The Refined Swampland Distance Conjecture in Calabi-Yau Moduli Spaces

The Swampland Distance Conjecture claims that effective theories derived from a consistent theory of quantum gravity only have a finite range of validity. This will imply drastic consequences for string theory model building. The refined version of this conjecture says that this range is of the order of the naturally built in scale, namely the Planck scale. It is investigated whether the Refined Swampland Distance Conjecture is consistent with proper field distances arising in the well understood moduli spaces of Calabi-Yau compactification. Investigating in particular the non-geometric phases of Kahler moduli spaces of dimension $h^{11}\in\{1,2,101\}$, we always found proper field distances that are smaller than the Planck-length.


Contents
For relating a theory of quantum gravity, like string theory, to the real world it is of utmost importance to understand which properties of the low-energy effective action can be realized in the string theory landscape and which are outside its reach. The set of theories that cannot be consistently UV completed by a quantum gravity theory has been termed the swampland [1]. If one could make a clear statement that a certain property of the low-energy effective action cannot be realized in the landscape, this would open up the possibility of in principle falsifying string theory. During the last years progress in this direction has been made in particular in the realm of string cosmology, where the question arose whether string theory admits controllable models of large field inflation. In such scenarios the inflaton transverses trans-Planckian field ranges and, due to the Lyth bound, gives a tensor-to-scalar ratio r > 10 −3 , i.e. values that can be measured with current and future experiments. Well motivated candidates for such models are based on axions, whose shift symmetry can protect the scalar potential against quantum gravity corrections.
However, it was argued that the Weak Gravity Conjecture (WGC) [2] provides strong constraints on models where the axion potential is generated by nonperturbative effects [3][4][5][6]. In effect, the WGC implies that for models with one [7] or more axions [8,9], increasing the field range to the trans-Planckian regime means that one moves outside the regime of a controlled low-energy effective action (see also the early work [10]).
A second approach towards realizing axion inflation is to impose a controlled spontaneous breaking of the axionic shift symmetry [11] by adding branes or fluxes. This ansatz is called axion monodromy inflation and was introduced in the stringy context in [12]. One at first sight promising mechanism to generate a polynomial potential for axion monodromy inflation is to turn on background fluxes generating a tree-level F-term scalar potential [13][14][15]. However, concrete attempts to realize such a scenario in a consistent scheme of string theory moduli stabilization [16,17] showed that one encounters major obstacles. In fact, the prior assumptions about the range of validity of the low-energy effective action were violated. For instance, often one could not keep the moduli masses smaller than the Kaluza-Klein masses. A more general observation [18,19] was that taking the backreaction of the rolling axion onto the other moduli into account, the backreacted proper field distance showed a logarithmic behavior Θ ∼ λ −1 log θ.
Here λ −1 can be considered as the scale in field distance where the backreaction becomes substantial.
It was realized in [19,20] that this logarithmic scaling of the proper field distance is very generic and that it precisely reflects one of the conjectured behaviors by Ooguri/Vafa [21] to distinguish effective field theory models that can be realized in string theory (the landscape) from those that cannot be coupled in a UV complete way to gravity (the swampland) [1].
This now called 'Swampland Distance Conjecture (SDC)' [22] was abstracted from the very simple example of string theory compactified on a circle, where it is the Kaluza-Klein tower that shows this behavior in terms of the proper field distance. It says that if one moves over very large distances in the moduli space of an effective quantum gravity theory, there appears an infinite tower of states whose mass scales as m ∼ m 0 exp(−λ∆Θ). This means that for ∆Θ > λ −1 the effective theory breaks down. A new field theoretic perspective on the relation between the logarithmic scaling and the infinitely many exponentially light states was recently given in [22,23].
This paper is concerned with the question, at which scale λ −1 this happens, i.e. what the size of the region where the effective theory can be trusted is. In fact, the concrete models of axion backreaction discussed in [19] always had λ = O (1), that is the cut-off in the field distance was close to the Planck-scale. This motivated to formulate the Refined Swampland Distance Conjecture (RSDC) [20], that extends the original one of Ooguri/Vafa by the statement that λ = O (1). Clearly, if this conjecture holds also for axions with a potential, it will provide a generic quantum gravity obstacle to realize axion-monodromy inflation in a controlled way using a low energy effective action. Recent discussions of the Swampland Distance Conjecture in the context of axion monodromy inflation are [24][25][26][27] (see also [28] for a geometric reason for finite distances in moduli spaces).
It is the purpose of this paper to go a step back to the original work of Ooguri/Vafa and analyze the RSDC not only for moduli spaces of toroidal compactifications but for genuine Calabi-Yau (CY) compactifications of type II superstring theory. This means that the axions do not receive a potential and remain as periodic flat directions. More concretely, we will challenge the RSDC by computing proper field distances along geodesics (and sometimes non-geodesic trajectories) in the Kähler moduli spaces of Calabi-Yau manifolds. For that purpose we will use the available two methods. First one can compute the periods of the mirror dual CY manifold and second one can extract the Kähler potential from the 2-sphere partition function of the gauge linear sigma model (GLSM).
It is well known that these Kähler moduli spaces do not only contain (geometric) regions/phases, where points at infinite distance exist, but also non-geometric phases of stringy nature, like the Landau-Ginzburg (LG) phase. These often do only have a finite radius and therefore do not admit points at infinite distance. To reach the latter one first has to cross the non-geometric phase and move to another geometric phase where such a point do exist. If the distances one can travel along geodesics in such non-geometric phases were already larger than M pl , it would directly falsify the RSDC. Therefore, our main objective is to compute geodesic distances in the moduli space of Calabi-Yau compactifications and compare them with the expectation from the RSDC. We emphasize that very similar in spirit, in [29] axion decay constants have been evaluated in the geometric phases for h 11 ∈ {1, 2} CY threefolds with the result that they are bounded from above by an order one parameter times the Planck-scale.
In section 2, in more detail we explain the RSDC and our approach to check it in Calabi-Yau moduli spaces. For self-consistency, section 3 contains a summary of the known techniques we employed to gain the necessary information on the moduli spaces. The reader familiar with these techniques can safely skip this section. The sections 4 and 5 are the main sections of this paper. For a couple of one and two moduli examples we analyze (geodesic) proper field distances between points in their moduli spaces and compare them with the expectation from the RSDC. In section 6, based on a recent advance [30,31], we also investigate the full 101 dimensional Kähler moduli space of the mirror quintic. The result of this endeavor can be summarized by saying that in all instances our results are consistent with the RSDC, thus providing non-trivial evidence for it. We finally will make the compelling observation that our data seem to suggest that the finite proper field distance one can traverse in a single non-geometric phase scales inversely with the number of phases.

Prerequisites and objectives
Before we dwell into the more formal analysis, let us explain the objective of this paper. This is an analysis of the Refined Swampland Distance Conjecture in the moduli space of Calabi-Yau compactifications.

Basics on Calabi-Yau moduli spaces
Let us first introduce some very basics of type II compactifications on CY manifolds. Consider the compactification of type IIA superstring theory on a Calabi-Yau manifold M with Hodge numbers (h 21 , h 11 ). The four-dimensional effective theory has N = 2 space-time supersymmetry. The dimension of complex structure moduli space gives rise to h 21 hypermultiplets and the dimension of the Kähler moduli space to h 11 vectormultiplets. Such a compactification is dual to type IIB compactified on the mirror CY manifold W with Hodge numbers h 21 (W) = h 11 (M) and h 11 (W) = h 21 (M), which gives the same massless spectrum.
Since hyper-and vectormultiplets decouple in N = 2 supergravity, the vectormultiplet moduli space of the type IIB model on the mirror CY does not receive world-sheet instanton corrections and can be reliably computed at string tree-level (in α ). This complex structure moduli space is mapped via mirror symmetry to the Kähler moduli space of the type IIA model. The latter indeed receives α corrections which can be read-off once one knows the precise mirror map between the moduli.
In this paper we will be concerned with field distances in these vectormultiplet moduli spaces. In section 3, we will review methods to compute their Kähler potential and consequently their metric. The classic method of Candelas et al. [32] applies to the complex structure moduli space of the mirror Calabi-Yau manifold W where techniques were developed to compute the periods of the holomorphic three-form and from them all the information on the (classical) complex structure moduli space. More recently, methods were developed [33][34][35] that work directly for the Kähler moduli space of the original CY M and allow to compute the 2-sphere partition function utilizing the description in terms of gauged linear sigma models (GLSMs). From the partition function one can deduce the Kähler potential.
Of course, the two descriptions have to agree so that we are free to use either the language of the complex structure or the Kähler moduli space. Throughout this paper, we will use the Kähler moduli space, i.e. we will speak of large and small radius regime. When we say conifold locus (that is actually defined in the complex structure moduli space), we mean the mirror dual of it. As we will see in the next section, the advantage is that Kähler moduli more directly set the mass scale of the Kaluza-Klein modes.

The Refined Swampland Distance Conjecture
In this section, we briefly explain the Swampland Distance Conjecture and recall one of its motivations. In the original paper by Ooguri/Vafa [21], what later has been called the 'Swampland Distance Conjecture', was just one of the proposed criteria to discriminate effective field theories arising in the string landscape from those that do not admit a UV-completion, i.e. lie in the swampland. Certainly, this criterium was the most quantitative one and, as the name suggests, is about distances in field space. Let us explain its origin for the Kähler moduli space of the type IIA model on M.
In the large volume regime the Kähler potential for the Kähler moduli of M is given in terms of the triple intersection numbers as where the t i , with i = 1, . . . , h 11 , denote the complexified Kähler moduli where the two-cycles Σ i are a basis of H 2 (M). Following a generic trajectory inside the Kähler cone Im(t i ) ∼ α i r, α i ∈ R, for very large r the effective Kähler potential behaves as K = −3 log r. Hence, the Kähler metric along the trajectory becomes There might exist special trajectories for which the numerator is smaller than three but it will never be larger. The proper field distance Θ along a trajectory x α (τ ) is defined as which in this case becomes 15. This logarithmic scaling has a dramatic consequence for the validity of the effective field theory in which the Kaluza-Klein (KK) modes are assumed to be integrated out. The generic KK mass-scale can be estimated as which implies that for trans-Planckian field excursions Θ > λ −1 ≈ 0.87 an infinite tower of KK-states becomes light, thus spoiling the validity of the effective field theory.
In [21] Ooguri and Vafa formulated this in a more concise manner. They provided a couple of conjectured criteria that an effective theory in the landscape necessarily should satisfy. The most quantitative criterion was termed the Swampland Conjecture in [20] and later was renamed as Swampland Distance Conjecture [22]. It says: Swampland Distance Conjecture: For any point p 0 in the continuous scalar moduli space of a consistent quantum gravity theory (the landscape), there exist other points p at arbitrarily large distance. As the geodesic distance Θ = d(p 0 , p) diverges, an infinite tower of states exponentially light in the distance appears, meaning that the mass scale of the tower varies as Thus, the number of states in the tower which are below any finite mass scale diverges as Θ → ∞. The geodesic distance is measured with the metric on the moduli space.
In the initial version of the conjecture, λ is still an undetermined parameter that specifies when the exponential drop-off becomes significant. As we have seen in (2.5), for trajectories (not necessarily geodesic) in the large volume regime of CY compactifications one has Θ λ ∼ λ −1 ∼ O(1). Infinitely many states becoming exponentially light in field space indicates that the effective quantum gravity theory at the point p 0 only has a finite range of validity in the scalar moduli space. To determine the exact value of the displacement where the effective theory breaks down, all relevant mass scales have to be taken into account. Therefore, the exact upper bound on the displacement is highly model-dependent, but it is sure that in the presence of the exponential drop-off, any physics that we might derive for larger values Θ > Θ λ = λ −1 cannot be trusted.
However, it is not a priori clear at which finite value of the distance Θ 0 along a geodesic this exponential drop-off first sets in. Indeed, the scale Θ λ was derived already in the large radius regime without any reference to the point p 0 where the geodesic started. In [19,26], by analyzing a couple of string theory models, evidence was provided that Θ 0 is equal to the natural mass scale in quantum gravity, namely M pl 1 . For the simple examples chosen, all scales turned out to be related, i.e. Θ 0 Θ λ = λ −1 . Let us point out that these papers focused on stabilized moduli in contrast to the original work of [21]. In the case of unstabilized moduli, general arguments were given in [20] in favor of a Refined Swampland Distance Conjecture which states that not only Θ λ O(1) but also Θ 0 O(1) (in Planck units). In other words, for any starting point of a geodesic, one cannot follow it for a longer distance than M pl before the validity of the effective theory breaks down. The objective of this paper is to test this highly non-trivial conjecture in the Kähler moduli space of type IIA string compactications on CY manifolds. For that purpose we head out to compute the critical values Θ 0 and Θ λ for a plenitude of different trajectories/geodesics in various CY manifolds. Let us explain this idea in more detail.

