Gravity-mediated Dark Matter in Clockwork/Linear Dilaton Extra-Dimensions

We study for the first time the possibility that Dark Matter (represented by particles with spin 0, 1/2 or 1) interacts gravitationally with Standard Model particles in an extra-dimensional Clockwork/Linear Dilaton model. We assume that both, the Dark Matter and the Standard Model, are localized in the IR-brane and only interact via gravitational mediators, namely the Kaluza-Klein (KK) graviton and the radion/KK-dilaton modes. We analyse in detail the Dark Matter annihilation channel into Standard Model particles and into two on-shell Kaluza-Klein towers (either two KK-gravitons, or two radion/KK-dilatons, or one of each), finding that it is possible to obtain the observed relic abundance via thermal freeze-out for Dark Matter masses in the range mDM ∈ [1, 15] TeV for a 5-dimensional gravitational scale M5 ranging from 5 to a few hundreds of TeV, even after taking into account the bounds from LHC Run II and irrespectively of the DM particle spin. ar X iv :1 91 2. 02 68 9v 1 [ he pph ] 4 D ec 2 01 9


Introduction
The Standard Model of Fundamental Interactions is in a wonderful shape, after the discovery of the Higgs boson in 2012 [1], and it may very well be that a huge energy desert above the TeV will be painstakingly explored till we could get in contact with even a single new particle. However, a reasonable hope can alter this unappealing landscape: there it must be something more than the Standard Model out there, as the Standard Model is not able to explain what Dark Matter is. The Nature of Dark Matter (DM) is, indeed, one of the longest long-standing puzzles to be explained in order to claim that we have a "complete" picture of the Universe. On one side, both from astrophysical and cosmological data (see, e.g., Ref. [2] and refs. therein), rather clear indications regarding the existence of some kind of matter that gravitates but that does not interact with other particles by any other detectable mean can be gathered. On the other hand, no candidate to fill the rôle of DM has yet been observed in high-energy experiments at colliders, nor is present in the Standard Model (SM) spectrum. Extensions of the Standard Model usually do include some DM candidate, a stable (or long-lived, with a lifetime as long as the age of the Universe) particle, with very small or none interaction with Standard Model particles and with particles of its own kind. These states are usually supposed to be rather heavy and are called "WIMP's", or "weakly interacting massive particles". Examples of these are the neutralino in supersymmetric extensions of the SM [3] or the lightest Kaluza-Klein particle in Universal Extra-Dimensions [4]. The typical range of masses for these particles was expected to be m DM ∈ [100, 1000] GeV. However, searches for these heavy particles at the LHC have pushed bounds on the masses of the candidates above the TeV scale, into the multi-TeV region. Moreover, experiments searching for DM particles through their interactions with a fixed target, or "Direct Detection" (DD) experiments (see, e.g., Ref. [5]) or through their annihilation into Standard Model particles, or "Indirect Detection" (ID) experiments (see, e.g., Ref. [6]) have thoroughly explored the m DM ∈ [100, 1000] GeV region, pushing constraints on the interaction cross-section between DM and SM particles to very small values. In addition to this, both DD and ID experiments have a rather limited sensitivity above the TeV, as they have been mostly designed to look for O(100) GeV particles. Other hypotheses have, however, been advanced: DM particles could indeed be "feebly interacting massive particles" (FIMP's) [7], "strongly interacting massive particles" (SIMP's) [8] or "axion-like" very light particles (ALP's) [9]. All of these new proposals try to explore the possibility that DM is made of particles lighter than the expected WIMP range, a region where the exclusion bounds from DD and ID experiments are much weaker. If we take seriously the possibility that DM is made of O(1) TeV particles other options can be considered, though. One interesting option is that the interaction between DM and SM particles be only gravitational. Being, however, the gravitational coupling enhanced by the existence of more than 3 spatial dimensions. Several extra-dimensional models have been proposed in the last twenty years to explain a troublesome feature of the Standard Model, nicknamed as the "Hierarchy Problem", i.e. the large hierarchy between the electro-weak scale, Λ EW ∼ 250 GeV, and the Planck scale, M P ∼ 10 19 GeV. In short, the mass of a scalar particle (the Higgs boson) should be sensitive (through loops) to the scale at which the Standard Model may be replaced by a more fundamental theory. If there is no new physics between the energy frontier reached by the LHC and the Planck scale, then the mass of the Higgs boson should be as large as the latter. Being the experimentally measured mass of the Higgs m H = O(Λ EW ), either the SM is not an effective theory and it is, after all, the ultimate theory (something not very convincing, as the SM does not explain Dark Matter, Dark Energy, Baryogenesis, the source of neutrino masses and, of course, gravity) or an incredible amount of fine-tuning between loop corrections stabilizes m H at its value. Extra-dimensional models solve the hierarchy problem by either replacing the Planck scale M P with a fundamental gravitational scale M D (being D the number of dimensions) that could be as low as a few TeV (Large Extra-Dimensions models, or LED, see Refs. [10][11][12][13][14]), or by "warping" the space-time such that the effective Planck scale Λ felt by particles of the SM is indeed much smaller than the fundamental scale M D , similar to M P (see Refs. [15,16]), or by a mixture of the two options (see Refs. [17,18]).
The possibility that Dark Matter particles, whatever they be, may have an enhanced gravitational interaction with SM particles has been studied mainly in the context of warped extra-dimensions. The idea was first advanced in Refs. [19,20] and subsequently studied in Refs. [21][22][23][24][25]. The generic conclusion of these papers was that when all the matter content is localized in the so-called TeV (or infrared brane), after taking into account current LHC bounds it was not possible to achieve the observed Dark Matter relic abundance in warped models for scalar DM particles (whereas this was not the case for fermion and vector Dark Matter). However, an important caveat was that these conclusions were drawn assuming the DM particle being lighter than the first Kaluza-Klein graviton mode. In this case, the only kinematically available channel to deplete the Dark Matter density in the Early Universe is the annihilation of two DM particles into two SM particles through virtual KKgraviton exchange. However, in Ref. [26], we performed a check of the literature for the particular case of scalar DM in warped extra-dimensions, finding that as soon as the DM particle is allowed to be heavier than the first KK-graviton, annihilation of two DM particles into two KK-gravitons becomes kinematically possible and, through this channel, the observed relic abundance can indeed be achieved in a significant region of the parameter space within the freeze-out scenario. In the same paper, we included previously overlooked contributions to the DM annihilation cross-section, such as the possibility that DM annihilation into any pair of KK-gravitons can occur (regardless of the KK-number of the gravitons), and additional contributions to the thermally-averaged cross-section arising at second order in the expansion of the metric around a background Minkowski 5-dimensional space-time (the correct order to reach, once considering production of two KK-gravitons). Eventually, we also study the impact of a Goldberger-Wise radion [27], both in DM annihilation through virtual radion exchange and through direct production of two radions. The region of the parameter space for which the observed DM relic abundance is achieved in the freeze-out framework corresponds to DM masses in the range m DM ∈ [1, 10] TeV, with first KK-graviton mass ranging from hundreds of GeV to some TeV. The price to pay to achieve the freeze-out thermally-averaged cross-section is that the scale Λ for which interactions between SM particles and KK-gravitons occur must be larger than 10 TeV, approximately. Therefore, in this scenario, the hierarchy problem cannot be completeley solved and some hierarchy between Λ and Λ EW is still present. This is something, however, common to most proposals of new physics aiming at solving the hierarchy problem, as the LHC has found no hint whatsoever of new physics to date. One of the most interesting features of the scenario proposed in Ref. [26] is that a large part of the allowed parameter space could be tested using either the LHC Run III or the HL-LHC data. By the end of the next decade, therefore, only tiny patches of the allowed parameter space should survive in case of no experimental signal, tipically corresponding to DM mass m DM ∼ 10 TeV, near the theoretical unitarity bounds.
In this paper, we extend the study of DM in an extra-dimensional framework to the case of a 5-dimensional ClockWork/Linear Dilaton (CW/LD) model. This model was proposed in Ref. [17] and its phenomenology at the LHC has been studied in Ref. [18]. In this scenario, a KK-graviton tower with spacing very similar to that of LED models starts at a mass gap k with respect to the zero-mode graviton. The fundamental gravitational scale M 5 can be as low as the TeV, where k is typically chosen in the GeV to TeV range. To our knowledge, this paper is the first attempt to use the CW/LD framework to explain the observed Dark Matter abundance in the Universe. In order to study this possibility, we very much follow the outline of our previous paper on DM in warped extra-dimensions albeit in this case we will consider DM particles with spin 0, 1/2 and 1. Also in this scenario we have found that the freeze-out thermal relic abundance can be achieved in a significant region of the model parameter space, with the DM mass ranging from 1 TeV to approximately 15 TeV, for DM of any spin. The fundamental gravitational scale M 5 needed to achieve the target relic abundance goes from a few TeV to a few hundreds of TeV, thus introducing a little hierarchy problem. Notice that the LHC Run III data and those of the high-luminosity upgrade HL-LHC will be able to test most of this region.
The paper is organized as follows: in Sect. 2 we outline the theoretical framework, reminding shortly the basic ingredients of the ClockWork/Linear Dilaton extradimensional scenario and of how dark matter can be included within this hypothesis; in Sect. 3 we show our results for the annihilation cross-sections of DM particles into SM particles, KK-gravitons and radion/KK-dilatons; in Sect. 4 we review the present experimental bounds on the parameters of the model (the fundamental Planck scale M 5 , the mass gap k and the DM mass m DM ) from the LHC and from direct and indirect searches of Dark Matter, and recall the theoretical constraints (coming from unitarity violation and effective field theory consistency); in Sect. 5 we explore the allowed parameter space such that the correct relic abundance is achieved for DM particles; and, eventually, in Sect. 6 we conclude. In the Appendices we give some of the mathematical expressions used in the paper: in App. A we give the Feynman rules for the theory considered here; in App. B we give the expressions for the decay amplitudes of the KK-graviton; in App. C we remind how the sum over KKmodes is carried on; and, eventually, in App. D we give the formulae relative to the annihilation cross-sections of Dark Matter particles into Standard Model particles, KK-gravitons and radion/KK-dilatons.

