinematics test: if a 10 TeV photon collides with a photon of 0.03 eV and produces an electronpositron pair the case n = 1, η ∼ − 1 for the PKV0 test theory is ruled out. A 10 TeV photon and a 0.03 eV photon can produce an electronpositron pair according to ordinary specialrelativistic kinematics (and its associated requirement \({E_{th}} = m_e^2/\epsilon\)), but they cannot produce an electronpositron pair according to PKV0 kinematics with n = 1 and η∼−1.
For positive η the situation is somewhat different. While negative η increases the energy requirement for electronpositron pair production, positive η decreases the energy requirement for electronpositron pair production. In some cases, where one would expect electronpositron pair production to be forbidden, the PKV0 test theory with positive η would instead allow it. But once a process is allowed there is no guarantee that it will actually occur, not without some information on the description of dynamics (that allows us to evaluate cross sections). As in the case of photon decay, one must conclude that a purekinematics framework can be falsified when it predicts that a process cannot occur (if instead the process is seen) but in principle it cannot be falsified when it predicts that a process is allowed. Here too, one should gradually develop balanced criteria taking into account the remarks I offer in Section 3.3.1 concerning the plausibility (or lack thereof) of conspiracies between modifications of kinematics and modifications of the strengths of interaction.
Concerning the level of sensitivity that we can expect to achieve in this case one can robustly claim that Planckscale sensitivity is within our reach. This, as anticipated above, is best seen considering the “TeV photons” emitted by some blazars, for which (as they travel toward our Earth detectors) the photons of the IR diffuse extragalactic background are potential targets for electronpositron pair production. In estimating the sensitivity achievable with this type of analyses it is necessary to take into account the fact that, besides the form of the threshold condition, there are at least three other factors that play a role in establishing the level of absorption of TeV photons emitted by a given blazar: our knowledge of the type of signal emitted by the blazar (at the source), the distance of the blazar, and most importantly the density of the IR diffuse extragalactic background.
The availability of observations of the relevant type has increased very significantly over these past few years. For example, for the blazar “Markarian 501” (at a redshift of z = 0.034) and the blazar “H1426+428” (at a redshift of z = 0.129) robust observations up to the 20TeV range have been reported [15, 16], and for the blazar “Markarian 421” (at a redshift of z = 0.031) observations of photons of energy up to 45 TeV has been reported [438], although a more robust signal is seen once again up to the 20TeV range [355, 17].
The key obstruction for translating these observations into an estimate of the effectiveness of pairproduction absorption comes from the fact that measurements of the density of the IR diffuse extragalactic background are very difficult, and as a result our experimental information on this density is still affected by large uncertainties [235, 536, 111, 278].
The observations do show convincingly that some absorption is occurring [15, 16, 438, 355, 17]. I should stress the fact that the analysis of the combined Xray/TeVgammaray spectrum for the Markarian 421 blazar, as discussed in Ref. [333], provides rather compelling evidence. The Xray part of the spectrum allows one to predict the TeVgammaray part of the spectrum in a way that is rather insensitive to our poor knowledge of the source. This in turn allows us to establish in a sourceindependent way that some absorption is occurring.
For the associated quantumspacetimephenomenology analysis, the fact that some absorption is occurring does not allow us to infer much: the analysis will become more and more effective as the quantitative characterization of the effectiveness of absorption becomes more and more precise (as measured by the amount of deviation from the level of absorption expected within a classicalspacetime analysis that would still be compatible with the observations). And we are not yet ready to make any definite statement about this absorption levels. This is not only a result of our rather poor knowledge of the IR diffuse extragalactic background, but it is also due to the status of the observations, which still presents us with some apparent puzzles. For example, it is not yet fully understood why, as observed by some [15, 355, 17, 536], there is a difference between the absorptioninduced cutoff energy found in data concerning Markarian 421, \(E_{{\rm{mk}}421}^{{\rm{cutoff}}} \simeq 3.6\;{\rm{TeV}}\), and the corresponding cutoff estimate obtained from Markarian501 data, \(E_{{\rm{mk}}501}^{{\rm{cutoff}}} \simeq 6.2\;{\rm{TeV}}\). And the observation of TeV γrays emitted by the blazar H1426+428, which is significantly more distant than Markarian 421 and Markarian 501, does show a level of absorption that is higher than the ones inferred for Markarian 421 and Markarian 501, but (at least assuming a certain description [16] of the IR diffuse extragalactic background) the H1426+428 TeV luminosity “seems to exceed the level anticipated from the current models of TeV blazars by far” [16].
Clearly, the situation requires further clarification, but it seems reasonable to expect that within a few years we should fully establish facts such as “γrays with energies up to 20 TeV are absorbed by the IR diffuse extragalactic background”.^{18} This would imply that at least some photons with energy smaller than ∼ 200 meV can create an electronpositron pair in collisions with a 20 TeV γray. In turn this would imply for the PKV0 test theory, with n = 1, that necessarily η ≥ −50 (i.e., either η is positive or η is negative with absolute value smaller than 50). This means that this strategy of analysis will soon take us robustly to sensitivities that are less than a factor of a 100 away from Planckscale sensitivities, and it is natural to expect that further refinements of these measurements will eventually take us to Planckscale sensitivity and beyond.
The line of reasoning needed to establish whether this Planckscale sensitivity could apply to purekinematics frameworks is somewhat subtle. One could simplistically state that when we see a process that is forbidden by a certain set of laws of kinematics then those laws are falsified. However, in principle this statement is correct only when we have full knowledge of the process, including a full determination of the momenta of the incoming particles. In the case of the absorption of multiTeV gamma rays from blazars it is natural to assume that this absorption be due to interactions with IR photons, but we are not in a position to exclude that the absorption be due to higherenergy background photons. Therefore, we should contemplate the possibility that the PKV0 kinematics be implemented within a framework in which the description of dynamics is such to introduce a largeenough modification of cross sections to allow absorption of multiTeV blazar gamma rays by background photons of energy higher than 200 meV. As mentioned above repeatedly, I advocate a balanced perspective on these sorts of issues, which should not extend all the way to assuming wild conspiracies centered on very large changes in cross sections, even when testing a purekinematics framework. But, as long as a consensus on criteria for such a balanced approach is not established, it is difficult to attribute a quantitative confidence level to experimental bounds on a purekinematics framework through mere observation of some absorption of multiTeV blazar gamma rays.
The concerns are not applicable to test theories that do provide a description of dynamics, such as the FTV0 test theory, with its effectivefieldtheory setup. However, for the FTV0 test theory one must take into account the fact that the modification of the dispersion relation carries the opposite sign to the two polarizations of the photon and might have an helicity dependence in the case of electrons and positrons. So, in the case of the FTV0 test theory, as long as observations only provide evidence of some absorption of TeV gamma rays (without much to say about the level of agreement with the amount of absorption expected in the classicalspacetime picture), and are, therefore, consistent with the hypothesis that only one of the polarizations of the photon is being absorbed, only rather weak limits can be established.
3.4.2 Threshold anomalies and modified energymoment um conservation
This shows very emphatically that modifications of the law of energymomentum conservation can compensate for the effects on threshold derivation produced by modified dispersion relations. The cancellation should typically be only partial, but in cases in which the two modifications are “matched exactly” there is no leftover effect. The fact that a DSRinspired modification of the law of conservation of energymomentum produces this exact matching admits a tentative interpretation that the interested reader can find in Refs. [58, 63].
3.5 Photopion production threshold anomalies and the cosmicray spectrum
Notice that whereas in discussing the pairproduction threshold relevant for observations of TeV gamma rays I had immediately specialized (13) to the case n = 1, here I am contemplating values of n that are even greater than 1. One could also admit n > 1 for the pairproduction threshold analysis, but it would be a mere academic exercise, since it is easy to verify that in that case Planckscale sensitivity is within reach only for n not significantly greater than 1. Instead (as I briefly stressed already in Section 1.5) the role of the photopionproduction threshold in cosmicray analysis is such that even for the case of values of n as high as 2 (i.e., even for the case of effects suppressed quadratically by the Planck scale) Planckscale sensitivity is not unrealistic. In fact, using for m_{ p } and m_{ π } the values of the masses of the proton and the pion and for ϵ a typical CMBRphoton energy one finds that for negative η of order 1 (effects introduced at the Planck scale) the shift of the threshold codified in (29) is gigantic for n = 1 and still observably large [38, 73] for n = 2.
For negative η the Planckscale correction shifts the photopionproduction threshold to higher values with respect to the standard classicalspacetime prediction, which estimates the photopionproduction threshold scale to be of about 5 · 10^{19} eV. Assuming^{19} that the observed cosmic rays of highest energies are protons, when the spectrum reaches the photopionproduction threshold one should first encounter a pileup of cosmic rays with energies just in the neighborhood of the threshold scale, and then above the threshold the spectrum should be severely depleted. The pileup results from the fact that protons with abovethreshold energy tend to lose energy through photopion production and slow down until their energy is comparable to the threshold energy. The depletion above the threshold is the counterpart of this pileup (protons emitted at the source with energy above the threshold tend to reach us, if they come to us from far enough away, with energy comparable to the threshold energy).
The availability in this cosmicray context of Planckscale sensitivities for values of n all the way up to n = 2 was fully established by the year 2000 [38, 73]. The debate then quickly focused on establishing what exactly the observations were telling us about the photopionproduction threshold. The fact that the AGASA cosmicray observatory was reporting [519] evidence of a behavior of the spectrum that was of the type expected in this Planckscale picture generated a lot of interest. However, more recent cosmicray observations, most notably the ones reported by the Pierre Auger observatory [448, 8], appear to show no evidence of unexpected behavior. There is even some evidence [5] (see, however, the updated Ref. [11]) suggesting that to the highestenergy observed cosmic rays, one can associate some relatively nearby sources, and that all this is occurring at scales that could fit within the standard picture of the photopionproduction threshold, without Planck scale effects.
These results reported by the Pierre Auger Observatory are already somewhat beyond the “preliminary” status, and we should soon have at our disposal very robust cosmicray data, which should be easily converted into actual experimental bounds on the parameters of Planckscale test theories.
Among the key ingredients that are still missing I should assign priority to the mentioned issue of correlation of cosmicray observations with the large scale distribution of matter in the nearby universe and the issue of the composition of cosmic rays (protons versus heavy nuclei). The rapidlyevolving [5, 11] picture of correlations with matter in the nearby universe focuses on cosmicray events with energy ≥ 5.7 · 10^{19} eV, while the growing evidence of a significant heavynuclei component at high energies is limited so far at energies of ≤ 4 · 10^{19} eV. And this state of affairs, as notably stressed in Ref. [242], limits our insight on several issues relevant for the understanding of the origin of cosmic rays and the related issues for tests of Lorentz symmetry, since it leaves open several options for the nature and distance of the sources above and below 5 · 10^{19} eV.
Postponing more definite claims on the situation on the experimental side, let me stress, however, that there is indeed a lot at stake in these studies for the hypothesis of quantumspacetimeinduced Planckscale departures from Lorentz symmetry. Even for purekinematics test theories this type of data analysis is rather strongly relevant. For example, the kinematics of the PKV0 test theory forbids (for negative η of order 1 and n ≤ 2) photopion production when the incoming proton energy is in the neighborhood of 5 · 10^{19} eV and the incoming photon has typical CMBR energies. For reasons already stressed (for other contexts), in order to establish a robust experimental limit on purekinematics scenarios using the role of the photopionproduction threshold in the cosmicray spectrum, it would be necessary to also exclude that other background photons (not necessarily CMBR photons) be responsible for the observed cutoff.^{20} It appears likely that such a level of understanding of the cosmicray spectrum will be achieved in the notsodistant future.
For the FTV0 test theory, since it goes beyond pure kinematics, one is not subject to similar concerns [381]. However, the fact that it admits the possibility of different effects for the two helicities of the incoming proton, complicates and renders less sharp this type of cosmicray analyses. It does lead to intriguing hypotheses: for example, exploiting the possibility of helicity dependence of the Planck scale effect for protons, one can rather naturally end up with a scenario that predicts a pileup/cutoff structure somewhat similar to the one of the standard classicalspacetime analysis, but softer, as a result of the fact that only roughly half of the protons would be allowed to lose energy by photopion production.
For the photopionproduction threshold one finds exactly the same mechanism, which I discussed in some detail for the pairproduction threshold, of possible compensation between the effects produced by modified dispersion relations and the effects produced by modified laws of energymomentum conservation. So, the analysis of frameworks where both the dispersion relation and the energymomentum conservation law are modified, as typical in DSR scenarios [63], should take into account that added element of complexity.
3.6 Pion nondecay threshold and cosmicray showers
Also relevant to the analysis of cosmicray observations is another aspect of the possible implications of quantumspacetimemotivated Planckscale departures from Lorentz symmetry: the possibility of a suppression of pion decay at ultrahigh energies. While in some cases departures from Lorentz symmetry allow the decay of otherwise stable particles (as in the case of γ → e^{+}e^{−}, discussed above, for appropriate choice of values of parameters), it is indeed also possible for departures from Lorentz symmetry to either introduce a threshold value of the energy of the particle, above which a certain decay channel for that particle is totally forbidden [179, 81], or introduce some sort of suppression of the decay probability that increases with energy and becomes particularly effective above a certain threshold value of the energy of the decaying particle [59, 115, 244]. This may be relevant [81, 59] for the description of the air showers produced by cosmic rays, whose structure depends rather sensitively on certain decay probabilities, particularly the one for the decay π → γγ.
This is rather intriguing since there is a report [81] of experimental evidence of anomalies for the structure of the air showers produced by cosmic rays, particularly their longitudinal development. And it has been argued in Ref. [81] that these unexpected features of the longitudinal development of air showers could be explained in terms of a severely reduced decay probability for pions of energies of 10^{15} eV and higher. This is still to be considered a very preliminary observation, not only because of the need to acquire data of better quality on the development of air showers, but also because of the role [59] that our limited control of nonperturbative QCD has in setting our expectations for what airshower development should look like without new physics.
It is becoming rather “urgent” to reassess this issue in light of recent data on cosmic rays and cosmicray shower development. Such an exercise has not been made for a few years now, and for the mentioned Auger data, with the associated debate on the composition of cosmic rays, the analysis of shower development (and, therefore, of the hypothesis of some suppression of pion decay) is acquiring increasing significance [509, 6, 36, 549].
As for the other cases in which I discuss effects of modifications of the dispersion relation for kinematics of particle reactions, for this piondecay argument scenarios hosting both a modified dispersion relation and modifications of the law of conservation of energymomentum, as typical in DSR scenarios, can lead to [63] a compensation of the correction terms.
3.7 Vacuum Cerenkov and other anomalous processes
The quantumspacetimephenomenology analyses I have reviewed so far have played a particularly significant role in the rapid growth of the field of quantumspacetime phenomenology over the last decade. This is particularly true for the analyses of the pairproduction threshold for gamma rays and of the photopionproduction threshold for cosmic rays, in which the data relevant for the Planckscale effect under study can be perceived as providing some encouragement for new physics. One can legitimately argue [463, 302] that the observed level of absorption of TeV gamma rays is low enough to justify speculations about “new physics” (even though, as mentioned, there are “conventionalphysics descriptions” of the relevant data). The opportunities for Planck scale physics to play a role in the neighborhood of the GZK scale of the cosmicray spectrum are becoming slimmer, as stressed in Section 3.5, but still it has been an important sign of maturity for quantumspacetime phenomenology to play its part in the debate that for a while was generated by the preliminary and tentative indications of an anomaly around the “GZK cutoff”. It is interesting how the hypothesis of a pionstability threshold, another Planckscalemotivated hypothesis, also plays a role in the assessment of the present status of studies of ultrahighenergy cosmic rays.
I am giving disproportionate attention to the particleinteraction analyses described in Sections 3.4, 3.5, 3.6 because they are the most discussed and clearest evidence in support of the claim that quantumspacetime Planckscale phenomenology does have the ability to discover its target new physics, so much so that some (however tentative) “experimental puzzles” have been considered and are being considered from the quantumspacetime perspective.
But it is of important to also consider the implications of quantumspacetimeinspired Planckscale departures from Lorentz symmetry, and particularly Planckscale modifications of the dispersion relation, for all possible particlephysics processes. And a very valuable type of particlephysics processes to be considered are the ones that are forbidden in a standard specialrelativistic setup but could be allowed in the presence of Planckscale departures from Lorentz symmetry. These processes could be called “anomalous processes”, and in the analysis of some of them one does find opportunities for Planckscale sensitivity, as already discussed for the case of the process γ → e^{−}e^{+} in Section 3.3.
For a comprehensive list (and more detailed discussion) of other analyses of anomalous processes, which are relevant for the whole subject of the study of possible departures from Lorentz symmetry (within or without quantum spacetime), readers can rely on Refs. [395, 308] and references therein.
I will just briefly mention one more significant example of an anomalous process that is relevant from a quantumspacetimephenomenology perspective: the “vacuum Cerenkov” process, e^{−} → e^{−}γ, which in certain scenarios [395, 308, 41] with broken Lorentz symmetry is allowed above a threshold value of electron energy. This is analyzed in close analogy with the discussion in Section 3.3 for the process γ → e^{−}e^{+} (which is another example of anomalous particle interaction).
Since we have no evidence at present of vacuumCerenkov processes, the relevant analyses are of the type that sets limits on the parameters of some test theories. Clearly, this observational evidence against vacuumCerenkov processes is also relevant for purekinematics test theories, but in ways that it is difficult to quantify, because of the dependence on the strength of the interactions (an aspect of dynamics). So, here too, one should contemplate the implications of these findings from the perspective of the remarks offered in Section 3.3.1 concerning the plausibility (or lack thereof) of conspiracies between modifications of kinematics and modifications of the strengths of interaction.
Within the FTV0 test theory one can rigorously analyze the vacuumCerenkov process, and there actually, if one arranges for oppositesign dispersionrelation correction terms for the two helicities of the electron, one can in principle have helicitychanging e^{−} → e^{−}γ at any energy (no threshold), but estimates performed [395, 308] within the FTV0 test theory show that the rate is extremely small at low energies.
Above the threshold for helicitypreserving e^{−} → e^{−}γ the FTV0 rates are substantial, and this in particular would allow an analysis with Planckscale sensitivity that relies on observations of 50TeV gamma rays from the Crab nebula. The argument is based on several assumptions (but all apparently robust) and its effectiveness is somewhat limited by the combination of parameters allowed by FTV0 setup and by the fact that for these 50TeV gamma rays we observe from the Crab nebula we can only reasonably guess a part of the properties of the emitting particles. According to the most commonly adopted model the relevant gamma rays are emitted by the Crab nebula as a result of inverse Compton processes, and from this one infers [395, 308, 40] that for electrons of energies up to 50 TeV the vacuum Cerenkov process is still ineffective, which in turn allows one to exclude certain corresponding regions of the FTV0 parameter space.
3.8 Invacuo dispersion for photons
Analyses of thresholds for particlephysics processes, discussed in the previous Sections 3.4, 3.5, 3.6, and 3.7, played a particularly important role in the development of quantumspacetime phenomenology over the last decade, because the relevant studies were already at Planckscale sensivity. In June 2008, with the launch of the Fermi (/GLAST) space telescope [436, 201, 440, 3, 4, 413] we gained access to Planckscale effects also for invacuo dispersion as well. These studies deserve particular interest because they have broad applicability to quantumspacetime test theories of the fate of Lorentz/Poincaré symmetry at the Planck scale. In the previous Sections 3.4, 3.5, 3.6, and 3.7, I stressed how the analyses of thresholds for particlephysics processes provided information that is rather strongly model dependent, and dependent on the specific choices of parameters within a given model. The type of insight gained through invacuodispersion studies is instead significantly more robust.
On the basis of the speed law (31) one would find that two simultaneouslyemitted photons should reach the detector at different times if they carry different energy. And this timeofarrivaldifference effect can be significant [66, 491, 459, 539, 232] in the analysis of shortduration gammaray bursts that reach us from cosmological distances. For a gammaray burst, it is not uncommon^{22} that the time traveled before reaching our Earth detectors be of order T ∼ 10^{17} s. Microbursts within a burst can have very short duration, as short as 10^{−3} s, and this should suggest that the photons that compose such a microburst are all emitted at the same time, up to an uncertainty of 10^{−3} s. Some of the photons in these bursts have energies that extend even above [3] 10 GeV, and for two photons with energy difference of order ΔE ∼ 10 GeV a ΔE/E_{ p } speed difference over a time of travel of 10^{17} s would lead [74] to a difference in times of arrival of order \(\Delta t\sim\eta T\Delta {E \over {{E_p}}}\sim\eta \cdot 1\) which is not negligible^{23} with respect to the typical variability time scales one expects for the astrophysics of gammaray bursts. Indeed, it is rather clear [74, 264] that the studies of gammaray bursts conducted by the Fermi telescope provide us access to testing Planckscale effects, in the linearmodification (“n = 1”) scenario.
Actually, Planckscale sensitivity to invacuo disperson can also be provided by observations of TeV flares from certain active galactic nuclei, at redshifts much smaller than 1 (cases in which spacetime expansion is not really tangible). In particular, studies of TeV flares from Mk 501 and PKS 2155304 performed by the MAGIC [233] and HESS [285] observatories have established [218, 29, 226, 18, 10, 129] bounds on the scale of dispersion, for the lineareffects (“n = 1”) scenario, at about 1/10 of the Planck scale.
But the present best constraints on quantumspacetimeinduced invacuo dispersion are derived from observations of gammaray bursts reported by the Fermi telescope. There are, so far, four Fermidetected gammaray bursts that are particularly significant for the hypothesis of invacuo dispersion: GRB 090816C [3], GRB 090510 [4], GRB 090902B [2], GRB 090926A [482]. The data for each one of these bursts has the strength of constraining the scale of invacuo dispersion, for the lineareffects (“n = 1”) scenario, at better than 1/10 of the Planck scale. In particular, GRB 090510 was a truly phenomenal short burst [4] and the structure of its observation allows us to conservatively establish that the scale of invacuo dispersion, for the lineareffects (“n = 1”) scenario, is higher than 1.2 times the Planck scale.
The simplest way to do such analyses is to take one highenergy photon observed from the burst and take as reference its delay Δt with respect to the burst trigger: if one could exclude conspiracies such that the specific photon was emitted before the trigger (we cannot really exclude it, but we would consider that as very unlikely, at least with present knowledge) evidently Δt would have to be bigger than any delay caused by the quantumspacetime effects. This, in turn, allows us, for the case of GRB 090510, to establish the limit at 1.2 times the Planck scale [4]. And, interestingly, even more sophisticated techniques of analysis, using not a single photon but the whole structure of the highenergy observation of GRB 090510, also encourage the adoption of a limit at 1.2 times the Planck scale [4]. It has also been noticed [427] that if one takes at face value the presence of highenergy photon bunches observed for GRB 090510, as evidence that these photons were emitted nearly simultaneously at the source and they are being detected nearly simultaneously, then the bound inferred could be even two orders of magnitude above the Planck scale [427].
I feel that at least the limit at 1.2 times the Planck scale is reasonably safe/conservative. But it is obvious that here we would feel more comfortable with a wider collection of gammaray bursts usable for our analyses. This would allow us to balance, using high statistics, the challenges for such studies of invacuo dispersion that (as for other types of studies based on observations in astrophysics discussed earlier) originate from the fact that we only have tentative models of the source of the signal. In particular, the engine mechanisms causing the bursts of gamma rays also introduce correlations at the source between the energy of the emitted photons and the time of their emission. This was in part expected by some astrophysicists [459], and Fermi data allows one to infer it at levels even beyond expectations [3, 4, 527, 376, 187, 256]. On a single observation of gammarayburst events such atthesource correlations are, in principle, indistinguishable from the effect we expect from invacuo dispersion, which indeed is a correlation between times of arrival and energies of the photons. And another challenge I should mention originates from the necessity of understanding at least partly the “precursors” of a gammaray burst, another feature that was already expected and to some extent known [362], but recently came to be known as a more significant effect than expected [4, 530].
So, we will reach a satisfactory “comfort level” with our bounds on invacuo dispersion only with “high statistics”, a relatively large collection [74] of gammaray bursts usable for our analyses. High statistics always helps, but in this case it will also provide a qualitatively new handle for the data analysis: a relatively large collection of highenergy gammaray bursts, inevitably distributed over different values of redshift, would help our analyses also because comparison of bursts at different redshifts can be exploited to achieve results that are essentially free from uncertainties originating from our lack of knowledge of the sources. This is due to the fact that the structure of invacuo dispersion is such that the effect should grow in predictable manner with redshift, whereas we can exclude that the exact same dependence on redshift (if any) could characterize the correlations at the source between the energy of the emitted photons and the time of their emission.
In this respect we might be experiencing a case of tremendous bad luck: as mentioned we really still only have four gammaray bursts to work with, GRB 090816C [3], GRB 090510 [4], GRB 090902B [2], GRB 090926A [482], but on the basis of how Fermi observations had been going for the first 13 months of operation we were led to hope that by this time (end of 2012), after 50 months of operation of Fermi, we might have had as many as 15 such bursts and perhaps 4 or 5 bursts of outstanding interest for invacuo dispersion, comparable to GRB 090510. These four bursts we keep using from the Fermi data set were observed during the first 13 months of operation (in particular GRB 090510 was observed during the 10th month of operation) and we got from Fermi nothing else of any use over the last 37 months. If our luck turns around we should be able to claim for quantumspacetime phenomenology a first small but tangible success: ruling out at least the specific hypothesis of Planckscale invacuo dispersion, at least specifically for the case of lineareffects (“n= 1”).
This being said about the opportunities and challenges facing the phenomenology of invacuo dispersion, let me, in closing this section, offer a few additional remarks on the broader picture. From a quantumspacetimephenomenology perspective it is noteworthy that, while in the analyses discussed in the previous Sections 3.4, 3.5, 3.6, and 3.7, the amplifier of the Planckscale effect was provided by a large boost, in this invacuodispersion case the amplification is due primarily to the long propagation times, which essentially render the analysis sensitive to the accumulation [52] of very many minute Planckscale effects. For propagation times that are realistic in controlled Earth experiments, in which one perhaps could manage to study the propagation of photons of TeV energies, over distances of 10^{6} m, the invacuo dispersion would still induce, even for n = 1, only time delays of order ∼ 10^{−18} s.
Invacuodispersion analyses of gammaray bursts are also extremely popular within the quantumspacetimephenomenology community because of the very limited number of assumptions on which they rely. One comes very close to having a direct test of a Planckscale modification of the dispersion relation. In comparing the PKV0 and the FTV0 test theories, one could exploit the fact that whereas for the PKV0 test theory the Planckscaleinduced timeofarrival difference would affect a multiphoton microburst by producing a difference in the “average arrival time” of the signal in different energy channels, within the FTV0 test theory, for an ideally unpolarized signal, one would expect a dependence of the timespread of a microburst that grows with energy, but no effect for the average arrival time in different energy channels. This originates from the polarization dependence imposed by the structure of the FTV0 test theory: for lowenergy channels the whole effect will be small, but in the highestenergy channels, the fact that the two polarizations travel at different speed will manifest itself as spreading in time of the signal, without any net averagetimeofarrival effect for an ideally unpolarized signal. Since there is evidence that at least some gammaray bursts are somewhat far from being ideally unpolarized (see evidence of polarization reported, e.g., in Refs. [359, 556, 528]), one could also exploit a powerful correlation: within the FTV0 test theory one expects to find some bursts with sizeable energydependent averagetimeofarrival differences between energy channels (for bursts with some predominant polarization), and some bursts (the ones with no net polarization) with much less averagetimeofar11rival differences between energy channels but a sizeable difference in time spreading in the different channels. Polarizationsensitive observations of gammaray bursts would allow one to look directly for the polarization dependence predicted by the FTV0 test theory.
Clearly, these invacuo dispersion studies using gamma rays in the GeVTeV range provide us at present with the cleanest opportunity to look for Planckscale modifications of the dispersion relation. Unfortunately, while they do provide us comfortably with Planckscale sensitivity to linear (n = 1) modifications of the dispersion relation, they are unable to probe significantly the case of quadratic (n = 2) modifications.