Objective: Testing the RSDC in CY moduli spaces
As we have recalled, the intuition for the Swampland Distance Conjecture derives from the form of the Kähler potential in the large radius regime 2 . It is known that the Kähler moduli space of a Calabi-Yau manifold also contains non-geometric regions where α corrections become important. For instance, for the quintic the form of the Kähler moduli space has the structure shown in figure 1. As indicated, there are three distinguished points: the large volume point, the conifold and the Landau-Ginzburg (LG) point. The LG or Gepner point is the one of minimal radius. To cover the whole moduli space, one needs at least two charts, whose radii of convergence are shown by the dashed arc in figure 1.
The concrete description of this moduli space will be recalled in section 4.1. At this stage, we just want to mention that one can ask the question whether the RSDC still holds for points p 0 in the small volume regime. We will see that the conifold and LG points are at finite distance in the moduli space so that the only region featuring infinite distances is the large volume regime. Following a geodesic from the LG point to the large volume regime, one expects that the proper field distance depends on Im t like shown in figure 2. As long as one stays in the small volume regime the proper field distance scales polynomially with Im t and at some point (Im t 0 , Θ 0 ) the logarithmic scaling becomes dominant. As a consequence, we define the critical field distance as the sum which includes the distance Θ 0 . This makes sense as we would like to know how much distance can one travel along a geodesic before the effective field theory breaks down. For the quintic example, displacing the Kähler modulus from the LG point towards the large volume phase, Θ 0 would be at least the proper distance to the edge of the convergence region of the LG phase, which is approximately the same as the distance between the LG and conifold point. Clearly, if Θ 0 determined in this way was already larger than the Planck-scale, the RSDC would be falsified. Said the other way around, if the RSDC is correct, the proper field distance that can be traveled in the small volume regime must be smaller than M pl . Therefore, the (proper) radius of convergence for any chart that does not contain a region of infinite distance should be sub-Planckian. Now, let us confirm that the identification of Θ 0 with the radius of convergence is really a good approximation. In the case of a single modulus, the general asymptotic form of the prepotential is [32] where the constant is the one-loop contribution and the dots denote non-perturbative corrections. From this we find that the asymptotic form of the proper distance is The point where the perturbative 1/t 3 contribution is of the same order as the asymptotic logarithm is found to be at where W (x) is the Lambert W -function. For the quintic with Euler characteristic χ = −200, this is approximately at t eq 1.06, a value well below the minimal value of t in the large radius phase t min 1.21. Indeed, at the phase boundary, the logarithm is approximately twice the size of the 1/t 3 term, which can be considered a small correction for all t larger than this. This is the case for all models that we analyzed and of course consistent with the fact that the 1/t expansion is a perturbative expansion which breaks down in the non-geometric regions of the moduli space.
As a result, the logarithm is a good approximation for the behavior of the proper distance over the whole large volume phase and only breaks down at the boundary to non-geometric regions. Thus, the only relevant contribution to Θ 0 comes from inside the non-geometric phases and the behavior predicted by the SDC sets in immediately after crossing the phase boundary.
It is the goal of this paper to check two very concrete predictions of the RSDC, namely that both Θ λ and Θ 0 should be bounded by O(1) in Planck units.

The Kähler metric on moduli spaces
To be able to test the RSDC, for concrete examples of CY manifolds one needs the explicit form of the metric on the Kähler moduli space. In this rather technical section we describe the two employed methods to calculate this metric.
First we use the conjecture of [34] which was proven by [35]. There the Kähler potential and thereby the metric can be read-off from the partition function of a corresponding gauged linear sigma model (GLSM). Second one calculates the periods of the holomorphic three-form for the mirror CY and transforms them into an integral symplectic basis. Using two different methods allows us to also compare the numerical results.
Moreover the two methods have different advantages and disadvantages. While the GLSM construction is very efficient and mathematically easier, it is hard to extract the periods and thereby the mirror map from the partition function in the non-geometric phases. The period formalism on the other hand becomes quite involved, but from the periods one also obtains the mirror map directly.

Sphere partition function for GLSM
In the GLSM approach the Kähler potential is given in terms of the 2-sphere partition function of the gauged linear sigma model (3.1) The partition function for a general N = (2, 2) GLSM was calculated in [33,36].
In the Coulomb branch the relevant fields in the path integral are the scalar parts a j of the vector multiplets and the field strengths F j of the vector part of the vector multiplet. The index j labels the s vector multiplets of the theory, while the index i labels the M chiral fields. As the sphere is a compact space, the field strengths are quantized, 1 2π S 2 F j = m j with the m j being integers. Thus for an abelian gauge group G = U (1) s it can be written as where the purely imaginary integration contour for the scalar fields a i is chosen to simplify the expressions. For an abelian gauge group Z gauge = 1 is trivial. The classical contribution is and the contribution from the 1-loop determinants of the chiral fields are given by After performing the integration, the partition function only depends on the complexified Fayet-Iliopoulos (FI) parameters ξ j = 2πr j + iθ j , and the gaugeand R-charges Q i,j and R i of the chiral fields. In the next section we describe how to identify these parameters for a given Calabi-Yau.

Data of GLSM
The GLSM is a two-dimensional N = 2 supersymmetric gauge theory build out of M chiral multiplets Φ m with m = 1, . . . , M − N and Σ n with n = 1, . . . , N . In addition there are s vector multiplets V j . The chiral multiplets carry the U (1) charges shown in table 3.5.
In addition there exist a superpotential that is linear in the Σ n and the polynomials are such that W carries vanishing charges. Moreover, one associates R-charges R i to the chiral fields such that the superpotential has R-charge 2. The superpotential only depends on the complex structure, therefore the A-model partition function is independent of the superpotential itself. The superpotential only restricts the value of the R-charges. The R-charges of the fields are determined by the condition that R(W ) = 2 with the R-charges of all chiral field positive. This does not uniquely fix the R-charges, but the remaining freedom corresponds to a rescaling of the partition function or equivalently a Kähler transformation of the Kähler potential. In this paper we will be concerned with for instance non-singular hypersurfaces in weighted projective spaces If the space is singular, the singularities have to be resolved. If this is possible by toric methods, additional U (1) gauge symmetries are added. The gauge charges of the chiral fields are in this case determined by the generators of the Mori cone, which can be calculated using the PALP package [37].

Coordinates on Kähler moduli space
The partition function (3.2) is given in terms of the FI-parameters ξ j of the GLSM used to describe the CY. We define z j = exp(2πiξ j ) and q j = exp(2πit j ), where in the second definition t i are the complexified Kähler moduli, t i = Σ i (B + iJ). While the calculations are simpler in the z coordinate system, most results in the literature are stated in terms of the "algebraic" coordinates, denoted by φ or ψ. These are the coefficients of the deformations of the defining polynomial in the mirror dual. To relate these coordinates to each other, one determines special points in the moduli space. These special points are the Landau-Ginzburg point at φ = 0, the large complex structure point φ = ∞ and the singular loci. In the GLSM coordinates, the singular loci are located at the solutions to the equations [ where δ i denotes the VEV of the operator δ i = s j=1 Q i,j a j . Here a j is the scalar part of the vector multiplet. The δ i | H are obtained from δ i by setting all a which are charged under a subgroup H of G to 0 and by only taking the uncharged chiral fields into account. The equation has to be fulfilled for all subgroups of G whose charges span R M −D−rank(H) with positive coefficients.
In the algebraic coordinates, the manifold becomes singular at the points where the transversality condition is violated, i.e.
Matching these two loci allows to fix the coordinate transformation z → φ. The procedure is the same for all models, so we will demonstrate it in the case of the two parameter model Inserting this into (3.9) and expressing the δ i in terms of a j gives where for ease of notation a j = s j . These equations have solutions if Moreover, the only subgroup of G whose charges span R is the first U (1). The remaining charges are Q H = (1 1 − 2). Therefore (3.10) produces the additional relation Turning to the algebraic coordinates, the defining polynomial is (3.16) Solving the system of equations (3.11) with this polynomial gives the conditions φ 2 = 1 and (φ + 8ψ) 2 = 1. The equations φ 2 = 1 and z 2 = 1/4 fix the transformation After some algebraic manipulations the remaining equations fix (3.18) Note that these transformations agree with [39] up to an interchange of the indices.

Evaluating the partition function
The partition function (3.2) is of the Mellin-Barnes type where h(τ ) is an entire function, p i and g i are polynomials in τ and γ and p are constant vectors. In the literature, numerical algorithms solving this type of integrals are described. We use the method of [40] which applies a construction of [41]. Moreover, in some phases it is possible to directly rewrite the integral as an infinite sum over residues, which will be demonstrated in the examples where it applies.

Examples
In this section we apply the methods of the sections 3.1 and 3.1 to some CY spaces. We start with the quintic, which was well studied in [32]. Second, we look at the one parameter models of [42]. Finally we study the two-parameter models of [43].
Quintic P 4 11111 [5] The quintic P 4 11111 [5] has h 11 = 1 and is one of the simplest examples. The gauge group is G = U (1). The defining polynomial is 20) so that one chooses the superpotential 21) and the charges Q = (1, 1, 1, 1, 1, −5). The superpotential forces the R-charges to be of the form R = (2q, 2q, 2q, 2q, 2q, 2 − 10q), up to the choice of a single parameter q. With this choice, q is limited to be taken from the open interval (0, 2/5), such that all R i > 0. The actual value of q does not influence the results.
Inserting these values in the partition function (3.2) and choosing q = 1/5 one obtains In the case a > 0, i.e. the geometric phase, one can close the contour to the left, while for a < 0, i.e. the LG phase, one closes the contour to the right. The gamma functions in the denominator cancel the poles such that only one type of gamma functions contribute in each phase. In the LG phase this is only the gamma function corresponding to the Σ 1 field, leading to first order poles. The partition function can be rewritten in terms of a sum over the residues at these poles. Shifting the summation index m and using the identity for integer b, in terms of hypergeometric functions one obtains [34] Z LG = 1 5 where thef term is omitted. The partition function in this LG phase does not contain any logarithms. In the large volume phase, the five Q = 1 chiral fields contribute, leading to fourth order poles. These result in logarithms and polygamma functions in the partition function and a quite lengthy expression. The metric following from these two partition functions is shown in figure 4. It perfectly agrees with [32].