Theoretical framework
In this Section, we first review the freeze-out mechanism that could produce the observed DM relic abundance in the Universe. We then sketch the basic ingredients of the ClockWork/Linear Dilaton Extra-Dimensions scenario (CW/LD) needed to compute the thermally-averaged DM annihilation cross-section.

The DM Relic Abundance in the Freeze-Out scenario
The fact that a significant fraction of the Universe energy appears in the form of a non-baryonic (i.e. electromagnetically inert) matter is the outcome of experimental data ranging from astrophysical to cosmological scales. This component of the Universe energy density is called Dark Matter and, in the cosmological "standard model", the ΛCDM, it is usually assumed to be represented by stable (or long-lived) heavy particles (i.e. non-relativistic, or "cold"). Within the thermal DM production scenario, DM particles were in thermal equilibrium with the rest of SM particles in the Early Universe. The DM density is governed by the Boltzmann equation [28]: with T the temperature and H(T ) the Hubble parameter as a function of the temperature. The Boltzmann equation depends on a term proportional to the Hubble expansion rate at temperature T and a term proportional to the thermally-averaged cross-section, σv . To obtain the correct population of DM particles within this scenario, the rate of decay and annihilation of DM particles should be such that, below a certain temperature T FO , the DM density n DM (T ) "freezes out" and thermal fluctuations cannot any longer modify it. This occurs when σv × n DM falls below H(T ), DM decouples from the rest of particles and leaves an approximately constant number density in the co-moving frame, called relic abundance. The experimental value of the relic abundance can be derived starting from the DM density in the ΛCDM model. From Ref. [29] we have Ω CDM h 2 = 0.1198 ± 0.0012, being h the Hubble parameter. Solving eq. (2.1), it can be found for the thermally-averaged cross-section at the freeze-out σ FO v 2.2 × 10 −26 cm 3 /s [30]. It is very common to compute σv in a given model in the so-called velocity expansion (i.e. assuming small relative velocity between the two DM particles). However, this approximation may fail in the neighbourhood of resonances. In the CW/LD model, the virtual graviton exchange cross-section is indeed the result of an infinite sum of KK-graviton modes. For this reason, we computed the value of σv using the exact expression from Ref. [31]: being K 1 and K 2 the modified Bessel functions and v the relative velocity between DM particles.