And, while, as stressed, these studies apply to a wide range of quantumspacetime scenarios with modified dispersion relations, mostly as a result of their insensitivity to the whole issue of description of dynamical aspects of a quantumspacetime theory, one should be aware of the fact that it might be inappropriate to characterize these studies as tests that must necessarily apply to all quantumspacetime pictures with modified dispersion relations. Most notably, the assumption of obtaining the velocity law from the dispersion relation through the formula υ = dE/dp may or may not be valid in a given quantumspacetime picture. Validity of the formula υ = dE/dp essentially requires that the theory is still “Hamiltonian”, at least in the sense that the velocity along the x axis is obtained from the commutator with a Hamiltonian (υ_{ x } ∼ [x, H]), and that the Heisenberg commutator preserves its standard form ([x, p_{ x }] ∼ ℏ so that x ∼ ∂/∂p_{ x }). Especially this second point is rather significant since heuristic arguments of the type also used to motivate modified dispersion relations suggest [22, 122, 323, 415, 243, 408] that the Heisenberg commutator might have to be modified in the quantumspacetime realm.
3.9 Quadratic anomalous invacuo dispersion for neutrinos
Observations of gamma rays in the GeVTeV range could provide us with a very sharp picture of Planckscaleinduced dispersion, if it happens to be a linear (n = 1) effect, but, as stressed above, one would need observations of similar quality for photons of significantly higher energies in order to gain access to scenarios with quadratic (n = 2) effects of Planckscaleinduced dispersion. The prospect of observing photons with energies up to 10^{18} eV at ground observatories [471, 74] is very exciting, and should be pursued very forcefully [74], but it represents an opportunity whose viability still remains to be fully established. And in any case we expect photons of such high energies to be absorbed rather efficiently by background soft photons (e.g., CMBR photons) so that we could not observe them from very distant sources.
One possibility that could be considered [65] is the one of 1987atype supernovae; however such supernovae are typically seen at distances not greater than some 10^{5} light years. And the fact that neutrinos from 1987atype supernovae can be definitely observed up to energies of at least tens of TeV’s is not enough to compensate for the smallness of the distances (as compared to typical gammarayburst distances). As a result, using 1987atype supernovae one might have serious difficulties [65] even to achieve Planckscale sensitivity for linear (n = 1) modifications of the dispersion relation, and going beyond linear order clearly is not possible.
The most advanced plans for invacuodispersion studies with sensitivity up to quadratic (n = 2) Planckscale modifications of the dispersion relation actually exploit [230, 168, 61, 301] (also see, for a similar argument within a somewhat different framework, Ref. [116]) once again the extraordinary properties of gammaray bursters, but their neutrino emissions rather than their production of photons. Indeed, according to current models [411, 543], gammaray bursters should also emit a substantial amount of highenergy neutrinos. Some neutrino observatories should soon observe neutrinos with energies between 10^{14} and 10^{19} eV, and one could either (as it appears to be more feasible [301]) compare the times of arrival of these neutrinos emitted by gammaray bursters to the corresponding times of arrival of lowenergy photons or compare the times of arrivals of differentenergy neutrinos (which, however, might require larger statistics than it seems natural to expect).
In assessing the significance of these foreseeable studies of neutrino propagation within different test theories, one should again take into account issues revolving around the possibility of anomalous reactions. In particular, in spite of the weakness of their interactions with other particles, within an effectivefieldtheory setup neutrinos can be affected by Cherenkovlike processes at levels that are experimentally significant [175], though not if the scale of modification of the dispersion relation is as high as the Planck scale. The recent overall analysis of modified dispersion for neutrinos in quantum field theory given in Ref. [379] shows that for the linear (n = 1) case we are presently able to establish constraints at levels of about 10^{−2} times the Planck scale (and even further from the Planck scale for the quadratic case, n = 2).
3.10 Implications for neutrino oscillations
It is well established [179, 141, 225, 83, 421, 169] that flavordependent modifications to the energymomentum dispersion relations for neutrinos may lead to neutrino oscillations even if neutrinos are massless. This point is not directly relevant for the three test theories I have chosen to use as frameworks of reference for this review. The PKV0 test theory adopts universality of the modification of the dispersion relation, and also the FTV0 test theory describes flavorindependent effects (its effects are “nonuniversal” only in relation to polarization/helicity). Still, I should mention this possibility both because clearly flavordependent effects may well attract gradually more interest from quantumspacetime phenomenologists (some valuable analyses have already been produced; see, e.g., Refs. [395, 308] and references therein), and because even for researchers focusing on flavorindependent effects, it is important to be familiar with constraints that may be set on flavordependent scenarios (those constraints, in a certain sense, provide motivation for the adoption of flavor independence).
Most studies of neutrino oscillations induced by violations of Lorentz symmetry were actually not motivated by quantumgravity/quantumspacetime research (they were part of the general Lorentzsymmetrytest research area) and assumed that the flavordependent violations would take the form of a flavordependent speedoflight scale [179], which essentially corresponds to the adoption of a dispersion relation of the type (13), but with n = 0, and flavordependent values of η. A few studies have considered the case^{24} n = 1 with flavordependent η, which is instead mainly of interest from a quantumspacetime perspective,^{25} and found [141, 225, 421] that for n = 1 from Eq. (13) one naturally ends up with oscillations lengths that depend quadratically on the inverse of the energies of the particles (L ∼ E^{−2}), whereas in the case n = 0 (flavordependent speedoflight scale) such a strong dependence on the inverse of the energies is not possible [141]. In principle, this opens an opportunity for the discovery of manifestations of the flavordependent n = 1 case through studies of neutrino oscillations [141, 421]; however, at present there is no evidence of a role for these effects in neutrino oscillations and, therefore, the relevant data analyses produce bounds [141, 421] on flavor dependence of the dispersion relation.
In a part of the next section (4.6), I shall comment again on neutrino oscillations, but in relation to the possible role of quantumspacetimeinduced decoherence (rather than Lorentzsymmetry violations).
3.11 Synchrotron radiation and the Crab Nebula
Assuming that the only Planckscale modification in this formula should come from the velocity law (described using υ = dE/dp in terms of the modified dispersion relation), one finds that in some instances the characteristic energy of synchrotron radiation may be significantly modified by the presence of Planckscale modifications of the dispersion relation. This originates from the fact that, for example, according to (31), for n = 1 and η < 0, an electron cannot have a speed that exceeds the value \(v_e^{\max} \simeq 1  (3/2){(\vert \eta \vert {m_e}/{E_p})^{2/3}}\), whereas in SR υ_{ e } can take values arbitrarily close to 1.
As an opportunity to test such a modification of the value of the synchrotronradiation characteristic energy one can attempt to use data [306] on photons emitted by the Crab nebula. This must be done with caution since the observational information on synchrotron radiation being emitted by the Crab nebula is rather indirect: some of the photons we observe from the Crab nebula are attributed to sychrotron processes, but only on the basis of a (rather successful) model, and the value of the relevant magnetic fields is also not directly measured. But the level of Planckscale sensitivity that could be within the reach of this type of analysis is truly impressive: assuming that indeed the observational situation has been properly interpreted, and relying on the mentioned assumption that the only modification to be taken into account is the one of the velocity law, one could [306, 378] set limits on the parameter η of the PKV0 test theory that go several orders of magnitude beyond η ∼ 1, for negative η and n = 1, and even for quadratic (n = 2) Planckscale modifications the analysis would fall “just short” of reaching Planckscale sensitivity (“only” a few orders of magnitude away from η ∼ 1 sensitivity for n = 2).
However, the assumptions of this type of analysis, particularly the assumption that nothing changes but the velocity law, cannot even be investigated within purekinematics test theories, such as the PKV0 test theory. Synchrotron radiation is due to the acceleration of the relevant charged particles and, therefore, implicit in the derivation of the formula (35) is a subtle role for dynamics [62]. From a quantumfieldtheory perspective, the process of synchrotronradiation emission can be described in terms of Compton scattering of the electrons with the virtual photons of the magnetic field, and its analysis is, therefore, rather sensitive even to details of the description of dynamics in a given theory. Indeed, essentially this synchrotronradiation phenomenology has focused on the FTV0 test theory and its generalizations, so that one can rely on the familiar formalism of quantum field theory. Making reasonably prudent assumptions on the correct model of the source one can establish [378] valuable (subPlanckian!) experimental bounds on the parameters of the FTV0 test theory.
3.12 Birefringence and observations of polarized radio galaxies
As I stressed already a few times earlier in this review, the FTV0 test theory, as a result of a rigidity of the adopted effectivefieldtheory framework, necessarily predicts birefringence, by assigning different speeds to different photon polarizations. Birefringence is a purekinematics effect, so it can also be included in straightforward generalizations of the PKV0 test theory, if one assigns a different dispersion relation to different photon polarizations and then assumes that the speed is obtained from the dispersion relation via the standard υ = dE/dp relation.
I have already discussed some ways in which birefringence may affect other tests of dispersioninducing (energydependent) modifications of the dispersion relation, as in the example of searches of timeofarrival/energy correlations for observations of gammaray bursts. The applications I already discussed use the fact that for large enough travel times birefringence essentially splits a group of simultaneouslyemitted photons with roughly the same energy and without characteristic polarization into two temporally and spatially separated groups of photons, with different circular polarization (one group being delayed with respect to the other as a result of the polarizationdependent speed of propagation).
Another feature that can be exploited is the fact that even for travel times that are somewhat shorter than the ones achieving a separation into two groups of photons, the same type of birefringence can already effectively erase [261, 262] any linear polarization that might have been there to begin with, when the signal was emitted. This observation can be used in turn to argue that for given magnitude of the birefringence effects and given values of the distance from the source it should be impossible to observe linearly polarized light, since the polarization should have been erased along the way.
Using observations of polarized light from distant radio galaxies [395, 261, 262, 158, 342, 495] one can comfortably achieve Planckscale sensitivity (for “n = 1” linear modifications of the dispersion relation) to birefringence effects following this strategy. In particular, the analysis reported in Ref. [261, 262] leads to a limit of η_{ γ } < 2 · 10^{−4} on the parameter η_{ γ } of the FTV0 test theory. And more recent studies of this type allowed even more stringent bounds to be established(see Refs. [395, 365] and references therein).
Interestingly, even for this strategy based on the effect of removal of linear polarization, gammaray bursts could in principle provide formidable opportunities. And there was a report [173] of observation of polarized MeV gamma rays in the prompt emission of the gammaray burst GRB 021206, which would have allowed very powerful bounds on energydependent birefringence to be established. However, Ref. [173] has been challenged (see, e.g., Ref. [481, 124]). Still, experimental studies of polarization for gammaray bursts continue to be a very active area of research (see, e.g., Refs. [359, 556, 528]), and it is likely that this will gradually become the main avenue for constraining quantumspacetimeinduced birefringence.
3.13 Testing modified dispersion relations in the lab
Over this past decade there has been growing awareness of the fact that data analyses with good sensitivity to effects introduced genuinely at the Planck scale are not impossible, as once thought. It is at this point well known, even outside the quantumgravity/quantumspacetime community, that Planckscale sensitivity is achieved in certain (however rare) astrophysics studies. It would be very very valuable if we could establish the availability of analogous tests in controlled laboratory setups, but this is evidently more difficult, and opportunities are rare and of limited reach. Still, I feel it is important to keep this goal as a top priority, so in this Section I mention a couple of illustrative examples, which can at least show that laboratory tests are possible. Considering these objectives it makes sense to focus again on quantumspacetimemotivated Planckscale modifications of the dispersion relation, so that the estimates of sensitivity levels achievable in a controlled laboratory setup can be compared to the corresponding studies in astrophysics.
One possibility is to use laserlight interferometry to look for invacuodispersion effects. In Ref. [68] two examples of interferometric setups were discussed in some detail, with the common feature of making use of a frequency doubler, so that part of the beam would be for a portion of its journey through the interferometer at double the reference frequency of the laser beam feeding the interferometer. The setups must be such that the interference pattern is sensitive to the fact that, as a result of invacuo dispersion, there is a nonlinear relation between the phase advancement of a beam at frequency ω and a beam at frequency 2ω. For my purposes here it suffices to discuss briefly one such interferometric setup. Specifically, let me give a brief description of a setup in which the frequency (or energy) is the parameter characterizing the splitting of the photon state, so the splitting is in energy space (rather than the more familiar splitting in configuration space, in which two parts of the beam actually follow geometrically different paths). The frequency doubling could be accomplished using a “second harmonic generator” [487] so that if a wave reaches the frequency doubler with frequency ω then, after passing through the frequency doubler, the outgoing wave in general consists of two components, one at frequency ω and the other at frequency 2ω.
If two such frequency doublers are placed along the path of the beam at the end, one has a beam with several components, two of which have frequency 2ω: the transmission of the component that left the first frequency doubler as a 2ω wave, and another component that is the result of frequency doubling of that part of the beam that went through the first frequency doubler without change in the frequency. Therefore, the final 2ω beam represents an interferometer in energy space.
Since the intensity only depends on the distance L between the frequency doublers through the Planckscale correction to the phase, (k′ − 2k) L, by exploiting a setup that allows one to vary L, one should rather easily disentangle the Planckscale effect. And one finds [68] that the accuracy achievable with modern interferometers is sufficient to achieve Planckscale sensitivity (e.g., sensitivity to η ∼ 1 in the PKV0 test theory with n = 1). It is rather optimistic to assume that the accuracy achieved in standard interferometers would also be achievable with this peculiar setup, particularly since it would require the optics aspects of the setup (such as lenses) to work with that high accuracy simultaneously with two beams of different wavelength. Moreover, it would require some very smart techniques to vary the distance between the frequency doublers without interfering with the effectiveness of the optics aspects of the setup. So, in practice we would not presently be capable of using such setups to set Planckscalesensitive limits on invacuo dispersion, but the fact that the residual obstructions are of rather mundane technological nature encourages us to think that in the notsodistant future tests of Planckscale invacuo dispersion in controlled laboratory experiments will be possible.
Besides invacuo dispersion, another aspect of the physics of Planckscale modified dispersion relations that we should soon be able to test in controlled laboratory experiments is the one concerning anomalous thresholds, at least in the case of the γγ → e^{+}e^{−} process that I already considered from an astrophysics perspective in Section 3.4. It is not so far from our present technical capabilities to set up collisions between 10 TeV photons and 0.03 eV photons, thereby reproducing essentially the situation of the analysis of blazars that I discussed in Section 3.4. And notice that with respect to the analysis of observations of blazars, such controlled laboratory studies would give much more powerful indications. In particular, for the analysis of observations of blazars discussed in Section 3.4, a key limitation on our ability to translate the data into experimental bounds on parameters of a purekinematics framework was due to the fact that (even assuming we are indeed seeing absorption of multiTeV photons) the astrophysics context does not allow us to firmly establish whether the absorption is indeed due to the IR component of the intergalactic background radiation (as expected) or instead is due to a higherenergy component of the background (in which case the absorption would instead be compatible with some corresponding Planckscale pictures). If collisions between 10 TeV and 0.03 eV photons in the lab do produce pairs, since we would in that case have total control of the properties of the particles in the in state of the process, we would then have firm purekinematics bounds on the parameters of certain corresponding Planck scale test theories (such as the PKV0 test theory).
These laboratory studies of Planckscalemodified dispersion relations could also be adapted to the FTV0 test theory, by simply introducing some handles on the polarization of the photons that are placed under observation (also see Refs. [254, 255]), with sensitivity not far from Planckscale sentivity in controlled laboratory experiments.
3.14 On test theories without energydependent modifications of dispersion relations
Readers for which this review is the first introduction to the world of quantumspacetime phenomenology might be surprised that this long section, with an ambitious title announcing related tests of Lorentz symmetry, was so heavily biased toward probing the form of the energymomentum dispersion relation. Other aspects of the implications of Lorentz (and Poincaré) symmetry did intervene, such as the law of energymomentum conservation and its deformations (and the form of the interaction vertices and their deformations), and are in part probed through the data analyses reviewed, but the feature that clearly is at center stage is the structure of the dispersion relation. The reason for this is rather simple: researchers that recognize themselves as “quantumspacetime phenomenologists” will consider a certain data analysis as part of the field if that analysis concerns an effect that can be robustly linked to quantum properties of spacetime (rather than, for example, some classicalfield background) and if the analysis exposes the availability of Planckscale sensitivities, in the sense I described above. At least according to the results obtained so far, the aspect of Lorentz/Poincaré symmetry that is most robustly challenged by the idea of a quantum spacetime is the form of the dispersion relation, and this is also an aspect of Lorentz/Poincaré symmetry for which the last decade of work on this phenomenology robustly exposed opportunities for Planckscale sensitivities.
For the type of modifications of the dispersion relation that I considered in this section we have at present rather robust evidence of their applicability in certain noncommutative pictures of spacetime, where the noncommutativity is very clearly introduced at the Planck scale. And several independent (although all semiheuristic) arguments suggest that the same general type of modified dispersion relations should apply to the “Minkowski limit” of LQG, a framework where a certain type of discretization of spacetime structure is introduced genuinely at the Planck scale. Unfortunately, these two frameworks are so complex that one does not manage to analyze spacetime symmetries much beyond building a “case” (and not a waterproof case) for modified dispersion relations.
A broader range of Lorentzsymmetry tests could be valuable for quantumspacetime research, but without the support of a derivation it is very hard to argue that the relevant effects are being probed with sensitivities that are significant from a quantumspacetime/Planckscale perspective. Think, for example, of a framework, such as the one adopted in Ref. [179], in which the form of the dispersion relation is modified, but not in an energydependent way: one still has dispersion relations of the type \({E^2} = c_\# ^2{p^2} + m_\# ^2\), but with a different value of the velocity scale c_{#} for different particles. This is not necessarily a picture beyond the realm of possibilities one would consider from a quantumspacetime perspective, but there is no known quantumspacetime picture that has provided direct support for it. And it is also essentially impossible to estimate what accuracy must be achieved in measurements of c_{proton} − c_{electron}, in order to reach Planckscale sensitivity. Some authors qualify as “Planckian magnitude” of this type of effect, the case in which the dimensionless parameter has value on the order of the ratio of the mass of the particles involved in the process versus the Planck scale (as in c_{proton} − c_{electron} ∼ (m_{proton} ± m_{electron})/E_{ p }) but this arbitrary criterion clearly does not amount to establishing genuine Planckscale sensitivity, at least as long as we do not have a derivation starting with spacetime quantization at the Planck scale that actually finds such magnitudes of these sorts of effects.
Still, it is true that the general structure of the quantumgravity problem and the structure of some of the quantum spacetimes that are being considered for the Minkowski limit of quantum gravity might host a rather wide range of departures from classical Lorentz symmetry. Correspondingly, a broad range of Lorentzsymmetry tests could be considered of potential interest.
I shall not review here this broader Lorentzsymmetrytests literature, since it is not specific to quantumspacetime research (these are tests that could be done and in large part were done even before the development of research on Lorentz symmetries from within the quantumspacetime literature) and it has already been reviewed very effectively in Ref. [395]. Let me just stress that for these broad searches of departures from Lorentz symmetry one needs test theories with many parameters. Formalisms that are well suited to a systematic program of such searches are already at an advanced stage of development [180, 181, 340, 343, 123, 356, 357] (also see Ref. [239]), and in particular the “standardmodelextension” framework [180, 181, 340, 343] has reached a high level of adoption of preference for theorists and experimentalists as the language in which to characterize the results of systematic multiparameter Lorentzsymmetrytest data analyses. The “Standard Model Extension” was originally conceived [340] as a generalization of the Standard Model of particlephysics interactions restricted to powercountingrenormalizable correction terms, and as such it was of limited interest for the bulk of the quantumspacetime/quantumgravity community: since quantum gravity is not a (perturbatively) renormalizable theory, many quantumspacetime researchers would be unimpressed with Lorentzsymmetry tests restricted to powercountingrenormalizable correction terms. However, over these last few years [123] most theorists involved in studies of the “Standard Model Extension” have started to add correction terms that are not powercounting renormalizable.^{26} A good entry point for the literature on limits on the parameters of the “Standard Model Extension” is provided by Refs. [395, 123, 346].
From a quantumgravityphenomenology perspective it is useful to contemplate the differences between alternative strategies for setting up a “completely general” systematic investigation of possible violations of Lorentz symmetry. In particular, it has been stressed (see, e.g., Refs. [356, 357]) that violations of Lorentz symmetry can be introduced directly at the level of the dynamical equations, without assuming (as done in the Standard Model Extension) the availability of a Lagrangian generating the dynamical equations. This is more general than the Lagrangian approach: for example, the generalized Maxwell equation discussed in Ref. [356, 357] predicts effects that go beyond the Standard Model Extension. And charge conservation, which automatically comes from the Lagrangian approach, can be violated in models generalizing the field equations [356, 357]. The comparison of the StandardModelExtension approach and of the approach based on generalizations introduced directly at the level of the dynamical equations illustrates how different “philosophies” lead to different strategies for setting up a “completely general” systematic investigation of possible departures from Lorentz symmetry. By removing the assumption of the availability of a Lagrangian, the second approach is “more general”. Still, no “general approach” can be absolutely general: in principle one could always consider removing an extra layer of assumptions. As the topics I have reviewed in this section illustrate, from a quantumspacetimephenomenology perspective it is not necessarily appropriate to seek the most general parametrizations. On the contrary, we would like to single out some particularly promising candidate quantumspacetime effects (as in the case of modified dispersion relations) and focus our efforts accordingly.
4 Other Areas of UV QuantumSpacetime Phenomenology
Tests of Lorentz symmetry, and particularly of the form of the dispersion relation, probably make up something on the order of half of the whole quantumspacetimephenomenology literature. The other half is spread over a few other, evidently less developed, research lines. Nonetheless, for some of these other research lines the literature has reached some nonnegligible maturity, and even those that are at preliminary stages of development could be precious potential opportunities for quantumspacetime research.
Evidently, the most challenging part of this review work concerns these other components of quantumspacetimephenomenology research, since it is harder to summarize and organize intelligibly the results and scopes of research programs that are still in early stages of development. But it is also the part of this review that could be most valuable, since there is already some work [52, 308, 485, 294] attempting to summarize and review, although more concisely than done here in Section 3, the results obtained by the quantumspacetime phenomenology of Planckscale modified dispersion relations.
This is the type of quantumspacetime effect that one traditionally one to be inevitably produced by any form of spacetime quantization, and is the focus of this section. The possibility of “IR quantumspacetime effects”, effects that are due to Planckscale spacetime quantization but are significant in some deepIR regime, came to the attention of the community only rather recently, emerging mainly from work on “IR/UV mixing in quantum spacetime”, and I shall focus on it in the next Section 5.
4.1 Preliminary remarks on fuzziness
In this review, as natural for phenomenology, I am primarily looking at quantumspacetime effects from the perspective of the type of prequantumspacetime laws that they affect (so we have “departures from classical spacetime symmetries”, “violations of the quantummechanical coherence”, and so on). And our experimental opportunities are such that the main focus is on how spacetime quantization could affect particle propagation (and, for a restricted sample of phenomenological opportunities, interactions among particles). For this section on “other UV quantumspacetime effects” a significant role (particularly noticeable in Sections 4.2, 4.3, and 4.5 will be played by the idea that quantumspacetime effects may introduce an additional irreducible contribution to the fuzziness of the worldlines of particles.
This should be contrasted to the content of Section 3, which focuses mainly on phenomenological proposals involving mechanisms for systematic departures from the currentlyadopted laws of propagation of (and interaction among) particles. In most cases such systematic effects amount to departures from the predictions of Lorentz symmetry (such as a systematic dependence on the velocity of a massless particle on its energy, which would produce a systematic difference between the arrival times of highenergy and lowenergy photons that are simultaneously emitted). If it ends up being the case that the correct quantumspacetime picture does not provide us any such systematic effects, then we will be left with nonsystematic effects, i.e., “fuzziness” [57]. In looking for such effects we can be guided by the intuition that spacetime quantization might act as an environment inducing apparently random fluctuations in certain observables. For example, by distance fuzziness one does not describe an effect that would systematically gives rise to larger (or smaller) distancemeasurement results, but rather one describes a sort of new uncertainty principle for distance measurements.
4.2 Spacetime foam, distance fuzziness and interferometric noise
The scenarios for spacetime fuzziness that are most studied from a quantumspacetime perspective are intuitively linked to the notion of “spacetime foam”, championed by Wheeler and studied extensively in the quantumgravity literature, more or less directly, for several decades (see, e.g., Refs. [547, 203, 178, 281, 150, 250, 553]). From a modern perspective one is attempting to characterize the physics of matter particles as effectively occurring in an “environment” of shortdistance quantumgravitational degrees of freedom. And one may expect that for propagating particles with wavelength much larger than the Planck length, when it may be appropriate to integrate out these shortdistance quantumgravitational degrees of freedom, the main residual effect of shortdistance gravity would indeed be an additional contribution to the fuzziness of worldlines.
While the only direct/deductive derivations of such results are for 3D quantum gravity, it is natural to take that as a starting point for the study of real 4D quantum gravity, whereas analogous results are still unavailable. And a sizable literature has been devoted to the search of possible experimental manifestations of “spacetime foam”. Several subsections of this section concern related phenomenological proposals. I start with spacetimefoam test theories, whose structure renders them well suited for interferometric tests.
4.2.1 Spacetime foam as interferometric noise
The first challenge for a phenomenology investigating the possibility of spacetime foam originates in the fact that Wheeler’s spacetime foam intuition, while carrying strong conceptual appeal, cannot on its own be used for phenomenology, since it is not characterized in terms of observable properties. The phenomenology then is based on test theories inspired by the spacetimefoam intuition.
A physical/operative definition of at least one aspect of spacetime foam is given in Refs. [51, 54, 53, 433] and is well suited for a phenomenology based on interferometry^{27}. According to this definition the fuzziness/foaminess of a spacetime is established[51, 54, 53, 433] on the basis of an analysis of strain noise^{28} in interferometers set up in that spacetime. In achieving their remarkable accuracy, modern interferometers must deal with several classicalphysics strain noise sources (e.g., thermal and seismic effects induce fluctuations in the relative positions of the test masses). And importantly strain noise sources associated with effects due to ordinary quantum mechanics are also significant for modern interferometers (the combined minimization of photon shot noise and radiation pressure noise leads to a noise source that originates from ordinary quantum mechanics [486]). One can give an operative definition [51, 53] of fuzzy/foamy spacetime in terms of a corresponding additional source of strain noise. A theory in which the concept of distance is fundamentally fuzzy in this operative sense would be such that the readout of an interferometer would still be noisy (because of quantumspacetime effects) even in the idealized limit in which all classicalphysics and ordinaryquantummechanics noise sources are completely eliminated/subtracted.
4.2.2 A crude estimate for laserlight interferometers
Before even facing the task of developing test theories for spacetime foaminess in interferometry it is best to first check whether there is any chance of using realistic interferometric setups to uncover effects as small as expected if introduced at the Planck scale. A first encouraging indication comes from identifying the presence of a huge amplifier in modern interferometers: a wellknown quality of these modern interferometers is their ability to detect gravity waves of amplitude ∼ 10^{−18} m by carefully monitoring distances of order ∼ 10^{4} m, and this should provide opportunities for an “amplifier” that is of order 10^{22}.
In modern interferometers such as LIGO [9, 1] and VIRGO [157, 12] the power spectral density of the noise is controlled at a level of Σ(ω) ∼ 10^{−44} Hz^{−1} at observation frequencies ω of about 100 Hz, and in turn this (also considering the length of the arms of these modern interferometers) implies [9, 1, 157, 12] that for a gravity wave with 100 Hz frequency the detection threshold is indeed around 10^{−18} m.
The challenge here for quantumspacetime phenomenologists is to characterize the relevant quantumspacetime effects in terms of a novel contribution Σ^{[QG]} (ω) to the power spectral density of the noise. If at some point experimentalists manage to bring the total noise Σ(ω), for some range of observation frequencies ω, below the level predicted by a certain quantumspacetime test theory, then that test theory will be ruled out.
Is there any hope for a reasonable quantumspacetime test theory to predict noise at a level comparable to the ones that are within the reach of modern interferometry? Well, this is the type of question that one can only properly address in the context of models, but it may be valuable to first use dimensional analysis, assuming the most optimistic behavior of the quantumspacetime effects, and check if the relevant order of magnitude is at all providing any encouragement for the painful (if at all doable) analysis of the relevant issues in quantumspacetime models.