Hypersurface in weighted projective space
There are four CYs constructed by the vanishing of a polynomial in a single weighted projected spaces with h 11 = 1. These are P 4 11111 [5], P 4 11112 [6], P 4 11114 [8] and P 4 11125 [10]. The gauge charges are given by the weights of the projective space and the degree of the polynomial, Q m = k m , Q 6 = −d, and the R-charges are given by R m = (2−q)·km d , R 6 = q. The value of q can be chosen in the open interval (0, 2), without changing the result. To obtain the highest numerical stability one has to integrate as far away from the poles as possible, making q = 1 the most stable choice. All models in this category have a similar geometry as the quintic, i.e. they consist of a geometric phase and a Landau-Ginzburg-orbifold phase with a Z d -symmetry.

Two parameter models
In addition we look at CYs with h 11 = 2. This class of CYs contains for example P 4 11222 [8], P 4 11226 [12] or P 4 11169 [18]. In these models the charge matrix Q i,j is given by the l-vectors, which span the Mori cone of the given model. These are known for a great variety of CYs or can be calculate using the PALP package [37]. The gauge charges are listed in table 1.
Here, the R-charges of the Σ field is denoted q 1 and the R-charge of the field corresponding to the exceptional divisor q 2 . The R charges for the remaining five fields are generally determined by the superpotential condition to be for the fields with gauge charge (0, 1) and for the other fields. With this choice of parameterization q 1 and q 2 have to fulfil the conditions 0 < q 1 < 2 and 0 < q 2 < 2−q 1 d/Q 6,2 . These parameters contain all information needed to evaluate the partition function and consequently the metric. The result is given in terms of the FI parameters which, as described, can be mapped to the algebraic complex structure moduli of the mirror dual CY. In order to compare with the large volume regime, we finally need the map from the algebraic complex structure moduli to the Kähler moduli t i = Σ i (B + iJ) of the original CY. For that purpose we need the mirror map that is best computed via the periods of the holomorphic three-form on the mirror CY. Let us review how this works.

Kähler potential and mirror map via periods
The Kähler potential can also be determined from the periods of the mirror dual. This will provide us with a cross-check for the GLSM method, as well as with a way to compute the more detailed information of the periods and the mirror map. These are not easily extracted from the 2-sphere partition function.
For computing an independent set of periods all over the complex structure moduli space, for a simple set of mirror dual CYs, one can proceed as follows. For CYs that are mirror dual to hypersurfaces in a weighted projective space, one basic period can be computed by direct integration of the holomorphic three-form in the large complex structure regime. Then one can analytically continue this expression into the Landau-Ginzburg region, in which one can generate a linearly independent set of periods by using the symmetries of the deformed polynomial. A subsequent analytic continuation allows to cover the whole moduli space.
If the Calabi-Yau threefold M is defined by a vanishing polynomial P in a weighted projective space W CP, then the mirror W can be constructed as a quotient M/G, where G is a product of Z n symmetries [44]. This is the so-called Greene-Plesser construction. The polynomial P is split into a defining (Fermat type) polynomial P 0 , a fundamental deformation Φ 0 · 5 i=1 x i = Φ 0 e 0 and all other possible deformations Φ α e α . The Φ i can be considered as variables on the complex structure moduli space of W.
The holomorphic three-form is given by the residue , (3.27) and the fundamental period is defined as where C is an arbitrary constant and the sign as well as factors of 2πi can be reabsorbed into it. Moreover, B 0 is the fundamental cycle which is a T 3 in the limit Φ 0 → ∞, while Γ is an auxiliary contour in C 5 , which allows for a rewriting as a residue integral. In [42], in the large complex structure limit Φ 0 → ∞, the residue integral (3.28) has been carried out perturbatively in 1/Φ 0 to all orders. Given the fundamental period in the large Φ 0 region of the moduli space, one can analytically continue the fundamental period to small Φ 0 . In this region, one can obtain a complete set of periods by where A is the symmetry group of the Fermat type polynomial P 0 . Afterwards, these periods can be analytically continued back to the large Φ 0 region.

Periods for one-parameter models
The first class of CY threefolds are hypersurfaces with h 21 = 1, like the mirror duals of non-singular hypersurfaces in weighted projective spaces In this case (3.28) evaluates to A full basis of the periods for the one-parameter CY hypersurfaces have been determined in [45,46]. For the quintic, i.e. P 4 1,1,1,1,1 [5] with Φ 0 = 5ψ, the fundamental period in the large complex structure/large volume regime |ψ| > 1 reads (3.31)

Mirror map for one-parameter models
To obtain the mirror map, from the literature [42,47] we take the known form of the fundamental period around the large complex structure point For CYs with h 11 given as smooth hypersurfaces in weighted projective space, the coordinate z is related to the deformation parameter of the fundamental deformation via For complete intersections, d is replaced by the sum of hypersurface degrees. The Picard-Fuchs equation admits exactly one solution linear in logarithms The series coefficientsc n can be determined algorithmically from ω 0 [47] as where implicitly the coefficients c n have to be analytically continued in n. The mirror map in the large complex structure/large radius regime is determined by its monodromy properties as The continuation to small ψ is achieved by finding a Mellin-Barnes integral representation for the power series over c n andc n . For degree d hypersurfaces in W CP 4 , with projective weights k j , we have Ψ(k j n + 1) .

(3.37)
Here Ψ denotes the polygamma function. From the coefficients one can see that the series converge in the region |z| < j k For small z, corresponding to large ψ, i.e. the LCS phase, we pick up the residues of the sine at ν ∈ N 0 . The residue integral for ω 0 (z) only gets contributions from the simple poles of the gamma function at ν = −n/d, n ∈ N. The second integrand also has poles at the same values of ν, but now up to second order from the combination of the gamma and polygamma functions. For the analytic continuation of ω 0 (z) into the Landau-Ginzburg regime, we find On the other hand, for the period containing the logarithm in the LCS phase we obtaiñ From this information one can now determine the mirror map via (3.36).

Periods for two-parameter models
The second class of CYs is a set of five two-parameter (h 11 = 2) Fermat hypersurfaces in W CP 4 , for which the full set of periods in the Landau-Ginzburg phase was calculated in [42]. These are the manifolds Their mirrors are given by the vanishing set of the polynomial after modding out an appropriate discrete symmetry group. Here d denotes the degree of the polynomial, the k i are the projective weights, D = d/q 1 is always an integer and the q i (i = 1) can be computed from the projective weights and D through For the computation of the periods it suffices to know that D = 2 for all of the above models, except for the case 3 of P 4 (1,1,1, 6,9) , where D = 3. The fundamental period ω 0 in the large complex structure/large volume regime has been computed in [42] to be given by where the function U ν (φ) can be written in terms of hypergeometric functions as For fixed values of φ the series converges for sufficiently large ψ. The actual convergence criterion is model-dependent.
In order to obtain a full set of periods, this expression has to be analytically continued to small ψ. The result is [42] which converges for sufficiently small ψ. By acting with the phase symmetry of the polynomial one derives the remaining periods where α is a d-th root of unity. As this set of periods is overcomplete, we have to choose a linearly independent subset 4 . This form of the periods is useful for performing the analytic continuation to large φ, since it can be done by standard techniques for the hypergeometric function. In order to continue the periods back to the region where ψ is large, we will find it useful to use an alternative form, where the principal summation runs over powers of φ times a certain generalized hypergeometric function in ψ. The result of a rather lengthy computation is that ω j (ψ, φ) can be decomposed into eigenfunctions η j,r (ψ, φ) of the phase symmetry (ψ, φ, j) → (αψ, −φ, j + 1) as Now, the full ψ-dependence is contained in the functions V n,r (ψ) that are analogues of the function U ν (φ) in (3.45). They consist of a generalized hypergeometric function H n,r (ψ) and a numerical prefactor N n,r . The first is explicitly given by where the underbrackets indicate that for each value in the allowed index range for i, l i , l we have to insert the corresponding parameter in the hypergeometric function. For the relevant models k 1 = 1, so we indeed obtain a hypergeometric function with (p, q) = (2 + k 2 + · · · + k 5 , d) = (d + 1, d).
The numerical prefactor can explicitly be expressed as This expression is valid for φ < 1 and arbitrary ψ, with implicit analytic continuation of the hypergeometric function understood. In practice the degree of the generalized hypergeometric function p F q is reduced in all these examples to at most (p, q) = (13,12).
To compute the metric on moduli space, we first have to transform a linearly independent set of periods into a symplectic basis Π = (F Λ , X Λ ). Then one can calculate the Kähler potential via is the symplectic scalar product. The basis transformation can be found case by case by a monodromy calculation [43,48] or by the algorithmic procedure of [49]. In our analysis of the RSDC for two parameter models, we will focus on the three manifolds P 4 11222 [8], P 4 11169 [18] and P 4 11226 [12]. For the first two, the mirror map and change to symplectic basis can be found in [43,48]. For P 4 11226 [12], we will compute it in the following.
An Example: P 4 11226 [12] To illustrate the calculation of the periods, the mirror map and the metric on the whole moduli space, we consider the CY defined as the mirror of the hypersurface P 4 11226 [12]. A cousin of this model, P 4 11222 [8], has first been analyzed in great detail in [43], although the emphasis has been mostly on the LCS region. The defining polynomial is where we have to mod out a H = Z 2 6 × Z 2 phase symmetry [43]. The transformation (φ, ψ) → (−φ, αψ) can be absorbed into a coordinate redefinition of the ambient space which leaves the hypersurface constraint P (x) invariant, so the actual (uncompactified) moduli space becomes the corresponding Z 12 quotient of C 2 . The manifold develops a conifold singularity at (3.56) Before analytic continuation, a detailed analysis of the asymptotic behavior of U ν (φ) and application of the Cauchy root test shows that the periods (3.46) converge in the region |φ| < 1 and |864ψ 6 | < |φ ± 1|, where the "±" indicates the minimum of the two values. Upon analytical continuation one finds four distinct regions of the moduli space as summarized in table 2.
The LG and LCS regions are familiar from the quintic. In addition we get two hybrid regions, which share properties of the LG and LCS regions. The hybrid region where φ → ∞ and ψ stays small will be called the P 1 (-fibration)-phase, whereas the region with ψ → ∞ and φ small will be referred to as the orbifold(hybrid)-phase, for reasons that will become clear in section 5. The reduced set of periods (ω 0 , . . . , ω 5 ) form a basis. We can calculate these in the LG phase by expanding the hypergeometric function in (3.46) around φ = 0. The result is polynomial in both φ and ψ. In the P 1 fibration region we expand the hypergeometric function around i∞. We find that the even periods ω 2j now contain simple logarithms in φ In a similar fashion, in order to obtain an expression for the periods in the orbifold hybrid phase, we expand the generalized hypergeometric function in (3.48) around i∞, upon which all of the periods except ω 0 acquire logarithmic terms up to third order log(ψ) 3 .
For the LCS region, standard tools are available to compute the metric and periods such as INSTANTON [47]. For this reason we will not further pursue the analytic continuation of the periods into the LCS region.