A short summary on ClockWork/Linear Dilaton Extra-Dimensions
The metric considered in the CW/LD scenario (see Refs. [17,18]) is: where the signature of the metric is (+, −, −, −, −) and, as usual, we use capital latin indices M, N to run over the 5 dimensions and greek indices µ, ν only over 4 dimensions. Notice that we have rescaled the coordinate in the extra-dimension such that y is adimensional. This particular metric was first proposed in the context of Linear Dilaton (LD) models and Little String Theory (see, e.g. Refs. [32][33][34] and references therein). The metric in eq. (2.3) implies that the space-time is nonfactorizable, as the length scales on our 4-dimensional space-time depending on the particular position in the extra-dimension due to the warping factor exp(2/3 kr c |y|).
Notice, however, that in the limit k → 0 the standard, factorizable, flat LED case [10][11][12][13][14] is immediately recovered. As for the case of the Randall-Sundrum model, also in the CW/LD scenario the extra-dimension is compactified on a S 1 /Z 2 orbifold (with r c the compactification radius), and two branes are located at the fixed points of the orbifold, y = 0 ("IR" brane) and at y = π ("UV" brane). Standard model fields are located in one of the two branes (usually the IR-brane). The scale k, also called the "clockwork spring" (a term inherited by its rôle in the discrete version of the Clockwork model [17]), is the curvature along the 5th-dimension and it can be much smaller than the Planck scale (indeed, it can be as light as a few GeV). Being the relation between M P and the fundamental gravitational scale M 5 in the CW/LD model: it can be shown that, in order to solve or alleviate the hierarchy problem, k and r c must satisfy the following relation: For M 5 = 10 TeV and r c saturating the present experimental bound on deviations from the Newton's law, r c ∼ 100 µm [35], this relation implies that k could be as small as k ∼ 2 eV, and KK-graviton modes would therefore be as light as the eV, also. This "extreme" scenario does not differ much from the LED case, but for the important difference that the hierarchy problem could be solved with just one extra-dimension (for LED models, in order to bring M 5 down to the TeV scale, an astronomical lenght r c is needed and, thus, viable hierarchy-solving LED models start with at least 2 extra-dimensions). In the phenomenological application of the CW/LD model in the literature, however, k is typically chosen above the GeV-scale and, therefore, r c is accordingly diminished so as to escape direct observation. Notice that, differently from the case of warped extra-dimensions, where scales are all of the order of the Planck scale (M 5 , k ∼ M P ) or within a few orders of magnitude, in the CW/LD scenario, both the fundamental gravitational scale M 5 and the mass gap k are much nearer to the electro-weak scale Λ EW than to the Planck scale, as in the LED model. The action in 5D is: where the gravitational part is, in the Jordan frame: with G M N and R (5) the 5-dimensional metric and Ricci scalar, respectively, and S the (dimensionless) dilaton field, S = 2kr c |y|. We consider for the two brane actions the following expressions: and UV e S −f 4 UV + . . . , (2.9) where f IR , f UV are the brane tensions for the two branes and g (4) IR,UV = −G (5) /G (5) 55 is the determinant of the induced metric on the IR-and UV-brane, respectively. Throughout the paper, we consider all the SM and DM fields localized on the IRbrane, whereas on the UV-brane we could have any other physics that is Plancksuppressed. We assume that DM particles only interact with the SM particles gravitationally by considering only DM singlets under the SM gauge group. More complicated DM spectra with several particles will also not be studied here.
Notice that the gravitational action is not in its canonical form. Going to the Einstein frame changing G (5) M N → exp(−2/3S)G (5) M N , we get : where now the gravitational action is the Einstein action and from the kinetic term of the dilaton field we can read out that the physical field must be rescaled as M Eventually, it is important to stress that, in the Einstein frame, the brane action terms still have an exponential dependence e −S/3 from the dilaton field. This action has a shift symmetry S → S + const in the limit k → 0, that makes a small value of k with respect to M 5 "technically natural" in the 't Hooft sense. Using the action above in the Einstein frame, it can be shown that the metric in eq. (2.3) can be recovered as a classical background if the brane tensions are chosen as: Notice that, in a pure 4-dimensional scenario, the gravitational interactions would be enormously suppressed by powers of the Planck mass, while in an extradimensional one the gravitational interaction is actually enhanced. Expanding the metric at first order around its static solution, we have: (2.12) The 4-dimensional component of the 5-dimensional field h M N can be expanded in a Kaluza-Klein tower of 4-dimensional fields as follows: The h n µν (x) fields are the KK-modes of the 4-dimensional graviton and the χ n (y) factors are their wavefunctions. Notice that in the 4-dimensional decomposition of the 5-dimensional metric, two other fields are generally present: the graviphoton, h µ5 , and the graviscalar h 55 . The KK-tower of the graviscalar is absent from the lowenergy spectrum, as they are eaten by the KK-tower of graviphotons to get a mass (due to the spontaneous breaking of translational invariance caused by the presence of one or more branes). These are, in turn, eaten by the KK-gravitons to get a mass (having, thus, five degrees of freedom). The surviving graviphoton zero-mode does not couple with the energy-momentum tensor in the weak gravitational field limit [36], whereas the graviscalar zero-mode will generically mix with the radion needed to stabilize the extra-dimension size.
The eigenfunctions χ n (y) can be computed by solving the equation of motion in the extra-dimension of the fields: with Neumann boundary conditions ∂ y χ n (y) = 0 at y = 0 and π. Normalizing the eigenmodes such that the KK-modes have canonical kinetic terms in 4-dimensions, we get: χ n (y) = n mnrc e −krc|y| krc n sin n|y| + cos n|y| , At the IR-brane one gets: from which it is clear that the coupling between KK-graviton modes with n = 0 is suppressed by the effective scale Λ n and not by the Planck scale, differently from the LED case and similarly to the Randall-Sundrum one.
It is useful to remind here the explicit form of the energy-momentum tensor for a scalar, fermion and vector field: for an abelian gauge field and for a non-abelian gauge field. In both cases, the expressions above refers to the unitary gauge. For the case of the SM massless gauge fields the expression is T V µν | m V =0 (whilst we do not specify how the gauge field V µ gets a mass).

Introducing the radion
Stabilization of the radius of the extra-dimension r c is an issue. In general (see, e.g., Refs. [37][38][39]), bosonic quantum loops have a net effect on the boundaries of the extra-dimension such that the extra-dimension itself should shrink to a point. This feature, in a flat extra-dimension, can only be compensated by fermionic quantum loops and, usually, some supersymmetric framework is invoked to stabilize the radius of the extra-dimension (see, e.g., Ref. [40]). An additional advantage of supersymmetry in the bulk is that the CW/LD background metric may protect eq. (2.11) by fluctuations of the 5-dimensional cosmological constant (see, however, Ref. [41] for a non-supersymmetric clockwork implementation).
In the CW/LD scenario we can use the already present bulk dilaton field S to stabilize the compactification radius. If localized brane interactions generate a potential for S at y = π, then we could fix the value of the field S at the UV-brane, S UV = S | π . This is indeed an additional boundary condition that fixes the distance between the two branes to be πk r c = S UV /2 [17]: with µ IR and µ UV two parameters with the dimension of a mass. In order to compute the scalar spectrum, we should introduce quantum fluctuations over the background values of S(x, y) = S 0 (y) + ϕ(x, y) (where S 0 (y) = 2kr c |y|) and of the metric, eq. (2.12). After deriving the Einstein equations for the two scalar degrees of freedom, ϕ and 1 Φ, and imposing the junction conditions at the boundaries, it can be shown that both satify the following equation of motion: ] has a canonical kinetic term.
Expanding Φ and ϕ over a 4-dimensional plane-waves basis, (2.23) we can eventually derive the scalar fluctuations wave-functions (for example, in Φ): Φ n (y) = N n e −krcy [sin(β n y) + ω n cos(β n y)] , (2.24) with N n a normalization factor, β n = m 2 Φn − k 2 , and In the so-called rigid limit, µ UV → ∞, the scalar spectrum is given by: first obtained in Ref. [42], where we have identified the radion as the lightest state. Out of the rigid limit, the spectrum can be obtained expanding in inverse powers of µ UV , introducing the adimensional parameters IR,UV = 2k/µ IR,UV . At first order in the 's, There are no massless states for non-vanishing µ's (i.e., when the extra-dimension is stabilized). In the unstabilized regime (for µ UV , µ IR → 0), the graviscalar and lowest-lying dilaton mode decouple and we expect two massless modes.
The interactions of the radion and of the dilaton KK-tower with SM fields arises [34] from the term: (2.28) The main difference between the CW/LD case and the Randall-Sundrum case is that in the former case a dilaton dependence e −S/3 is still present in the brane term action going from the Jordan frame to the Einstein frame. On the other hand, the Randall-Sundrum action is already in the Einstein frame (its gravitational action is in the canonical form) and the brane action term couples to gravity minimally, i.e. through the −g (4) coefficient, only. Expanding the background metric and the dilaton field at first order in quantum fluctuations, we get (after KK-decomposition): Notice that the scalar fluctuations of metric AND dilaton couple with 4-dimensional fields through the usual energy-momentum trace and with a direct coupling with the 4-dimensional lagrangian. This is different from the case of the Randall-Sundrum model, where only the first kind of coupling is present, being the radion of purely gravitational origin (see, for example, Ref. [43]). In the CW/LD model, thus, there are two kinds of coupling between the radion and the KK-dilaton fields and the 4-dimensional fields sitting on the IR-brane. Again, at first order in UV,IR , we get: In the rigid limit (µ UV,IR → ∞) the coupling of dilaton modes with the SM lagrangian vanishes (1/Λ 0 ϕ , 1/Λ n ϕ → 0). In the rest of the paper, we will work in this limit in order to get a sound insight of how the radion and dilaton KK-modes may affect the generation of the freeze-out thermal abundance. A complete study of the impact of scalar perturbations to the DM phenomenology would imply considering general values for UV and IR and it is beyond the scope of this paper.
A further simplification that we are going to consider is the following: in the presence of a scalar field on the brane (such as the Higgs field), a non-minimal coupling of the scalar with the Ricci scalar is not forbidden by any symmetry. This may arise as a new term in the action: (2.32) Such term induces an additional kinetic mixing between the graviscalar Φ 0 , the lowest-lying dilaton ϕ 0 and the Higgs and, therefore, additional couplings with the SM fields. We will neglect this non-minimal coupling in the rest of the paper, taking ξ = 0. Summarizing, in the rigid limit and in the absence of a mixing between the Higgs and the other scalar fields, the scalar perturbation interaction lagrangian with SM and DM particles at first order is: where r = v 0 is the radion field and v n for n ≥ 1 is the dilaton KK-tower, and T SM is the trace of the SM energy-momentum tensor. The coefficients of the coupling between scalar perturbations and massless gauge fields are given in App. A.2. Notice that massless gauge fields do not contribute to the trace of the energy-momentum tensor, but they generate effective couplings from two different sources: quarks and W bosons loops contribution and the trace anomaly [44].