To get what is likely to be the most optimistic (and certainly the simplest, but not necessarily the most realistic) Planckscale estimate of the effect, let us assume that quantumspacetime noise is “white noise”, Σ^{[QG]}(ω) = Σ_{0} (frequency independent), so that it is fully specified by a single dimensionful number setting the level of this white noise. And since Σ carries units of Hz^{−1} one easily notices [54] a tempting simple naive estimate in terms of the Planck length and the speedoflight^{29} scale: Σ_{0} ∼ L_{ p }/c, which, since L_{ p }/c ∼ 10^{−44} Hz^{−1}, encouragingly happens to be just at the mentioned level of sensitivity of LIGOVIRGOtype interferometers. This provides some initial encouragement for a phenomenology based on interferometric noise, though only within the limitations of a very crude and naive estimate.
4.2.3 A simpleminded mechanism for noise in laserlight interferometers
My next task is going beyond assuming for simplicity that the quantumspacetime noise be white and beyond adopting a naive dimensionalanalysis estimate of what could constitute a Planckscale level of such a noise. The ultimate objective here would be to analyze an interferometer in the framework of a compelling quantumspacetime theory, but this is beyond our capabilities at present. However, we can start things off by identifying some semiheuristic pictures (the basis for a test theory) with effects introduced genuinely at the Planck scale that turn out to produce strain noise at the level accessible with modern interferometers.
Having in mind this objective, let us take as a starting point for a first naive picture of spacetime fuzziness the popular arguments suggesting that the Planck scale should also set some absolute limitation on the measurability of distances. And let us (optimistically) assume that this translates to the fact that any experiment in which a distance L plays a key role (meaning that one is either measuring L itself or the observable quantity under study depends strongly on L) is affected by a mean square deviation \(\sigma _L^2\).
It is noteworthy that \(\sigma _L^2 \simeq {L_p}T\) can be motivated independently (without having in mind the idea of such effective spacetime fluctuations) on the basis of some aspects of the quantumgravity problem [50]. And the study of certain quantumspacetime pictures that have been of interest to the quantumgravity community, such as the κMinkowski noncommutative spacetime of Eq. (4), provide some support for this randomwalk picture: from [x_{ j }, t] = iL_{ P }x_{ j } one could guess roughly a law of the form \(\sigma _x^2 \sim \delta x\delta t \sim {L_P}x\).
Before I get to that issue, let me stress that there is a possible source of confusion for terminology (and content) in the literature. In the quantumgravity literature there has been some discussion for several years of “holographyinspired noise” in the sense of my Eq. (49) and of Refs. [433, 430, 170]. More recently, a different mechanism for quantumspacetimeinduced noise, also labeled as “holography inspired”, was proposed in a series of papers by Hogan [287, 286, 288]. There is no relation between the two “holographyinspired” proposals for quantumspacetimeinduced interferometric noise. I do not think it is particularly important at the present time to establish which (if either) of the two proposals is more directly inspired by holography. I must instead stress that the holographic noise of Refs. [433, 430, 170] is a rather mature proposal, centered on Eq. (49) and meaningful at least as a quantumspacetime test theory in the sense I just described. Instead it is probably fair to describe the alternative version of holographic noise more recently proposed in Ref. [287, 286, 288] as a young proposal still looking for some maturity: it does not amount to any howeverwild variant of the description of interferometric noise I summarized here, and actually it is claimed [288] to be immune not only to the sort of interferometric noise I discussed in this Section but also to all other effects that have been typically associated with spacetime quantization in the literature. It would be a quantumspacetime picture whose effects “can only be detected in an experiment that coherently compares transverse positions over an extended spacetime volume to extremely high precision, and with high time resolution or bandwidth” [288]. Evidently some work is still needed on the conceptual aspects (as a rigorous theory of spacetime quantization) and on the phenomenological aspects (as a computably predictive and broadly applicable test theory of spacetime quantization) of this proposal. Only time will tell if this present lack of maturity is due to intrinsic unsurmountable limitations of the proposal or is simply a result of the fact that the proposal was made only rather recently (so there was not much time for this maturity to be reached). I should note that at some point, in spite of its lack of maturity, this proposal started to attract some pronounced interest in relation to reports by the GEO600 interferometer [550] of unexplained excess noise [373]: it had been claimed [286] that Hogan’s version of holographic noise could match exactly the anomaly that was being reported by GEO600. However, it appears that experimenters at GEO600 have recently achieved a better understanding of their noise sources, and no unexplained contribution is at this point reported (this is at least implicit in Ref. [462] and is highlighted at http://www.aei.mpg.de/hannoveren/05research/GEO600/). The brief season of the “GEO600 anomaly” (at some point known among specialists as the “mystery noise”) is over.
4.2.4 Insight already gained and ways to go beyond it
At the present time the “state of the art” of phenomenologicallyspendable descriptions of Planckscaleinduced strain noise does not go much beyond the simpleminded estimates I just described in relation to Eqs. (47), (49), and (50). But some lessons were nonetheless learned, as usually happens even with the most humble phenomenology. And these lessons do point toward some directions worthy of exploration in the future. In this section I highlight some of these lessons and possible future developments.
Among the few steps of simple derivation, which I described in Section 4.2.3, evidently much scrutiny should be particularly directed toward the assumption \({\Sigma ^{[{\rm{QG}}]}} = \Sigma _L^{[{\rm{QG}}]}/{L^2}\): I motivated some candidate forms for \(\Sigma _L^{[{\rm{QG}}]}\) using essentially the sort of arguments that usually allow us to establish uncertainty principles for single particles, such as the ones taking as a starting point a postulated noncommutativity of singleparticle coordinates; however, the strain noise Σ^{[QG]} relevant for our interferometers is not at all a singleparticle feature. Let me use the example of randomwalk fuzziness for illustrating how the relationship between singleparticle quantumspacetime arguments and interferometric strain noise could be more subtle than assumed in \({\Sigma ^{[{\rm{QG}}]}} = \Sigma _L^{[{\rm{QG}}]}/{L^2}\). For this, I shall follow Ref. [57] (a similar thesis was also reported in Ref. [170]). I specialize the more general idea of randomwalk quantumspacetime fuzziness in the sense of assuming that each single photon in an interferometer experiences a randomwalk path: a random Plancklength fluctuation per Plancktime would affect the path of each photon of the beam. This would imply in particular that as a photon goes from one mirror of the interferometer to the other, over a distance L, it reaches its destination with an uncertainty corresponding to \(\sigma _L^2 \sim {L_P}T \sim {L_P}L\). However, the interferometer (and this is key to its outstanding sensitivity) does not depend on determining the position of each single photon in the beam: on the contrary the key observable is the average position of the photons composing the beam, which may be viewed as the putative “position of the mirror” (when such a beam reaches the mirror). If L is now viewed as the distance between positions of mirrors defined in this way, rather than as the distance of propagation of an individual photon, then evidently the result is an estimate \(\sigma _L^2 \sim {L_P}T \sim {L_P}L/{N_\gamma}\), where N_{ γ } is the (very large!) number of photons contributing to each such determination of the “position of the mirror”.
This observation is not specific to the randomwalk scenario. A similar N_{ γ } suppression could naturally be expected for the holographic noise scenario of Eq. (49). As discussed in the previous Section 4.2.3, that holographic noise scenario would be safe from LIGO/VIRGO bounds even without the N_{ γ } suppression. (In some sense that holographic noise scenario would turn into unpleasantly “too safe from LIGO/VIRGO”, i.e., probably beyond the reach of any foreseeable interferometric experiment, if it were to take into account the plausible N_{ γ } suppression).
Concerning the scenario for weak quantumspacetimeinduced fuzziness, the one of Eq. (50), contemplating the possibility of an N_{ γ } suppression is of mere academic interest: those noise levels are so low, even without the possible additional N_{ γ } suppression, that we should exclude their testability for the foreseeable future.
But for randomwalk noise and for the holographicnoise scenario of Eq. (49) this issue of a possible N_{ γ } suppression needs to be investigated and understood. This is probably not for the LIGO/VIRGO season: LIGO and VIRGO have not found any excess noise so far, and at this point it is unlikely they will ever find it. But a completely new drawing board for phenomenology would materialize with the advent of LISA [282]: LISA will operate at lower observational frequencies ω than LIGO/VIRGOtype interferometers, which is important from the quantumspacetime perspective since both randomwalk noise, as described by Eq. (47), and the holographicnoise scenario of Eq. (49) predict effects that increase at lower observational frequencies.^{30} The outcome of such LISA quantumspacetimenoise studies may then depend on issues such as the possible N_{ γ } suppression.
I should also stress that the analysis of these opportunities for quantumspacetime phenomenology from experiments operating at low observational frequencies ω, is perhaps the most significant and most robust conceptual achievement of the sort of phenomenology of spacetime foam that I am discussing in this Section. When these pictures were first proposed it was seen by many as a total surprise that one could contemplate Planckscale effects at frequencies of observation of only 100 Hz. The naive argument goes something like “Planckscaleinduced noise must be studied at Planck frequency”, and the Planck frequency is E_{ p }/ℏ ∼ 10^{43} Hz. However, in analyzing actual pictures of quantumspacetime fuzziness, even the simpleminded ones described above, one becomes familiar with wellknown facts establishing (and we should expect this lesson to apply even to more sophisticated picture of quantumspacetimeinduced fuzziness) that discrete fluctuation mechanisms tend to produce very significant effects at low observational frequencies ω, with typical behaviors of the type ω^{−α}, even when their charateristic time scale is ultrashort.
4.2.5 Distance fuzzyness for atom interferometers
Since the phenomenology of the implications of spacetime foam for interferometry is at an early stage of development, at the present time it may be premature to enter into detailed discussions of what type of interferometry might be best suited for uncovering quantumspacetime/Planckscale effects. Accordingly, in Section 4.2 I focus by default on the simplest case of interferometric studies, the one using a laserlight beam. However, in recent times atom interferometry has reached equally astonishing levels of sensitivity and for several interferometric measurements it is presently the best choice. Laserlight interferometry is still preferred for certain wellestablished techniques of interferometric studies of spacetime observables, as in the case of searches for gravity waves, and the observations I reported above for the phenomenology of strain noise induced by quantumspacetime effects appear to be closely linked to the issues encountered in the search for gravity waves. However, it seems plausible that soon there will be some atominterferometry setups that are competitive for gravitywave searches (see, e.g., Refs. [526, 208]). This in turn might imply that searches of quantumspacetimeinduced strain noise could rely on atom interferometry.
The alternative between light and matter interferometry might prove valuable at later more mature stages of this phenomenology. It is likely that different test theories will give different indications in this respect, so that atom interferometry might provide the tightest constraints on some spacetimefoam test theories, whereas laserlight interferometry might provide the best constraints on other spacetimefoam test theories. A key aspect of the description of Planckscale effects for atom interferometry to be addressed by the test theories (and hopefully, some day, by some fullydeveloped quantumspacetime/quantumgravity theories) is the role played by the mass of the atoms. With respect to laserlight interferometry, the case of atom interferometry challenges us with at least two more variables to be controlled at the theory level, which are the mass of the atoms and their compositeness. How do these two aspects of atom interferometry interface with the quantumspacetime features that are of interest here? Do they effectively turn out to introduce suppressions of the relevant effects or on the contrary could they be exploited to see the effects? For none of the quantumspacetime models that are presently studied have we reached a level of understanding of physical implications robust enough for us to answer confidently these questions. Perhaps we should also worry about (or exploit) another feature that is in principle tunable in atom interferometry, which is the velocity of the particles in the beam.
4.3 Fuzziness for waves propagating over cosmological distances
Interferometric studies of spacetimefoam are another rare example of tests of quantumspacetime effects that can be conducted in a controlled laboratory setup (also see Section 3.13). Astrophysics may turn into the most powerful arena for this type of study. Indeed, the studies I discussed in the previous Section 4.2, which started toward the end of the 1990s, inspired a few years later some followup studies from the astrophysics side. As should be expected, the main opportunities come from observations of waves that have propagated over very large distances, thereby possibly accumulating a significant collective effect of the fuzziness encountered along the way to our detectors.
4.3.1 Time spreading of signals
An implication of distance fuzziness that one should naturally consider for waves propagating over large distances is the possibility of “time spreading” of the signal: if at the source the signal only lasted a certain very short time, but the photons that compose the signal travel a large distance L, affected by uncertainty \(\sigma _L^2\), before reaching our detectors the observed spread of times of arrival might carry little trace of the original time spread at the source and be instead a manifestation of the quantumgravityinduced σ_{ L }. If the distance L is affected by a quantumspacetime uncertainty σ_{ L } then different photons composing the signal will effectively travel distances that are not all exactly given by L but actually differ from L and from each other up to an amount σ_{ L }.
Again, it is of particular interest to test laws of the type discussed in the previous Section 4.2, but it appears that these effects would be unobservably small even in the case that provides the strongest effects, which is the randomwalk ansatz \(\sigma _L^2 \simeq {L_P}L \simeq {L_P}T\) (assuming ultrarelativistic particles, for which L is at least roughly equal to the time duration T of the journey). To see this let me consider once again gammaray bursts, which often travel for times on the order of 10^{17} s before reaching Earth detectors and are sometimes characterized by time structures (microbursts within the burst) that have durations as short as 10^{−3} s. Values of \(\sigma _L^2\) as small as \(\sigma _L^2 \sim {c^2}{10^{ 8}}{{\rm{s}}^2}\sigma _L^2 \sim {c^2}{10^{ 27}}{{\rm{s}}^2}\) could be noticeable in the analysis of such bursts. However, the estimate \(\sigma _L^2 \simeq c{L_p}T\) only provides \(\sigma _L^2\sim{c^2}{10^{ 27}}{{\rm{s}}^2}\) and is, therefore, much beyond our reach.
I shall comment in Section 4.8 on an alternative formulation of the phenomenology of quantumspacetimeinduced worldline fuzziness, the one in Ref. [490] inspired by the causalset approach (the approach on which Section 4.8 focuses).
4.3.2 Fuzziness from nonsystematic symmetrymodification effects
As an alternative way to model spacetime fuzziness, there has been some interest [431, 72, 37] in the possibility that there might be effects resembling the ones discussed in Section 3, which are systematic deviations from the predictions of Poincaré symmetry, but are “nonsystematic” in the sense discussed at the beginning of this section. The possibility of fuzziness of particle worldlines governed by E/E_{ p }, mentioned in the previous Section 4.3.1, is an example of such nonsystematic violations of Poincaré symmetry.
These speculations are not on firm ground on the theory side, in the sense that there is not much in support of this among available results on actual analysis of formalizations of spacetime quantization. But it is legitimate to expect that this might be due to our limited abilities in mastering these complex formalisms. After all, as suggested in Ref. [431], if spacetime geometry is fuzzy then it may be inevitable for the operative procedures that give sense to the notion of energy and momentum of a particle to also be fuzzy.
This sort of picture could have tangible observational consequences. For example, it can inspire, as suggested in Refs. [74, 57, 72], scenarios such that spacetime fuzziness effectively produces an uncertainty in the velocity of particles of order E/E_{ p }. This would give rise to a magnitude of these nonsystematic effects comparable to the one discussed in Section 3.8 for the corresponding systematic effects. After a journey of ∼ 10^{17} s the acquired fuzziness of arrival times could be within the reach [74] of suitably arranged gammarayburst studies. However, there is no significant effort to report here on establishing bounds following this strategy.
This describes a single photonphoton collision taking into account the nonsystematic effects. One should next consider that for a hard photon traveling toward our Earth detectors from a distant astrophysical source there are many opportunities to collide with soft photons with energy suitable for pair production to occur (the mean free path is much shorter than the distance between the source and the Earth). Thus, one expects [72, 37] that even a small probability of producing an electronpositron pair in a single collision would be sufficient to lead to the disappearance of the hard photon before reaching our detectors. The probability is small in a single collision with a soft background photon, but the fact that there are, during the long journey, many such pairproduction opportunities renders it likely that in one of the many collisions the hard photon would indeed disappear into an electronpositron pair. Therefore, for this specific scheme of nonsystematic effects it appears that a characteristic prediction is that the detection of such hard photons from distant astrophysical sources should start being significantly suppressed already at the energy level described by (57), which is below the threshold corresponding to the classicalspacetime kinematics.
It is interesting [57, 72, 74] to contemplate in this case the possibility that systematic and nonsystematic effects may both be present. It is not unnatural to arrange the framework in such a way that the systematic effects tend to give higher values of the threshold energy, but then the nonsystematic effects would allow (with however small probability) configurations below threshold to produce the electronpositron pair. And for very large propagation distances (very many “target soft photons” available) the nonsystematic effect can essentially erase [72] the systematic effect (no noticeable upward shift of the threshold).
I illustrated the implications of nonsystematic effects within a given scenario and specifically for the case of observations of gamma rays from blazars. One can implement the nonsystematic effects in some alternative ways and the study of the observational implications can consider other contexts. In this respect I should bring to the attention of my readers the studies of nonsystematic effects for ultrahighenergy cosmic rays reported in Refs. [37, 310, 106].
Combinations of systematic and nonsystematic effects can also be relevant [57, 74] for studies of the correlations between times of arrival and energy of simultaneouslyemitted particles. For that type of study both the systematic and the nonsystematic effects could leave an observable trace [74] in the data, codified in the mean arrival time and the standard deviation of arrival times found in different energy channels.
4.3.3 Blurring images of distant sources
The two examples of studies in astrophysics of quantumspacetimeinduced distance fuzziness I discuss in Sections 4.3.1 and 4.3.2 have only been moderately popular. I have left as last the most intensely studied opportunity in astrophysics for quantumspacetimeinduced distance fuzziness. These are studies essentially looking for effects blurring the images of distant sources.
It is interesting that these studies were started by Ref. [367], which cleverly combined some aspects of Refs. [51, 54, 53, 433], providing the main concepts for the proposal summarized in Section 4.2, and some aspects of Ref. [66], providing the main concepts for the proposal summarized in Section 3.8. Ref. [367] was interested in the same phenomenology of distance fuzziness introduced and analyzed for controlled interferometers in Refs. [51, 54, 53, 433], but looked for opportunities to perform analogous tests using the whole Universe as laboratory, in the sense first introduced in Ref. [66].
Gradually over the last decade this became a rather active research area, as illustrated by the studies reported in Refs. [367, 434, 189, 464, 363, 171, 167, 402, 514, 403, 404, 520, 456, 405].
The phenomenological idea is powerfully simple: effects of quantumspacetimeinduced spacetime fuzziness had been shown [51, 54, 53, 433] to be potentially relevant for LIGO/VIRGOlike (and LISAlike) intereferometers, exploiting not only the distancemonitoring accuracy of those interferometers, but also the fact that such accuracy on distance monitoring is achieved for rather large terrestrial distances. Essentially the Universe gives much larger distances for us to monitor [66], and although we can monitor them with accuracy inferior to the one of a LIGO/VIRGOlike intereferometer, on balance, the astrophysics route may also be advantageous also for studies of quantumspacetimeinduced spacetime fuzziness [367].
Evidently, this phenomenology still has a few too many quantitative details subject to further scrutiny and a few too many alternative scenarios. This is the result of the fact that work on actual formalizations of spacetime quantization, while encouraging the general intuitive picture, has been unable to provide detailed guidance. And the heuristic arguments based on these preliminary studies have been unable to narrow the range of possibilities. But pursuing this path further appears to be an exciting opportunity for quantumspacetime phenomenology, and we should, therefore, persevere. In particular, based on the (however alternative) estimates given by Eqs. (61), (62), and (63), several authors (see, e.g., Refs. [171, 514, 520]) have concluded that a phenomenology based on blurring of the images of distant sources can provide Planckscale sensitivity for a rather broad range of possible phenomenological test theories and for values of α significantly greater than 1/2, possibly [520] going all the way up to values of α close to 1. In Ref. [514] one even finds a preliminary data analysis suggesting that for observations of quasars there might be a trend towards lower observed Strehl ratios with increasing redshift, which would provide encouragement for the hope of discovering quantumspacetimeinduced image blurring.
The main opportunities appear to be provided by observations of distant quasars [171, 514, 520], whose dimensions are small and are rather abundantly observed at high redshift.
4.4 Planckscale modifications of CPT symmetry and neutralmeson studies
Investigations of spacetime symmetries and distance fuzziness are evidently relevant for some of the core features of the idea of spacetime quantization. My next task concerns CPTsymmetry tests, and the possibility that indirectly some scenarios for the quantization of spacetime might affect CPT symmetry.
A complication, but also an opportunity, for quantumspacetimemotivated tests of CPT symmetries comes from the fact that CPT symmetry should be and is tested independently of the quantumspacetime motivation. From this perspective the situation is somewhat analogous to that discussed earlier concerning quantumspacetimemotivated tests of Lorentz symmetry. The quantum spacetime literature can provide special motivation for probing CPT symmetry in certain specific ways, but there is already plenty of motivation, even without quantumspacetime research, for testing CPT symmetry as broadly as possible [389, 439, 234].
Also, in this case, the Standard Model Extension provides a much appreciated and widely adopted formalization, finding a good balance between the desire of searching for violations of CPT symmetry (and/or, as mentioned, violations of Lorentz symmetry) within the confines of quantum field theory but allowing for both effects that have been discussed from the quantumspacetime perspective and effects for which so far there is no quantumspacetime motivation. I shall focus here on the hypothesis of quantumspacetimeinduced and Planckscalemagnitude CPT violation effects, so I shall not review the broad subject of CPT violation within the Standard Model Extension, for which readers can find valuable reviews and perspectives in Refs. [345, 117, 180, 339, 299, 341, 346] (see also parts of Ref. [395]).
Another issue that should always be kept in mind in relation to CPT symmetry is the fact that it can be derived as a theorem for local quantum field theories with Lorentz invariance. In approaches based on local field theory, it is natural to perform combined studies of CPT and Lorentz symmetry.^{31} However, the notion of spacetime quantization at the Planck scale involves some aspects of nonlocality (at least the notion of points that coincide with accuracy better than the Planck length is typically abandoned) and in most quantumspacetime studies of the fate of CPT symmetry the expectation is that these aspects of nonlocality may be primarily responsible for the conjectured violations of CPT symmetry.
I shall not attempt to summarize here the results on violations of CPT symmetry arising from spacetime quantization not introduced at the Planck scale (but rather at some much lower scale), for which readers can find valuable starting points to the related literature in Refs. [162, 43, 417, 496, 28] and references therein.
Consistent with the scope of this review, I shall focus exclusively on scenarios for violations of CPT symmetry based on nonclassicality (“quantization”) of spacetime introduced at the Planck scale. As a result of some technical challenges, mentioned in Section 2.2.2, this literature can only rely on preliminary theory results, but does suggest convincingly that Planckscale sensitivity to quantumspacetimeinduced violations of CPT symmetry is within our reach.
4.4.1 BrokenCPT effects from Liouville strings
In the case of the test of CPT symmetry it is easier for me to start by discussing the availability of Planckscale sensitivity, postponing briefly some comments on test theories based on the idea of spacetime quantization.
There is a sizable literature establishing that CPT symmetry can be tested with Planckscale sensitivity in the neutralkaon and the neutralB systems (see, e.g., Refs. [219, 220, 298, 108]). It turns out that in these neutralmeson systems there are plenty of opportunities for Planckscale departures from CPT symmetry to be amplified. In particular, the neutralkaon system hosts the peculiarly small mass difference between longlived and shortlived kaons M_{ L } − M_{ S }/M_{ L,S } ∼ 7·10^{−15} and other small numbers naturally show up in the analysis of the system, such as the ratio Γ_{ L } − Γ_{ S }/M_{ L,S } ∼ 1.4 · 10^{−14}. And for certain types of departures from CPT symmetry the inverse of one of these small numbers amplifies the small CPTviolation effect [219, 220, 298, 108]. In particular, this mechanism turns out to provide sufficient amplification for Planckscale effects, inducing a difference of order \(M_{{K^0}}^2/{E_p}\) between the terms on the diagonal of the \({K^0},{\bar K^0}\) mass matrix (exact classical CPT symmetry would require the terms on the diagonal to be identical). It should be noticed that \({M_{{K^0}}}/{E_p} \sim {10^{ 19}}\), which is not overwhelmingly smaller than M_{ L } − M_{ S }/M_{ L,S } ∼ 7·10^{−15}.
A much studied quantumspacetime description of violations of CPT symmetry is centered on the mentioned Liouvillestrings approach [221, 220], particularly with its description of spacetime foam and its nonclassical description of time, involving a nontrivial role for the Liouville field [224]. This model is, in particular, the reference for the analysis of Planckscale limits on quantumspacetimeinduced CPT violation reported by the CPLEAR collaboration on the basis of studies of neutral kaons [13] (also see the related results reported using neutralkaon data gathered at the particlephysics laboratory in Frascati [13, 534, 205]). Interestingly, the Liouvillestring model hosts both departures from CPT symmetry and decoherence, and I find it most convenient to discuss it in the later part of this section devoted to decoherence studies.
Let me highlight a recent development that is in part inspired by these Liouvillestring studies. It was recently observed (primarily in Refs. [112, 113]) that quantumspacetime scenarios with violations of CPT symmetry might also require some corresponding modifications of the recipe for obtaining multiparticle states from singleparticle states for identical particles. This may apply in particular to the neutralkaon \({K_0}  {\bar K_0}\) system, since standard CPT transformations take K_{0} into \({\bar K_0}\) but violations of CPT symmetry are likely to also induce a modification of the link between K_{0} and \({\bar K_0}\).
Stringent constraints on ω can be placed by performing measurements of the chain of processes ϕ → KK → XY, in which first the ϕ meson decays into a pair of neutral kaons and then one of the kaons decays at time t_{1} into a final state X, while the other kaon decays at time t_{2} into a final state Y. By following this strategy the KLOE experiment [534, 522] at DAΦNE is setting [204, 205] experimental limits on ω at the level 10^{−3} (Re(ω) < 10^{−3}, Im(ω) < 10^{−3}).
It is not easy at present to establish robustly what level of sensitivity to ω could really amount to Planckscale sensitivity, but it is noteworthy that there are semiquantitative/semiheuristic estimates based on a certain intuition for spacetime foam suggesting [112, 113, 398] that sensitivities in the neighborhood of ω ∼ 10^{−3}, ω ∼ 10^{−4} could already be significant.
4.4.2 Departures from classical CPT symmetry from spacetime noncommutativity at the Planck scale
Considering that, as mentioned, neutralkaon experiments at Φ factories are now sensitive at the level δM ∼ 10^{−18} GeV, one infers a sensitivity to this type of candidate quantumgravity effect that, for kaons of momenta of about 110 MeV (at the ϕ resonance), corresponds to a sensitivity to values of λ around 10^{−32} m, i.e., not far (just 3 orders of magnitude away) from the Planck scale. Because of the premium on high momenta of this scenario, better limits could be set using experiments with highmomentum kaons Fermilab’s E731 [554, 450]. And studies with neutral B mesons of relatively high momenta could also be valuable from this perspective.
However, we are at a very early stage of understanding of the fate of CPT symmetry in these spacetimes with quantization at the Planck scale. Specifically, for the case of κMinkowski spacetime, analyses such as the one in Ref. [70] suggest that CPT symmetry is deformed rather than broken/lost. Indeed, in κMinkowski the anomalies one can presently preliminarily see for CPT symmetry are all linked to the peculiarity of Pparity transformations. It appears that in κMinkowski Pparity transformations for momenta should not take a momentum \(\vec p\) into \( \vec p\), but rather \(\vec p \rightarrow \ominus \vec p\), where \(\ominus \vec p\) denotes the “antipode operation”: \(\ominus \vec p \equiv  \vec p{e^{ \lambda {p_0}}}\) (where λ denotes again the κMinkowski noncommutativity length scale).
4.5 Decoherence studies with kaons and atoms
4.5.1 Spacetime foam as decoherence effects and the “α, β, γ test theory”
As stressed earlier in this review the idea of “spacetime foam” appears to appeal to everyone involved in quantumspacetime research, but this is in part due to the fact that this idea is not really well defined, not by the qualitative intuitive picture proposed by Wheeler. In order to set up a phenomenology for effects induced by this spacetime foam, it is necessary to provide for it physical/experimentallymeaningful characterizations. I already discussed one possible such characterization, given in terms of distance fuzziness and associated strain noise for interferometry. Another attempt to physically characterize spacetime foam can be found in Refs. [220, 221] (other valuable perspectives on this subject can be found in Refs. [108, 251]), focusing on the possibility that the rich dynamical properties of spacetime foam might act as a decoherenceinducing environment.