Mirror map and intersection matrix for two-parameter models
We now explain the computation of the mirror map and intersection matrix. These can both be determined calculating the monodromy matrices of the periods around certain boundary divisors of the compactified moduli space. For the manifolds P 4 11222 [8] and P 4 11169 [18] this has been done in [43] and [48], respectively. Next, we analyse the case P 4 11226 [12], for which the procedure is analogous to P 4 11222 [8] (see [43]). Using the just determined explicit form of the periods, it is straightforward to calculate the monodromy transformations. For the monodromy obtained by moving around φ = 1, we find ω → B ω with The monodromy matrix T about the conifold is determined to be (3.59) Finally, we calculate the monodromy matrix A corresponding to the monodromy around ψ = 0 Following [43] we define the matrix T ∞ = (AT) −1 . The monodromies around the boundary divisors whose intersection is the large complex structure point are We check that the triple products between the R i reproduce the triple intersection numbers of P 4 11226 [12]. Using the ansatz where A i , i = 1, 2 are row vectors and demanding that monodromies around the LCS boundary divisors correspond to shifts of the B-field, hence gauge transformations we can solve for the mirror map up to a constant shift. The result for the Avectors is where we fix the constants to be c 1 = − 1 2 and c 2 = 1 2 . By demanding that the monodromy in the symplectic basis of periods are in fact integral and symplectic, we determine the basis transformation to be This can then be used to compute the Kähler potential (3.53).

RSDC for CY manifolds with h 11 = 1
In this section we investigate the manifestation of the RSDC for regions of one dimensional Calabi-Yau Kähler moduli spaces beyond the large volume phase. As our prototype example, we will discuss the quintic in very much detail. Besides the large volume point, there also exist the conifold and Landau-Ginzburg orbifold points. Recall that in proper distance, the large volume point was infinitely far away from any other point in moduli space, but that for field distances larger than Θ λ = 3/4M pl < M pl a logarithmic scaling sets in that renders infinitely many states exponentially light. Thus, at distances larger than M pl the effective field theory could not be trusted anymore. The question is whether proper distances Θ 0 , accumulated before by traversing non-geometric phases, are also smaller than the Planck-scale. Besides the quintic we also check the RSDC for the other three one-parameter Calabi-Yau manifolds given as smooth hypersurfaces in W CP.

An illustrative example: The quintic P 4 11111 [5]
After investigating the local properties of the metric on the quintic moduli space at the LG and conifold point, we move on to discuss the global properties of the moduli space and test the RSDC in this setting. This requires finding the shortest geodesics between two points in moduli space. Because of the complicated form of the metric, described in terms of hypergeometric functions, we solve the geodesic equation numerically. To obtain the metric for the Kähler moduli space of the quintic we use known results for the periods of the complex structure moduli space of the mirror quintic as well as the mirror map. Later, for the other one-parameter Calabi-Yau threefolds, we will obtain the metric by the GLSM construction of section 3. The availability of these two separate computational methods provides us with a useful crosscheck.

The Landau-Ginzburg point of the quintic
We want to compute the metric on the Kähler moduli space of the quintic threefold. For this purpose we consider the mirror dual of the quintic P 4 [5] (101,1) , whose single complex structure modulus is given by the complex parameter ψ appearing in the hypersurface constraint The transformation ψ → αψ, where α 5 = 1, can be absorbed into a redefinition of the coordinates x i . For this reason the moduli space has the simple form of an angular wedge 0 ≤ Arg(ψ) < 2π/5. By mirror symmetry the complex structure moduli space of this Calabi-Yau is equivalent to the Kähler moduli space of the quintic. After applying the mirror map, it has the structure depicted in figure 1 . At ψ = ∞ there is the large complex structure point, which is mapped to the large volume point t = i∞ of the quintic. For the co-dimension one conifold locus ψ 5 = 1, which is mapped to t i1.21, this hypersurfaces becomes singular, i.e. P = ∂ i P = 0 for i = 1, . . . , 5. Moreover, at ψ = 0 one has the Landau-Ginzburg point which is the point of smallest (but still finite) volume in the mirror dual description where it is located at t = 0.5 + i cot(π/5)/2. Because of this property, it is also the point deepest inside the non-geometric regime of the moduli space. Following [32], one can solve the Picard-Fuchs equations around the Landau-Ginzburg point where an independent set of solutions is given by 5 for k = 1, 2, 3, 4. These infinite sums converge for |ψ| < 1 and have the fundamental domain 0 ≤ Arg(ψ) < 2π/5. In the Kähler moduli space of the quintic, this corresponds to the non-geometric phase. They can be rewritten in terms of hypergeometric functions, whose analytic continuation to the region |ψ| > 1, corresponding to the large volume region, is straightforward. The transformation to a symplectic basis is performed by applying a matrix m, so that Π = m ω, whose inverse was explicitly stated in [50]. Thus, the symplectic basis of the periods can be expanded around the Landau-Ginzburg point as where we have actually expanded them up to order 100. Writing ψ = |ψ| exp(iθ), the resulting Kähler potential takes the simple form  5 Note that a different basis of the periods can be obtained from the fundamental period (3.31) by acting with the Z 5 symmetry of this model, see [32].
We notice that the first three terms feature a continuous phase shift symmetry θ → θ + ∆θ that is broken by the fourth and higher order terms to a discrete shift symmetry θ → θ + 2πn/5. This behavior is very similar to the large complex structure point where also the tree-level Kähler potential features a continuous shift symmetry that is broken to a discrete one by non-perturbative instanton corrections 6 .

Swampland Distance Conjecture
The Swampland Distance Conjecture says that any quantum gravity effective action has only a finite range of validity in field space. In its refined version this critical distance is of the order of the Planck-length. Recall that the intuition for this conjecture came from reasoning in the volume regime. There, the proper field distance Θ was related to the distance t appearing in the masses of KK modes as Θ ∼ λ −1 log t so that for Θ > Θ λ = λ −1 infinitely many states became exponentially light, thus spoiling the validity of the effective field theory.
The question we can now approach is, how this picture generalizes to the stringy quantum regime of small volumes/radii. Here, where the asymptotic logarithmic scaling of the proper distance is not present, we may potentially accumulate a contribution Θ 0 to the proper distance without a significant change in mass scales. If this was already above the Planck scale, it would be in contradiction with the RSDC.
First, we can compute the proper field distance between the Landau-Ginzburg point ψ = 0 and a point ψ = re iθ inside the radius of convergence 0 ≤ r < 1. As we will see shortly, for r < 0.5 we can approximate the Kähler potential by its first three shift symmetric terms. In this case the geodesic is just a ray of constant θ so that the proper field distance is ∆Θ ∼  integrand G ψψ (r, θ) along the two rays θ = 0 and θ = 2π 10 . In the figure we also included the contribution from the first three shift symmetric terms. It shows that up to r = 1/2 this is a good approximation and the angle dependence sets in once one reaches the boundary. The divergence for the line θ = 0 at r = 1 reflects the fact that here one hits the conifold singularity, where the metric diverges. For the mid point θ = 2π 10 , the metric even becomes smaller close to the radius of convergence. However, for the proper field distance we find the numerical results ∆Θ(θ = 0) = 0.45 , ∆Θ(θ = 2π 10 ) = 0.42 . Let us make two remarks • Unlike the large volume point, the Landau-Ginzburg point is at finite proper field distance. Therefore, one does not get the log-behavior for large field distances, as for the large complex structure point. As a consequence the points at large distance are still those in the large volume region.
• In order to reach those points, one has to cross the chart 0 ≤ |ψ| < 1. Therefore, if this region had already a trans-Planckian radius, the RSDC would be violated. The Refined Swampland Distance Conjecture in such a case means that the radius of convergence should not be larger than M pl . This is consistent with the ∆Θ we found.

The conifold point
As we have seen, even though the metric diverges at the conifold point ψ 5 = 1, the distance to it converges. The conifold point is not as interesting as the Landau-Ginzburg point with regards to violating the RSDC because it sits right at the boundary between the two phases. It is at maximum distance to the Landau-Ginzburg point, but this distance is still finite and below the Planck scale. The distance to the large volume phase is infinitesimal. This means that independent of the direction in which we displace, there will be no tension with the RSDC.
In the following discussion we will therefore focus on geodesics which start at the point deepest inside the non-geometric phase, i.e. the Landau-Ginzburg point, and continue into the large volume phase.