Contributions to σv in the CW/LD scenario
We are not assuming any particular spin for the DM particle; our only assumptions are that there is just one particle responsible for the whole DM relic abundance and that this particle interacts with the SM only gravitationally. Therefore, in the following we label such particles generically by DM's. The total annihilation crosssection is: where in the first term, σ ve ("ve" stands for "virtual exchange"), we sum over all SM particles. The second term, σ GG , corresponds to DM annihilation into KK-gravitons G n . Notice that we do not consider DM annihilation into zero-mode gravitons G 0 , as it is Planck-suppressed. The third term, σ ΦΦ , corresponds to DM annihilation into radions and KK-dilaton modes. Eventually, the fourth term, σ GΦ , is the production of one tower of KK-gravitons in association with a tower of radion/KK-dilatons (a channel previously overlooked in the literature on the subject). Notice that the KK-number is not conserved in the second, third and fourth term of eq. (2.34) due to the explicit breaking of momentum conservation in the 5th-dimension induced by the brane terms and, therefore, we must sum over all values of (m, n) as long as the condition 2m DM ≥ m n + m m (being m n the mass of the n-th KK-graviton or radion/KK-dilaton) is fulfilled. graviton If the DM mass m DM is smaller than the mass of the first KK-graviton and of the radion, only the first channel is open. Formulae for the DM annihilation into SM particles through virtual KK-graviton and radion/KK-dilaton exchange are given in App. D in the small relative velocity approximation, expanding the centre-of-mass energy s around s 4m 2 DM . Notice that, when computing the contribution of the radion/KK-dilaton exchange and KK-graviton exchange to the annihilation DM cross-section into SM particles, it is of the uttermost importance to take into account properly the decay width of the radion/KK-dilaton and of the KK-gravitons. Formulae for the radion/KK-dilaton and KK-graviton decays 2 are given in App. B.
If the DM mass is larger than the radion or the first KK-graviton mass 3 , m DM ≤ (m r , m G 1 ), the direct production of KK-graviton and/or radion/KK-dilaton towers becomes possible and the other three channels of eq. (2.34) open. The analytic expressions for σ GG (DM DM → G m G n ), σ GΦ (DM DM → G m Φ n ) and σ ΦΦ (DM DM → Φ m Φ n ) in the small relative velocity approximation are given in App. D.
A DM singlet could have other interactions with the SM besides the gravitational one, through several so-called "portals". Such scenarios have been extensively studied in the literature and are strongly constrained (see for instance [45,46] for recent analyses), so we will neglect those couplings and focus only on the gravitational mediators that have not been previously considered.