It should be stressed that this test theory necessarily violates CPT symmetry whenever δH ≠ 0. Additional CPT violating features may be introduced in the ordinaryquantummechanics Hamiltonian H, by allowing for differences in masses and/or differences in widths between particles and antiparticles. Therefore, this test theory is an example of a framework that could be used in a phenomenology looking simultaneously for departures from CPT symmetry of types admissible within ordinary quantum mechanics and for departures from CPT symmetry that require going beyond quantum mechanics (by allowing for decoherence). It is noteworthy that the two types of CPT violation (within and beyond quantum mechanics) can be distinguished experimentally.
where the indices S, L, I stand respectively for shortlived, longlived, interference, and the combination \(\varsigma \equiv 1  {C_I}/{\sqrt {{C_S}C_L}}\) provides a good phenomenological characterization of the amount of decoherence induced in the system [398].
Using data gathered by the CPLEAR experiment [13], one can set bounds on α, β, γ at the levels α ∼ 10^{−17} GeV, β ∼ 10^{−19} GeV, and γ ∼ 10^{−21} GeV. A comparable limit on γ has been placed by DAΦNE’s KLOE experiment, and in that case the analysis was based [398, 534, 205] on entangled kaon states.
I should stress that this is clearly a quantumspacetime picture (at least in as much as it models spacetime foam) and the objective of the associated research program is to introduce quantum/foamy properties of spacetime at the Planck scale, but it is at present still unclear which levels of sensitivity to α, β, γ would correspond to foaminess of spacetime at the Planck scale. We are still unable to perform a derivation starting from foaminess at the Planck scale and deriving corresponding values for α, β, γ. It is nonetheless encouraging that the present experimental limits on these (dimensionful) parameters are in a neighborhood of the Planckscaleinspired quantification m_{ K }/E_{ p } ∼ 10^{−19} (but it should be noticed that as much “Planckscale inspiration” should be attributed, for example, to the scale \(m_K^2/E_p^2 \sim {10^{ 38}}\)).
4.5.2 Other descriptions of foaminduced decoherence for matter interferometry
Another attempt to characterize spacetime foam as a decoherenceinducing medium was developed by Percival and collaborators (see, e.g., Refs. [452, 453, 454]). This approach assumes that ordinary quantum systems should all be treated as open systems due to neglecting the degrees of freedom of the spacetime foam, but, rather than a formalization using density matrices, Refs. [452, 453, 454] adopt a formalism in which an open quantum system is represented by a pure state diffusing in Hilbert space. The dynamics of such states is formulated in terms of “Primary state diffusion”, an alternative to quantum theory with only one free parameter, a time scale τ_{0}, which one can set to be the Planck time L_{ p }/c.
A key characteristic of this picture would be [454] a suppression of the interference pattern for interferometers using beams of massive particles (such that the original beam is first split and then reunited to seek an interference pattern). The suppression increases with the mass of the particles, so it could more easily be tested with atom interferometers (rather than neutron interferometers). Unfortunately, a realistic analysis of an interferometer in the relevant primarystatediffusion formalism is much beyond the level of answers one is (at least presently) able to extract from the primarystatediffusion setup. Ref. [454] considered resorting to some simpleminded simplifications, including the assumption that the Hamiltonian be given by the mass together with projectors onto the wave packets in the arms of the interferometer, neglecting the kineticenergy terms. Within such simplifications one does find that values of τ_{0} at or even a few orders of magnitude below the Planck time would leave an observably large trace in modern atom interferometers. However, these simplifications amount to a model of the interferometer that is much too crude (as acknowledged by the authors themselves [454]) and this does not allow us to meaningfully explore the possibility of genuine Planckscale sensitivities being achieved by this strategy. Note that by taking τ_{0} as the Planck time it is not obvious that the effects are being introduced genuinely at the Planck scale, since the nature of the effects is characterized not only by τ_{0} but also by other aspects of the framework, such as the description of the fluctuations. Moreover, even if all other aspects of the picture were understood, the crudity of the model used for matter interferometers would still not allow us to investigate the Planckscalesensitivity issue.
Recently, Ref. [498] and Ref. [541] presented somewhat different pictures of quantumgravityinduced decoherence for atom interferometers. Several aspects of the Percival setup are maintained but different interpretations are applied in some aspects of the analysis. For example, Ref. [541] removes some of the assumptions adopted by Percival and collaborators, particularly in relation to the description of the “quantum fluctuations” of the metric, and proposes an estimate of the amount of suppression of the interference pattern,^{32} that is perhaps more intriguing from a phenomenology perspective, since it would suggest that the effect is just beyond present sensitivities (but within the reach of sensitivities achievable by atom interferometers in the notsodistant future). For these recent proposals one is still (for reasons analogous to these just discussed for the Percival approach) unable to meaningfully explore the issue of “genuine Planckscale sensitivity”, but they may represent a step in the direction of a more detailed description of spacetime foam, if intended as fluctuations of the metric.
4.6 Decoherence and neutrino oscillations
The growing evidence for ordinaryphysics neutrino oscillations, which one expects to be much more significant than the foaminduced ones, provides a formidable challenge for the phenomenology based on these test theories for foaminduced decoherence in the neutrino sector. Some preliminary ideas on how to overcome this difficulty are described in Ref. [400]. From the strict quantumspacetimephenomenology perspective of requiring one to establish that the relevant measurements could be sensitive to effects introduced genuinely at the Planck scale, these neutrinodecoherence test theories must face challenges already discussed for a few other test theories: there is at present no rigorous/constructive derivation of the values of the parameters of these test theories from a description (be it a full quantumspacetime theory or simply a toy model) of effects introduced genuinely at the Planck scale, so one can only express these parameters in terms of the Planck scale using some dimensionalanalysis arguments.
4.7 Planckscale violations of the Pauli Exclusion Principle
A case for Planckscale sensitivity was recently made [97, 99] for the hypothesis of possible violations of the Pauli Exclusion Principle. This has still not been metabolized by an appreciablywide quantumgravity community, but it certainly deserves to be highlighted briefly in this review, since the chances for gradually gaining a strong impact on quantumspacetime phenomenology are rather high.
As observed already a few times in this review, the spinstatistics theorem assumes a classical spacetime with ordinary locality. Therefore, it is legitimate to speculate that small departures from the implications of the spinstatistics theorem may arise in a quantum spacetime. Some earlier suggestions that this might be the case can be found, e.g., in Refs. [98, 163, 86], but the setup then was not such that one could see an emerging case for Planckscale sensitivity.
It is rather easy to show that this form of noncommutativity imposes a corresponding modification of the “flip operator”, i.e., the operator that is used for symmetrization (antisymmetrization) purposes in the commutativespacetime case. In turn this gives rise to a deformed description of bosons and fermions. And the end result is that certain transitions that would be Pauliforbidden in a commutative spacetime are actually allowed, although at a small rate (suppressed by the smallness of χ).
Computing these rates on the basis of Eq. (73) is at present only possible by relying on an uncomfortable number of simplifying assumptions [97, 99], but the outcome is nonetheless intriguing since it suggests that sensitivity to values of χ on the order of the Planck length is within reach. This exploits the high sensitivity toward possible violations of the Pauli Exclusion Principle at ongoing experiments, such as Borexino [107] and VIP [105].
4.8 Phenomenology inspired by causal sets
Most of the quantumspacetime phenomenology of this past decade has been inspired by results on spacetime noncommutativity and/or LQG. But several other approaches are getting closer to inspiring phenomenological programs. I share the view of many quantumspacetime phenomenologists who are looking at the approach based on causal dynamical triangulations [45, 371, 46, 47, 372, 49] as a maturing opportunity for inspiring the phenomenology work. And first indications are coming from the “asymptotic safety approach” [544, 466, 212, 469, 468], on which I shall comment in relation to a tangible proposal for phenomenology later in this review. Certainly in recent years we have seen a blossoming phenomenology emerging from the the causalset program.
I place here an aside on this recent phenomenology inspired by the causalset program, which also allows me to return, from a different perspective, on the important subject of nonsystematic effects, already briefly discussed in Section 4.3.2. Indeed, because of the perspective that guides that research program, most (if not all) new effects predicted within the causal set program will be of nonsystematic type.
Causal sets are a discretization of spacetime that allows the symmetries of GR to be preserved in the continuum approximation [131, 470, 284]. And causal sets can be used to construct simple models suitable for exploring possible manifestations of fuzziness of quantum spacetime. Moreover, the causal set proposal has recently been combined with the loop representation to formulate “causal spin foams” [392], thereby establishing a link to an already mature source of inspiration for quantumspacetime phenomenology.
Clearly, some of the manifestations one must expect from a causalset setup fall within the class of phenomena already briefly described in Section 4.3.1: at a coarsegrained level of analysis a causalset background should introduce an intrinsic limitation to the accuracy of lengths and durations. Several recent works were aimed at formalizing and modeling these aspects of fuzziness for propagation [311, 312, 215]. The preliminary indications that are emerging appear to suggest that, if discreteness is indeed introduced at the Planck scale, the effects are very soft (hard to detect). Nonetheless we do already have a few examples of studies aiming for tangible predictions to be compared to actual data: for example, Ref. [490] reports a causalsetinspired analysis of possible fuzziness of arrival times (the sort of effects already discussed in Section 4.3.1), relevant for studies conducted by gammaray telescopes.
An intriguing effect of random fluctuations in photon polarization can also be motivated by the causalset framework [186]. The presentlyavailable models of this causalsetinduced effect are to be viewed as very crude/preliminary, particularly since the present understanding of the framework is still not at the point of providing a definite model of photons propagating on a causal set background (from which one could derive the polarizationfluctuation feature). Still, this appears a very promising direction, especially since experimental information on CMB polarization is improving quickly and will keep improving in the coming years.
The tightest limit on Κ is Κ < 10^{−61} GeV^{3}, and was obtained [316] from limits on the amount of relicneutrino contribution to hot dark matter. This follows from the observation that energy on the mass shell is bound from below by the mass, so that particles close to rest, when swerving, can essentially only increase their energy.
Interestingly these Κgoverned effects can also be relevant [396] for some of the phenomenology already discussed in this review, concerning the threshold requirements for certain particlephysics processes. Essentially the expected implications of swerving for these threshold analyses is similar to that already discussed in Section 4.3.2: in any given opportunity of interaction between a hard photon and a soft photon the swerving can effectively raise or lower (from the perspective of the asymptoticallyincoming states) the threshold requirements for pion production. However, it appears that the bound Κ < 10^{−61} GeV^{3}, if applicable also to protons,^{33} brings the magnitude of such effects safely beyond the reach [396] of ongoing cosmicray studies.
4.9 Tests of the equivalence principle
4.9.1 Aside on tests of the equivalence principle in the semiclassicalgravity limit
I am focusing in this review on tests motivated by (and on effects modeled within) proposals of spacetime quantization at the Planck scale, but concerning tests of the equivalence principle inspired by quantumspacetime models there is some merit in making a small digression on tests of the equivalence principle in the semiclassical limit of quantum gravity (where, by construction, no quantumspacetime effects could be seen). This will allow me to compellingly setup the issue of testing the equivalence principle from a general quantumgravity perspective and specifically from the perspective of spacetime quantization at the Planck scale.
Of relevance here is the fact that some of the issues that have been most extensively considered by researchers involved in these studies concern the equivalence principle. This is signaled by the adoption of separate notation for inertial and gravitational mass in Eq. (75). In principle the gravitational mass M_{ G } governs the accrual of gravityinduced phases, while the inertial mass M_{ I } intervenes in determining the ratio between wave vector and velocity vector in the Galilean limit (p ≪ m). And even for M_{ G } = M_{ I } the mass does not factor out of the freefall evolution of the quantum state (but for M_{ G } = M_{ I } one at least recovers [535] a complete identification between the effects of gravitation and the effects of acceleration).
Besides neutrons, these studies can also be performed with atoms [14]. And, interestingly, one can also perform rather similar analyses in studying neutrino oscillations, finding (see, e.g., Refs. [252, 272, 148] and references therein), that gravity may induce neutrino oscillations if different neutrino flavors are coupled differently to the gravitational field, thereby violating the equivalence principle.
4.9.2 On the equivalence principle in quantum spacetime
Evidently, searches of possible violations of the equivalence principle in the semiclassicalgravity limit of quantum gravity have significant intrinsic interest. And some of these tests of the equivalence principle in semiclassicalgravity limit also find explicit motivation in approaches to the study of the full quantumgravity problem: most notably the stringtheoryinspired studies reported in Refs. [521, 195, 196, 194, 193, 192], and references therein, predict violations of the equivalence principle in the semiclassicalgravity limit.
This very recent proposal illustrates a type of path that could be followed to introduce violations of the equivalence principle originating genuinely from spacetime quantization at the Planck scale: one might find a way to describe spacetime foaminess n terms of effects of genuinely Planckian size, and then elaborate the implications of this spacetime foaminess for the equivalence principle. The formalization adopted in Ref. [263] is still too crude to allow such an explicit link between the Planckscale picture of spacetime foam and the nature and magnitude of the effects, but provides a significant step in that direction.
5 Infrared QuantumSpacetime Phenomenology
Work on Planckscale quantumspacetime phenomenology is a rather recent development, with a significant effort taking place over only little more than a decade. But one can already make a distinction between “traditional” and “novel” quantumspacetime phenomenology approaches. The proposals I have reviewed in the previous two Sections 3 and 4 cover the scope of the “traditional” approach, considering UV effects that could be relevant for observations in astrophysics and/or in controlledlaboratory experiments. I devote this and the next Section 6 to the “novel” idea that Planckscale quantization of spacetime could have valuable phenomenological implications in some IR regimes and/or that the tests could rely on cosmology.
Considering that these “novel” areas of quantumspacetime phenomenology are in a preliminarily exploratory phase I will adopt a lower standard in the selection of topics, meaning that I will even mention some proposals that have not fully established a link to a definite scheme of spacetime quantization and/or have not fully established the availability of sensitivities that could be compellingly linked with the introduction of spacetime quantization at the Planck scale. I will rather rely on an (inevitably subjective) assessment of whether the relevant proposals provide valuable first steps in the direction of establishing in the notsodistant future robust Planckscale quantumspacetime phenomenology.
5.1 IR quantumspacetime effects and UV/IR mixing
In the long [508, 475], and so far inconclusive, search for quantum gravity and quantum spacetime the main strategy was inspired by the discovery paradigm of the 20th century, the “microscope paradigm” with discovery potential measured in terms of the shortness of the distance scales probed. But recent research has raised the possibility that by quantizing spacetime at the Planck scale one might have not only some new phenomena in a farUV regime, but also some new phenomena in a “dual” IR regime. Actually, as compellingly stressed in Ref. [176], our present understanding of blackhole thermodynamics, and particularly the scaling S ∝ R^{2} of the entropy of a black hole of radius R, suggests that such effects of “UV/IR mixing” may be inevitable. It is on the basis of apparently robust hypotheses concerning the behavior of quantum gravity in the UV (Planckian) regime that we arrive at this quadratic dependence, which is surprising with respect to what one might expect in particular in quantum field theory, where cubic scaling (S ∝ R^{3}) naturally arises. But this feature originating from the UV sector clearly should have its most profound implications in the largedistance/IR regime since the difference between quadratic dependence on the radius and cubic dependence on the radius becomes more and more significant as the radius is increased.^{35}
Another argument in favor of UV/IR mixing is found considering a popular intuition for quantum spacetime, which relies on the introduction of an uncertainty principle for spacetime itself (in addition to the Heisenberg one, which acts in phase space). The link with UV/IR mixing can be already seen simply by considering a principle of the form \(\delta x\delta y \geq \lambda _\ast^2\) for spatial coordinates, with λ_{*} plausibly on the order of the Planck length. This type of uncertainty relation would evidently imply that small uncertainty in x should require large uncertainty in y, and this suggests a link between probing short distance scales (small δx) and probing large distance scales (large δy).
5.2 A simple model with soft UV/IR mixing and precision Lambshift measurements
The phenomenology of models such as this requires a complete change of strategy with respect to the phenomenology of quantumspacetime UV effects that I discussed in previous Sections 3 and 4 of this review. Whereas the typical search for those UV effects relied on lowprecision highenergy data, for the type of IR effects that I am now considering the best options come from highprecision lowenergy data. A first example of this was given in Ref. [155], most notably with a (however brief) discussion of how a dispersion relation of type (84) could be relevant for Lambshift measurements. Indeed, assuming Eq. (84) holds for the electron, then one should have a modification of the energy levels of the hydrogen atom. And in light of the high precision of certain Lamb shift measurements (which Ref. [155] assesses as being better than one part in 10^{5}, see also, e.g., Refs. [328, 546]) one can use this observation to place valuable limits on parameters such as ξ (and χ) for the electron.
5.3 Soft UV/IR mixing and atomrecoil experiments
Evidently the ansatz (84) is such that if particles of different mass had the same value^{38} of ξ then the effect would be seen more easily for heavier (more massive) types of particles.
This turns out to be just enough to provide the desired “Planckscale sensitivity”: one easily finds that combining the measurements on cesium reported in Ref. [548] and the determination of α^{2} reported in Ref. [277], one can establish [69] that ξ_{ Cs } = −1.8 ± 2.1.
It is interesting that, besides tests of IR modifications of the dispersion relation, these atomrecoil studies can also be used to investigate possible IR modifications of the law of conservation of momentum. An example of such an analysis is given in Ref. [89].
5.4 Opportunities for BoseEinstein condensates
The use of atoms in quantumspacetime phenomenology immediately confronts us with issues that are presently beyond the reach of available theoretical results. A legitimate expectation is that quantumspacetime effects for atoms could be weaker than for the particles that compose atoms, as a result of the sort of “averageout effects” that one is often expected in the quantumspacetime literature. This would have to be modeled by introducing an extra suppression factor (a sort of “compositeness factor”) in addition to the Planckscale suppression that is standard in quantumspacetime phenomenology. Analyses not making room for such an additional suppression might overestimate the Planckscalesensitivity reach of the relevant experiments. On the other hand we are at present not sure whether such compositenesssuppression factors are truly needed, or at least if they are needed in all contexts and in all quantumspacetime models. For example, it is not unreasonable to imagine that in appropriate quantumspacetime models, when we achieve the ability to analyze them in detail, we might find that as long as a particle is to be handled as a quantum state (far from its classical limit) then it might be irrelevant for the magnitude of quantumspacetime effects whether the particle is composite or “fundamental”.
This issue of compositeness will surely gradually take an important role in quantumspacetime research, but at present it is at a very preliminary stage of investigation, and I shall therefore set it aside. However, do note that if particles composed of a very large number of constituent particles experience Planckscale effects unsuppressed by their compositeness, then not only atoms but also (and perhaps more powerfully) BoseEinstein condensates could prove to be a very valuable opportunity for quantumspacetime phenomenology.
And it is noteworthy that in the recent quantumspacetimephenomenology literature there has already been a surge of interest in the possibilities offered by BoseEinstein condensates, as seen in Refs. [542, 472, 139, 138]. In particular, Refs. [139, 138] study BoseEinstein condensates adopting a perspective on soft UV/IR mixing that is closely related to the one discussed for atoms in the previous Section 5.3.
5.5 Soft UV/IR mixing and the end point of tritium beta decay
Perhaps the most tempting opportunity for the phenomenology of UV/IR mixing comes from studies of the lowenergy beta decay spectrum of tritium, \(^3{\rm{H}}{\rightarrow ^3}{\rm{He +}}{{\rm{e}}^ } + {\bar v_e}\), which have produced so far some rather puzzling results [545, 370]. It is well understood (see, e.g., Refs. [121, 174]) that these puzzles could be addressed by introducing deformed rules of kinematics. And it is intriguing that studies conducted near the endpoint of tritium beta decay are the only known way to accurately investigate the properties of neutrinos in a nonrelativistic (nonultrarelativistic) regime, where their momenta could be comparable to their (tiny) masses. So, it would seem to be a very natural opportunity for advocating UV/IR mixing as a possible explanation. However, the evidence available so far is not very encouraging for the hope of attributing the magnitude of the reported anomalies to IR effects induced by the Planck scale. Still, it is noteworthy that specifically the simple model for soft UV/IR mixing that I described in the previous Sections 5.2 and 5.3 has just the right structure for producing the sort of anomalies that are being reported, as was first stressed in Ref. [154].
5.6 NonKeplerian rotation curves from quantumgravity effects
In addition to precision measurements on particles of peculiarly low momentum, another very clear opportunity for UVIR mixing is provided by data on the behavior of gravity on very large distance scales. And in that context speculating about newphysics phenomena is fully justified by the observed nonKeplerian features of the rotation curves of galaxies or clusters [183]. These nonKeplerian features are usually interpreted as motivation for introducing dark matter (or other nonquantumgravity new physics, such as MOND [416]), but, in light of the recent awareness of the possibility of UV/IR mixing, it is legitimate to speculate that they may be at least in part due to quantumspacetime effects.
The perspective one might adopt in trying to profit from this opportunity is similar to when one works within standard quantum field theories and derives an “effective potential” (usually obtained through the calculation of loop contributions) that corrects the treelevel classical potential.
A more articulated argument for modifications of the Newton potential at large distances from a quantumspacetime perspective has been put forward as part of the mentioned research program on “asymptotic safety”. This is done in Ref. [469], which indeed adopts as a working assumption the availability of a quantum field theory of gravity whose underlying degrees of freedom are those of the spacetime metric, defined nonperturbatively as a fundamental, “asymptoticallysafe” theory. Obtaining definite predictions for the rotation curves of galaxies or clusters within this formalism is presently well beyond our technical capabilities. However, preliminary studies of the renormalizationgroup behavior provide encouragement for a certain level of analogy between this theory and nonAbelian YangMills theories, and, relying in part on this analogy, Ref. [469] argued that one could obtain nonKeplerian features from renormalization.
5.7 An aside on gravitational quantum wells
Another opportunity for studies of UV/IR mixing is provided by measurements performed on neutron quantum states in the gravity field of the Earth, such as the striking ones reported in Refs. [428, 429]. I have nothing to report on this that would fit the main focus of this review, concerning Planckscale quantum pictures of spacetime, but it seemed worth mentioning this nonetheless, especially in light of the fact that this class of lowenergy studies (candidates for the investigation of UV/IR mixing) have already been analyzed from the perspective of some quantum spacetimes, even though so far all such studies have introduced spacetime quantization at scales that are very far from the Planck scale (much lower energy scales, much greater distance scales).
And Refs. [118, 102, 483] agree on the fact that pure space/space noncommutativity (θ_{j0} = 0) has no significant implications for the gravitational quantum well. However, Ref. [483] notices that with space/time noncommutativity (θ_{j0} ≠ 0) there are tangible consequences for the gravitational quantum well so that in turn one can use the measurement results of Refs. [428, 429] to put bounds on space/time noncommutativity,^{40} although only at the level θ_{j0} < 10^{−9} m^{2} (whereas interest from the Planckscalequantumspacetime side would focus in the neighborhood of θ_{j0} ∼ 10^{−70} m^{2}).
6 QuantumSpacetime Cosmology
In the previous Sections 3, 4, 5, I discussed several opportunities for investigating candidate quantumspacetime effects through observations in astrophysics and, occasionally, some controlled laboratory setups. However, it is likely that gradually cosmology will acquire more and more weight in the search for manifestations of quantumspacetime effects. In the earliest stages of evolution of the Universe, the typical energies of particles were much higher than the ones we can presently achieve, and highenergy particles are the ideal probes for the shortdistance structure of spacetime. Over these past few years, several studies that could be viewed as preparing the ground for this use of cosmology have been presented in the literature. Most of these proposals do not have the structure and robustness necessary for actual phenomenological analyses, such as the ones setting bounds on the parameters of a given quantumspacetime picture. But the overall picture emerging from these studies confirms the expectation that cosmology has the potential to be a key player in quantumspacetime phenomenology.
For a combination of reasons, I shall review this recent literature in an even more sketchy way than other parts of this review. This reflects the fact that I view this area as still at a very early stage of development: we are probably just starting to learn what could be the observable manifestations of the quantization of spacetime in cosmology. Even in cases when the quantumspacetime side is reasonably well understood, the study of the implications for cosmology, when focused on possible observablylarge manifestations, is still in its infancy. Moreover, most of the work done so far in this area does not even invoke a definite role for spacetime quantization, which is the main focus of this review, but rather finds inspiration in generic features of the quantumgravity problem, or relies on string theory (which, as stressed, is a fully legitimate quantumgravity candidate, but is one such candidate that, as presently understood, would rather lead us to assume that quantum properties of spacetime are absent/negligible).
In light of these considerations, the list of proposals and ideas that composes this section is not representative of the list of scenarios being considered in quantumspacetime cosmology. It mainly serves the purpose of offering some illustrative examples of how one might go about proposing a quantumspacetimecosmology scenario and giving some strength to my opening remarks foreseeing a great future for quantumspacetime cosmology.
In the last Section 6.5, I briefly mention some examples of quantumgravitycosmology proposals, which in their present formulation do not invoke a role for the quantization of spacetime (but could inspire future reformulations centered on a quantumspacetime perspective).
6.1 Probing the transPlanckian problem with modified dispersion relations
In the long run, one of the most significant opportunities for quantumspacetime phenomenology could be an aspect of quantumspacetime cosmology: the transPlanckian problem. Inflation works in such a way that some of the scales that are presently of cosmological interest should have been transPlanckian scales at the beginning of inflation, and, therefore, cannot be handled satisfactorily without (the correct) quantum gravity [134, 393, 197]. In extrapolating the evolution of cosmological perturbations according to linear theory to very early times, we are implicitly making the assumption that the theory remains perturbative to arbitrarilyhigh energies. And it is easy to see that the expected new physics at the Planck scale could affect our predictions. For example, if there was a sharp Planckscale cutoff in the theory, then, if inflation lasts many efolding, the modes which represent fluctuations on galactic scales today would not be present [134] in the theory since their wavelength would have been smaller than the cutoff length at the beginning of inflation.
While in the long run this might get very exciting, I feel we are at present only at a very early stage of exploration of the potentialities of this opportunity for quantumspacetime phenomenology. But there is growing awareness of this opportunity and the related literature starts to grow large (see, e.g., Refs. [393, 197, 435, 136, 320, 172, 410, 217, 266, 198, 321, 145, 274, 510, 383, 135], and references therein). Many of these studies [136, 172, 410, 217, 266, 198, 321, 274] have probed the possibility that a shortdistance cutoff might leave a trace in cosmology measurements such as the ones conducted on the cosmic microwave background.
These results (and those of Refs. [248, 318, 437, 273]) establish a connection with previous attempts at replacing inflation by scenarios accommodating departures from Lorentz symmetry, such as the scenario with a timevarying speed of light, introduced in works by Moffat [419] and in works by Albrecht and Magueijo [30] (see also Ref. [104]). By postulating an appropriate time variation of the speed of light one can affect causality in a way that is somewhat analogous to inflation: very distant regions of the Universe, which could have never been in causal contact with a timeindependent speed of light, could have been in causal contact at very early times if at those early times the speed of light was much higher than at the present time. As argued in the recent review given in Ref. [385], this alternative to inflation is rather severely constrained but still to be considered a viable alternative to inflation.
6.2 Randomlyfluctuating metrics and the cosmic microwave background
Ref. [460] also explored the possibility that lightcone fluctuations might have observable implications for the gravitationalwave background. The gravitationalwave background is always emitted much before the cosmic microwave background, but it was found [460] that the flat nature of the gravitationalwavebackground spectrum is such that the effects of lightcone fluctuations are negligible.
6.3 Loop quantum cosmology
An area of quantumspacetime cosmology that is not directly linked to the tools and scenarios considered in other areas of quantumspacetime phenomenology is the Loop Quantum Cosmology (LQC) [125, 94, 126, 92]. This is a framework for implementing several effects seen to arise for the quantum spacetime of LQG in a cosmological setting. The most popular formulations of LQC are defined on “minisuperspace”, where one quantizes homogeneous spacetimes using the methods of LQG. And one finds that the characteristic discreteness of the LQG spacetime quantization change the dynamics of expanding Universe models. These changes are particularly significant at high densities, giving rise to mechanisms avoiding classical singularities.
And one can also consider the novel quantumspacetime effects at later stages of the Universe expansion, when densities are lower and the corrections can be treated perturbatively in a gaugeinvariant way. This can be done in particular for linear perturbations around spatially flat FriedmannRobertsonWalker models, and the results are found to be primarily characterized in terms of “inversevolume corrections”, due to the fact that the quantized densitized triad has a discrete spectrum, with the value zero contained in the spectrum. Essentially one finds that the LQG quantumspacetime effects can be effectively described in terms of a novel repulsive force [92]. This repulsion can compete with the standard gravitational attraction, and can even become the dominant contribution, thereby evading the singularity, when the curvature is strong.