Trajectories traversing multiple patches
After locally checking some necessary conditions for the Refined Swampland Distance Conjecture to hold, we will now consider geodesics which traverse multiple coordinate patches. For that purpose, we use the following general procedure • Determine the metric on the moduli space and compute the corresponding geodesics x µ (Θ), parametrized by proper distance Θ.
• Identify a tower of states whose mass should decrease along the geodesics.
• Find the mass M KK (ψ) of this tower as a function of the position in moduli space.
• Express the mass M KK (Θ) in terms of the proper distance along the geodesics.
The moduli space metric of the quintic is obtained patchwise from the periods in the Landau-Ginzburg and large volume regions respectively up to order ψ 50 , or alternatively by the GLSM construction of section 3. The resulting metric is illustrated in figure 4. The geodesics can be obtained numerically by solving the geodesic equation where τ = aΘ + b is an affine parameter and in our case x = (r, θ). We set b = 0 without loss of generality. The parameter a can then be determined from the initial conditions by computing the square root of the pullback of the metric onto the geodesic . We first want to investigate the fate of geodesics going radially outward from the Landau-Ginzburg point ψ = 0. While the coordinate ψ = r exp(iθ) is periodic, θ ≡ θ + 2π/5, the metric additionally enjoys an enhanced Z 2 reflection symmetry along the ray θ = π/5. This allows us to restrict to geodesics in the angular region θ ∈ (0, π/5). We can also directly infer that the rays θ = 0, π/5 are exact geodesics.
The behavior of the radially outgoing geodesics can be qualitatively deduced as follows. The geodesic equation implies For small r the metric is approximately constant so that, with the initial conditionθ(0) = 0, θ stays approximately constant while r increases. When r 1, the θ gradient of the metric becomes important and equation (4.11) implies that the initially straight line is attracted towards the region of increasing G rr , i.e. the conifold point. Once the geodesic passes into the region r 1, the metric becomes approximately flat in the θ direction but the r gradient becomes important. Since nowθ < 0,ṙ > 0, G θθ,r < 0, the minus sign in the second term of (4.11) implies that the geodesic continues towards decreasing θ until it hits the Re(ψ) = 0 axis. It then re-enters the moduli space from the θ = 2π/5 ray.
Since we are interested in the geodesic distance and hence shortest geodesics between points, we can stop integrating the geodesic when it hits the axis. This is because of the symmetry properties of the metric we will always find a shorter geodesic connecting the relevant points in the "upper" half-cone of the moduli space. Figure 5 shows a few representative geodesics.
We can see directly from the discussion of the radius of the Landau-Ginzburg region that geodesics passing too close to the conifold point will not be interesting, since they hit the Re(ψ) = 0 axis shortly after crossing the phase boundary. This means that they will not have total length much bigger than the distance between the Landau-Ginzburg and conifold point ∆Θ 0.45. In fact for the geodesic with θ = π/50 we find the numerical result ∆Θ ≈ 0.5.
In order to test the RSDC in this moduli space we will consider another set of geodesics with a slightly finer scanning of the angle, θ = π/5 − iπ/60, for i = 0, . . . , 11. Disregarding the geodesic θ = π/5, which continues straight to the large volume point, the longest geodesic in this family has θ = 11 60 π, which hits the axis at Re(ψ) ≈ 110, after traveling for a total proper distance of ∆Θ ≈ 1.53.
By performing an asymptotic expansion of the metric in the large volume phase, we realize that it has the asymptotic form g rr (r) ≈ 3 4 (r log r) 2 (4.12) with λ = 2/ √ 3. From this one can see that the geodesic distance from the Landau-Ginzburg point asymptotically grows as the double logarithm Θ(r) 1 λ log log(r) . After identifying a family of relevant geodesics, the next step is to identify a tower of states, whose mass we expect to display the exponential behavior predicted by the Refined Swampland Distance Conjecture. Through mirror symmetry, the complex structure moduli space of the mirror quintic is mapped to the Kähler moduli space of the quintic. The single complex structure modulus ψ is mapped to the overall volume modulus t = B + i J of the quintic. Working in the Kähler moduli space of the quintic, we have as a natural candidate the Kaluza-Klein tower associated to the overall volume. As we have computed in section 2.2, the associated mass scale is then (4.14) In order to express this in terms of the proper field distance, one needs the mirror map t = t(ψ).
Let us now be more precise about the computation of the mirror map, which is defined by Using the explicit form of the periods X 0 and X 1 , we find for the mirror map near the Landau-Ginzburg point Figure 6 shows t LG for different Arg(ψ), which agrees with the more qualitative plot in figure 1. where we used results from section 3.3. At this point we can already see the exponential relation between M KK and Θ. Combining the doubly logarithmic behavior of Θ(r) (4.13) with the logarithmic one of t M (ψ) (4.18), we have 7 This is precisely the behavior predicted by the RSDC. Since we know both the proper distance Θ and the value of the complexified Kähler modulus t = B + i J along the geodesics, we can plot the logarithm of Im(t) against Θ. The Refined Swampland Distance Conjecture predicts a linear behavior after some critical distance Θ 0 1. Figure 7 shows that this is precisely the case. The expected linear behavior is reached for Θ = Θ 0 O(1). The depicted red 7 The factor of two in the exponential should not be taken too seriously, as we just gave a rough estimate for the KK mass scale, M KK ∼ M s /Vol 1 6 . We note that in [22] another proposal for the infinite tower of exponentially light states has been given. There, these were BPS wrapped D-branes, i.e. non-perturbative states. graph corresponds to the central geodesic with initial angle θ = π/5. We find that this is the geodesic for which Θ 0 is the largest. The dotted blue line shows the fit to the asymptotic linear behavior, while the dashed grey fit also captures corrections to Θ 1 λ log(Im(t)) up to order 1/Im(t) 3 . The parameters λ and Θ 0 are determined as follows. The value of Θ 0 is defined to be the value of the proper distance along the geodesics from the Landau-Ginzburg point to the phase boundary at |ψ| = 1. We also define t 0 to be the value of the Kähler modulus at the phase boundary, t 0 (θ) ≡ t(r = 1, θ). To determine λ, we perform a fit of the asymptotic behavior of the proper distance as a function of the Kähler modulus according to the leading order terms (4.20) The angular distribution of the fit-parameters as well as Θ λ , Θ 0 and Θ c is shown in Table 3.  Table 3: Values of the fit-parameters α 0 , α 1 , λ −1 , critical distance Θ 0 and combined critical distance Θ c for the family of geodesics with initial angles θ init = π/5 − iπ/60, for i = 2, . . . , 11. We see that Θ 0 is approximately constant for the quintic. The total critical distance varies mostly because of the angular dependence of λ.
We have excluded the geodesics with i = 10, 11 from the analysis because the fact that they hit the Re(ψ) axis almost immediately after the phase transition did not allow for a good fit. As a result we find that the critical distance is always of order one and satisfies the bound Θ c ≤ 1.387 . The amount of variation of Θ 0 is minimal, while λ deviates noticably between the different geodesics.
As a cross-check of our method, for the central geodesic with θ = π/5 we can compare the result for λ and α 1 with the analytic result (2.10). The value for Θ λ 0.866 agrees perfectly with the expected value of Θ λ = 3/4. For α 1 , we insert the Euler characteristic of the quintic (χ = −200) into the formula (2.10) and obtain α 1 0.168, which deviates from the fit value only by one percent. This can be explained by the fact that we neglected the higher order 1/t corrections in our fit.
We observe that those geodesics passing closer to the conifold and thus deviate the most from being straight lines in the ψ-plane have the largest Θ λ . This is because of the fact that while both the real and imaginary part of the complexified Kähler modulus contribute to the proper distance, only the imaginary part controls a mass scale. The imaginary part of the Kähler modulus is (asymptotically) mapped to the absolute value |ψ| through the mirror map, while the real part is mapped to Arg(ψ). Curving into the "axionic" direction in moduli space thus decreases the rate of the exponential mass fall-off. The fact that we still find Θ λ < M pl for all geodesics is a non-trivial test of the RSDC. It seems to be not unrelated to the statement that periodic directions of the moduli space should have a sub-Planckian periodicity.
For the average over all sampled geodesics of t 0 , the value of the Kähler modulus at the phase transition, we obtain the value Im(t 0 ) 1. 31 [10]. After having discussed the quintic rather detailed in the last section, we are now turning towards the other three manifolds. These are per construction very similar to the quintic so that the results we are going to compute will be qualitatively equivalent and only differ by slightly altered numerical values.
In particular the structure of the moduli space agrees exactly with the one of the quintic. That is, there exists a conifold singularity at ψ = 1 with ψ being the coordinate of the moduli space. The regime |ψ| > 1 is covered by the large volume chart, whereas the region |ψ| < 1 corresponds to the (orbifolded) Landau-Ginzburg phase. There is again a residual Z d symmetry depending on the degree d of the analyzed projective space.
The behavior of the metric for P 4 11112 [6] is qualitatively the same as for the quintic. For these two CY threefolds the metric is approximately flat around the origin G ψψ const, whereas the asymptotic behavior of the metric is like G ψψ 1/(|ψ| 2 log |ψ| 2 ). For the other two threefolds P 4 11114 [8] and P 4 11125 [10] the metrics differ slightly around the origin, in that they have G ψψ const · |ψ| 2 , but show the same asymptotic behavior.
In the following we shall determine average values for λ, Θ 0 and Θ c based on characteristic geodesic trajectories for each of the three moduli spaces. Analogously to figure 5 we will investigate geodesics starting close to ψ = r exp(iθ) = 0 and moving outwards in radial direction. All of them will transit from the Landau-Ginzburg phase into the large volume regime. More precisely, we analyze 12 geodesics γ j , j = 0, . . . , 11 with start points (r i , θ i ) = r i , π d 1 − j 12 and choose an initial velocity (r i , θ i ) = (1, 0). Note that r i has to be adjusted model by model since numerical fluctuations disturb the metric near the origin. Apparently γ 0 corresponds to the angle bisector and γ 11 comes close to the conifold singularity. Before presenting the results for each model, let us point out that we determined the Kähler metric from the partition function of the corresponding GLSM, as described in section 3. A formula to calculate the mirror map of one-parameter models was given in section 3.3. The evaluation of the geodesics follows the procedure described for the quintic. Hence, in order to determine the slope parameter λ, we will again fit the ansatz Now, let us present our results case by case.    The distance between the Landau-Ginzburg and conifold points is ∆Θ 0.23. All results can be found in table 5.

RSDC for CY manifolds with h 11 = 2
In this section we will extend our analysis to CY threefolds with two Kähler moduli. As a consequence, in addition to the LG and large volume phase (LV) we obtain also two hybrid regimes. As a new feature, these hybrid phases have solely one complex parameter ψ or φ bounded, whereas the other one is able to reach infinite distances. Our goals are to determine the precise proper length of finite directions in the different phases of the moduli space, extract the logarithmic behavior of proper distances along infinite directions and last but not least compute the critical distance Θ λ for certain accessible regimes.
More precisely, if we consider an infinite direction, we will always encounter a log-structure in the mirror map. Thus the corresponding Kähler modulus may grow only logarithmically past some critical distance, which is expected to cause a Kaluza-Klein state becoming exponentially light. Therefore, the appearance of the logarithm is in agreement with the Swampland Distance Conjecture [21], where the state in question is given by this Kaluza-Klein mode.
Recall that the RSDC makes a stronger statement by predicting the invalidity of the effective theory after having traversed at most O(1) M pl in moduli space. Hence, the log-term behavior in the proper distance has to occur roughly at proper distance one and finite directions in the moduli space have to have proper length less than one. In this section, we will explicitly confirm the latter and asymptotically approach the log scaling.
Similar to the one-parameter section we shall discuss one example, that is P 4 11222 [8], quite extensively and briefly list the results for other two parameter CY threefolds.