DM annihilation cross-section in CW/LD model
In this section we study in detail the different contributions to the thermally-averaged DM annihilation cross-section, comparing the results for scalar, fermion and vector DM particles.
As we reminded in the previous section, for relatively low DM particles mass the first annihilation channel to open is the annihilation into SM particles through KKgraviton or radion/KK-dilaton exchange. Differently from the RS case (see Ref. [26]), both the virtual KK-graviton and radion/KK-dilaton exchange cross-section do not behave as the sum of relatively independent channels with well-separated peaks, one per KK-mode. For the typical values of M 5 and k that may solve the hierarchy problem, in the CW/LD case a huge number of KK-modes must be coherently summed in σ ve (DM DM → SM SM). The thermally-averaged virtual exchange cross-section, Fig. 1 for a scalar (left panel), a fermion (middle panel) and a vector (right panel) DM particle, respectively, for the particular choice k = 1 TeV and M 5 = 7 TeV 4 . Virtual radion/KK-dilaton exchange is shown with (green) dot-dashed lines, virtual KK-graviton exchange with (blue) solid lines. In all cases, σ ve (DM DM → SM SM) is extremely small below m DM ∼ 500 GeV, whilst rapidly increasing when m DM approaches half the mass of the lightest mode (the radion). From that point onward, for larger and larger DM masses the cross-section starts to rapidly oscillate crossing threshold after threshold with new KK-modes entering the game. This behaviour can be clearly seen in the dot-dashed lines representing radion/KK-dilaton virtual exchange, where the difference between on-peak and off-peak cross-section can be as large as one order of magnitude. The sum over KK-dilaton modes does not increase the cross-section going to larger DM masses, as interferences from the near-continuum of modes collectively result in a slow decrease of σ ve,Φ going from m DM ∼ 1 TeV to m DM ∼ 10 TeV. The KK-graviton exchange cross-section shows a different behaviour: the difference between on-and off-peak is extremely small, and the sum over virtual KK-graviton modes gives a net (albeit slow) increase of the cross-section going to larger DM masses. These results are common to scalar, fermion and vector DM particles.
In the three panels, we also show the DM annihilation cross-section into real KK-gravitons, represented by an (orange) dashed line, and the freeze-out thermallyaveraged cross-section σ FO v , represented by the horizontal red-dotted line . The DM annihilation cross-section into two real radion/KK-dilaton towers and into one KK-graviton and one radion/KK-dilaton tower are not shown, as both are much smaller and, therefore, irrelevant. For a scalar or a vector DM particle the real KK-graviton production cross-sections are very similar. This component of the total cross-section takes over both the radion/KK-dilaton and KK-graviton virtual exchange and rapidly dominates the total cross-section for m DM above a few TeVs. On the other hand, the fermion DM real KK-graviton production cross-section is substantially smaller than those for scalar and vector DM particles in the considered range of m DM and its growth with m DM is much slower (the corresponding cross-sections can be found in App. D.1). We can see that, for the considered values of M 5 and k, the total fermion DM annihilation cross-section is dominated by virtual KK-graviton exchange up to m DM ∼ 10 TeV. Comparing the results for different spin of the DM particle, we see that the scalar DM case is the only one where, for relatively low DM masses, the radion/KK-dilaton virtual exchange cross-section actually dominates over the KK-graviton virtual exchange one. The difference between the two contributions can be as large as two orders of magnitude for m DM smaller than a few TeV, whereas the two become comparable for m DM ∼ 10 TeV (at a scale where, however, the real KK-graviton production has already become the dominant process). In this particular scenario, as it was the case for the RS model, the thermally-averaged virtual KK-graviton exchange cross-section is much lower than σ FO v . On the other hand, the virtual radion/KKdilaton exchange cross-section can actually reach the target value for m 2 DM ∼ m 2 r /4 (i.e. m 2 DM = 2/9k 2 in the rigid limit). For fermion and vector DM particles, this is not the case: the virtual radion/KK-dilaton exchange cross-section is of the same order or smaller than the virtual KK-graviton exchange cross-section 5 . In summary, for the particular choice of k and M 5 shown in Fig. 1, for a scalar DM particle the target freeze-out value σ FO v is achievable either through virtual radion/KK-dilaton exchange for low m DM or via real KK-graviton production for m DM a few TeV; for a fermion DM particle σ FO v is not achieved for m DM < 10 TeV; and, for a vector DM particle, the target relic abundance is achieved through virtual KK-graviton exchange for m DM ∼ 1 TeV (as it was found in the RS scenario [19,22]  In Fig. 2 we show the total cross-section involving KK-gravitons, only (summing virtual KK-graviton exchange and KK-graviton production) as a function of the DM particle mass m DM for different choices of k: k = 10 GeV (left panel), k = 100 GeV (middle panel) and k = 1 TeV (right panel). In all cases, M 5 = 7 TeV. In all panels, we plot σ G v = (σ ve,G + σ GG ) v for scalar (blue, solid lines), fermionic (orange, dot-dashed lines) and vector (green, dashed lines) DM particles, thus making comparison easier. The red dotted horizontal line shows σ FO v . For all choices of k, at very low values of m DM the scalar DM scenario give a much lower thermallyaveraged cross-section with respect to the fermion and vector case. It rapidly catches up, though, eventually merging with the vector case. We see that σ G v = σ FO v at approximately m DM ∼ 10 k for k below the TeV and m DM = O(k) for k at the TeV in the scalar and vector case. On the other hand, a much larger value of m DM is needed to achieve the freeze-out target value if the DM particle is a fermion. The red-shaded area represents the theoretical unitarity bound σv ≥ 1/s, where we can no longer trust the theory outlined in Sect. 2 and higher-order operators should be taken into account.
We have seen that it is relatively easy to achieve the freeze-out relic abundance for DM particles with a mass at the TeV scale or below for M 5 = 7 TeV. However, it is important to understand how this scales with M 5 so as to see how much having a DM candidate is compatible with solving the hierarchy problem. This is shown in Fig. 3, where we draw the value of M 5 needed to achieve the freeze-out DM annihilation cross-section σ FO v for a given choice of k and m DM . In the top-left panel we show our results for a scalar DM particle using only virtual KK-graviton exchange and real KK-graviton production; in the top-right panel we again show our results for a scalar DM particle, albeit adding the contribution from virtual radion/KK-dilaton exchange and real radion/KK-dilaton production (since we saw in Fig. 1 that for this particular case these contributions are quite relevant); in the bottom-left and bottom-right panels, on the other hand, we show our results for a fermion and a vector DM particle, respectively, taking into account virtual KK-graviton exchange and real KK-graviton production only, as it was previously shown that in both cases the radion/KK-dilaton contribution is sub-dominant. The grey area represents the region of the (m DM , k) plane for which it is not possible to achieve the freeze-out relic abundance. The coloured area is the region for which σv can be as large as σ

Experimental bounds and theoretical constraints
As we have seen in Fig. 3, the target relic abundance can be achieved in a vast region of the (m DM , k) parameter space, if we allow M 5 to vary from 10 −1 TeV to 10 2 TeV. However, experimental searches strongly constrain k and M 5 . We will summarize here the relevant experimental bounds and see how only a relatively small region of the parameter space is allowed, indeed.

LHC bounds
The strongest constraints are given by the non-resonant searches at LHC. Differently from the results from resonance searches at the LHC [47,48], data from non-resonant searches are not easily turned into bounds in k and M 5 . We will therefore take advantage of the analysis performed in Ref. [18] and of the dedicated analysis from the CMS Collaboration described in Ref. [49]. The two bounds in the (k, M 5 ) plane are shown in Fig. 4, where the solid blue and dashed red lines represent results from Ref. [18] and Ref. [49], respectively. The orange-shaded area is the region of the parameter space for which the mass of the first KK-graviton m G 1 (where m G 1 = k) is larger than the scale of the theory, M 5 . In this region of the parameter space the low-energy gravity effective theory is not trustable (see Sect. 4.3). In the rest of the paper, we have applied the experimental LHC bounds from Ref. [49] as a conservative choice.

Direct and Indirect Dark Matter Detection
In order to understand the bounds from Direct Detection Dark Matter searches (DD) we need to compute the total cross-section for spin indepedent elastic scattering between Dark Matter and the nuclei [25]: where m p is the proton mass, while Z and A are the number of protons and the atomic number. The nucleon form factors are given by the same formula for Dark Matter of any spin (at zero momentum transfer): with q(2) the second moment of the quark distribution function and f N =p,n T q the mass fraction of light quarks in a nucleon: f p T u = 0.023, f p T d = 0.032 and f p T s = 0.020 for a proton and f n T u = 0.017, f n T d = 0.041 and f n T s = 0.020 for a neutron [50].
The strongest bounds come from the XENON1T experiment that uses 129 Xe, (Z = 54 and A − Z = 75) as a target. In our analysis we compute the second moment of the PDF's using Ref. [51] and the exclusion curve of XENON1T [52] to set constraints in the parameter space. In Fig. 5 we show the scale needed to achieve the freeze-out relic abundance, M FO 5 , as a function of the DM mass m DM , for k = 250 GeV. The three lines (solid orange, dot-dashed blue and dotted red) correspond to scalar, fermion and vector DM, respectively. The green-shaded area is the experimental bound in the (m DM , M 5 ) plane from XENON1T. We can see that the bounds imposed by DD only constrain very low values of m DM and they are irrelevant in the range of DM masses considered in the rest of this paper (m DM ≥ 100 GeV). We have checked that this result is general also for other values of k.  With respect to Indirect Detection Dark Matter searches (ID), several experiments are analysing differents signals. For instance, the Fermi-LAT Collaboration studied the γ-ray flux arriving at Earth from the galactic center [53,54] and from different Dwarf Spheroidal galaxies [55]. Other experiments detect charged particles instead of photons, as it is the case of AMS-02 that presented data about the positron [56] and anti-proton fluxes coming from the galactic center [57]. These results are relevant in various DM models that can generate a continuum spectra of SM particles, such as our case. However, current data from ID only allows to constrain DM masses below 100 GeV, a region which is already excluded by LHC data.