In Refs. [126, 92, 127], and references therein, readers can find a list of possible signatures of LQC. In my opinion, at present, such tests of predictions of LQC may tell us more about the choice of setup for incorporating the quantumspacetime effects, rather than providing actual information on the quantum structure of spacetime. But as this novel approach keeps maturing, it may well turn into a key resource for experimentally probing the quantum structure of spacetime.
6.4 Cosmology with running spectral dimensions
As mentioned earlier in this review, several formalisms relevant to the study of the quantumgravity problem have recently been shown to host the mechanism of running spectral dimensions. The spectral dimension of a spacetime is essentially defined [506] by considering a fictitious diffusion process, with the spectral dimension given in terms of the average return probability for given (fictitious) diffusion time. When the number of spectral dimensions matches the number of Hausdorff dimensions of a spacetime, the return probability depends on diffusion time in a characteristic way that is indeed found in all models for large diffusion times. But at short diffusion times one finds in several studies of interest for quantumgravity and quantumspacetime research that the average return probability has properties signaling a number of spectral dimensions smaller than the number of Hausdorff dimensions.
First results of this type were found in studies done within the framework of causal dynamical triangulations[48], naturally working with four Hausdorff dimensions and finding that the behavior at small diffusion times signaled two spectral dimensions. Two spectral dimensions for small diffusion times was then also found in studies inspired by asymptotic safety [360, 467] and studies based on HořavaLiftschitz gravity [290]. A somewhat different situation is found in studies inspired by spacetime noncommutativity [110, 87, 31] and by spin foams [418], but still giving fewer than four spectral dimensions for small diffusion times (also see Refs. [506, 153]).
These “running spectral dimensions” could have very significant implications for cosmology, as suggested at least intuitively by the definition of spectral dimensions based on the dependence of the return probability on the diffusion time. At present these potentialities are still largely unexplored, but one possibility has been debated in Refs. [424, 505, 425]. Ref. [424], citing as motivation some of the quantumgravity studies exhibiting running spectral dimensions, proposed that such studies should motivate the search for indirect evidence of the absence of gravitational degrees of freedom in the early Universe. However, Ref. [505] more prudently observed that gravitational degrees of freedom are indeed absent in spacetimes with three or fewer Hausdorff dimensions, but may well be present in spacetimes with four Hausdorff dimensions but with three or fewer spectral dimensions.
6.5 Some other quantumgravitycosmology proposals
So far in this section, consistent with the main goals of this review, I have focused on cosmology proposals that are based on (or at least directly linkable to) some theories of quantum spacetime. In this last part of the section, I mention just a few illustrative examples of ideas and proposals that are still based on the quantumgravity problem, but without invoking any definite quantum properties of spacetime. It is not unlikely that future exploitations of the associated phenomenological opportunities would involve spacetime quantization.
6.5.1 Quantumgravityinduced vector fields
An active area of quantumgravity cosmology focuses on Lorentzviolating vector fields. These studies do not have as reference scenarios for spacetime quantization, but they are being linked generically to the opportunities that the quantumgravity problem provides for the emergence of Lorentzviolating vector fields. Several possible implications are being considered, including the possibility that in the presence of such Lorentzviolating vector fields the Universe might experience a slower rate of expansion for a given matter content (see, e.g., Ref. [159]).
It is also emerging that the implications of such Lorentzviolating vector fields would be rather significant for the cosmic microwave background [368]. In particular, as stressed in other parts of this review, the presence of Lorentzviolating vector fields is often associated with energydependent birefringence. And the cosmic microwave background, since its radiation originates from the surface of last scattering, which is the most distant source of light, can be a very powerful opportunity to test anomalous features for the propagation of photons. Several techniques of data analysis have been developed that are capable of constraining the birefringence of photon propagation using cosmicmicrowavebackground data (see, e.g., Refs.[317, 315, 344, 270] and references therein).
6.5.2 A semiclassical WheelerDeWittbased description of the early Universe
Cosmology is also an arena where some interest is attracted by studies of the semiclassical limit of quantum gravity. These do not invoke a quantumspacetime picture and may not even rely on any given quantumgravity proposal. They are rather viewed in analogy [325] with the semiclassical limits of other quantum theories: one can consider, for example, the corrections to the classical Maxwell action described by Heisenberg and Euler (in a preQED era) in terms of quantum fluctuations of electrons and positrons, which can now be rederived [325] from QED by integrating out the fermions and expanding in powers of ℏ.
These studies of the semiclassical limit of quantum gravity are often centered around the WheelerDeWitt equation. While for the development of a full quantumgravity theory the WheelerDeWitt equation has proven to be extremely “cumbersome”, the fact that it is rather intuitively formulated is convenient for setting up a semiclassical approximation (see, e.g., Refs. [326, 447, 409]). A result that can be rather readily analyzed from a phenomenology perspective is the one providing [326] correction terms for the Schrödinger equation, obtained through a formal expansion of the WheelerDeWitt equation with respect to powers of the Planck mass. Unsurprisingly the relevant correction terms are far too small to matter in laboratory experiments [326]. However, it is plausible that such a procedure could give rise to observably large effects in the description of the early stages of the evolution of the Universe. In particular, the semiclassical approximation set up in Ref. [326] could be used rather straightforwardly to describe corrections to the Schrödinger equation for higher multipoles on a Friedman background.
6.5.3 Nosingularity cosmology from string theory
An interesting stringtheoryinspired area of cosmology research revolves around a scenario for singularity avoidance linked to the availability of duality tranformations, which allow one to set up a suitable “preBigBang” scenario [253, 143, 142]. In this scenario the Universe starts inflating from an initial state characterized by very small curvature and weak interactions. The smallcurvature initial state is gravitationally unstable and would naturally evolve [253, 143, 142] into states with higher curvature, until stringsize (roughly Planckscalesize) effects are strong enough to induce a “bounce” into a decreasingcurvature regime. Instead of a conventional hot big bang one would have [253, 143, 142] a “hot big bounce” in which in particular the heating mechanism is provided by the quantum production of particles in the prebounce phase characterized by high curvature and strong interactions.
For this stringinspired prebigbang scenario several possible observational consequences have been discussed [253, 143, 142], including the one of a stochastic background of gravity waves due to a background of gravitons from the prebigbang phase. It appears to be plausible [253, 143, 142] that the magnitude of the associated effects might be within the range of sensitivities of modern gravitywave interferometers.
7 QuantumSpacetime Phenomenology Beyond the Standard Setup

The effects we expect from spacetime quantization are rather striking, qualitatively virulent departures from the structure of our current theories. The fact that no trace of such “easily noticeable” effects has ever been seen surely provides further encouragement for the expectation of perturbative effects suppressed by an ultralarge scale.

I would list the evidence in favor of grand unification as an even more significant source of additional encouragement for the expectation of perturbative effects suppressed by an ultralarge scale. If that evidence is taken at face value (as, I would argue, we should, at least as a natural working assumption) it suggests that particle physics works well on its own up to a scale of about 10^{−3} the Planck scale. If quantumspacetime effects were nonperturbative in ways affecting grand unification or if the scale of spacetime quantization was much lower than the Planck scale, it would then be hard to explain the (preliminary) success of the grandunification idea.
In light of this, surely quantumspacetime phenomenologists should continue to focus most of their efforts on applications of the standard strategy, assuming perturbative effects suppressed by a scale in some neighborhood of the Planck scale. However, other scenarios and opportunities should not be completely overlooked. We are clearly presently unable to exclude that the correct quantum picture of spacetime might turn out to be unsuitable to the standard strategy of quantumspacetime phenomenology. As a way to give some substance to this assessment, I briefly discuss examples of mechanisms that could render ineffective the standard strategy of quantumspacetime phenomenology.
7.1 A totally different setup with large extra dimensions
Can the scale characteristic of quantumspacetime effects be much lower than the Planck scale? We surely know at least one mechanism by which the quantumgravity scale can be much lower than the Planck scale, and therefore quantumgravity models with spacetime quantization affected by this mechanism would describe quantumspacetime effects at a relatively low scale. I am thinking of the popular scenarios with large extra dimensions.
Through these scenarios one can achieve a sizeable reduction in the quantumgravity scale with the introduction of D extra space dimensions [80, 375, 552, 84] of finite size R_{*}. Then the fundamental length scale L_{ D } characteristic of quantum gravity in the 3+D+1dimensional spacetime can be much bigger than the Planck length. The smallness of the Planck length can emerge as the result of the fact that, as deduced from applying Gauss’s law in the 3+D+1dimensional context, the strength of gravitation at distance scales larger than the size R_{*} of the extra dimensions in the ordinary (infinitesize) 3+1dimensional spacetime would be proportional to the squareroot of the inverse of the volume of the external compactified space multiplied by an appropriate power of L_{ D }.
These scenarios need to be tuned rather carefully in order to get a phenomenologicallyviable picture. Essentially the only truly appealing possibility is the one of 2 extra dimensions of relatively “large” size, somewhere below millimeter size [84] (perhaps 10^{−4} or 10^{−5} meters). There might be other extra dimensions of smaller (possibly Planckian) size, but for the desired phenomenology one needs two and only two extra dimensions of relatively large size; otherwise one finds effects that either violate known experimental facts or are too small to ever be tested. But with these (however contrived) choices one does end up with a phenomenologicallyexciting scenario in which the fundamental length scale of quantum gravity L_{ D } is somewhere in the neighborhood of the (TeV)^{−1} length scale, and therefore within the reach of particlephysics experiments (see, e.g., Refs. [260, 258, 207, 82]). Moreover, there are phenomenologicallyrelevant implications for the behavior of (classical) gravity at submillimeter distances [84, 295].
7.2 The example of hard UV/IR mixing
The largeextradimension scenario is an example of inapplicability of the standard setup of quantumspacetime phenomenology due to the fact that, within that scenario, the characteristic scale of quantum gravity is not the Planck scale. There are also scenarios in which one may still assume that quantumspacetime effects are fundamentally introduced at the Planck scale, but the standard setup of quantumspacetime phenomenology is inapplicable because the most characteristic effects are not describable in terms of an expansion in powers of the Planck length.
I have already discussed this possibility in Section 5, devoted to soft UV/IR mixing. However, in that context one could fall back on roughly the standard strategy of quantumspacetime phenomenology, by looking for an IR scale playing the role of characteristic scale of the IR manifestations of the quantum properties of spacetime. Let me just stress that an even more pervasive revision of the standard strategy of quantumspacetime phenomenology would be required in the case of hard UV/IR mixing, which might take the form of correction terms with the behavior of inverse powers of momentum. With hard UV/IR mixing one should expect that in certain contexts the departures from known physical laws should be dramatic. The most efficacious tests of this hypothesis might not take the shape of searches of small corrections to standard predictions in ordinary contexts, but rather be based on the identification of those peculiar contexts where the implications of UV/IR mixing are large.
7.3 The possible challenge of notsosubleading higherorder terms
Some challenges for the standard setup of quantumspacetime phenomenology may also be present when the effects are genuinely introduced at the Planck scale and there is nothing peculiar about the IR sector. In particular, just because this standard setup is based on a (truncated) expansion in powers of the Planck length, it can happen that the formally subleading terms (higher powers of the Planck length), which are usually neglected in leadingorder analyses, are actually not really negligible. The fact that experiments suitable for quantumspacetime phenomenology must host, as I stressed in several points of this review, some ultralarge ordinaryphysics dimensionless “amplifiers” could play a role in these concerns: if some mechanism is allowing the tiny leadingorder Plancklength correction to be observably large it would not be so surprising to find that the same (or some other) amplifier is also such that some “formally subleading” Plancklength corrections, neglected in the analysis, are significant.
And another possible source of concern can originate from the fact that some of the contexts of interest for quantumspacetime phenomenology are characterized by several length scales: expansions in powers of the Planck length actually are expansions in powers of some dimensionless quantity obtained dividing the Planck length by a characteristic length scale of the physical context of interest, and some “pathologies” may be encountered if there are several candidate length scales for the expansion.
8 Closing Remarks
Clearly, the most significant development of these first few years of quantumspacetime phenomenology has been our ability to uncover some experimental/observational contexts in which, through appropriate data analyses, we could gain access to effects introduced genuinely at the Planck scale. The compellingness of such instances of genuine Planckscale sensitivity, which are most simply and clearly illustrated in Section 1.5, should be contrasted to the more frequent case of “dimensionalanalysis Planckscale sensitivities”, which typically involve a description of a plausible quantumspacetime effect in terms of a dimensionless parameter, estimated arbitrarily as a ratio of the Planck length and some characteristic length scale of the problem.
Looking at the results summarized in this review, different readers, depending on how stringent their criteria for genuine Planckscale sensitivity, will only recognize one or two examples. Not much, but much better than expected even just 15 years ago. And, as stressed, we do have, at this point, a rather encouraging list of contexts in which, while the availability of genuine Planckscale sensitivity has still not been fully established, it appears that sensitivity to effects introduced genuinely at the Planck scale could be achieved in a notsodistant future.
The fact that the development of this phenomenology is proving beneficial for the study of the idea of spacetime quantization is perhaps best testified by the fact that it is already managing to truly affect the directions taken by more formal work on spacetime quantization, especially in the areas of LQG and spacetime noncommutativity. Theorists in these areas follow the developments on the phenomenology side and do their best (the technical challenges they are facing are very severe) to derive results that can be exploited for the opportunities in phenomenology that are being established. In turn the phenomenology takes notice of the developments on the theory side, finding in them new input for enlarging the list of candidate quantumspacetime effects that one could attempt to investigate experimentally.
The goal of testing/falsifying rigorous theories of spacetime quantization appears to still be beyond our present reach. But while most of the work in quantumspacetime phenomenology so far has relied on simpleminded test theories describing candidate quantumspacetime effects, I see first indications of a phase of further maturation of this phenomenology, in which we will actually test/falsify at least the most virulent rigorous formalizations of quantum spacetime. Planckscale theories formulated in noncommutative versions of Minkowski spacetime are the example where we are presently closer to this goal.
The (however limited) information presently available to us appears to provide a clear invitation to continue to focus most of our efforts in the search for effects describable in terms of a (lowenergy) expansion in powers of the Planck length, though other opportunities clearly should not be overlooked. Concerning the type of data on which quantumspacetime phenomenology can rely, I have attempted to maintain throughout this review some visible separations between different proposals on the basis of whether they concern astrophysics, cosmology or controlled laboratory experiments. It is very clear that astrophysics has so far provided the most fruitful arena, but cosmology has the greatest potential reach (although for the most part this potential has not yet materialized). The role played so far in quantumspacetime phenomenology by controlled laboratory experiments is rather marginal, but it would be important for the future development of quantumspacetime phenomenology to find more opportunities for controlled laboratory experiments.
Footnotes
 1.
For simplicity, I am assuming the description of the collision is being given in the centerofmass frame. For example, we might have two identical particles, which in that frame have the same gigantic energy but propagate in opposite directions.
 2.
Note, however, that this type of Heisenbergmicroscopetype issues can be studied in some of the frameworks under consideration for the quantumgravity problem. In particular, this has attracted some interest by proponents of asymptotic safety, as illustrated by the study reported in Ref. [451] (for an alternative perspective see Ref. [216]).
 3.
Our familiarity with the Newtonian regime of gravity extends down to distance scales no shorter than ∼ 10^{−6} m, so the factor \(\ell _p^2/{r^2}\) would invite us to determine a Newtonian potential with accuracy of at least parts in 10^{58}.
 4.
Consistent with what is done in the relevant literature, I write Eq. (1) without assuming exact validity of the equivalence principle, and, therefore, introduce different symbols MI and MG for the inertial and gravitational mass respectively.
 5.
For a detailed discussion of the implications for the energymomentum relation of a given scheme of spacetime discretization see, e.g., Ref. [517].
 6.
η represents one of (or a linear combination of) the coefficients \({\eta _{{m_0},{m_1},{m_2},{m_3}}}\),m_{1},m_{2},m_{3}. The quantumgravity intuition for η is η ∼ 1. For example, in my simpleminded “spacetimelattice picture” η ∼ 1 is obtained when the lattice spacing is exactly \(E_p^{ 1}\). Sensitivity to values of η even smaller than 1 would reflect the ability to probe spacetime structure down to distance scales even smaller than the Planck length (in the “spacetimelattice picture” this would correspond to a lattice spacing of \(\sqrt \eta E_p^{ 1}\)).
 7.
Evidently, this might mean that the length scale of spacetime quantization might be somewhat lower or somewhat higher than the Planck scale. But notice that when reasoning in terms of \({\ell _{{\rm{QST}}}} \sim \sqrt {{G_N}({\ell _{{\rm{QST}}}})}\) one should then allow for the possibility that there might not be any spacetime quantization after all (the selfconsistent solution of \({\ell _{{\rm{QST}}}} \sim \sqrt {{G_N}({\ell _{{\rm{QST}}}})}\) might be ℓ_{QST} = 0).
 8.
Some colleagues even use the expression “theory of everything” without adding “we know so far”.
 9.
One may then argue that there are some indirect reasons why the Planck scale should appear in formulas setting the significance of the effects, but the connection with the Planck scale remains relatively weak.
 10.
While the type of quantumspacetime effects considered in the LQG literature makes it natural to question the fate of Lorentz symmetry in the quasiMinkowski limit, I should stress that at present no fully robust result is available, and some authors (notably Refs. [478, 479]) have observed that there could be ways to reconcile what is presently known about LQG with the presence of exact Lorentz symmetry in the quasiMinkowski limit.
 11.
A space with some elements of quantization/discreteness may have classical continuous symmetries, but only if things are arranged in an ad hoc manner. Typically quantization/discretization of spacetime observables does lead to departures from classical spacetime symmetries. So clearly spacetimesymmetry tests should be a core area of quantumspacetime phenomenology, but to be pursued with the awareness that spacetime quantization does not automatically affect spacetime symmetries (it typically does but not automatically).
 12.
In the case of canonical noncommutativity, evidence of some departures from Poincaré symmetry are found both if θ_{ μν } is a fixed tensor [213, 516] and if it is a fixed observerindependent matrix [161, 236, 100]. The possibility to preserve classical Poincaré symmetry is instead still not excluded in what was actually the earliest approach [211] based on [x_{ μ }, x_{ ν }] =iθ_{ μν }, where for θ_{ μν } one seeks a formulation with richer algebraic properties.
 13.
While I shall not discuss it here, because it has so far attracted little interest from a quantumspacetime perspective, I should encourage readers to also become acquainted with the fact that studies such as the ones in Refs. [196, 192], through the mechanism for violation of the equivalence principle, also provide motivation for “varying coupling constants” [531, 394].
 14.
Think of the limitations that the speedoflight limit imposes on certain setups for clock synchronization and of the contexts in which it is impossible to distinguish between a constant acceleration and the presence of a gravitational field.
 15.
And this assessment does not improve much upon observing that exact supersymmetry could protect from the emergence of any energy density of the sort relevant to such cosmologicalconstant studies. In fact, nature clearly does not have supersymmetry at least up to the TeV scale, and this would still lead to a natural prediction of the cosmological constant, which is some 60 orders of magnitude too high.
 16.
As stressed earlier in this section, one can restore a relativistic formulation by appropriately matching the modification of the dispersion relation and a modification of energymomentum conservation. When the modifications of the dispersion relation and of energymomentum conservation (even when both present) do not match, one has a framework that requires a preferred frame.
 17.
While Myers and Pospelov have the merit of alerting the community to several opportunities and issues within a simple model, we now understand that many of these aspects uncovered through their simple model (such as birefringence) are common aspects of a more general class of fieldtheory models with rotationallyinvariant operators of odd dimension (see, e.g., Ref. [337]).
 18.
While some observers understandably argue that the the residual grey areas that I discuss force us to still be extremely prudent, even at the present time one could legitimately describe as robust [62] the observational evidence indicating that some γrays with energies up to 20 TeV are absorbed by the IR diffuse extragalactic background. And some authors (see, e.g., Ref. [511]) actually see in the presentlyavailable data an even sharper level of agreement with the classicalspacetime picture, which would translate in having already achieved Planckscale sensitivity.
 19.
It used to be natural to expect [111] that indeed the highest energy cosmic rays are protons. However, this is changing rather rapidly in light of recent dedicated studies using Auger data [7, 242, 509], which favor a significant contribution from heavy nuclei. The implications for the Lorentz symmetry analysis of the differences between protons and heavy nuclei, while significant in the detail (see, e.g., Ref. [488]), are not as large as one might naively expect. This is due to the fact that it just happens to be the case that the photodisintegration threshold is reached when the energy of typical heavy nuclei, such as Fe, is ∼ 5 · 10^{19} eV, i.e., just about the value of the photopionproduction threshold, expected for cosmicray protons.
 20.
We are dealing again with the limitations that purekinematics particlereaction analyses suffer when the properties of the incoming particles are not fully under control. The pure kinematics of the PKV0 test theory definitely forbids (for negative η of order 1 and n ≤ 2) pion production resulting from collisions between a 5 · 10^{19} eV proton and a CMBR photon. But it allows pion production resulting from collisions between a 5 · 10^{19} eV proton and more energetic photons, and in order to exclude that possibility one ends up formulating assumptions about dynamics (the low density of relevant photons may be compensated for by an unexpected increase in cross section).
 21.
For the related subject of the description of light propagation in models of emergent spacetime, see, e.g., Ref. [275] and references therein.
 22.
Up to 1997, the distances from gammaray bursts to Earth were not established experimentally. Starting with the 1997 result of Ref. [188], we are now able to establish, through a suitable analysis of the gammarayburst “afterglow”, the distance between the gammaray bursts and Earth for a significant portion of all detected bursts. Sources at a distance of ∼ 10^{10} light years (∼ 10^{17} s) are not uncommon.
 23.
There are ordinaryphysics effects that could be relevant for these analyses, such as ordinary electromagnetic dispersion, but it is easy to show [66, 132] that already at energies of a few GeV these ordinaryphysics effects would be negligible with respect to the candidate quantumgravity effect here considered.
 24.
Also noteworthy is the analysis reported in Ref. [156], which argues that neutrino oscillations may play a role for other aspects of quantumspacetime phenomenology, in addition to their use in relation to flavordependent Planckscale modifications of the dispersion relation.
 25.
This is in part due to the fact that “naive quantum gravity” is not a renormalizable theory, and as a result the restriction to powercounting renormalizable correction terms (which is standard outside quantumgravity research) is expected not to be necessarily applicable to quantumgravity research.
 26.
A warning to readers: whereas originally the denomination “Standard Model Extension” was universally used to describe a framework implementing the restriction to powercountingrenormalizable correction terms, recently (see, e.g., Ref. [123]) some theorists describe as “Standard Model Extension” the generalization that includes correction terms that are not powercounting renormalizable, while they describe as a “Minimal Standard Model Extension” the case with the original restriction to powercountingrenormalizable correction terms. Still, even as I write this review, many authors (in particular the near totality of experimentalists involved in such studies) continue to adopt the original description of the “Standard Model Extension”, restricted to powercountingrenormalizable correction terms, and this may create some confusion (for example experimentalists reporting results on the “Standard Model Extension” are actually, according to the terminology now used by some theorists, describing experimental limits on the “Minimal Standard Model Extension”).
 27.
 28.
Since modern interferometers were designed to look for classical gravity waves (gravity waves are their sought “signal”), it is reasonable to denominate as “noise” all testmassdistance fluctuations that are not due to gravity waves. I adopt terminology that reflects the original objectives of modern interferometers, even though it is somewhat awkward for the type of quantumspacetimephenomenology studies discussed, in which interferometers would be used for searches of quantumgravityinduced distance fluctuations (and, therefore, in these studies quantumgravityinduced distance fluctuations would play the role of “signal”).
 29.
While most formulas in this review adopt ℏ = c = 1 conventions, I do make some exceptions (with explicit ℏ or c) when I believe it can help to characterize the conceptual ingredients of the formula.
 30.
The fact that, according to some of these test theories, quantumspacetimeinduced noise becomes increasingly significant as the characteristic frequency of observation is lowered, also opens the way to possible studies [492] using cryogenic resonators, which are rigid optical interferometers with good sensitivities down to frequencies of about 10^{−6} Hz.
 31.
 32.
 33.
It is not implausible that different particles would be characterized by different values of Κ. This in particular could reflect the expectation that more pointlike particles, such as neutrinos, should be more sensitive to the spacetimelattice structure with respect to composite particles (such as protons and, even more evidently, atoms). However, it appears natural to assume [396], at least in these first explorations of causalset phenomenology, that different particles would have values of Κ that are not too far apart.
 34.
 35.
For example, for Plancklength radii one might even imagine to satisfy the BekensteinHawking bound S ≤ R^{2} in a theory where entropy actually scales with a cubic law of the type S = αR^{3}, if the proportionality parameter α is such that S = αR^{3} ≤ R^{2}. But evidently for any such α there are values of the radius large enough that instead the BekensteinHawking bound would be violated.
 36.
 37.
 38.
As already stressed, this is not necessarily a natural expectation. In particular, several arguments appear to suggest that composite particles may be less sensitive to quantumspacetime effects than “fundamental” particles. Still, it is interesting to study this issue experimentally, and a way to do that is to look for opportunities for the “universality assumption” to break down.
 39.
 40.