An illustrative example: P 4 11222 [8]
Let us at first focus on the weighted projective space P 4 11222 [8] which was studied in great detail in the literature, see for instance [39,42,43]. Recall the construction of the Kähler metric on the mirror dual in section 3, where we had already introduced basic facts about the geometry of P 4 11222 [8]. In terms of the homogeneous coordinates [x 1 , x 2 , x 3 , x 4 , x 5 ], consider the Calabi-Yau hypersurface with two complex parameters (ψ, φ) corresponding to complex structure moduli. The smooth family of threefolds given by the quotient {P = 0}/(Z 4 ) 3 identifies the mirror of P 4 11222 [8]. Following [43] it is convenient to mod the hypersurfaces {P = 0} by an even larger group, which requires to mod the parameter space (ψ, φ) by a Z 8 . Its generators act according to with α being the 8th root of unity. The special points of the moduli space appear when the hypersurface constraint (5.1) becomes singular, that is, for nontrivial solutions to P = 0 and ∂P/∂x i = 0 for all x i . One finds a conifold singularity at as well as another singularity for 8 The two singularities above split the moduli space into four phases: a smooth Calabi-Yau, a Landau-Ginzburg (orbifold) and two hybrid regimes, which we call hybrid P 1 and hybrid orbifold. The singularity of C 5 /Z 8 can be "blown-up" by replacing the singularity with an exceptional divisor. Here, it turns out that this divisor has two irreducible components [39]: C 3 × P 1 and P 4 . The four different phases are obtained by separately blowing up to these components of the divisor. For instance, consider blowing-up to the component C 3 × P 1 . This leads to a one dimensional target space given by a Landau-Ginzburg (orbifold) bundle over a P 1 space. That is why we denote this regime as hybrid P 1 phase. Again, some of the x i were only fixed classically, such that one still faces a residual Z 4 symmetry at every point of P 1 .
In a second step, also blowing-up along the second component P 4 of the exceptional divisor resolves the Z 4 singularities in each fiber. Satisfying in addition a hypersurface constraint gives a K3 surface fibered over the P 1 base. Thus, one arrives at a smooth Calabi-Yau manifold. The full procedure can be summarized as follows phase LG theory resolved by Alternatively, one may first blow-up the P 4 component. In this case one ends up in a hybrid orbifold phase. This regime is an orbifold because its target space is still equipped with Z 2 quotient singularities. Following [39] let us introduce the coordinates The separation of the four phases of the complex structure moduli space can be nicely depicted in these coordinates, see figure 8. Moreover, the ρ 1,2 coordinates make the spatial extension of the conifold singularity (φ + 8ψ 4 ) 2 = 1 apparent, which is marked by the shaded area in the plot.  [8] in four regimes [39]. Note that one is in principle able to transit between the phases if the moduli are equipped with a non-zero imaginary part.
An obvious question is whether one can circumvent the singular area in plot 8 or in other words, transit between any of the four phase of the moduli space. In principle this is indeed possible by computing the periods in charts covering the whole moduli space. However, our periods derived in section 3.3 do not converge for the entire moduli space. Instead they cannot be trusted arbitrarily close to the conifold singularity. Let us explain this point in more detail for the case of P 4 11222 [8].
The singular loci are fixed by (φ + 8ψ 4 ) 2 = 1 as well as φ 2 = 1, hence one can clearly circumvent the singularities simply by giving ψ or φ a non-zero imaginary part. So, there are in fact trajectories starting and ending in different phases. However, in practice the period computation of section 3.3 converges for |8 ψ 4 | ≶ |φ ± 1|, which agrees with the conifold constraint only for real moduli. Obviously, rotating ψ by some phase shift does not affect the convergence relation, but adding a phase to φ does. Figure 9 shows three plots of the convergence LG Orbi and LV |8 ψ 4 | < |φ ± 1| Figure 9: These plots depict the convergence regions of the periods for P 4 11222 [8], where the blue regions covers |8 ψ 4 | > |φ ± 1| and yellow |8 ψ 4 | < |φ ± 1|. Shown are three different phases of φ. In the left graph we have chosen φ = |φ|, hence the convergence area agrees with the phase picture from the conifold constraint (φ + 8ψ 4 ) 2 = 1. In the middle graph we have φ = |φ| e 1 2 i , i.e. the periods derived in section 3.3 cannot describe transitions between blue and yellow phases. As shown in the right graph, the non-convergence area vanishes precisely for choosing φ = |φ| e π 2 i . In all plots ψ is real.
regions of the periods differing by the phase of φ. As one can see, a small phase for φ opens the border between Landau-Ginzburg and hybrid P 1 phase. Only if the phase is precisely Arg (φ) = π 2 , the convergence relations reduce to a single condition |8 ψ 4 | ≶ |φ| 2 + 1, such that one is able to traverse between any of the four phases. This is only possible due to the Z 2 symmetry of φ determining the convergence relation.
The same statement holds true for P 4 11226 [12], but not for P 4 11169 [18] as one can observe later. In the case of P 4 11169 [18], φ has a Z 3 symmetry and thus the convergence relations cannot reduce to a single one (see equation 5.54 for details). As a consequence, it is impossible to cover the entire moduli space with the charts derived in section 3.3.

Tests of the RSDC: computing Θ 0 and log-behavior
As shown in figure 10, schematically the different phases of the moduli space can also be depicted in the coordinates (ψ, φ). Here we are assuming to have real fields, i.e. setting Im(ψ) = Im(φ) = 0 for simplicity.
Before starting the discussion about the lengths of curves in the moduli space, let us stress that we are distinguishing three different types of curves: we call any arbitrary path a trajectory. If the trajectory is additionally satisfying the geodesic equation it is called geodesic. The length of the globally shortest geodesic Landau Ginzburg orbifold Figure 10: A schematic plot of the four phases of P 4 11222 [8] in real (φ, ψ) coordinates. The singular locus |8ψ 4 | ∼ |φ ± 1| is actually a two dimensional surface due to the ± indicating a logical "and". Directions bounded in field space do not necessarily have to be bounded in their proper distance.
is denoted as the distance or proper length. The reason for making such a clear separation between different types of curves will become apparent in the following. Figure 10 might be misleading in the sense that finite sized directions in the fields ψ and φ do not necessarily have to be finite in their proper length. In the case of P 4 11222 [8], it will eventually turn out that all these seemingly finite directions in ψ, φ are in fact bounded in their proper lengths. To compare with the prediction of RSDC, in the following we shall calculate the proper length of such finite directions.
Secondly, in this section we will be concerned with trajectories along infinite directions. Both in the large volume and in the hybrid phases the Swampland Distance Conjecture implies that they show a log behavior in their distances. One has to be cautious here, as actually, this has to hold for the globally shortest geodesics between two arbitrary points in the moduli space. Hence, one would have to solve the geodesic differential equations for certain start and end points and minimize the set of solutions regarding their proper lengths. Due to the huge variety of possible trajectories in the four real dimensional moduli space of P 4 11222 [8], this is obviously very elaborate and exceeds our computational capabilities. Therefore, we proceed by doing the analysis in asymptotic regimes of the moduli space where we are able to determine the shortest geodesics.
To see the exponentially light KK-modes it is important to express the final result in terms for the Kähler coordinates t i that can be determined via the mirror map. As discussed, the mirror map can be found by analyzing the monodromy properties of the periods. For the case at hand this has been done by [43] and the mirror map in all phases is given by where the periods ω i have been computed in section 3.3. Later, we will find it useful to state the asymptotic behavior of the Kähler coordinates at special points in moduli space. Let us emphasize that the Kähler metrics that we are going to employ, have all been computed with the period method presented in section 3.3. The GLSM method introduced in section 3 was primarily used to cross check results.

Landau-Ginzburg phase
The Landau-Ginzburg regime is similar to the example of the quintic 4.1 in the sense that the algebraic parameters |φ| and |ψ| are both bounded The upper bound ψ c is determined as a solution of the convergence condition |8ψ 4 | < |φ ± 1| for fixed φ. The reader is referred to section 3.3 for details. As already pointed out, whether all geodesics in the LG phases stay finite is a priori not obvious. If they are finite, it is important to compute their proper lengths. For that purpose let us investigate three trajectories as depicted in figure 11. All of these trajectories start close to the smallest possible values of the algebraic moduli ψ = φ = 0. Then, we consider one trajectory only in direction of ψ or φ, respectively. Additionally, there will be one moving directly towards the conifold singularity. The labeling of the curves follows figure 11. Using the metric computed in section 3, we obtain the following lengths for these trajectories where we have denoted x µ = {ψ, φ}. All these directions are finite and smaller than one, as expected from the RSDC. For the sake of completeness, let us point out that the mirror map coordinates in the Landau-Ginzburg regime approach the finite values t 1 = 1 2 (−1 + i) and t 2 0.5 + 0.21 i for φ, ψ → 0. Hybrid phase -P 1 The conceptually new regimes of this moduli space are clearly the hybrid phases P 1 and orbifold. We begin with the hybrid P 1 phase, where the two complex structure parameters are limited by the regime Again, the upper bound ψ c is determined as solution of the convergence condition |8ψ 4 | < |φ ± 1| for fixed φ. The phase diagram of figure 8 leads naturally to the following questions: First, does really only one Kähler modulus t i exhibit a logarithmic behavior for large distances in field space? That is to be expected for trajectories parallel to the φ axis, but not for the ones parallel to the Landau-Ginzburg regime. Second, does there exist a geodesic moving towards |ρ 1 | → ∞ or is the attractive effect of the conifold singularity strong enough to bend any geodesic into the singularity? Finally, will the RSDC hold true even for geodesic passing the Landau-Ginzburg and a hybrid phase before entering the large volume regime? It seems to be challenging for arbitrary geodesics to collect less than O(1) M pl in the proper distance after crossing two regimes. In order to answer the latter two questions one has to consider actual geodesics. Thus we will comment on these questions later and focus now on the first one by analyzing the trajectories shown in figure  12. Note that we assume again for simplicity ψ, φ to be real-valued.
The curve γ 1 starts near ψ = 0, φ = 1 and moves only in ψ direction, hence along the Landau-Ginzburg regime towards the singularity. Via integration we Landau-Ginzburg orbifold Figure 12: The hybrid P 1 fibration regime has one finite as well as one infinite direction.
find its length This result is consistent with the RSDC and with our expectations, as it is close to to the Landau-Ginzburg phase. Besides, we can estimate the asymptotic distance for large φ as depicted by curve γ 2 in figure 12. According to section 3.3, in the P 1 phase the asymptotic behavior of the metric for (φ → 0, ψ → ∞) is Integrating this asymptotic metric for large φ leads to a finite and non-zero value Finally, we want to point out that the trajectory γ 3 "parallel" to the large volume phase has infinite length. To see that, we would have to integrate the Kähler metric of P 1 in the φ direction towards ∞. But asymptotically this integral is given by As a consequence, the direction φ in P 1 is infinite, in contrast to the ψ direction.
As we have seen, it is the Kähler coordinates Im(t i ) (following from the mirror map) that control the exponential drop-off of the KK-modes. As explained in section 3.3 and using eq. (5.6), deep inside the P 1 phase (ψ → 0, φ → ∞), we find t 1 1 2 (−1 + i) + . . . ,

Hybrid phase -orbifold
As one might guess from figure 10, the hybrid orbifold phase is qualitatively quite similar to the P 1 hybrid phase. Now the algebraic coordinates may vary in the interval with ψ c as in the other phases. Again, we focus on three trajectories: a finite one γ 1 along the Landau-Ginzburg regime, its asymptotic equivalent γ 2 for large ψ and an infinite direction γ 3 along the large volume regime. Figure 13 summarizes these curves schematically.
Landau-Ginzburg orbifold Figure 13: In the hybrid orbifold phase we find again an infinite direction γ 3 plus a finite one γ 1 : (0, 0.59) → (1, 0.59). The distance in the φ direction asymptots (indicated by dashed arrow) to a finite γ 2 , more precisely the distance will be zero.
We begin by computing the distance from φ = 0 to the conifold singularity. Keeping ψ fixed, the integral leads to the length which is very close to our result (5.8) in the Landau-Ginzburg phase.
Let us now check whether this asymptots to a finite distance γ 2 as in the P 1 fibration regime. The asymptotic metric for real moduli near φ 0 (see section 3.3 for details) reads (5.18) Consequently, the asymptotic distance γ 2 is indeed finite This is interesting since the distance to the large volume phase vanishes. In other words, for large ψ we end up at the φ = 1 singularity and hence on the one-parameter subspace P 5 11111 [2 4]. From the metric one can see that the pure ψ direction γ 3 of the hybrid orbifold phase is infinite. The metric in the ψ direction leads again to a Θ ∼ log(log ψ) growth of the distance. The asymptotic form of the mirror map confirms exactly our observation. For (ψ → ∞, φ → 0), we find

(5.20)
Thus, the distance is in agreement with the Swampland Distance Conjecture as now Θ ∼ log (log ψ) ∼ log(Im t 1 ). Only t 1 grows logarithmically for large values of ψ, whereas t 2 approaches a constant. Note that this was exchanged in the P 1 regime. In addition, the imaginary part Im(t 2 ) = Σ 2 J asymptotes to zero 9 . This means that one has a vanishing two-cycle Σ 2 , validating the interpretation of being located at the one-parameter subspace P 5 11111 [2 4].

Large volume phase
In the remaining phase of the moduli space under investigation, the algebraic parameters may take values in and ψ c again as in the other phases. By definition it is clear that both directions, φ and ψ, are infinite. Therefore we expect the Θ ∼ log log(−)-behavior, demanded by the swampland distance conjecture, in any of these directions. The mirror map confirms this expectation. Around the large volume point, according to [43] they are given by where the dots denote polynomial corrections. So, whenever one of the algebraic coordinates becomes large, the corresponding Kähler coordinate will grow logarithmically.