Theoretical constraints
Besides the experimental limits, there are mainly two theoretical concerns about the validity of our calculations which affect part of the (m DM , k, M 5 ) parameter space. The first one is related to the fact that we are performing just a tree-level computation of the relevant DM annihilation cross-sections, and we should worry about unitarity issues. In particular, the annihilation cross-section into a pair of real KK-gravitons, σ(DM DM → G n G m ), diverges as . When the DM mass becomes very large with respect to the KK-graviton masses, it is important to check that the effective theory is still unitary [58]. Asking for the crosssection to be bounded, σ < 1/s 1/m 2 DM , we got the red-shaded areas shown in Fig. 2. If we combine the unitarity requirement with the request that the freeze-out thermally-averaged cross-section is achieved to get the correct DM relic abundance, we have an upper bound on the DM mass: m DM 1/ √ σ FO , independently on the parameters that determine the geometry of the space-time, (k and M 5 ). This will be shown by a vertical line in the (m DM , k) plane in Fig. 6. The second theoretical issue refers to the consistency of the effective theory framework: in the CW/LD scenario, at energies somewhat larger than M 5 the KKgravitons are strongly coupled and the five-dimensional field theory from which we start is no longer valid. We therefore impose that at least m G 1 = k < M 5 to trust our results. Notice that this constraint is general for any effective field theory: since we are including the KK-graviton tower in the low-energy spectrum, for the effective theory to make sense the cut-off scale M 5 should be larger than the masses of such states. For the same reason, we also ask for the Dark Matter mass m DM to be lighter than M 5 , m DM < M 5 , although we will see that, in the allowed region, this requirement is almost always fulfilled.

Results
We show in Fig. 6 the allowed parameter space in the (m DM , k) plane for which the target value of σv needed to achieve the correct DM relic abundance in the freezeout scenario, ( σ FO v = 2.2 × 10 −26 cm 3 /s), can be obtained, taking into account both the experimental bounds and the theoretical constraints outlined in Sec. 4.
In the upper left panel we show our results for a scalar DM particle, considering only decays into SM particles through virtual KK-graviton exchange or into KKgravitons. This corresponds to the unstabilized regime, i.e. when the coefficients µ IR , µ UV of the localized potential terms in eq. (2.21) vanish. In the upper right panel we show our results for scalar DM when the extra-dimension is stabilized in the rigid limit, µ IR , µ UV → ∞, and in the absence of non-minimal coupling with gravity, ξ = 0 (see Sect. 2 for details). In this case, the annihilation of DM particles occurs through virtual KK-graviton and radion/KK-dilaton exchange into SM particles and through direct KK-graviton and radion/KK-dilaton production. In the bottom left and right panels we show our results for a fermion and a vector DM particle, respectively. In both cases, the radion/KK-dilaton contribution (in the rigid limit with ξ = 0) is included but it is irrelevant.
As a guidance, dashed lines taken from Fig. 3 represent the values of M 5 needed to achieve the relic abundance in a particular point of the (m DM , k) plane. The legend for the four plots is given in the Figure caption.

Scalar Dark Matter
In the case of scalar DM, depicted in the upper left and right panels, virtual KKgraviton exchange is not enough to achieve the freeze-out relic abundance. For this reason, when the extra-dimension is unstabilized (left panel), σ FO v can be obtained only when the KK-graviton production channel opens, as it was the case for the RS scenario [26]. As a consequence, the DM particle mass has to be in a given relation with the mass of the KK-graviton tower and, therefore, a grey region for which it is impossible to achieve σ FO v can be seen. The red diagonally-meshed area represents the region of the parameter space for which the correct relic abundance is achieved with a value of M 5 lower than the mass of the first KK-graviton, m G 1 = k. Above this line the low-energy effective theory we are using is untrustable, as new dynamical particles in the spectrum are heavier than the scale of the theory. The blue-shaded area represents the excluded region from searches of non-resonant channels at LHC Run II with 36 pb − 1 from Ref. [18]. The green vertically-meshed area is the upper bound on the DM mass that must be fulfilled to comply with unitarity.
When the extra-dimension is stabilized (right panel), the virtual radion/KKdilaton exchange channel may reach the target value for the cross-section in the low DM mass range m DM < m G 1 (see Fig. 1) and, therefore, no grey area is found. However most of this region is excluded because the value of M 5 is lower than k and, thus, the effective theory we are using is untrustable (red-meshed region). As a consequence, the allowed region that complies with experimental bounds and theoretical constraints is very similar to the unstabilized case and, roughly speaking, corresponds to m DM ∈ [1,15] TeV and k < 6 TeV. Within the allowed region, M 5 may vary between 10 TeV's and a few hundreds of TeV's.

Fermion Dark Matter
The case of fermion DM is depicted in the lower left panel. The meaning of the coloured areas is the same as for the upper panels: the grey area is the region of the parameter space for which is impossible to achieve σ FO v ; the blue-shaded area corresponds to the LHC Run II exclusion bound [18]; the red diagonally-meshed and green vertically-meshed areas represent theoretical unitarity bounds; and, the white area is the allowed region of the parameter space, where dashed lines represent extra-dimension in the rigid limit without non-minimal coupling with gravity). In all panels, the greyshaded area represents the part of the parameter space for which it is impossible to achieve the correct relic abundance; the red diagonally-meshed area is the region for which the low-energy CW/LD effective theory is untrustable, as M 5 < k; the blue-shaded area is excluded by non-resonant searches at the LHC with 36 fb −1 at √ s = 13 TeV [18]; eventually, the green vertically-meshed area on the right is the region where the theoretical unitarity constraints are not fulfilled, m DM 1/ √ σ FO . In all panels, the white area represents the region of the parameter space for which the correct relic abundance is achieved (either through direct KK-graviton and/or radion/KK-dilaton production, as in the case of scalar DM, or through virtual KK-graviton exchange, as for fermion and vector DM) and not excluded by experimental bounds and theoretical constraints. The dashed lines depicted in the white region represent the values of M 5 needed to obtain the correct relic abundance (from Fig. 3).
benchmark values of M 5 useful to understand its scaling. The main difference with the scalar (and vector) DM case is that for fermion DM a rather small region of the parameter space is compatible with all bounds and constraints. This is a consequence of the slower dependence of the direct KK-graviton production cross-section with m DM (see Figs. 1 and 2 and eq. (D.15) in App. D). Eventually, the allowed region that complies with experimental bounds and theoretical constraints corresponds to m DM ∈ [4,15] TeV and k < 1 TeV. Within the allowed region, M 5 may vary between 10 TeV's and a few tens of TeV's.

Vector Dark Matter
The case of vector DM is depicted in the lower right panel. The meaning of the coloured areas is the same as for the upper panels: the grey area is the region of the parameter space for which is impossible to achieve σ FO v ; the blue-shaded area corresponds to the LHC Run II exclusion bound [18]; the red diagonally-meshed and green vertically-meshed areas represent theoretical unitarity bounds; and, the white area is the allowed region of the parameter space, where dashed lines represent benchmark values of M 5 useful to understand its scaling. The main difference with the scalar and fermion DM case is that for vector DM it is possible to achieve the correct relic abundance through the virtual KK-graviton exchange channel, and the requirements on M 5 are less stringent. As a consequence, a rather large region of the parameter space is compatible with all bounds and constraints. The allowed region that complies with experimental bounds and theoretical constraints corresponds to m DM ∈ [0. 6,15] TeV and k may be as large as ∼ 20 TeV. Within the allowed region, M 5 may vary between a 5 TeV's and a few hundreds of TeV's.