References
 [1]Abbott, B.P. et al. (LIGO Scientific Collaboration), “LIGO: The Laser interferometer gravitationalwave observatory”, Rep. Prog. Phys., 72, 076901, (2009). [DOI], [arXiv:0711.3041 [grqc]]. (Cited on page 69.)ADSCrossRefGoogle Scholar
 [2]Abdo, A.A. et al., “Fermi Observations of GRB 090902B: A Distinct Spectral Component in the Prompt and Delayed Emission”, Astrophys. J., 706, L138–L144, (2009). [DOI], [arXiv:0909.2470 [astroph.HE]]. (Cited on pages 56 and 57.)ADSCrossRefGoogle Scholar
 [3]Abdo, A.A. et al. (The Fermi LAT and Fermi GBM Collaborations), “Fermi Observations of HighEnergy GammaRay Emission from GRB 080916C”, Science, 323, 1688–1693, (2009). [DOI], [ADS]. (Cited on pages 55, 56, and 57.)ADSCrossRefGoogle Scholar
 [4]Abdo, A.A. et al. (Fermi LAT and Fermi GBM), “A limit on the variation of the speed of light arising from quantum gravity effects”, Nature, 462, 331–334, (2009). (Cited on pages 55, 56, and 57.)ADSCrossRefGoogle Scholar
 [5]Abraham, J. et al. (The Pierre Auger Collaboration), “Correlation of the HighestEnergy Cosmic Rays with Nearby Extragalactic Objects”, Science, 318, 938–943, (2007). [DOI], [arXiv:0711.2256 [astroph]]. (Cited on pages 51 and 52.)ADSCrossRefGoogle Scholar
 [6]Abraham, J. et al. (Pierre Auger Collaboration), “Studies of Cosmic Ray Composition and Air Shower Structure with the Pierre Auger Observatory”, arXiv, eprint, (2009). [arXiv:0906.2319]. (Cited on page 53.)Google Scholar
 [7]Abraham, J. et al. (Pierre Auger Observatory), “Measurement of the Depth of Maximum of Extensive Air Showers above 10^{18} eV”, Phys. Rev. Lett., 104, 091101, (2010). [DOI], [arXiv:1002.0699 [astroph.HE]]. (Cited on page 51.)ADSCrossRefGoogle Scholar
 [8]Abraham, J. et al. (Pierre Auger collaboration), “Measurement of the energy spectrum of cosmic rays above 10^{18} eV using the Pierre Auger Observatory”, Phys. Lett. B, 685, 239–246, (2010). [DOI], [arXiv:1002.1975 [astroph.HE]]. (Cited on page 51.)ADSCrossRefGoogle Scholar
 [9]Abramovici, A. et al., “LIGO: The Laser Interferometer GravitationalWave Observatory”, Science, 256, 325–333, (1992). [DOI], [ADS]. (Cited on page 69.)ADSCrossRefGoogle Scholar
 [10]Abramowski, A. et al. (HESS Collaboration), “Search for Lorentz invariance breaking with a likelihood fit of the PKS 2155304 flare data taken on MJD 53944”, Astropart. Phys., 34, 738–747, (2011). [DOI], [arXiv:1101.3650 [astroph.HE]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [11]Abreu, P. et al. (Pierre Auger Observatory), “Update on the correlation of the highest energy cosmic rays with nearby extragalactic matter”, Astropart. Phys., 34, 314–326, (2010). [DOI], [arXiv:1009.1855]. (Cited on pages 51 and 52.)ADSCrossRefGoogle Scholar
 [12]Acernese, F. et al. (The Virgo Collaboration), “Virgo status”, Class. Quantum Grav., 25, 184001, (2008). [DOI], [ADS]. (Cited on page 69.)ADSCrossRefGoogle Scholar
 [13]Adler, R. et al. (CPLEAR Collaboration), “Test of CPT Symmetry and Quantum Mechanics with Experimental data from CPLEAR”, Phys. Lett. B, 364, 239–245, (1995). [DOI], [arXiv:hepex/9511001]. (Cited on pages 13, 80, and 82.)ADSCrossRefGoogle Scholar
 [14]Adunas, G.Z., RodriguezMilla, E. and Ahluwalia, D.V., “Probing quantum violations of the equivalence principle”, Gen. Relativ. Gravit., 33, 183–194, (2001). [grqc/0006022]. (Cited on pages 13 and 87.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [15]Aharonian, F. et al. (HEGRA Collaboration), “Reanalysis of the high energy cutoff of the 1997 Mkn 501 TeV energy spectrum”, Astron. Astrophys., 366, 62–67, (2000). [DOI], [arXiv:astroph/0011483]. (Cited on pages 48 and 49.)CrossRefGoogle Scholar
 [16]Aharonian, F. et al. (HEGRA Collaboration), “TeV gamma rays from the blazar H 1426+428 and the diffuse extragalactic background radiation”, Astron. Astrophys., 384, L23–L26, (2002). [DOI], [arXiv:astroph/0202072]. (Cited on pages 48 and 49.)ADSCrossRefGoogle Scholar
 [17]Aharonian, F. et al. (HEGRA Collaboration), “Variations of the TeV energy spectrum at different flux levels of Mkn 421 observed with the HEGRA system of Cherenkov telescopes”, Astron. Astrophys., 393, 89–99, (2002). [DOI], [arXiv:astroph/0205499]. (Cited on pages 48 and 49.)ADSCrossRefGoogle Scholar
 [18]Aharonian, F. et al. (HESS Collaboration), “Limits on an Energy Dependence of the Speed of Light from a Flare of the Active Galaxy PKS 2155304”, Phys. Rev. Lett., 101, 170402, (2008). [DOI], [arXiv:0810.3475 [astroph]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [19]Aharony, O., Gomis, J. and Mehen, T., “On theories with lightlike noncommutativity”, J. High Energy Phys., 09, 023, (2000). [arXiv:hepth/0006236]. (Cited on page 90.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [20]Ahluwalia, D.V., “Quantum measurements, gravitation, and locality”, Phys. Lett. B, 339, 301–303, (1994). [DOI], [arXiv:grqc/9308007]. (Cited on pages 12, 31, and 35.)ADSCrossRefGoogle Scholar
 [21]Ahluwalia, D.V., “Reconciling superkamiokande, LSND, and homestake neutrino oscillation data”, Mod. Phys. Lett. A, 13, 2249–2264, (1998). [hepph/9807267]. (Cited on page 32.)ADSCrossRefGoogle Scholar
 [22]Ahluwalia, D.V., “Waveparticle duality at the Planck scale: Freezing of neutrino oscillations”, Phys. Lett. A, 275, 31–35, (2000). (Cited on pages 32 and 58.)ADSCrossRefGoogle Scholar
 [23]Ahluwalia, D.V., “Ambiguity in source flux of cosmic / astrophysical neutrinos: Effects of bimaximal mixing and quantumgravity induced decoherence”, Mod. Phys. Lett. A, 16, 917–926, (2001). [DOI], [arXiv:hepph/0104316]. (Cited on page 84.)ADSMathSciNetCrossRefGoogle Scholar
 [24]Ahluwalia, D.V., “At the interface of quantum and gravitational realms”, arXiv, eprint, (2002). [arXiv:grqc/0202098]. (Cited on page 68.)Google Scholar
 [25]Ahluwalia, D.V. and Kirchbach, M., “Primordial spacetime foam as an origin of cosmological matterantimatter asymmetry”, Int. J. Mod. Phys. D, 10, 811–824, (2001). [DOI], [arXiv:astroph/0107246]. (Cited on page 68.)ADSCrossRefGoogle Scholar
 [26]AhluwaliaKhalilova, D.V., “Operational indistinguishabilty of doubly special relativities from special relativity”, arXiv, eprint, (2002). [arXiv:grqc/0212128]. (Cited on pages 36, 37, and 38.)Google Scholar
 [27]Akhundov, A.A., Bellucci, S. and Shiekh, A., “Gravitational interaction to one loop in effective quantum gravity”, Phys. Lett. B, 395, 16–23, (1997). [DOI], [arXiv:grqc/9611018 [grqc]]. (Cited on page 11.)ADSMathSciNetCrossRefGoogle Scholar
 [28]Akofor, E., Balachandran, A.P., Jo, S.G. and Joseph, A., “Quantum Fields on the GroenewoldMoyal Plane: C, P, T and CPT”, J. High Energy Phys., 08, 045, (2007). [DOI], [arXiv:0706.1259 [hepth]]. (Cited on page 79.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [29]Albert, J. et al. (MAGIC Collaboration), “Probing quantum gravity using photons from a flare of the active galactic nucleus Markarian 501 observed by the MAGIC telescope”, Phys. Lett. B, 668, 253–257, (2008). [DOI], [arXiv:0708.2889 [astroph]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [30]Albrecht, A. and Magueijo, J., “A time varying speed of light as a solution to cosmological puzzles”, Phys. Rev. D, 59, 043516, (1999). [DOI], [arXiv:astroph/9811018]. (Cited on page 97.)ADSCrossRefGoogle Scholar
 [31]Alesci, E. and Arzano, M., “Anomalous dimension in semiclassical gravity”, Phys. Lett. B, 707, 272–277, (2012). [DOI], [arXiv:1108.1507 [grqc]]. (Cited on page 98.)ADSMathSciNetCrossRefGoogle Scholar
 [32]Alexander, S., Brandenberger, R. and Magueijo, J., “Noncommutative inflation”, Phys. Rev. D, 67, 081301, (2003). [DOI], [arXiv:hepth/0108190]. (Cited on page 97.)ADSMathSciNetCrossRefGoogle Scholar
 [33]Alfaro, J., MoralesTécotl, H.A. and Urrutia, L.F., “Quantum gravity corrections to neutrino propagation”, Phys. Rev. Lett., 84, 2318–2321, (2000). [DOI], [arXiv:grqc/9909079]. (Cited on pages 15, 31, 36, 55, 90, and 91.)ADSCrossRefGoogle Scholar
 [34]Alfaro, J., MoralesTécotl, H.A. and Urrutia, L.F., “Quantum gravity and spin 1/2 particles effective dynamics”, Phys. Rev. D, 66, 124006, (2002). [DOI], [arXiv:hepth/0208192]. (Cited on pages 90 and 91.)ADSMathSciNetCrossRefGoogle Scholar
 [35]Alfaro, J. and Palma, G., “Loop quantum gravity corrections and cosmic rays decays”, Phys. Rev. D, 65, 103516, (2002). [DOI], [arXiv:hepth/0111176]. (Cited on page 50.)ADSCrossRefGoogle Scholar
 [36]Aloisio, R., Berezinsky, V., Blasi, P. and Ostapchenko, S., “Signatures of the transition from galactic to extragalactic cosmic rays”, Phys. Rev. D, 77, 025007, (2008). [DOI], [arXiv:0706.2834 [astroph]]. (Cited on page 53.)ADSCrossRefGoogle Scholar
 [37]Aloisio, R., Blasi, P., Galante, A., Ghia, P.L. and Grillo, A.F., “Space time fluctuations and ultra high energy cosmic ray interactions”, Astropart. Phys., 19, 127–133, (2003). [DOI], [arXiv:astroph/0205271]. (Cited on pages 75 and 77.)ADSCrossRefGoogle Scholar
 [38]Aloisio, R., Blasi, P., Ghia, P.L. and Grillo, A.F., “Probing the structure of spacetime with cosmic rays”, Phys. Rev. D, 62, 053010, (2000). [DOI], [arXiv:astroph/0001258]. (Cited on pages 14, 16, 17, 36, 42, 47, 50, and 51.)ADSCrossRefGoogle Scholar
 [39]Altschul, B., “Lorentz violation and synchrotron radiation”, Phys. Rev. D, 72, 085003, (2005). [DOI], [arXiv:hepth/0507258]. (Cited on page 60.)ADSCrossRefGoogle Scholar
 [40]Altschul, B., “Limits on Lorentz violation from synchrotron and inverse Compton sources”, Phys. Rev. Lett., 96, 201101, (2006). [DOI], [arXiv:hepph/0603138]. (Cited on page 54.)ADSCrossRefGoogle Scholar
 [41]Altschul, B., “Vacuum Cerenkov radiation in Lorentzviolating theories without CPT violation”, Phys. Rev. Lett., 98, 041603, (2007). [DOI], [arXiv:hepth/0609030]. (Cited on page 54.)ADSCrossRefGoogle Scholar
 [42]ÁlvarezGaumé, L. and Gomez, C., “Remarks on Quantum Gravity”, Commun. Math. Phys., 89, 235, (1983). [DOI]. (Cited on page 32.)ADSMathSciNetCrossRefGoogle Scholar
 [43]ÁlvarezGaumé, L. and VázquezMozo, M.A., “General properties of noncommutative field theories”, Nucl. Phys. B, 668, 293–321, (2003). [DOI], [arXiv:hepth/0305093]. (Cited on page 79.)ADSzbMATHCrossRefGoogle Scholar
 [44]Amati, D., Ciafaloni, M. and Veneziano, G., “Can spacetime be probed below the string size?”, Phys. Lett. B, 216, 41–47, (1989). [DOI]. (Cited on pages 12, 27, 31, and 33.)ADSCrossRefGoogle Scholar
 [45]Ambjørn, J., Jurkiewicz, J. and Kristjansen, C.F., “Quantum gravity, dynamical triangulations and higher derivative regularization”, Nucl. Phys. B, 393, 601–632, (1993). [DOI], [arXiv:hepth/9208032 [hepth]]. (Cited on pages 29 and 85.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [46]Ambjørn, J., Jurkiewicz, J. and Loll, R., “Emergence of a 4D world from causal quantum gravity”, Phys. Rev. Lett., 93, 131301, (2004). [DOI], [arXiv:hepth/0404156]. (Cited on pages 29 and 85.)ADSMathSciNetCrossRefGoogle Scholar
 [47]Ambjørn, J., Jurkiewicz, J. and Loll, R., “Reconstructing the universe”, Phys. Rev. D, 72, 064014, (2005). [DOI], [arXiv:hepth/0505154]. (Cited on pages 29 and 85.)ADSCrossRefGoogle Scholar
 [48]Ambjørn, J., Jurkiewicz, J. and Loll, R., “Spectral dimension of the universe”, Phys. Rev. Lett., 95, 171301, (2005). [DOI], [arXiv:hepth/0505113 [hepth]]. (Cited on pages 30 and 98.)ADSCrossRefGoogle Scholar
 [49]Ambjørn, J., Jurkiewicz, J. and Loll, R., “Causal dynamical triangulations and the quest for quantum gravity”, in Murugan, J., Weltman, A. and Ellis, G.F.R., eds., Foundations of Space and Time: Reflections on Quantum Gravity, pp. 321–337, (Cambridge University Press, Cambridge; New York, 2012). [arXiv:1004.0352 [hepth]]. (Cited on pages 29 and 85.)CrossRefGoogle Scholar
 [50]AmelinoCamelia, G., “Limits on the measurability of spacetime distances in the semiclassical approximation of quantum gravity”, Mod. Phys. Lett. A, 9, 3415–3422, (1994). [DOI], [arXiv:grqc/9603014]. (Cited on pages 12, 31, 32, 35, and 70.)ADSCrossRefGoogle Scholar
 [51]AmelinoCamelia, G., “Gravitywave interferometers as quantumgravity detectors”, Nature, 398, 216–218, (1999). [DOI], [arXiv:grqc/9808029]. (Cited on pages 14, 68, 70, 77, and 78.)ADSCrossRefGoogle Scholar
 [52]AmelinoCamelia, G., “Are We at the Dawn of QuantumGravity Phenomenology?”, in KowalskiGlikman, J., ed., Towards Quantum Gravity, Proceeding of the XXXV International Winter School on Theoretical Physics Held in Polanica, Poland, 2–11 February 1999, Lecture Notes in Physics, 541, pp. 1–49, (Springer, Berlin; New York, 2000). [arXiv:grqc/9910089]. (Cited on pages 9, 17, 20, 23, 58, and 66.)CrossRefGoogle Scholar
 [53]AmelinoCamelia, G., “Gravitywave interferometers as probes of a lowenergy effective quantum gravity”, Phys. Rev. D, 62, 024015, (2000). [DOI], [arXiv:grqc/9903080]. (Cited on pages 14, 68, 70, 77, and 78.)ADSCrossRefGoogle Scholar
 [54]AmelinoCamelia, G., “A phenomenological description of quantumgravityinduced spacetime noise”, Nature, 410, 1065–1069, (2001). [DOI], [arXiv:grqc/0104086]. (Cited on pages 14, 68, 70, 77, and 78.)ADSCrossRefGoogle Scholar
 [55]AmelinoCamelia, G., “Testable scenario for relativity with minimumlength”, Phys. Lett. B, 510, 255–263, (2001). [DOI], [arXiv:hepth/0012238]. (Cited on pages 31, 36, and 37.)ADSzbMATHCrossRefGoogle Scholar
 [56]AmelinoCamelia, G., “DoublySpecial Relativity: First Results and Key Open Problems”, Int. J. Mod. Phys. D, 11, 1643–1669, (2002). [DOI], [arXiv:grqc/0210063]. (Cited on page 36.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [57]AmelinoCamelia, G., “Quantumgravity phenomenology: Status and prospects”, Mod. Phys. Lett. A, 17, 899–922, (2002). [DOI], [arXiv:grqc/0204051]. (Cited on pages 67, 72, 75, and 77.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [58]AmelinoCamelia, G., “Relativity in spacetimes with shortdistance structure governed by an observerindependent (Planckian) length scale”, Int. J. Mod. Phys. D, 11, 35–60, (2002). [DOI], [arXiv:grqc/0012051]. (Cited on pages 31, 36, 37, 38, and 50.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [59]AmelinoCamelia, G., “Spacetime quantum solves three experimental paradoxes”, Phys. Lett. B, 528, 181–187, (2002). [DOI], [arXiv:grqc/0107086]. (Cited on pages 45, 50, and 53.)ADSCrossRefGoogle Scholar
 [60]AmelinoCamelia, G., “Kinematical solution of the UHEcosmicray puzzle without a preferred class of inertial observers”, Int. J. Mod. Phys. D, 12, 1211–1226, (2003). [DOI], [arXiv:astroph/0209232]. (Cited on page 40.)ADSCrossRefGoogle Scholar
 [61]AmelinoCamelia, G., “Proposal of a second generation of quantumgravitymotivated Lorentzsymmetry tests: Sensitivity to effects suppressed quadratically by the Planck scale”, Int. J. Mod. Phys. D, 12, 1633–1640, (2003). [DOI], [arXiv:grqc/0305057]. (Cited on page 59.)ADSCrossRefGoogle Scholar
 [62]AmelinoCamelia, G., “Phenomenology of Planckscale Lorentzsymmetry test theories”, New J. Phys., 6, 188, (2004). [DOI], [arXiv:grqc/0212002]. (Cited on pages 23, 44, 49, 60, and 61.)ADSCrossRefGoogle Scholar
 [63]AmelinoCamelia, G., “DoublySpecial Relativity: Facts, Myths and Some Key Open Issues”, Symmetry, 2, 230–271, (2010). [arXiv:1003.3942 [grqc]]. (Cited on pages 32, 36, 37, 47, 50, 52, and 53.)MathSciNetzbMATHCrossRefGoogle Scholar
 [64]AmelinoCamelia, G. and Arzano, M., “Coproduct and star product in field theories on Liealgebra noncommutative spacetimes”, Phys. Rev. D, 65, 084044, (2002). [DOI], [arXiv:hepth/0105120]. (Cited on page 40.)ADSMathSciNetCrossRefGoogle Scholar
 [65]AmelinoCamelia, G., Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “Distance measurement and wave dispersion in a Liouvillestring approach to quantum gravity”, Int. J. Mod. Phys. A, 12, 607–624, (1997). [DOI], [arXiv:hepth/9605211]. (Cited on pages 29, 42, and 59.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [66]AmelinoCamelia, G., Ellis, J.R., Mavromatos, N.E., Nanopoulos, D.V. and Sarkar, S., “Potential Sensitivity of GammaRay Burster Observations to Wave Dispersion in Vacuo”, Nature, 393, 763–765, (1998). [DOI], [arXiv:astroph/9712103]. (Cited on pages 14, 36, 42, 55, and 77.)ADSCrossRefGoogle Scholar
 [67]AmelinoCamelia, G., Freidel, L., KowalskiGlikman, J. and Smolin, L., “Principle of relative locality”, Phys. Rev. D, 84, 084010 (2011). [DOI], [arXiv:1101.0931 [hepth]]. (Cited on pages 36 and 38.)ADSzbMATHCrossRefGoogle Scholar
 [68]AmelinoCamelia, G. and Lämmerzahl, C., “Quantumgravity motivated Lorentz symmetry tests with laser interferometers”, Class. Quantum Grav., 21, 899–916, (2004). [DOI], [arXiv:grqc/0306019]. (Cited on pages 62 and 63.)ADSzbMATHCrossRefGoogle Scholar
 [69]AmelinoCamelia, G., Lämmerzahl, C., Mercati, F. and Tino, G.M., “Constraining the EnergyMomentum Dispersion Relation with PlanckScale Sensitivity Using Cold Atoms”, Phys. Rev. Lett., 103, 171302, (2009). [DOI], [arXiv:0911.1020 [grqc]]. (Cited on pages 90, 91, and 92.)ADSCrossRefGoogle Scholar
 [70]AmelinoCamelia, G. and Majid, S., “Waves on noncommutative spacetime and gammaray bursts”, Int. J. Mod. Phys. A, 15, 4301–4324, (2000). [DOI], [arXiv:hepth/9907110]. (Cited on pages 28, 32, 55, and 81.)ADSMathSciNetzbMATHGoogle Scholar
 [71]AmelinoCamelia, G., Matassa, M., Mercati, F. and Rosati, G., “Taming nonlocality in theories with deformed Lorentz symmetry”, Phys. Rev. Lett., 106, 071301, (2011). [arXiv:1006.2126 [grqc]]. (Cited on page 36.)ADSCrossRefGoogle Scholar
 [72]AmelinoCamelia, G., Ng, Y.J. and Vanm Dam, H., “Anomalous particleproduction thresholds through systematic and nonsystematic quantumgravity effects”, Astropart. Phys., 19, 729–738, (2003). [DOI], [arXiv:grqc/0204077]. (Cited on pages 75 and 77.)ADSCrossRefGoogle Scholar
 [73]AmelinoCamelia, G. and Piran, T., “Planckscale deformation of Lorentz symmetry as a solution to the UHECR and the TeVgamma paradoxes”, Phys. Rev. D, 64, 036005, (2001). [DOI], [arXiv:astroph/0008107]. (Cited on pages 14, 16, 17, 36, 42, 47, 50, and 51.)ADSCrossRefGoogle Scholar
 [74]AmelinoCamelia, G. and Smolin, L., “Prospects for constraining quantum gravity dispersion with near term observations”, Phys. Rev. D, 80, 084017, (2009). [DOI], [arXiv:0906.3731 [astroph.HE]]. (Cited on pages 42, 55, 57, 59, 75, and 77.)ADSCrossRefGoogle Scholar
 [75]AmelinoCamelia, G., Smolin, L. and Starodubtsev, A., “Quantum symmetry, the cosmological constant and Planck scale phenomenology”, Class. Quantum Grav., 21, 3095–3110, (2004). [DOI], [arXiv:hepth/0306134]. (Cited on pages 15, 31, and 67.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [76]Anandan, J., “Gravitationally coupled electromagnetic systems and quantum interference”, Class. Quantum Grav., 1, L51 (1984). (Cited on page 13.)ADSMathSciNetCrossRefGoogle Scholar
 [77]Anandan, J., “Relativistic thermoelectromagnetic gravitational effects in normal conductors and superconductors”, Phys. Lett. A, 105, 280–284, (1984). (Cited on page 13.)ADSCrossRefGoogle Scholar
 [78]Anselmi, D., “Weighted power counting, neutrino masses and Lorentz violating extensions of the Standard Model”, Phys. Rev. D, 79, 025017, (2009). [DOI], [arXiv:0808.3475 [hepph]]. (Cited on page 45.)ADSCrossRefGoogle Scholar
 [79]Anselmi, D. and Halat, M., “Renormalization of Lorentz violating theories”, Phys. Rev. D, 76, 125011 (2007). [DOI], [arXiv:0707.2480 [hepth]]. (Cited on page 45.)ADSzbMATHCrossRefGoogle Scholar
 [80]Antoniadis, I., “A possible new dimension at a few TeV”, Phys. Lett. B, 246, 377–384, (1990). [DOI]. (Cited on pages 26 and 101.)ADSMathSciNetCrossRefGoogle Scholar
 [81]Antonov, E.E., Dedenko, L.G., Kirillov, A.A., Roganova, T.M., Fedorova, G.F. and Fedunin, E.Y., “Test of Lorentz Invariance through Observation of the Longitudinal Development of UltrahighEnergy Extensive Air Showers”, JETP Lett., 73, 446–450, (2001). [DOI], [ADS]. (Cited on page 53.)ADSCrossRefGoogle Scholar
 [82]Appelquist, T., Cheng, H.C. and Dobrescu, B.A., “Bounds on universal extra dimensions”, Phys. Rev. D, 64, 035002, (2001). [DOI], [arXiv:hepph/0012100]. (Cited on page 102.)ADSCrossRefGoogle Scholar
 [83]Arias, P., Gamboa, J., LopezSarrion, J., Mendez, F. and Das, A.K., “CPT / Lorentz invariance violation and neutrino oscillation”, Phys. Lett. B, 650, 401–406, (2007). [DOI], [arXiv:hepph/0608007]. (Cited on page 59.)ADSCrossRefGoogle Scholar
 [84]ArkaniHamed, N., Dimopoulos, S. and Dvali, G.R., “The hierarchy problem and new dimensions at a millimeter”, Phys. Lett. B, 429, 263–272, (1998). [DOI], [arXiv:hepph/9803315]. (Cited on pages 26, 101, and 102.)ADSCrossRefGoogle Scholar
 [85]ArkaniHamed, N., Dimopoulos, S. and MarchRussell, J., “Stabilization of submillimeter dimensions: The new guise of the hierarchy problem”, Phys. Rev. D, 63, 064020, (2001). [DOI], [arXiv:hepth/9809124]. (Cited on page 26.)ADSCrossRefGoogle Scholar
 [86]Arzano, M. and Benedetti, D., “Rainbow statistics”, Int. J. Mod. Phys. A, 24, 4623–4641, (2009). [DOI], [arXiv:0809.0889 [hepth]]. (Cited on page 85.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [87]Arzano, M., Calcagni, G., Oriti, D. and Scalisi, M., “Fractional and noncommutative spacetimes”, Phys. Rev. D, 84, 125002, (2011). [DOI], [arXiv:1107.5308 [hepth]]. (Cited on page 98.)ADSCrossRefGoogle Scholar
 [88]Arzano, M. and KowalskiGlikman, J., “Kinematics of a relativistic particle with de Sitter momentum space”, Class. Quantum Grav., 28, 105009, (2011). [DOI], [arXiv: 1008.2962 [hepth]]. (Cited on page 36.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [89]Arzano, M., KowalskiGlikman, J. and Walkus, A., “A Bound on Planckscale modifications of the energymomentum composition rule from atomic interferometry”, Europhys. Lett., 90, 30006, (2010). [DOI], [arXiv:0912.2712 [hepth]]. (Cited on page 92.)ADSCrossRefGoogle Scholar
 [90]Aschieri, P., “Duality rotations and BPS monopoles with space and time noncommutativity”, Nucl. Phys. B, 617, 321–347, (2001). [DOI], [arXiv:hepth/0106281]. (Cited on page 90.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [91]Ashtekar, A., “Quantum mechanics of geometry”, arXiv, eprint, (1999). [arXiv:grqc/9901023]. (Cited on page 15.)Google Scholar
 [92]Ashtekar, A., “Some recent advances in loop quantum cosmology”, J. Phys.: Conf. Ser., 360, 012001, (2012). [DOI]. (Cited on pages 27 and 98.)ADSGoogle Scholar
 [93]Ashtekar, A., “Introduction to Loop Quantum Gravity”, in Calcagni, G., Papantonopoulos, L., Siopsis, G. and Tsamis, N., eds., Quantum Gravity and Quantum Cosmology, Sixth Aegean School, held in Chora on Naxos Island, Greece, 12–17 September 2011, Lecture Notes in Physics, 863, pp. 31–56, (Springer, Berlin; New York, 2013). [DOI], [arXiv: 1201.4598 [grqc]]. (Cited on pages 15 and 27.)CrossRefGoogle Scholar
 [94]Ashtekar, A., Bojowald, M. and Lewandowski, J., “Mathematical structure of loop quantum cosmology”, Adv. Theor. Math. Phys., 7, 233–268, (2003). [arXiv:grqc/0304074]. (Cited on pages 27 and 98.)MathSciNetCrossRefGoogle Scholar
 [95]Ashtekar, A. and Lewandowski, J., “Quantum theory of geometry. I: Area operators”, Class. Quantum Grav., 14, A55–A82, (1997). [DOI], [arXiv:grqc/9602046]. (Cited on page 27.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [96]Ashtekar, A. and Lewandowski, J., “Background independent quantum gravity: A status report”, Class. Quantum Grav., 21, R53–R152, (2004). [DOI], [arXiv:grqc/0404018 [grqc]]. (Cited on pages 15 and 27.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [97]Balachandran, A.P., Joseph, A. and Padmanabhan, P., “NonPauli Transitions From Spacetime Noncommutativity”, Phys. Rev. Lett., 105, 051601, (2010). [DOI], [arXiv: 1003.2250 [hepth]]. (Cited on page 85.)ADSMathSciNetCrossRefGoogle Scholar
 [98]Balachandran, A.P., Mangano, G., Pinzul, A. and Vaidya, S., “Spin and statistics on the GroenwaldMoyal plane: Pauliforbidden levels and transitions”, Int. J. Mod. Phys. A, 21, 3111–3126, (2006). [DOI], [arXiv:hepth/0508002]. (Cited on pages 28 and 85.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [99]Balachandran, A.P. and Padmanabhan, P., “NonPauli Effects from Noncommutative Spacetimes”, J. High Energy Phys., 1012, 001, (2010). [DOI], [arXiv:1006.1185 [hepth]]. (Cited on page 85.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [100]Balachandran, A.P., Pinzul, A. and Queiroz, A.R., “Twisted Poincare Invariance, Noncommutative Gauge Theories and UVIR Mixing”, Phys. Lett. B, 668, 241–245, (2008). [DOI], [arXiv:0804.3588 [hepth]]. (Cited on page 31.)ADSMathSciNetCrossRefGoogle Scholar
 [101]Banerjee, R., “Dissipation and Noncommutativity in Planar Quantum Mechanics”, Mod. Phys. Lett. A, 17, 631, (2002). [DOI], [arXiv:hepth/0106280]. (Cited on page 26.)ADSzbMATHCrossRefGoogle Scholar
 [102]Banerjee, R., Dutta Roy, B. and Samanta, S., “Remarks on the noncommutative gravitational quantum well”, Phys. Rev. D, 74, 045015, (2006). [DOI], [arXiv:hepth/0605277]. (Cited on page 95.)ADSCrossRefGoogle Scholar
 [103]Barcelo, C., Visser, M. and Liberati, S., “Einstein gravity as an emergent phenomenon?”, Int. J. Mod. Phys. D, 10, 799–806, (2001). [DOI], [grqc/0106002]. (Cited on page 30.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [104]Barrow, J.D., “Cosmologies with varying light speed”, Phys. Rev. D, 59, 043515, (1999). [DOI]. (Cited on page 97.)ADSMathSciNetCrossRefGoogle Scholar
 [105]Bartalucci, S. et al. (VIP Collaboration), “New experimental limit on the Pauli exclusion principle violation by electrons”, Phys. Lett. B, 641, 18–22, (2006). [DOI], [arXiv:quantph/0605047]. (Cited on page 85.)ADSCrossRefGoogle Scholar
 [106]Basu, S. and Mattingly, D., “Constraints from cosmic rays on nonsystematic Lorentz violation”, Class. Quantum Grav., 22, 3029–3044, (2005). [DOI], [astroph/0501425]. (Cited on page 77.)ADSzbMATHCrossRefGoogle Scholar
 [107]Bellini, G. et al. (Borexino Collaboration), “New experimental limits on the Pauli forbidden transitions in C12 nuclei obtained with 485 days Borexino data”, Phys. Rev. C, 81, 034317, (2010). [DOI], [arXiv:0911.0548 [hepex]]. (Cited on page 85.)ADSCrossRefGoogle Scholar
 [108]Benatti, F. and Floreanini, R., “Completely positive dynamical maps and the neutral kaon system”, Nucl. Phys. B, 488, 335–363, (1997). [DOI]. (Cited on pages 13, 80, and 82.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [109]Benatti, F. and Floreanini, R., “Open system approach to neutrino oscillations”, J. High Energy Phys., 2000(02), 032, (2000). [DOI], [arXiv:hepph/0002221]. (Cited on page 84.)CrossRefGoogle Scholar
 [110]Benedetti, D., “Fractal properties of quantum spacetime”, Phys. Rev. Lett., 102, 111303, (2009). [DOI], [arXiv:0811.1396 [hepth]]. (Cited on page 98.)ADSMathSciNetCrossRefGoogle Scholar
 [111]Berezinsky, V., “Puzzles in astrophysics in the past and present”, Phys. Atom. Nucl., 66, 423–434, (2003). [DOI], [arXiv:astroph/0107306]. (Cited on pages 48 and 51.)ADSCrossRefGoogle Scholar
 [112]Bernabeu, J., Mavromatos, N.E. and Papavassiliou, J., “Novel type of CPT violation for correlated EPR states”, Phys. Rev. Lett., 92, 131601, (2004). [DOI], [arXiv:hepph/0310180]. (Cited on pages 80 and 81.)ADSCrossRefGoogle Scholar
 [113]Bernabeu, J., Mavromatos, N.E. and Sarkar, S., “Decoherence induced CPT violation and entangled neutral mesons”, Phys. Rev. D, 74, 045014, (2006). [DOI], [arXiv:hepth/0606137]. (Cited on pages 80 and 81.)ADSCrossRefGoogle Scholar
 [114]Bernadotte, S. and Klinkhamer, F.R., “Bounds on length scales of classical spacetime foam models”, Phys. Rev. D, 75, 024028, (2007). [DOI], [arXiv:hepph/0610216]. (Cited on page 16.)ADSCrossRefGoogle Scholar
 [115]Bertolami, O., “Threshold Effects and Lorentz Symmetry”, in Elze, H.T., ed., Decoherence and Entropy in Complex Systems, Selected Lectures from DICE 2002, Lecture Notes in Physics, 633, pp. 96–102, (Springer, Berlin; New York, 2004). [DOI], [arXiv:hepph/0301191]. (Cited on pages 45, 50, and 53.)CrossRefGoogle Scholar
 [116]Bertolami, O. and Carvalho, C.S., “Proposed astrophysical test of Lorentz invariance”, Phys. Rev. D, 61, 103002, (2000). [DOI], [arXiv:grqc/9912117]. (Cited on page 59.)ADSCrossRefGoogle Scholar
 [117]Bertolami, O., Colladay, D., Kostelecký, V.A. and Potting, R., “CPT violation and baryogenesis”, Phys. Lett. B, 395, 178–183, (1997). [DOI], [arXiv:hepph/9612437]. (Cited on pages 32 and 79.)ADSCrossRefGoogle Scholar
 [118]Bertolami, O., Rosa, J.G., de Aragao, C.M.L., Castorina, P. and Zappala, D., “Noncommutative gravitational quantum well”, Phys. Rev. D, 72, 025010, (2005). [DOI], [arXiv:hepth/0505064]. (Cited on page 95.)ADSMathSciNetCrossRefGoogle Scholar
 [119]Biller, S.D. et al., “Limits to Quantum Gravity Effects on Energy Dependence of the Speed of Light from Observations of TeV Flares in Active Galaxies”, Phys. Rev. Lett., 83, 2108–2111, (1999). [DOI], [arXiv:grqc/9810044]. (Cited on page 14.)ADSCrossRefGoogle Scholar
 [120]BjerrumBohr, N.E.J., Donoghue, J.F. and Holstein, B.R., “Quantum gravitational corrections to the nonrelativistic scattering potential of two masses”, Phys. Rev. D, 67, 084033, (2003). [DOI], [arXiv:hepth/0211072 [hepth]]. (Cited on page 11.)ADSMathSciNetCrossRefGoogle Scholar
 [121]Blasone, M., Magueijo, J. and PiresPacheco, P., “Neutrino mixing and Lorentz invariance”, Europhys. Lett., 70, 600, (2005). [DOI], [arXiv:hepph/0307205]. (Cited on page 93.)ADSCrossRefGoogle Scholar
 [122]Blaut, A., Daszkiewicz, M., KowalskiGlikman, J. and Nowak, S., “Phase spaces of doubly special relativity”, Phys. Lett. B, 582, 82–85, (2004). [DOI], [arXiv:hepth/0312045]. (Cited on pages 32 and 58.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [123]Bluhm, R., “Overview of the Standard Model Extension: Implications and Phenomenology of Lorentz Violation”, in Ehlers, J. and Lämmerzahl, C., eds., Special Relativity: Will it Survive the Next 101 Years?, 71st WEHeraeus Seminar, Potsdam from February 13–18, 2005, Lecture Notes in Physics, 702, pp. 191–226, (Springer, Berlin; New York, 2006). [DOI], [arXiv:hepph/0506054]. (Cited on pages 64 and 65.)CrossRefGoogle Scholar
 [124]Boggs, S.E. and Coburn, W., “Statistical Uncertainty in the ReAnalysis of Polarization in GRB021206”, arXiv, eprint, (2003). [arXiv:astroph/0310515]. (Cited on page 62.)Google Scholar
 [125]Bojowald, M., “Absence of singularity in loop quantum cosmology”, Phys. Rev. Lett., 86, 5227–5230, (2001). [DOI], [arXiv:grqc/0102069]. (Cited on pages 27 and 98.)ADSMathSciNetCrossRefGoogle Scholar
 [126]Bojowald, M., “Loop Quantum Cosmology”, Living Rev. Relativity, 11, lrr20084 (2008). [DOI]. URL (accessed 10 June 2013): http://www.livingreviews.org/lrr20084. (Cited on pages 27 and 98.)