Tests of the RSDC: computing Θ λ
So far, we have only motivated the logarithmic behavior of proper distances by analyzing the mirror maps of each phase in the moduli space. Let us now turn towards the critical distance Θ λ where the logarithm is significant, i.e. challenge the RSDC. For that purpose, two different approaches are presented: calculating Kähler potentials and geodesics in asymptotic regions of the moduli space. Both methods will turn out to give the same results for Θ λ .

Asymptotic Kähler potentials
Before commenting on geodesics in two-parameter models, recall that the value for Θ λ deep inside the large volume regime (LV) can be derived from the generic form (2.1) of the asymptotic Kähler potential. It is interesting to compare this Kähler potential in the large volume region to the asymptotic ones in the two hybrid phases. For the mirror of P 4 11222 [8] the prepotential depending on the Kähler coordinates t i is asymptotically given by [43] where the dots denote subleading corrections. Employing the standard formula for the periods Π(t 1 , , we obtain the Kähler potential In the hybrid phases we are able to compute an asymptotic expression for the Kähler potential as well: Hybrid P 1 phase Expanding the Kähler potential K P 1 of this regime around ψ ≈ 0 and φ → ∞, we find asymptotically which is consistent with the metric (5.11). Taking the mirror map (5.14) into account, in leading-order leads to the simple result Obviously, the large volume Kähler potential (5.24) reduces to the P 1 expression for small t 1 and very large t 2 . It also confirms the target space geometry since the Kähler modulus t 2 measures the size of the P 1 space. Moreover, even without calculating geodesics one can derive a value for Θ λ in this asymptotic region. That is, using the induced metric G t 2 t 2 = 1 4 (Im t 2 ) 2 (5.27) and carrying out an analogous calculation as in section 2, we obtain a critical proper distance Θ λ = √ 0.25 0.5. As Θ λ < O(1), this is in agreement with the RSDC.
Hybrid orbifold phase Similarly, we approximate the Kähler potential K orbi in the hybrid orbifold phase around φ ≈ 0 and ψ → ∞ by which is as expected from the large volume expression (5.24) for t 1 much larger than t 2 . From the target space point of view, t 1 corresponds to the overall volume of the orbifold. The critical proper distance is the same as already computed in section 2, Θ λ = √ 0.75 0.87. Next, we challenge the refined conjecture from the perspective of geodesics.

Tests of the RSDC: asymptotic geodesics
In order to investigate the refined version of the Swampland Distance Conjecture one has to check whether the proper lengths of geodesics grow at best logarithmically after having traversed Θ λ ∼ O(1)M pl distances. This behavior is expected to occur for trajectories moving sufficiently far along one of the infinite directions pointed out above. Obviously, in the two-parameter model the most interesting geodesics cross various phases. It is crucial to note that not every geodesic is automatically the globally shortest path between two points.
Basically the reason boils down to the attractive effect of the singularities in the moduli space at hand. However, the RSDC holds only for the shortest geodesic, which leads to technical difficulties. In fact, it is quite delicate to find the solution to the geodesic equation with minimal proper length for given start and end points. In particular so, as we are now working in real four dimensional space. One could only determine rough upper bounds for Θ λ from several typical trajectories.
Here we will instead pursue a different approach, where the goal is to compute geodesics in asymptotic regions of the moduli space, where we have already derived a simple analytic expression for the Kähler metric on the moduli space.
Hybrid P 1 phase At first consider the hybrid P 1 phase and in particular the regime ψ ≈ 0 and φ → ∞. In this regime a trajectory purely in the φ direction will be a geodesic and moreover it will be the shortest one. We show in the following that such a trajectory solves the geodesic equation and compute the critical distance Θ λ . Note that if it is a geodesic, it is automatically the shortest one due to the symmetric influence of the singularities.
Taking into account that we want to keep ψ ≈ 0, we assume the initial values ψ i = dψ i /dτ = 0 with an affine proper time parameter τ . As a consequence the two interesting geodesic equations simplify to Recall that the metric in this regime is asymptotically given by eq. (5.11) Due to the simple structure of the metric, the Christoffel symbols are straightforward to compute Hence the geodesic equation (5.31) for ψ shows that there is no movement in the ψ direction, i.e. we stay at ψ ≈ 0. In other words, a trajectory γ purely in φ direction is indeed a geodesic. The geodesic equation (5.30) for φ can be solved analytically with two integration constants C 1 , C 2 . The solution turns out to be a double exponential of the form If we then evaluate the proper distance Θ for the geodesic γ, we find a direct proportionality to τ . This is clear since Θ and τ are affine parameters. The crucial factor is the √ 0.25 from the numerator of G asymp P 1 , φφ . More precisely we find the following proper distance The SDC predicts an exponential growth of the Kähler coordinate depending on the proper distance. Here, one can observe this directly for the geodesic (5.34) and the mirror map t 2 from eq. (5.14) The exponential factor becomes relevant beyond a critical distance Θ λ = 0.5 according to our definition in section 2. Since we satisfy Θ λ < 1, we are clearly in agreement with the RSDC.
Hybrid orbifold phase One can perform the same analysis for the hybrid orbifold phase with similar results. There, we consider a trajectory at φ ≈ 0 in the limit ψ → ∞, i.e. moving far from the origin purely in the ψ direction. The asymptotic metric (5.18) was again diagonal and included the component G asymp orbi, ψψ = 0.75/|ψ log ψ| 2 . Assuming now dψ/dτ ≈ 0, the geodesic equations and its solutions are equivalent to the hybrid P 1 phase (with two constants C 1 , C 2 ). The proper distance is now given by Θ = √ 0.75 C 1 τ , such that the mirror map (5.20) obeys the following relation The critical distance is now found to be Θ λ = √ 0.75 ∼ 0.87 < 1 and hence satisfies the RSDC, as well. Note that all results from investigating geodesics agree precisely with the one derived from asymptotic Kähler potentials.
To consolidate our results, we consider other two-parameter moduli spaces and perform a similar analysis.

P 4
11226 [12] In this section we analyse, by analogy with P 4 11222 [8], the moduli space of P 4 11226 [12], which was also investigated in [43]. The defining hypersurface polynomial is now given by The mirror of P 4 11226 [12] can again be identified with the Calabi-Yau threefold satisfying the constraint {P = 0}/G, where in this case the group G may be enlarged to include a Z 12 symmetry. Its action on the algebraic parameters reads with α = exp (2πi/12). As explained in [43], the structure of the moduli space is very similar to the one of P 4 11222 [8]. In particular, the four different phases appear again: Landau-Ginzburg, large volume, hybrid P 1 and hybrid orbifold. The singular loci in case of P 4 11226 [12] are φ 2 = 1 and the conifold surface (φ + 864ψ 6 ) 2 = 1. The singular threefolds at φ 2 = 1 are again birationally equivalent to the mirror of a one-parameter model. In this case they correspond to the CICY P 5 111113 [2 6]. The periods may be calculated with the techniques described in section 3.3. The series expansion of the fundamental period converges for depending on the regime we want to investigate. Note that the ± stands again for a logical "and". Let us now briefly investigate various distances in the moduli space of the mirror P 4 11226 [12] in analogy with the schematic drawings in figures 11, 12, 13. In particular we want to determine infinite directions and estimate characteristic finite ones. Let us point out that we assume again real moduli ψ, φ for simplicity.
Furthermore, we shall calculate the mirror map and analyze its asymptotic behavior for each phase. Eventually, we will encounter the same structure as for the P 4 11222 [8] including the logarithms. The derivation of the formula for the mirror map follows [43] and is summarized in section 3.3. The result turns out to be where the periods ω i have been computed in section 3.3.
Landau-Ginzburg phase The boundaries of this phase are governed by the constraints 0 ≤ φ < 1 and 0 ≤ ψ < ψ c , where the maximal value ψ c is the real solution to |864ψ 6 c | < |φ ± 1|. Then, we start at ψ = φ = 0 deep in the Landau-Ginzburg regime and consider two trajectories: one purely in direction φ keeping ψ fixed and one vice versa. By integration we find the maximal length in these directions P 1 hybrid phase The algebraic parameters of P 1 are constrained by the intervals 1 < φ < ∞ and 0 ≤ ψ < ψ c with ψ c as above. We begin with a trajectory along the boundary to the Landau-Ginzburg phase. That is, we start at ψ = 0, φ = 1.1 and integrate in ψ direction up to ψ c without altering φ. The length turns out to be finite and quite small According to example P 4 11222 [8], we expect this length to asymptote to a finite value. Therefore, we approximate the asymptotic metric for (ψ, φ) → (0, ∞). At leading order we find G asymp Instead of this approximate analytic approach, one may also evaluate the integral over the full metric numerically, which confirms our result for ∆Θ 2 . In contrast, distances of the hybrid P 1 phase in φ may become infinite. One way to see this, is that the integral On the one hand, t 1 is finite as in the Landau-Ginzburg phase. On the other hand, t 2 growths logarithmically in φ and hence the proper distance is Θ ∼ log t 2 in agreement with the SDC.
Orbifold hybrid phase In this regime the algebraic parameter may vary within 0 ≤ φ < 1 and ψ c < ψ < ∞, employing the constraint |864 ψ 6 c | ≥ |φ ± 1|. At first, we compute the trajectory from φ = 0 to φ = 1 keeping ψ constant at a minimal value ψ ∼ 0.32. Basically we integrate along the border to the Landau-Ginzburg phase. A simple calculation shows: Recall that asymptotically for large ψ this length was decreasing to zero in the example P 4 11222 [8]. In fact, we will observe the same behavior here. The metric near φ 0 and ψ → ∞ leads to the expression (5.49) Thus, the asymptotic proper distance in φ direction is again vanishing due to its scaling 1 0 dφ G asymp orbi, φφ (ψ) ∼ 1/| log ψ|. One then ends up at the φ = 1 locus which is birational equivalent to the complete intersection CY P 5 111113 [2 6]. Note that one may traverse infinite distances in ψ direction as expected. This is easy to see from the metric and in direct analogy with P 4 11222 [8]. This time, for ψ → ∞ and φ 0 the mirror map (5.41) approaches the values indicating a logarithmic growth of the proper distance depending on the Kähler modulus t 1 . Analogously to P 4 11222 [8], the imaginary part of t 2 vanishes asymptotically, i.e. the two-cycle Σ 2 shrinks to zero [51]. Again, we arrive then on the φ = 1 locus which corresponds to the one-parameter CICY P 5 111113 [2 6].
Large volume phase Finally, the large volume regime 1 < φ < ∞ and ψ c < ψ < ∞ (ψ c as above) is infinite in both directions φ, ψ. As expected, we find a logarithmic growth of the proper distances in any direction, after employing the mirror map [43] The dots indicate polynomial corrections that are sub-leading at infinity.
Summary The different regimes of the moduli space of the mirror P 4 11226 [12] with its finite lengths are schematically depicted in figure 14. The results are qualitatively very similar to P 4 11222 [8]. In accordance with the RSDC, all finite characteristic lengths are smaller than O(1) M pl . Infinite directions show a logbehavior in their corresponding Kähler modulus. This confirms again the predictions from the SDC.
In addition, we were able to determine the critical distance Θ λ , where the logarithmic behavior becomes essential. The computation is indeed equivalent to the one of section (5.1.4). By using the metrics (5.44) and (5.49), we find therefore in the hybrid P 1 phase Θ λ = 1/2 and in the hybrid orbifold phase Θ λ = √ 0.75. 11226 [12] with finite as well as infinite directions as calculated above.