Conclusions
In this paper we have explored the possibility that the observed Dark Matter component in the Universe is represented by some new particle with mass in the TeV range which interacts with the SM particles only gravitationally, in agreement with non-observation of DM signals at both direct and indirect detection DM experiments.
In standard 4-dimensional gravity, the interaction between such DM particles and SM particles would be too feeble to reproduce the observed DM relic abundance. However, we have found that this is not the case once this setup is embedded in a Clockwork/Linear Dilaton scenario, along the ideas of the CW/LD proposal of Refs. [17,18]. We consider two 4-dimensional branes in a 5-dimensional space-time with non-factorizable CW/LD metric [32] at a separation r c , very small compared with present bounds on deviations from Newton's law. On one of the branes, the so-called "IR-brane", both the SM particles and a DM particle (with spin 0, 1/2 or 1) are confined, with no particle allowed to escape from the branes to explore the bulk. It can be shown that gravitational interaction between particles on the IR-brane (in our case between a DM particle and any of the SM particles) occurs with an amplitude proportional to 1/M 2 P when the two particles exchange a graviton zero-mode, but with a suppression factor 1/Λ 2 n when they interact exchanging the n-th KK-graviton mode. As the effective coupling Λ n can be as low as a few TeV (depending on the particular choices of the two parameters that determine the geometry of the space-time, k and M 5 ), a huge enhancement of the cross-section is then possible with respect to standard linearized General Relativity.
Once fixed the setup we have computed the relevant contributions to the thermallyaveraged DM annihilation cross-section σ v , taking into accont both virtual KKgraviton and radion/KK-dilaton exchange as well as the direct production of radion/KKdilatons and KK-gravitons. We have then scanned the parameter space of the model (represented by m DM , k and M 5 ), looking for regions in which the observed relic abundance can be achieved, σ v ∼ σ FO v . This region has been compared with experimental bounds from resonant searches at the LHC Run II and from direct and indirect DM detection searches, finding which portion of the allowed parameter space is excluded by data. Eventually, we have studied the theoretical unitarity bounds on the mass of the DM particle and on the validity of the CW/LD model as a consistent low-energy effective theory. We have found that the correct relic abundance may be achieved in a significant region of the parameter space, corresponding typically to a DM mass of a few TeV's.
Depending on the spin and the mass of the DM particle, σ FO v is reached either through virtual exchange or direct production of radion/KK-dilatons and/or KK-gravitons. For scalar DM particles, we have found that σ FO v can be obtained for DM masses in the range m DM ∈ [1, 15] TeV and k 6 TeV. In this case the radion/KK-dilaton virtual exchange increases the cross-section for low DM masses (below 1 TeV), thus making possible to achieve σ FO v in a much larger portion of the parameter space with respect to the KK-gravitons only case. However, most of this extra region corresponds to values of m G 1 larger than M 5 and, thus, in a part of the parameter space where the effective theory is untrustable. As a consequence, we find no difference between the unstabilized case (no radion/KK-dilatons) and the stabilized case in the rigid limit (with radion/KK-dilatons). For fermion DM particles the allowed mass range is somewhat smaller, m DM ∈ [4,15] TeV and k 4 TeV. Eventually, for vector DM particles, the allowed mass range is somewhat larger, m DM ∈ [0. 6,15] TeV and k 20 TeV. Notice that the upper limit on the DM mass comes from theoretical unitarity bounds.
Our results for DM in the CW/LD scenario are very similar to those we have found with AdS 5 metric (the so-called Randall-Sundrum model) in Ref. [26], where we studied only the case of scalar DM. In the Randall-Sundrum scenario it was known that, for scalar DM and SM particles localized in the IR brane, it is not possible to achieve σ FO v through the virtual KK-graviton or radion exchange channel (see also Refs. [19,22]). However, we showed that when the DM mass is large enough so that the direct production of KK-gravitons or radions becomes possible, then the correct relic abundance can be achieved for DM particle masses of a few TeV's, much as in the case of the CW/LD model studied here. Notice that the value of M 5 needed to achieve the correct relic abundance in the CW/LD model is M 5 ∈ [10, 100] TeV, whereas in the Randall-Sundrum scenario the effective coupling Λ needed to achieve the freeze-out was in Λ ∈ [10, 1000] TeV range. In both cases, some hierarchy between the fundamental gravitational scale (either M 5 or Λ) and the electro-weak scale Λ EW is needed.
It is worth to emphasize that in both extra-dimensional scenarios, Randall-Sundrum and CW/LD, it is possible to obtain the correct relic abundance via thermal freeze-out with DM masses in the TeV scale, so they are already quite constrained by LHC data. Moreover, most part of the still allowed parameter space may be tested by the LHC Run III and by the proposed High-Luminosity LHC. While the prospects for the Randall-Sundrum were already analysed in Ref. [26], it would be very interesting to explore in detail the limits that these next LHC phases could set on the CW/LD model.

A Feynman rules
We remind in this Appendix the different Feynman rules corresponding to the couplings of DM particles and of SM particles of any spin with KK-gravitons and radion/KK-dilatons.

A.1 Graviton Feynman rules
The vertex that involves one KK-graviton and two scalars S of mass m S is given by: This expression can be used for the coupling of both scalar DM and the SM Higgs boson to gravitons. The vertex that involves one KK-graviton and two fermions ψ of mass m ψ is given by:ψ The interaction between two vector bosons V of mass m V and one KK-graviton is given by: and Eventually, the interaction between two particles (S, ψ or V µ depending on their spin) and two KK-gravitons (coming from a second order expansion of the metric g µν around the Minkowski metric η µν ) is given by: The Feynman rules for the n = 0 KK-graviton can be obtained by the previous ones by replacing Λ with M P . We do not give here the triple KK-graviton vertex, as it is irrelevant for the phenomenological applications of this paper.

A.2 Radion/KK-dilaton Feynman rules
The radion/KK-dilatons, φ n , couple with particles localized in the IR-brane with the trace of the energy-momentum tensor, T = g µν T µν (in the rigid limit with ξ = 0, see Sect. 2.3). The only exception are photons and gluons that, being massless, do not contribute to T at tree-level. However, effective couplings of these fields to the radion/KK-dilatons are generated through quarks and W loops, and the trace anomaly.
The interaction between one radion/KK-dilaton and two scalar fields S of mass m S is given by: The vertex that involves one radion/KK-dilaton and two Dirac fermions ψ of mass m ψ takes the form: and: The interaction between two massive vector bosons V of mass m V and one radion/KK-dilaton is given by: whereas the vertex corresponding to the interaction between two massless SM gauge bosons and one radion/KK-dilaton is: where α i = α EM , α s for the case of the photons or gluons, respectively, and [44]: U V = −11 + 2n/3, where n is the number of quarks whose mass is smaller than m r /2. The explicit form of F 1/2 and F 1 is given by: Eventually, the 4-legs diagrams are given by: .20) and

B Decay widths
In this Appendix we compute the decay widths of KK-gravitons and radion/KKdilatons, using the Feynman rules given in App. A.