 [127]Bojowald, M., Calcagni, G. and Tsujikawa, S., “Observational constraints on loop quantum cosmology”, Phys. Rev. Lett., 107, 211302, (2011). [DOI], [arXiv:1101.5391 [astroph.CO]]. (Cited on page 98.)ADSCrossRefGoogle Scholar
 [128]Bojowald, M., MoralesTécotl, H.A. and Sahlmann, H., “On loop quantum gravity phenomenology and the issue of Lorentz invariance”, Phys. Rev. D, 71, 084012, (2005). [DOI], [arXiv:grqc/0411101]. (Cited on page 15.)ADSMathSciNetCrossRefGoogle Scholar
 [129]Bolmont, J. and Jacholkowska, A., “Lorentz symmetry breaking studies with photons from astrophysical observations”, Adv. Space Res., 47, 380–391, (2011). [DOI], [arXiv:1007.4954 [astroph.HE]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [130]Bolokhov, P.A., Groot Nibbelink, S. and Pospelov, M., “Lorentz violating supersymmetric quantum electrodynamics”, Phys. Rev. D, 72, 015013, (2005). [DOI], [arXiv:hepph/0505029]. (Cited on page 45.)ADSCrossRefGoogle Scholar
 [131]Bombelli, L., Lee, J., Meyer, D. and Sorkin, R.D., “SpaceTime as a Causal Set”, Phys. Rev. Lett., 59, 521–524, (1987). [DOI]. (Cited on pages 29 and 85.)ADSMathSciNetCrossRefGoogle Scholar
 [132]Bombelli, L. and Winkler, O., “Comparison of QG induced dispersion with standard physics effects”, Class. Quantum Grav., 21, L89–L96, (2004). [grqc/0403049]. (Cited on page 55.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [133]Borgman, J. and Ford, L.H., “Effects of stress tensor fluctuations upon focusing”, Phys. Rev. D, 70, 064032, (2004). [DOI], [arXiv:grqc/0307043 [grqc]]. (Cited on page 97.)ADSMathSciNetCrossRefGoogle Scholar
 [134]Brandenberger, R.H., “Inflationary cosmology: Progress and problems”, in Mansouri, R. and Brandenberger, R.H., eds., Large Scale Structure Formation, 1st Iranian International School on Cosmology, Kish Island, Iran, 22 January–4 February 1999, Astrophysics and Space Science Library, 247, pp. 169–211, (Kluwer; Springer, Dordrecht, 2000). [DOI], [arXiv:hepph/9910410 [hepph]]. (Cited on page 96.)CrossRefGoogle Scholar
 [135]Brandenberger, R.H., “Do we have a Theory of Early Universe Cosmology?”, arXiv, eprint, (2012). [arXiv:1204.6108 [astroph.CO]]. (Cited on page 97.)Google Scholar
 [136]Brandenberger, R.H. and Martin, J., “The robustness of inflation to changes in superPlanckscale physics”, Mod. Phys. Lett. A, 16, 999–1006, (2001). [DOI], [arXiv:astroph/0005432]. (Cited on page 97.)ADSzbMATHCrossRefGoogle Scholar
 [137]Brau, F. and Buisseret, F., “Minimal length uncertainty relation and gravitational quantum well”, Phys. Rev. D, 74, 036002, (2006). [DOI], [arXiv:hepth/0605183]. (Cited on page 95.)ADSCrossRefGoogle Scholar
 [138]Briscese, F., “Trapped BoseEinstein condensates with Planckscale induced deformation of the energymomentum dispersion relation”, Phys. Lett. B, 718, 214–217, (2012). [DOI], [arXiv:1206.1236]. (Cited on page 93.)ADSCrossRefGoogle Scholar
 [139]Briscese, F., Grether, M. and de Llano, M., “Planckscale effects on BoseEinstein condensates”, Europhys. Lett., 98, 60001, (2012). [DOI], [arXiv: 1204.4670 [grqc]]. (Cited on page 93.)ADSCrossRefGoogle Scholar
 [140]Bruno, N.R., AmelinoCamelia, G. and KowalskiGlikman, J., “Deformed boost transformations that saturate at the Planck scale”, Phys. Lett. B, 522, 133–138, (2001). [DOI], [arXiv:hepth/0107039]. (Cited on pages 36 and 37.)ADSzbMATHCrossRefGoogle Scholar
 [141]Brustein, R., Eichler, D. and Foffa, S., “Probing the Planck scale with neutrino oscillations”, Phys. Rev. D, 65, 105006, (2002). [DOI], [arXiv:hepph/0106309]. (Cited on pages 59 and 60.)ADSMathSciNetCrossRefGoogle Scholar
 [142]Brustein, R., Gasperini, M., Giovannini, M., Mukhanov, V.F. and Veneziano, G., “Metric perturbations in dilaton driven inflation”, Phys. Rev. D, 51, 6744–6756, (1995). [DOI], [arXiv:hepth/9501066]. (Cited on page 100.)ADSCrossRefGoogle Scholar
 [143]Brustein, R., Gasperini, M., Giovannini, M. and Veneziano, G., “Relic gravitational waves from string cosmology”, Phys. Lett. B, 361, 45–51, (1995). [DOI], [arXiv:hepth/9507017]. (Cited on page 100.)ADSMathSciNetCrossRefGoogle Scholar
 [144]Burgess, C.P., “Quantum Gravity in Everyday Life: General Relativity as an Effective Field Theory”, Living Rev. Relativity, 7, lrr20045 (2004). [DOI], [arXiv:grqc/0311082 [grqc]]. URL (accessed 10 June 2013): http://www.livingreviews.org/lrr20045. (Cited on page 7.)
 [145]Burgess, C.P., “Lectures on cosmic inflation and its potential stringy realizations”, Class. Quantum Grav., 24, 795, (2007). [DOI], [arXiv:0708.2865 [hepth]]. (Cited on page 97.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [146]Calmet, X., Hsu, S.D.H. and Reeb, D., “Grand unification and enhanced quantum gravitational effects”, Phys. Rev. Lett., 101, 171802, (2008). [DOI], [0805.0145 [hepph]]. (Cited on page 19.)ADSMathSciNetCrossRefGoogle Scholar
 [147]Calmet, X., Hsu, S.D.H. and Reeb, D., “Grand unification through gravitational effects”, Phys. Rev. D, 81, 035007, (2010). [DOI], [arXiv:0911.0415 [hepph]]. (Cited on page 19.)ADSCrossRefGoogle Scholar
 [148]Camacho, A., “Flavoroscillation clocks, continuous quantum measurements and a violation of Einstein equivalence principle”, Mod. Phys. Lett. A, 14, 2545–2556, (1999). [DOI], [arXiv:grqc/9911112]. (Cited on page 87.)ADSCrossRefGoogle Scholar
 [149]Camacho, A., “Decoherenceinduced violations of Einstein equivalence principle”, Int. J. Mod. Phys. D, 10, 767–774, (2001). [DOI], [arXiv:grqc/0107028]. (Cited on page 33.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [150]Carlip, S., “Spacetime foam and the cosmological constant”, Phys. Rev. Lett., 79, 4071–4074, (1997). [DOI], [arXiv:grqc/9708026 [grqc]]. (Cited on page 67.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [151]Carlip, S., “Quantum gravity: A progress report”, Rep. Prog. Phys., 64, 885–942, (2001). [DOI], [arXiv:grqc/0108040]. (Cited on page 15.)ADSMathSciNetCrossRefGoogle Scholar
 [152]Carlip, S., “Quantum Gravity in 2+1 Dimensions: The Case of a Closed Universe”, Living Rev. Relativity, 8, lrr20051 (2005). [DOI], [arXiv:grqc/0409039 [grqc]]. URL (accessed 10 June 2013): http://www.livingreviews.org/lrr20051. (Cited on page 67.)
 [153]Carlip, S., Mosna, R.A. and Pitelli, J.P.M., “Vacuum Fluctuations and the Small Scale Structure of Spacetime”, Phys. Rev. Lett., 107, 021303, (2011). [DOI], [arXiv:1103.5993 [grqc]]. (Cited on page 98.)ADSCrossRefGoogle Scholar
 [154]Carmona, J.M. and Cortes, J.L., “Testing Lorentz invariance violations in the tritium betadecay anomaly”, Phys. Lett. B, 494, 75–80, (2000). [DOI], [arXiv:hepph/0007057]. (Cited on pages 90, 91, 93, and 94.)ADSCrossRefGoogle Scholar
 [155]Carmona, J.M. and Cortes, J.L., “Infrared and ultraviolet cutoffs of quantum field theory”, Phys. Rev. D, 65, 025006, (2002). [DOI], [arXiv:hepth/0012028]. (Cited on pages 90 and 91.)ADSCrossRefGoogle Scholar
 [156]Carmona, J.M., Cortés, J.L. and Induráin, J., “Interpretation of neutrino oscillations based on new physics in the infrared”, J. High Energy Phys., 2008(06), 033, (2008). [DOI], [arXiv:0709.2267 [hepph]]. (Cited on page 60.)CrossRefGoogle Scholar
 [157]Caron, B. et al. (The Virgo Collaboration), “The Virgo interferometer”, Class. Quantum Grav., 14, 1461–1469, (1997). [DOI], [ADS]. (Cited on page 69.)ADSGoogle Scholar
 [158]Carroll, S.M., Field, G.B. and Jackiw, R., “Limits on a Lorentz and parityviolating modification of electrodynamics”, Phys. Rev. D, 41, 1231–1240, (1990). [DOI]. (Cited on page 61.)ADSCrossRefGoogle Scholar
 [159]Carroll, S.M. and Lim, E.A., “Lorentzviolating vector fields slow the universe down”, Phys. Rev. D, 70, 123525, (2004). [DOI], [arXiv:hepth/0407149]. (Cited on page 99.)ADSCrossRefGoogle Scholar
 [160]Chaichian, M., Dolgov, A.D., Novikov, V.A. and Tureanu, A., “CPT Violation Does Not Lead to Violation of Lorentz Invariance and Vice Versa”, Phys. Lett. B, 699, 177–180, (2011). [DOI], [arXiv:1103.0168 [hepth]]. (Cited on page 79.)ADSCrossRefGoogle Scholar
 [161]Chaichian, M., Kulish, P.P., Nishijima, K. and Tureanu, A., “On a Lorentzinvariant interpretation of noncommutative spacetime and its implications on noncommutative QFT”, Phys. Lett. B, 604, 98–102, (2004). [DOI], [arXiv:hepth/0408069]. (Cited on page 31.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [162]Chaichian, M., Nishijima, K. and Tureanu, A., “Spinstatistics and CPT theorems in noncommutative field theory”, Phys. Lett. B, 568, 146–152, (2003). [DOI], [arXiv:hepth/0209008]. (Cited on page 79.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [163]Chakraborty, B., Gangopadhyay, S., Hazra, A.G. and Scholtz, F.G., “Twisted Galilean symmetry and the Pauli principle at low energies”, J. Phys. A: Math. Gen., 39, 9557–9572, (2006). [DOI], [arXiv:hepth/0601121 [hepth]]. (Cited on page 85.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [164]Chandrasekhar, S., “The maximum mass of ideal white dwarfs”, Astrophys. J., 74, 81–82, (1931). [DOI]. (Cited on page 12.)ADSzbMATHCrossRefGoogle Scholar
 [165]Chandrasekhar, S., “The highly collapsed configurations of a stellar mass (Second paper)”, Mon. Not. R. Astron. Soc., 95, 207–225, (1935). [ADS]. (Cited on page 12.)ADSzbMATHCrossRefGoogle Scholar
 [166]Chapline, G., Hohlfeld, E., Laughlin, R.B. and Santiago, D.I., “Quantum phase transitions and the breakdown of classical general relativity”, Int. J. Mod. Phys. A, 18, 3587–3590, (2003). [DOI], [arXiv:grqc/0012094]. (Cited on page 36.)ADSCrossRefGoogle Scholar
 [167]Chen, Y. and Wen, L., “Probing Spacetime Foam with Photons: Suppression of Observable Effects due to Uncertainty in Optical Paths”, arXiv, eprint, (2006). [arXiv:grqc/0605093 [grqc]]. (Cited on pages 77 and 78.)Google Scholar
 [168]Choubey, S. and King, S.F., “Gamma ray bursts as probes of neutrino mass, quantum gravity, and dark energy”, Phys. Rev. D, 67, 073005, (2003). [DOI], [arXiv:hepph/0207260]. (Cited on page 59.)ADSCrossRefGoogle Scholar
 [169]Christian, J., “Testing quantum gravity via cosmogenic neutrino oscillations”, Phys. Rev. D, 71, 024012, (2005). [grqc/0409077]. (Cited on page 59.)ADSCrossRefGoogle Scholar
 [170]Christiansen, W.A., Ng, Y.J., Floyd, D.J.E. and Perlman, E.S., “Limits on Spacetime Foam”, Phys. Rev. D, 83, 084003, (2011). [DOI], [arXiv:0912.0535 [astroph.CO]]. (Cited on pages 70, 71, and 72.)ADSCrossRefGoogle Scholar
 [171]Christiansen, W.A., Ng, Y.J. and van Dam, H., “Probing spacetime foam with extragalactic sources”, Phys. Rev. Lett., 96, 051301, (2006). [DOI], [arXiv:grqc/0508121 [grqc]]. (Cited on pages 77, 78, and 79.)ADSMathSciNetCrossRefGoogle Scholar
 [172]Chu, C.S., Greene, B.R. and Shiu, G., “Remarks on inflation and noncommutative geometry”, Mod. Phys. Lett. A, 16, 2231–2240, (2001). [DOI], [arXiv:hepth/0011241]. (Cited on page 97.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [173]Coburn, W. and Boggs, S.E., “Polarization of the prompt γray emission from the γray burst of 6 December 2002”, Nature, 423, 415–417, (2003). [DOI]. (Cited on page 62.)ADSCrossRefGoogle Scholar
 [174]Cohen, A.G. and Glashow, S.L., “A Lorentzviolating origin of neutrino mass?”, arXiv, eprint, (2006). [arXiv:hepph/0605036]. (Cited on page 93.)Google Scholar
 [175]Cohen, A.G. and Glashow, S.L., “Pair Creation Constrains Superluminal Neutrino Propagation”, Phys. Rev. Lett., 107, 181803, (2011). [DOI], [arXiv:1109.6562 [hepph]]. (Cited on page 59.)ADSCrossRefGoogle Scholar
 [176]Cohen, A.G., Kaplan, D.B. and Nelson, A.E., “Effective field theory, black holes, and the cosmological constant”, Phys. Rev. Lett., 82, 4971–4974, (1999). [DOI], [arXiv:hepth/9803132]. (Cited on page 89.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [177]Colella, R., Overhauser, A.W. and Werner, S.A., “Observation of gravitationally induced quantum interference”, Phys. Rev. Lett., 34, 1472–1474, (1975). (Cited on pages 13 and 87.)ADSCrossRefGoogle Scholar
 [178]Coleman, S.R., “Black Holes as Red Herrings: Topological Fluctuations and the Loss of Quantum Coherence”, Nucl. Phys. B, 307, 867, (1988). [DOI]. (Cited on page 67.)ADSMathSciNetCrossRefGoogle Scholar
 [179]Coleman, S.R. and Glashow, S.L., “HighEnergy Tests of Lorentz Invariance”, Phys. Rev. D, 59, 116008, (1999). [DOI], [arXiv:hepph/9812418]. (Cited on pages 53, 59, 60, and 64.)ADSCrossRefGoogle Scholar
 [180]Colladay, D. and Kostelecký, V.A., “CPT violation and the standard model”, Phys. Rev. D, 55, 6760–6774, (1997). [DOI], [arXiv:hepph/9703464]. (Cited on pages 64 and 79.)ADSCrossRefGoogle Scholar
 [181]Colladay, D. and Kostelecký, V.A., “Lorentzviolating extension of the standard model”, Phys. Rev. D, 58, 116002, (1998). [DOI], [arXiv:hepph/9809521]. (Cited on page 64.)ADSCrossRefGoogle Scholar
 [182]Collins, J., Perez, A., Sudarsky, D., Urrutia, L. and Vucetich, H., “Lorentz invariance and quantum gravity: an additional finetuning problem?”, Phys. Rev. Lett., 93, 191301 (2004). [DOI], [arXiv:grqc/0403053]. (Cited on pages 16, 40, and 44.)ADSMathSciNetCrossRefGoogle Scholar
 [183]Combes, F., Boissé, P., Mazure, A. and Blanchard, A., Galaxies and Cosmology, Astronomy and Astrophysics Library, (Springer, Berlin; New York, 2002), 2nd edition. (Cited on page 94.)CrossRefGoogle Scholar
 [184]Connes, A., Noncommutative Geometry, (Academic Press, San Diego, CA, 1994). [Google Books]. (Cited on page 28.)zbMATHGoogle Scholar
 [185]Connes, A., “Noncommutative geometry and reality”, J. Math. Phys., 36, 6194–6231, (1995). [DOI]. (Cited on page 28.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [186]Contaldi, C.R., Dowker, F. and Philpott, L., “Polarization Diffusion from Spacetime Uncertainty”, Class. Quantum Grav., 27, 172001, (2010). [DOI], [arXiv:1001.4545 [grqc]]. (Cited on page 86.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [187]Corsi, A., Guetta, D. and Piro, L., “GeV emission from short GammaRay Bursts: the case of GRB 081024B”, arXiv, eprint, (2009). [arXiv:0905.1513 [astroph.CO]]. (Cited on page 57.)Google Scholar
 [188]Costa, E. et al., “Discovery of the Xray afterglow of the γray burst of 28 February 1997”, Nature, 387, 783–785, (1997). [DOI], [arXiv:astroph/9706065 [astroph]]. (Cited on page 55.)ADSCrossRefGoogle Scholar
 [189]Coule, D.H., “Comment: Planck scale still safe from stellar interferometry”, Class. Quantum Grav., 20, 3107–3112, (2003). [DOI], [arXiv:astroph/0302333]. (Cited on pages 77 and 78.)ADSzbMATHCrossRefGoogle Scholar
 [190]Crichigno, P.M. and Vucetich, H., “Quantum corrections to Lorentz invariance violating theories: Finetuning problem”, Phys. Lett. B, 651, 313–318, (2007). [DOI], [arXiv:hepth/0607214]. (Cited on pages 16, 40, and 44.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [191]Czerhoniak, P., “Force in Kappa deformed relativistic dynamics”, Mod. Phys. Lett. A, 15, 1823–1831, (2000). [DOI], [arXiv:hepth/0012066 [hepth]]. (Cited on page 55.)ADSCrossRefGoogle Scholar
 [192]Damour, T., “String theory, cosmology and varying constants”, Astrophys. Space Sci., 283, 445–456, (2003). [DOI], [arXiv:grqc/0210059]. (Cited on pages 33 and 87.)ADSCrossRefGoogle Scholar
 [193]Damour, T., Piazza, F. and Veneziano, G., “Runaway dilaton and equivalence principle violations”, Phys. Rev. Lett., 89, 081601, (2002). [DOI], [arXiv:grqc/0204094]. (Cited on pages 26, 33, and 87.)ADSCrossRefGoogle Scholar
 [194]Damour, T., Piazza, F. and Veneziano, G., “Violations of the equivalence principle in a dilatonrunaway scenario”, Phys. Rev. D, 66, 046007, (2002). [DOI], [arXiv:hepth/0205111]. (Cited on pages 33 and 87.)ADSMathSciNetCrossRefGoogle Scholar
 [195]Damour, T. and Polyakov, A.M., “The string dilaton and a least coupling principle”, Nucl. Phys. B, 423, 532–558, (1994). [DOI], [arXiv:hepth/9401069]. (Cited on pages 33 and 87.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [196]Damour, T. and Polyakov, A.M., “String theory and gravity”, Gen. Relativ. Gravit., 26, 1171–1176, (1994). [DOI], [arXiv:grqc/9411069]. (Cited on pages 33 and 87.)ADSMathSciNetCrossRefGoogle Scholar
 [197]Danielsson, U.H., “A note on inflation and transPlanckian physics”, Phys. Rev. D, 66, 023511, (2002). [DOI], [arXiv:hepth/0203198 [hepth]]. (Cited on pages 96 and 97.)ADSMathSciNetCrossRefGoogle Scholar
 [198]Danielsson, U.H., “Transplanckian signatures in WMAP3?”, arXiv, eprint, (2006). [arXiv:astroph/0606474]. (Cited on page 97.)Google Scholar
 [199]Daszkiewicz, M., Imilkowska, K. and KowalskiGlikman, J., “Velocity of particles in doubly special relativity”, Phys. Lett. A, 323, 345–350, (2004). [DOI], [arXiv:hepth/0304027]. (Cited on page 41.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [200]Daszkiewicz, M., Imilkowska, K., KowalskiGlikman, J. and Nowak, S., “Scalar field theory on kappaMinkowski spacetime and doubly special relativity”, Int. J. Mod. Phys. A, 20, 4925–4940, (2005). [DOI], [arXiv:hepth/0410058]. (Cited on pages 36 and 37.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [201]de Angelis, A., “GLAST, the gammaray large area space telescope”, arXiv, eprint, (2000). [arXiv:astroph/0009271]. (Cited on page 55.)Google Scholar
 [202]DeDeo, S. and PrescodWeinstein, C., “EnergyDependent Speeds of Light for CosmicRay Observatories”, arXiv, eprint, (2008). [arXiv:0811.1999 [astroph]]. (Cited on page 36.)Google Scholar
 [203]Deser, S., “General Relativity and the Divergence Problem in Quantum Field Theory”, Rev. Mod. Phys., 29, 417–423, (1957). [DOI]. (Cited on page 67.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [204]Di Domenico, A., “CPT and QM tests using kaon interferometry”, arXiv, eprint, (2009). [arXiv:0904.1976]. (Cited on page 80.)Google Scholar
 [205]Di Domenico, A. (KLOE Collaboration), “Status and Perspectives of CP and CPT Tests With Neutral Kaons at KLOE”, in Benussi, L. et al., eds., Discoveries in Flavour Physics at e^{+}e^{−} Colliders, Frascati, Italy, February 28th–March 3rd, 2006, Frascati Physics Series, XLI, pp. 79–85, (INFN, Frascati, 2006). Online version (accessed 10 June 2013): http://www.lnf.infn.it/sis/frascatiseries/. (Cited on pages 80 and 82.)Google Scholar
 [206]Di Stefano, R., Ford, L.H., Yu, H.W. and Fixsen, D.J., “Quantum gravity and astrophysics: The microwave background and other thermal sources”, arXiv, eprint, (2001). [arXiv:astroph/0107001]. (Cited on pages 88 and 97.)Google Scholar
 [207]Dienes, K.R., Dudas, E. and Gherghetta, T., “Extra spacetime dimensions and unification”, Phys. Lett. B, 436, 55–65, (1998). [DOI], [arXiv:hepph/9803466]. (Cited on page 102.)ADSMathSciNetCrossRefGoogle Scholar
 [208]Dimopoulos, S., Graham, P.W., Hogan, J.M., Kasevich, M.A. and Rajendran, S., “Gravitational Wave Detection with Atom Interferometry”, Phys. Lett. B, 678, 37–40, (2009). [arXiv:0712.1250 [grqc]]. (Cited on page 74.)ADSCrossRefGoogle Scholar
 [209]Diosi, L. and Lukacs, B., “Karolyhazy’s quantum spacetime generates neutron star density in vacuum”, Nuovo Cimento B, 108, 1419–1422, (1993). [DOI], [arXiv:grqc/9302028 [grqc]]. (Cited on page 70.)ADSCrossRefGoogle Scholar
 [210]Donoghue, J.F., “Leading quantum correction to the Newtonian potential”, Phys. Rev. Lett., 72, 2996–2999, (1994). [DOI], [arXiv:grqc/9310024 [grqc]]. (Cited on page 11.)ADSCrossRefGoogle Scholar
 [211]Doplicher, S., Fredenhagen, K. and Roberts, J.E., “Spacetime quantization induced by classical gravity”, Phys. Lett. B, 331, 39–44, (1994). [DOI]. (Cited on pages 12, 28, 31, and 35.)ADSMathSciNetCrossRefGoogle Scholar
 [212]Dou, D. and Percacci, R., “The running gravitational couplings”, Class. Quantum Grav., 15, 3449–3468, (1998). [DOI], [arXiv:hepth/9707239]. (Cited on pages 30 and 85.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [213]Douglas, M.R. and Nekrasov, N.A., “Noncommutative field theory”, Rev. Mod. Phys., 73, 977–1029, (2001). [DOI], [arXiv:hepth/0106048]. (Cited on pages 26, 31, 35, 40, 41, and 90.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [214]Dowker, F., Henson, J. and Sorkin, R.D., “Quantum gravity phenomenology, Lorentz invariance and discreteness”, Mod. Phys. Lett. A, 19, 1829–1840, (2004). [DOI], [arXiv:grqc/0311055]. (Cited on page 86.)ADSMathSciNetCrossRefGoogle Scholar