B.1 KK-gravitons decay widths
The KK-graviton can decay into scalar particles (including the Higgs boson, a scalar DM particle and radion/KK-dilatons), fermions (either SM or a fermion DM particle), vector bosons (either massive or massless SM gauge bosons or a vector DM particle) and lighter KK-gravitons. Decay widths of KK-gravitons into SM particles, Γ(G n → SM SM), are all proportional to 1/Λ 2 n . In particular, the decay width into SM Higgs bosons is given by: where m n is the mass of the n-th KK-graviton (in the main text, this was called m Gn , but we prefer here a shorter notation to increase readability of the formulae). The decay width of the n-th KK-graviton into SM Dirac fermions is given by: The decay width of the n-th KK-graviton into two SM massive gauge bosons reads:  For completeness, we computed the decay of KK-gravitons into KK-gravitons and radion/KK-dilatons, finding that these contributions are totally negligible. For a thorough description of these decays see Ref. [18].

B.2 Radion/KK-dilatons decay widths
The decay width of the radion/KK-dilatons into SM Higgs boson, is given by: The radion/KK-dilaton decay width into SM Dirac fermions is given by: The radion/KK-dilaton decay width into SM massive gauge bosons is: whereas the decay width into SM massless gauge bosons is: If m n > 2m DM , the n-th radion/KK-dilaton can decay into two DM particles: We computed the decay of KK-dilatons into KK-gravitons and radion/KKdilatons, finding that these contributions are totally negligible, as in the case of KK-gravitons.

C Sums over KK-gravitons and radion/KK-dilatons
In this Appendix we explain how to calculate the approximations of the sums over virtual KK-modes that are used in the main text, following Ref. [18]. Consider the sum over virtual KK-modes that arise both in virtual KK-graviton or virtual radion/KK-dilaton exchange cross-sections: where m n is the mass of the n-th KK-graviton or radion/KK-dilaton and Γ n its corresponding decay width. If s > k 2 , we can approximate the square modulus of the sum over KK-modes by the sum over KK-modes square moduli, such that: with F(m n ) a function that depends on the mass and the decay width of the virtual KK-modes. The mass difference between two nearby KK-modes, for the typical choices of k and M 5 considered in the paper, is small enough to approximate the sum by an integral: Using the narrow-width approximation for F(m n ) where n corresponds to the mode for which m n ∼ √ s, eq. (C.2) can be further approximated as: In the case of KK-gravitons, if we replace Λ n with the expression in eq. (2.18), we get: In the case of radion/KK-dilatons, we have to use the expression for Λ n in eq. (2.30). Then: Notice that these expressions are equivalent to an average over the KK-modes.

D Annihilation DM Cross section
In all the expressions of this Appendix we made use of the so-called velocity expansion for the DM particles: where v is the relative velocity of the two DM particles. Within this approximation, the different scalar products for processes in which two DM particles annihilate into two particles (either SM particles, KK-gravitons or radion/KK-dilatons), with incoming and outcoming momenta DM(k 1 ) DM(k 2 ) → Out(k 3 ) Out(k 4 ), become:

D.1 Annihilation through and into KK-gravitons
In the following sections we show the DM annihilation cross-sections through and into KK-gravitons. In all of this expressions S g KK is the sum over the KK-gravitons given in App. C.

D.1.1 Scalar DM
First we start with the scalar Dark Matter. The annihilation cross-section into two SM Higgs bosons is: The annihilation cross-section into two SM massive gauge bosons is: whereas for two massless gauge bosons we have: Eventually, the annihilation cross-section into two SM fermions is: As it was shown in Ref. [19], for DM particle masses larger than the mass of a given KK-graviton mode DM particles may annihilate into two KK-gravitons. In the small velocity approximation, the related cross-section is: where the three contributions to the cross-section come from the square of the t-and u-channels amplitudes, the square of the 4-points amplitude from the vertex A.8 and from the interference between the two classes of amplitudes, respectively: (D.9) In the particular case in which the two KK-gravitons have the same KK-number, m = n, eq. (D.8) becomes: where r ≡ (m n /m DM ) 2 .

D.1.2 Fermionic case
If the dark matter is a Dirac fermion (χ) the annihilation into two SM Higgs bosons is: The annihilation cross-section into two SM massive gauge bosons is: DM , (D.12) whereas for two massless gauge bosons we have: Eventually, the annihilation cross-section into two SM fermions is: (D.14) As in the case of scalar DM if the m DM > m G 1 theψ ψ → G n G m channel is open: Notice that, differently from the scalar and vector case, the contribution of the 4points diagram from the vertex A.9 vanishes (B g χ = C g χ = 0). The t-and u-channel contributions give, instead: 16) In the particular case when two KK-gravitons have the same KK-number, m = n, eq. (D.15) becomes: where 6 r ≡ (m n /m DM ) 2 .

D.1.3 Vectorial case
If the dark matter is a spin-1 particle (X) the annihilation into two Higgs bosons is: The annihilation cross-section into two SM massive gauge bosons is: 19) whereas for two massless gauge bosons we have: . (D.20) The annihilation cross-section into two SM fermions is: Eventually, the annihilation into gravitons will be given by: where:  where r ≡ (m n /m DM ) 2 .

D.2 Annihilation through and into radion/KK-dilatons
In the following subsections we discuss the different DM annihilation cross sections through and into radion/KK-dilatons, using the approximation for the sums over the radion/KK-dilaton modes described in app.C. The sum over the dilaton states will be represented as S r KK .

D.2.1 Scalar case
The DM annihilation cross-section into two SM Higgs bosons is: The cross-section for DM annihilation into SM massive gauge bosons is: Eventually, the DM annihilation cross-section into two radion/KK-dilatons is given by: where, as in the case of KK-gravitons, the three contributions to the cross-section come from the square of the t-and u-channels amplitudes (A r S ), the square of the 4-points amplitude from vertex A.19 (C r S ) and from the interference between the two classes of diagrams (B r S ), respectively: The annihilation cross-section into two SM massive gauge bosons is: whereas for two massless gauge bosons we have: (D.33) The DM annihilation cross-section into two SM fermions is: Eventually, the annihilation directly into dilatons is given by: where:

D.2.3 Vectorial case
If the Dark Matter is a spin-1 particle (X) the annihilation into two SM Higgs bosons is: The annihilation cross-section into two SM massive gauge bosons is: (D.38) whereas for two massless gauge bosons we have: (D.39) The DM annihilation cross-section into two SM fermions is: Eventually, the annihilation cross-section into two radion/KK-dilatons is given by: where: and where (m n , Λ n ) and (m m , Λ m ) are the masses and coupling of the n-th and m-th radion/KK-dilatons modes, respectively.

D.3 Annihilation into one KK-graviton and one radion/KK-dilaton
It exists another channel that was not previously considered in the literature: DM annihilation into one KK-graviton and one radion/KK-dilaton. The cross-section for this process is given by the following expressions: where the value of A gr is given by: In all of these expressions we have used (m g,n , Λ g,n ) and (m r,m , Λ r,m ) for the mass and coupling of the n-th KK-graviton and of the m-th radion/KK-dilaton, respectively. Notice that for this particular channel it does not exists a four-legs vertex.