 [215]Dowker, F., Henson, J. and Sorkin, R.D., “Discreteness and the transmission of light from distant sources”, Phys. Rev. D, 82, 104048, (2010). [DOI], [arXiv:1009.3058 [grqc]]. (Cited on page 86.)ADSCrossRefGoogle Scholar
 [216]Dvali, G., Folkerts, S. and Germani, C., “Physics of TransPlanckian Gravity”, Phys. Rev. D, 84, 024039, (2011). [DOI], [arXiv:1006.0984 [hepth]]. (Cited on page 10.)ADSCrossRefGoogle Scholar
 [217]Easther, R., Greene, B.R., Kinney, W.H. and Shiu, G., “Inflation as a probe of short distance physics”, Phys. Rev. D, 64, 103502, (2001). [DOI], [arXiv:hepth/0104102]. (Cited on page 97.)ADSMathSciNetCrossRefGoogle Scholar
 [218]Ellis, J.R., Farakos, K., Mavromatos, N.E., Mitsou, V.A. and Nanopoulos, D.V., “Astrophysical probes of the constancy of the velocity of light”, Astrophys. J., 535, 139–151, (2000). [astroph/9907340]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [219]Ellis, J.R., Hagelin, J.S., Nanopoulos, D.V. and Srednicki, M., “Search for Violations of Quantum Mechanics”, Nucl. Phys. B, 241, 381–405, (1984). [DOI]. (Cited on pages 13 and 80.)ADSMathSciNetCrossRefGoogle Scholar
 [220]Ellis, J.R., Lopez, J.L., Mavromatos, N.E. and Nanopoulos, D.V., “Precision tests of CPT symmetry and quantum mechanics in the neutral kaon system”, Phys. Rev. D, 53, 3846–3870, (1996). [DOI], [arXiv:hepph/9505340]. (Cited on pages 13, 14, 15, 32, 80, and 82.)ADSCrossRefGoogle Scholar
 [221]Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “String theory modifies quantum mechanics”, Phys. Lett. B, 293, 37–48, (1992). [DOI], [arXiv:hepth/9207103]. (Cited on pages 29, 32, 80, and 82.)ADSMathSciNetCrossRefGoogle Scholar
 [222]Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “Testing quantum mechanics in the neutral kaon system”, Phys. Lett. B, 293, 142–148, (1992). [DOI], [arXiv:hepph/9207268]. (Cited on page 32.)ADSMathSciNetCrossRefGoogle Scholar
 [223]Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “Some physical aspects of Liouville string dynamics”, arXiv, eprint, (1994). [arXiv:hepth/9405196]. (Cited on page 29.)Google Scholar
 [224]Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “A microscopic Liouville arrow of time”, Chaos Solitons Fractals, 10, 345–363, (1999). [DOI], [arXiv:hepth/9805120]. (Cited on pages 32 and 80.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [225]Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “Noncritical Liouville string escapes constraints on generic models of quantum gravity”, Phys. Rev. D, 65, 064007, (2002). [DOI], [arXiv:astroph/0108295]. (Cited on pages 59 and 60.)ADSMathSciNetCrossRefGoogle Scholar
 [226]Ellis, J.R., Mavromatos, N.E. and Nanopoulos, D.V., “Probing a Possible Vacuum Refractive Index with GammaRay Telescopes”, Phys. Lett. B, 674, 83, (2009). [arXiv:0901.4052]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [227]Ellis, J.R., Mavromatos, N.E., Nanopoulos, D.V. and Sakharov, A.S., “Synchrotron radiation and quantum gravity”, Nature, 428, 386, (2004). [astroph/0309144]. (Cited on pages 33 and 42.)CrossRefGoogle Scholar
 [228]Ellis, J.R., Mavromatos, N.E., Nanopoulos, D.V., Sakharov, A.S. and Sarkisyan, E.K.G., “Robust limits on Lorentz violation from gammaray bursts”, Astropart. Phys., 25, 402–411, (2006). [astroph/0510172 [astroph]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [229]Ellis, J.R., Mavromatos, N.E., Nanopoulos, D.V., Sakharov, A.S. and Sarkisyan, E.K.G., “Corrigendum to ‘Robust limits on Lorentz violation from gammaray bursts’”, Astropart. Phys., 29, 158 (2008). [astroph/0510172 [astroph]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [230]Ellis, J.R., Mavromatos, N.E., Nanopoulos, D.V. and Volkov, G., “Gravitationalrecoil effects on fermion propagation in spacetime foam”, Gen. Relativ. Gravit., 32, 1777–1798, (2000). [DOI], [arXiv:grqc/9911055]. (Cited on page 59.)ADSzbMATHCrossRefGoogle Scholar
 [231]Ellis, J.R., Mavromatos, N.E. and Sakharov, A.S., “Synchrotron radiation from the Crab Nebula discriminates between models of spacetime foam”, Astropart. Phys., 20, 669–682, (2004). [DOI], [arXiv:astroph/0308403]. (Cited on page 60.)ADSCrossRefGoogle Scholar
 [232]Falcone, A.D. et al., “Gamma Ray Burst Section of the White Paper on the Status and Future of Groundbased TeV Gammaray Astronomy”, arXiv, eprint, (2008). [arXiv:0810.0520 [astroph]]. (Cited on page 55.)Google Scholar
 [233]Ferenc, D. (MAGIC Collaboration), “The MAGIC gammaray observatory”, Nucl. Instrum. Methods A, 553, 274–281, (2005). [DOI]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [234]Fidecaro, M. and Gerber, H.J., “The fundamental symmetries in the neutral kaon system: A pedagogical choice”, Rep. Prog. Phys., 69, 1713–1770, (2006). [DOI], [arXiv:hepph/0603075]. (Cited on page 79.)ADSCrossRefGoogle Scholar
 [235]Finkbeiner, D.P., Davis, M. and Schlegel, D.J., “Detection of a Far IR Excess with DIRBE at 60 and 100 Microns”, Astrophys. J., 544, 81–97, (2000). [DOI], [arXiv:astroph/0004175]. (Cited on page 48.)ADSCrossRefGoogle Scholar
 [236]Fiore, G. and Wess, J., “On ‘full’ twisted Poincare’ symmetry and QFT on MoyalWeyl spaces”, Phys. Rev. D, 75, 105022, (2007). [DOI], [arXiv:hepth/0701078]. (Cited on page 31.)ADSMathSciNetCrossRefGoogle Scholar
 [237]Freidel, L., KowalskiGlikman, J. and Smolin, L., “2+1 gravity and doubly special relativity”, Phys. Rev. D, 69, 044001, (2004). [DOI], [arXiv:hepth/0307085]. (Cited on pages 31 and 67.)ADSMathSciNetCrossRefGoogle Scholar
 [238]Freidel, L. and Livine, E.R., “Effective 3D quantum gravity and noncommutative quantum field theory”, Phys. Rev. Lett., 96, 221301, (2006). [DOI], [arXiv:hepth/0512113 [hepth]]. (Cited on pages 67 and 68.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [239]Gaete, P. and Wotzasek, C., “Lorentz Violating JuliaToulouse Mechanism”, Phys. Rev. D, 75, 057902, (2007). [hepph/0607321]. (Cited on page 64.)ADSCrossRefGoogle Scholar
 [240]Gagnon, O. and Moore, G.D., “Limits on Lorentz violation from the highest energy cosmic rays”, Phys. Rev. D, 70, 065002, (2004). [DOI], [arXiv:hepph/0404196]. (Cited on page 50.)ADSCrossRefGoogle Scholar
 [241]Gago, A.M., Santos, E.M., Teves, W.J.C. and Zukanovich Funchal, R., “A study on quantum decoherence phenomena with three generations of neutrinos”, arXiv, eprint, (2002). [arXiv:hepph/0208166]. (Cited on page 84.)Google Scholar
 [242]Gaisser, T.K., “Cosmic rays: current status, historical context”, arXiv, eprint, (2010). [arXiv:1010.5996 [astroph.HE]]. (Cited on pages 51 and 52.)Google Scholar
 [243]Galán, P. and Mena Marugán, G.A., “Canonical Realizations of Doubly Special Relativity”, Int. J. Mod. Phys. D, 16, 1133–1147, (2007). [DOI], [arXiv:grqc/0702027 [grqc]]. (Cited on page 58.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [244]Galaverni, M. and Sigl, G., “Lorentz Violation in the Photon Sector and UltraHigh Energy Cosmic Rays”, Phys. Rev. Lett., 100, 021102, (2008). [DOI], [arXiv:0708.1737 [astroph]]. (Cited on page 53.)ADSCrossRefGoogle Scholar
 [245]Gambini, R., Porto, R.A. and Pullin, J., “Decoherence from discrete quantum gravity”, Class. Quantum Grav., 21, L51–L57, (2004). [arXiv:grqc/0305098]. (Cited on page 41.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [246]Gambini, R., Porto, Rafael A. and Pullin, J., “Realistic Clocks, Universal Decoherence, and the Black Hole Information Paradox”, Phys. Rev. Lett., 93, 240401, (2004). [DOI]. (Cited on page 32.)ADSMathSciNetCrossRefGoogle Scholar
 [247]Gambini, R. and Pullin, J., “Nonstandard optics from quantum spacetime”, Phys. Rev. D, 59, 124021, (1999). [DOI], [arXiv:grqc/9809038]. (Cited on pages 14, 15, 31, 36, 43, and 55.)ADSMathSciNetCrossRefGoogle Scholar
 [248]Gamboa, J., LópezSarrión, J. and Polychronakos, A.P., “Ultraviolet modified photons and anisotropies in the cosmic microwave background radiation”, Phys. Lett. B, 634, 471–473, (2006). [hepph/0510113]. (Cited on page 97.)ADSCrossRefGoogle Scholar
 [249]Garay, L.J., “Quantum gravity and minimum length”, Int. J. Mod. Phys. A, 10, 145–166, (1995). [DOI], [arXiv:grqc/9403008]. (Cited on pages 12, 17, 31, 35, and 70.)ADSCrossRefGoogle Scholar
 [250]Garay, L.J., “Spacetime foam as a quantum thermal bath”, Phys. Rev. Lett., 80, 2508–2511, (1998). [DOI], [arXiv:grqc/9801024 [grqc]]. (Cited on page 67.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [251]Garay, L.J., “Quantum evolution in spacetime foam”, Int. J. Mod. Phys. A, 14, 4079–4120, (1999). [DOI], [arXiv:grqc/9911002]. (Cited on page 82.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [252]Gasperini, M., “Testing the principle of equivalence with neutrino oscillations”, Phys. Rev. D, 38, 2635–2637, (1988). (Cited on pages 13 and 87.)ADSCrossRefGoogle Scholar
 [253]Gasperini, M. and Veneziano, G., “String Theory and Prebig bang Cosmology”, arXiv, eprint, (2007). [arXiv:hepth/0703055]. (Cited on page 100.)Google Scholar
 [254]Gharibyan, V., “Possible observation of photon speed energy dependence”, Phys. Lett. B, 611, 231–238, (2005). [DOI], [arXiv:hepex/0303010 [hepex]]. (Cited on page 63.)ADSCrossRefGoogle Scholar
 [255]Gharibyan, V., “Testing PlanckScale Gravity with Accelerators”, Phys. Rev. Lett., 109, 141103, (2012). [DOI], [arXiv:1207.7297 [hepph]]. (Cited on page 63.)ADSCrossRefGoogle Scholar
 [256]Ghirlanda, G., Ghisellini, G. and Nava, L., “The onset of the GeV afterglow of GRB 090510”, arXiv, eprint, (2009). [arXiv:0909.0016 [astroph.HE]]. (Cited on page 57.)Google Scholar
 [257]Giddings, S.B., “Is string theory a theory of quantum gravity?”, Found. Phys., 43, 115–139, (2013). [DOI], [arXiv:1105.6359 [hepth]]. (Cited on page 26.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [258]Giddings, S.B. and Thomas, S.D., “High energy colliders as black hole factories: The end of short distance physics”, Phys. Rev. D, 65, 056010, (2002). [DOI], [arXiv:hepph/0106219]. (Cited on page 102.)ADSCrossRefGoogle Scholar
 [259]Girelli, F., Livine, E.R. and Oriti, D., “Deformed special relativity as an effective flat limit of quantum gravity”, Nucl. Phys. B, 708, 411–433, (2005). [DOI], [arXiv:grqc/0406100 [grqc]]. (Cited on page 67.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [260]Giudice, G.F., Rattazzi, R. and Wells, J.D., “Quantum gravity and extra dimensions at highenergy colliders”, Nucl Phys. B, 544, 3–38, (1999). [DOI], [arXiv:hepph/9811291]. (Cited on page 102.)ADSCrossRefGoogle Scholar
 [261]Gleiser, R. J. and Kozameh, C.N., “Astrophysical limits on quantum gravity motivated birefringence”, Phys. Rev. D, 64, 083007, (2001). [DOI], [arXiv:grqc/0102093]. (Cited on page 61.)ADSCrossRefGoogle Scholar
 [262]Gleiser, R.J., Kozameh, C.N. and Parisi, F., “On low energy quantum gravity induced effects on the propagation of light”, Class. Quantum Grav., 20, 4375–4386, (2003). [DOI], [arXiv:grqc/0304048]. (Cited on page 61.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [263]Goklu, E. and Lämmerzahl, C., “Metric fluctuations and the Weak Equivalence Principle”, Class. Quantum Grav., 25, 105012, (2008). [DOI], [arXiv:0801.4553 [grqc]]. (Cited on pages 33 and 88.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [264]Granot, J. (Fermi LAT and GBM collaborations), “GRB Theory in the Fermi Era”, arXiv, eprint, (2009). [arXiv:0905.2206 [astroph.HE]]. (Cited on page 55.)Google Scholar
 [265]Greenberg, O.W., “CPT violation implies violation of Lorentz invariance”, Phys. Rev. Lett., 89, 231602, (2002). [DOI], [arXiv:hepph/0201258]. (Cited on page 79.)ADSCrossRefGoogle Scholar
 [266]Greene, BR., Schalm, K., Shiu, G. and van der Schaar, J.P., “Decoupling in an expanding universe: Backreaction barely constrains short distance effects in the CMB”, J. Cosmol. Astropart. Phys., 0502, 001, (2005). [DOI], [arXiv:hepth/0411217]. (Cited on page 97.)ADSCrossRefGoogle Scholar
 [267]Greisen, K., “End to the cosmicray spectrum?”, Phys. Rev. Lett., 16, 748–750, (1966). [DOI]. (Cited on page 50.)ADSCrossRefGoogle Scholar
 [268]Groot Nibbelink, S. and Pospelov, M., “Lorentz violation in supersymmetric field theories”, Phys. Rev. Lett., 94, 081601, (2005). [DOI], [arXiv:hepph/0404271]. (Cited on page 45.)ADSMathSciNetCrossRefGoogle Scholar
 [269]Gross, D. J. and Mende, P.F., “String Theory Beyond the Planck Scale”, Nucl. Phys. B, 303, 407–454, (1988). [DOI]. (Cited on pages 12, 27, 31, and 33.)ADSMathSciNetCrossRefGoogle Scholar
 [270]Gubitosi, G. and Pagano, L., “Planckscale sensitivity of CMB polarization data”, Nucl. Phys. B (Proc. Suppl.), 194, 69–75, (2009). [DOI]. (Cited on page 99.)ADSCrossRefGoogle Scholar
 [271]Gubitosi, G., Pagano, L., AmelinoCamelia, G., Melchiorri, A. and Cooray, A., “A Constraint on Planckscale Modifications to Electrodynamics with CMB polarization data”, J. Cosmol. Astropart. Phys., 2009(08), 021, (2009). [DOI], [arXiv:0904.3201 [astroph.CO]]. (Cited on page 43.)CrossRefGoogle Scholar
 [272]Halprin, A., Leung, C.N. and Pantaleone, J.T., “A Possible Violation of the Equivalence Principle by Neutrinos”, Phys. Rev. D, 53, 5365–5376, (1996). [DOI], [arXiv:hepph/9512220]. (Cited on page 87.)ADSCrossRefGoogle Scholar
 [273]Hamada, K., Horata, S., Sugiyama, N. and Yukawa, T., “Analyzing WMAP Observation by Quantum Gravity”, Prog. Theor. Phys., 119, 253–262, (2007). [DOI], [arXiv:0705.3490 [astroph]]. (Cited on page 97.)ADSCrossRefGoogle Scholar
 [274]Hamann, J., Hannestad, S., Sloth, M.S. and Wong, Y.Y.Y., “Observing transPlanckian ripples in the primordial power spectrum with future large scale structure probes”, J. Cosmol. Astropart. Phys., 2008(09), 015, (2008). [DOI], [arXiv:0807.4528 [astroph]]. (Cited on page 97.)ADSCrossRefGoogle Scholar
 [275]Hamma, A., Markopoulou, F., Lloyd, S., Caravelli, F., Severini, S. and Markström, K., “Quantum BoseHubbard model with an evolving graph as a toy model for emergent spacetime”, Phys. Rev. D, 81, 104032, (2010). [DOI], [arXiv:0911.5075 [grqc]]. (Cited on page 55.)ADSCrossRefGoogle Scholar
 [276]Han, T. and Willenbrock, S., “Scale of quantum gravity”, Phys. Lett. B, 616, 215–220, (2005). [DOI], [hepph/0404182]. (Cited on pages 7, 18, and 19.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [277]Hanneke, D., Fogwell, S. and Gabrielse, G., “New Measurement of the Electron Magnetic Moment and the Fine Structure Constant”, Phys. Rev. Lett., 100, 120801, (2008). [DOI], [arXiv:0801.1134 [physics.atomph]]. (Cited on page 92.)ADSCrossRefGoogle Scholar
 [278]Hauser, M.G. and Dwek, E., “The Cosmic Infrared Background: Measurements and Implications”, Annu. Rev. Astron. Astrophys., 39, 249–307, (2001). [DOI], [arXiv:astroph/0105539]. (Cited on page 48.)ADSCrossRefGoogle Scholar
 [279]Hawking, S.W., “Breakdown of Predictability in Gravitational Collapse”, Phys. Rev. D, 14, 2460–2473, (1976). [DOI]. (Cited on page 32.)ADSMathSciNetCrossRefGoogle Scholar
 [280]Hawking, S.W., “The Unpredictability of Quantum Gravity”, Commun. Math. Phys., 87, 395, (1982). [DOI]. (Cited on page 32.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [281]Hawking, S.W., “Virtual black holes”, Phys. Rev. D, 53, 3099–3107, (1996). [DOI], [arXiv:hepth/9510029 [hepth]]. (Cited on page 67.)ADSMathSciNetCrossRefGoogle Scholar
 [282]Heinzel, G. et al., “LISA interferometry: Recent developments”, Class. Quantum Grav., 23, S119–S124, (2006). [DOI], [ADS]. (Cited on page 73.)ADSCrossRefGoogle Scholar
 [283]Helling, R.C. and You, J., “Macroscopic Screening of Coulomb Potentials From UV/IRMixing”, J. High Energy Phys., 2008(06), 067, (2008). [DOI], [arXiv:0707.1885 [hepth]]. (Cited on page 94.)CrossRefGoogle Scholar
 [284]Henson, J., “The causal set approach to quantum gravity”, arXiv, eprint, (2006). [arXiv:grqc/0601121]. (Cited on page 85.)Google Scholar
 [285]Hinton, J.A. (HESS Collaboration), “The status of the HESS project”, New Astron. Rev., 48, 331–337, (2004). [DOI], [astroph/0403052 [astroph]]. (Cited on page 56.)ADSCrossRefGoogle Scholar
 [286]Hogan, C.J., “Indeterminacy of Holographic Quantum Geometry”, Phys. Rev. D, 78, 087501, (2008). [arXiv:0806.0665]. (Cited on pages 71 and 72.)ADSMathSciNetCrossRefGoogle Scholar
 [287]Hogan, C.J., “Measurement of Quantum Fluctuations in Geometry”, Phys. Rev. D, 77, 104031, (2008). [DOI], [arXiv:0712.3419 [grqc]]. (Cited on pages 71 and 72.)ADSMathSciNetCrossRefGoogle Scholar
 [288]Hogan, C.J., “Quantum Geometry and Interferometry”, in Auger, G., Binétruy, P. and Plagnol, E., eds., The 9th LISA Symposium, Bibliothéque Nationale de France, Paris, 21–25 May 2012, ASP Conference Series, 467, pp. 17–26, (Astronomical Society of the Pacific, San Francisco, 2013). [arXiv: 1208.3703 [quantph]]. (Cited on pages 71 and 72.)Google Scholar
 [289]Hořava, P., “Quantum Gravity at a Lifshitz Point”, Phys. Rev. D, 79, 084008, (2009). [DOI], [arXiv:0901.3775]. (Cited on page 45.)ADSMathSciNetCrossRefGoogle Scholar
 [290]Hořava, P., “Spectral Dimension of the Universe in Quantum Gravity at a Lifshitz Point”, Phys. Rev. Lett., 102, 161301, (2009). [DOI], [arXiv:0902.3657 [hepth]]. (Cited on page 98.)ADSMathSciNetCrossRefGoogle Scholar
 [291]Hossenfelder, S., “MultiParticle States in Deformed Special Relativity”, Phys. Rev. D, 75, 105005, (2007). [DOI], [arXiv:hepth/0702016]. (Cited on pages 36 and 37.)ADSMathSciNetCrossRefGoogle Scholar
 [292]Hossenfelder, S., “Bounds on an energydependent and observerindependent speed of light from violations of locality”, Phys. Rev. Lett., 104, 140402, (2010). [DOI], [arXiv:1004.0418 [hepph]]. (Cited on page 36.)ADSCrossRefGoogle Scholar
 [293]Hossenfelder, S., “Minimal Length Scale Scenarios for Quantum Gravity”, Living Rev. Relativity, 16, lrr20132 (2013). [DOI], [arXiv:1203.6191]. URL (accessed 10 June 2013): http://www.livingreviews.org/lrr20132. (Cited on page 70.)
 [294]Hossenfelder, S. and Smolin, L., “Phenomenological Quantum Gravity”, Phys. Canada, 66, 99–102, (2010). [arXiv:0911.2761 [physics.popph]]. (Cited on page 66.)Google Scholar
 [295]Hoyle, C.D., Schmidt, U., Heckel, B.R., Adelberger, E.G., Gundlach, J.H., Kapner, D.J. and Swanson, H.E., “Submillimeter Test of the Gravitational InverseSquare Law: A Search for ‘large’ Extra Dimensions”, Phys. Rev. Lett., 86, 1418–1421, (2001). [DOI], [arXiv:hepph/0011014]. (Cited on page 102.)ADSCrossRefGoogle Scholar
 [296]Hu, B.L., “A kinetic theory approach to quantum gravity”, Int. J. Theor. Phys., 41, 2091–2119, (2002). [DOI], [grqc/0204069]. (Cited on page 30.)MathSciNetzbMATHCrossRefGoogle Scholar
 [297]Hu, B.L., “Can spacetime be a condensate?”, Int. J. Theor. Phys., 44, 1785–1806, (2005). [DOI], [grqc/0503067]. (Cited on page 30.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [298]Huet, P. and Peskin, M.E., “Violation of CPT and quantum mechanics in the \({K_0}  {{\bar K}_0}\) system”, Nucl. Phys. B, 434, 3–38, (1995). [DOI]. (Cited on pages 13, 32, and 80.)ADSCrossRefGoogle Scholar
 [299]Jackiw, R. and Kostelecký, V.A., “Radiatively induced Lorentz and CPT violation in electrodynamics”, Phys. Rev. Lett., 82, 3572–3575, (1999). [DOI], [arXiv:hepph/9901358]. (Cited on page 79.)ADSCrossRefGoogle Scholar
 [300]Jackson, J.D., Classical Electrodynamics, (John Wiley & Sons, New York, 1999), 3rd edition. (Cited on page 60.)zbMATHGoogle Scholar
 [301]Jacob, U. and Piran, T., “Neutrinos from gammaray bursts as a tool to explore quantumgravityinduced Lorentz violation”, Nature Phys., 3, 87–90, (2007). (Cited on page 59.)ADSCrossRefGoogle Scholar
 [302]Jacob, U. and Piran, T., “Inspecting absorption in the spectra of extragalactic gammaray sources for insight on Lorentz invariance violation”, Phys. Rev. D, 78, 124010, (2008). [arXiv:0810.1318]. (Cited on page 53.)ADSCrossRefGoogle Scholar
 [303]Jacob, U. and Piran, T., “Lorentzviolationinduced arrival delays of cosmological particles”, J. Cosmol. Astropart. Phys., 2008(01), 031, (2008). [DOI], [arXiv:0712.2170 [astroph]]. (Cited on page 56.)CrossRefGoogle Scholar
 [304]Jacobson, T.A., “Thermodynamics of spacetime: The Einstein equation of state”, Phys. Rev. Lett., 75, 1260–1263, (1995). [DOI], [grqc/9504004]. (Cited on page 36.)ADSMathSciNetzbMATHCrossRefGoogle Scholar
 [305]Jacobson, T.A., Liberati, S. and Mattingly, D., “TeV astrophysics constraints on Planck scale Lorentz violation”, Phys. Rev. D, 66, 081302, (2002). [DOI], [arXiv:hepph/0112207]. (Cited on pages 45 and 50.)ADSCrossRefGoogle Scholar
 [306]