P 4 11169 [18]
The final example in this section is the moduli space of P 4 11169 [18]. An extensive analysis of this model can be found in [48]. In the literature it was shown that the most general possible polynomial of degree 18 employed to describe this moduli space may be reduced to The moduli space is again defined by the hypersurface constraint {P = 0}/G. There exists a scaling symmetry preserving the form of P , which is identified with an enlarged groupĜ. This group induces a Z 18 action on the algebraic parameters with the nontrivial 18 th root of unity α = exp (2πi/18). In fact, there are additional transformations leaving the hypersurface constraint invariant. For these and further details we simply refer to the literature. The qualitative structure of the moduli space is similar to the one of P 4 11222 [8], in the sense that there are four extended phases: Landau-Ginzburg, orbifold, large volume and an additional hybrid phase. However, now we do not have a hybrid P 1 phase, but instead the exceptional divisor has a P 2 component [52] and thus for large φ, small ψ we face a P 2 target space. Moreover, the large volume phase corresponds to a different geometry, that is not a K3 × P 1 fibration that we ended up with in P 4 11222 [8]. The singular loci in case of P 4 11169 [18] are slightly different as well. Both singularities correspond to conifolds and are located at φ 3 = 1 and (φ + 2 2 3 8 ψ 6 ) 3 = 1.
For the calculation of the periods we refer to section 3 and in particular to section 3.3. We will restrict our analysis again to the computation of finite distance in the moduli space according to the schematic curves plotted in figures 11, 12 and 13. One can show that the series expansion of the fundamental period converges for Landau-Ginzburg phase Here, the moduli take values within the intervals 0 ≤ φ < 1 and 0 ≤ ψ < ψ c , with ψ c being the maximal real solution to condition (5.54). We compute the following two trajectories: one purely in direction φ keeping ψ fixed and one vice versa, starting at ψ = φ = 0. Their lengths are given by Computing the mirror maps reveals a logarithmic growth of t 2 in φ and hence a logarithmic growth of the proper distance Θ in t 2 as expected due to the Swampland Distance Conjecture. On the other hand, t 1 approaches the finite value which we also found in the Landau-Ginzburg phase. Indeed, in the limit φ → ∞ and keeping ψ 0, inserting the periods computed in section 3.3 into (5.55) leads to (recall ω = exp(2πi/3)) t 1 ω −2 + · · · − 1 2 + 0.866 i + . . . , t 2 3 2 + 3 i 2π log(3φ) + . . . .

(5.60)
Orbifold hybrid phase In this regime the algebraic parameters are fixed by 0 ≤ φ < 1 and ψ c < ψ < ∞. As before, we begin with computing a trajectory from φ = 0 to φ = 1 keeping ψ constant at a minimal value ψ ∼ 0.32.
In the former examples P 4 11222 [8] and P 4 11226 [12] this distance was asymptotically vanishing for large ψ. Thus, we approximate the Kähler metric near φ 0 and ψ → ∞ (5.62) Thus, also here the distance in φ direction is asymptotically zero. However, in ψ direction it is possible to travel infinite distances. The mirror map coordinates (5.55) for ψ → ∞ and φ 0 are approximately given by Since the proper distance scales like Θ ∼ log log ψ, we end up once again with a logarithmic growth of Θ in t 1 .
As opposed to the P 2 hybrid phase, now it is t 1 which may become infinitely large. Again, the imaginary part of t 2 vanishes asymptotically and hence the twocycle Σ 2 shrinks to zero [51]. In this limit one finally hits the conifold singularity at φ = 1 as the proper distance to the singularity approaches zero. Recall that in the case of P 4 11222 [8] we were running into a non-singular one-parameter subspace instead.
Large volume phase Eventually, the large volume regime 1 < φ < ∞ and ψ c < ψ < ∞ (ψ c as above) is infinite in both directions φ, ψ with the mirror map given by [48]

(5.64)
Summary Overall, distances of the moduli space of P 4 11169 [18] behave similar to the ones of both other two-parameter models, which we discussed above. Figure  15 summarized all distances of P 4 11169 [18]. The logarithmic dependence of the different mirror maps underline the Swampland Distance Conjecture and the small finite lengths its refined version. Furthermore, we can compute the critical distance Θ λ in asymptotic regions of the moduli space. Following section 5.1 the metrics (5.58) and (5.62) lead to Θ λ = √ 0.5 ≈ 0.71 for the hybrid P 2 phase and Θ λ = √ 0.75 for the hybrid orbifold phase. In accordance with the RSDC both distances are less than M pl .

RSDC for a CY manifold with h 11 = 101
After a thorough analysis of the geometry of the moduli space of one-and twoparameter CYs, we now turn to the question of the description of higher dimensional moduli spaces. While the methods used so far are in principle applicable to models with many moduli, the computational effort increases drastically, rendering this approach unfeasible.
A new method, recently developed by Aleshkin and Belavin in [30] and [31], allows the computation of the periods of the complete 101-dimensional Kähler moduli space of the mirror quintic in the Landau-Ginzburg phase. We will apply this method with slight modifications to calculate the radii of the Landau-Ginzburg phase of the Kähler sector of the mirror quintic.
The periods are given by [30] σ µ (φ) = n 1 ≥0 . . . The Kähler potential is where deg(µ) = 5 i=1 µ i is the degree of the corresponding deformation. All moduli corresponding to the permutations of the same t-vector have the same periods and therefore the Kähler potential is symmetric. For computational feasibility we restrict to this five-dimensional subspace, i.e. from now on s = 0, . . . , 4 and µ = 0, . . . , 11. Including the (0, 0, 0, 0, 0) deformation corresponding to H 3,0 and the conjugated cycles, we obtain twelve periods. The Kähler potential becomes where π µ denote the numbers of permutations of the deformations, i.e. π µ = {1, 1, 20, 30, 30, 20, 1, 1, 20, 30, 30, 20}. In addition a combinatorial coefficient c(m s ) has to be included in the periods: . . . This coefficient can be calculated as follows. In principle one has to find 101dimensional vectors m, which solve (6.3). If one uses the symmetry of the problem to reduce to 5 dimensions, one deformation represents π s different deformations.
The calculation is most easily understood in an example. We look at a deformation which has 20 permutations, e.g. the (2,1,1,1,0). If this deformation contributes for example m s =3, there are 3 different ways to obtain this. Three deformations could contribute 1, one deformation contributes 1 and another one 2 or one single deformation contributes 3. Then one has to choose these deformations out of the 20 available, resulting in 20 3 + 20 1 19 1 + 20 1 different combinations. But these deformations are not of the same order in the fields, therefore one has to include the 1 ms! term of (6.2). The final coefficient then is 20 3 1!1!1! + The c(m s ) in (6.6) calculates exactly this number. For the general case, first we define the set of all possible integer partitions with less then π s integers of s as P (s). Then we count how often each integer appears in each permutation of this set. The resulting set is denoted A. We then define a set L k for each m s with elements L k,i as A k,j (6.8) In the example above, L k,j A k,j /(k!) A k,j (6.10) where |P (s)| denotes the number of elements in P (s). These formulas allow for the calculation of the Kähler potential. The final information needed to calculate the proper distances using (2.5) are the boundaries of integration. We start at the Landau-Ginzburg point and go along trajectories where only one deformation is turned on. The endpoint of the trajectory is the conifold. To determine the position of the conifold one has to solve the transversality conditions for each deformation. As we have combined several deformations into one, these conditions are highly non-trivial to solve. This is most easily done by reformulating the problem as a minimization problem which then can be solved by standard minimization techniques. As the objective function we choose Π = P 2 + i ∂P ∂x i 2 + Φ . (6.11) The first two terms are the transversality conditions squared. The last term, linear in the deformation parameter, is added to ensure that the global minimum is the smallest value for Φ, as we are interested in the boundary of the conifold which lies in the Landau-Ginzburg phase.
With the Kähler potential from (6.5) we calculate the proper distance between the Landau-Ginzburg point and the conifold. Table 7 lists these distances. The periods are evaluated up to twelfth order.
0.0089 Table 7: Proper distances between the conifold and the Landau-Ginzburg point in the complex structure moduli space of the quintic.
The distances are all smaller than one, with the distance for the fundamental deformation being the largest. This originates mainly from the conifold position, which depends on the amount of deformations included. For Φ 0 the polynomial is P = x 5 1 + x 5 2 + x 5 3 + x 5 4 + x 5 5 + Φ 0 x 1 x 2 x 3 x 4 x 5 . (6.12) This polynomial fails to be transversal at Φ 0 = −5, which is the known result for the quintic at ψ = 1. If one instead looks at the polynomial P = x 5 1 + x 5 2 + x 5 3 + x 5 4 + x 5 5 + Φ 1 x 2 1 x 2 x 3 x 4 (6.13) the singularity lies at Φ 1 = −5 2 2/5 . If one includes one more deformation, e.g.
P = x 5 1 + x 5 2 + x 5 3 + x 5 4 + x 5 5 + Φ 1 (x 2 1 x 2 x 3 x 4 + x 2 1 x 2 x 3 x 5 ) (6.14) the value changes to Φ 1 = −5/2 6/5 , i.e. it decreases. For more than two deformations this could not be analytically solved. Φ 1 couples in our case to 20 deformations, the numerical procedure described above results in a conifold position of Φ 1 = O(10 −9 ). So while one includes more moduli in the trajectories, the conifold in these direction is much closer to the Landau-Ginzburg point. The latter effect dominates, resulting in a total decrease of proper distance. In view of the RSDC this result is very compelling. It appears that the radii of the non-geometric phases decrease with the number of dimensions. In the oneparameter models, the Landau-Ginzburg phases have a radius of ≈ 0.4. In the two parameter models, the radii of the non-geometric and hybrid phases range between 0.1 and 0.3. Finally, in the 101 parameter example of the mirror quintic the proper distances are 1-2 orders of magnitude lower.
When the number of dimensions of the moduli space increases, one can travel through more phases before reaching a logarithmic behavior. But at the same time, the proper distance per phase decreases. This suggests that at the boundary to the geometric phase, eventually the total collected value of Θ 0 does not scale with the dimension of the moduli space. This implies that in the non-geometric phases Θ 0 phase · #(phases) < M pl (6.15) holds. That is, the average Θ 0 per phase times the number of phases the geodesic passes through is smaller than M pl . A generic geodesic does not pass through all phases. It would be nice to check this explicitly. Sadly, the convergence of the periods and the partition function of the GLSM at the boundaries of the phases is slow. Moreover, finding the global shortest geodesic between two points in a high-dimensional space is a difficult problem. Nevertheless, the fact that the diameters of the non-geometric phases are decreasing is a strong hint that this could be true.

Conclusions
In this paper we analyzed the full Kähler moduli space for a concrete set of Calabi-Yau manifolds with respect to the Refined Swampland Distance Conjecture. Because in the large radius phases the behavior could be expected to be very similar to toroidal models, special emphasis was put on the non-geometric phases. We first reviewed the available two techniques to compute the Kähler potential in these phases and applied and compared them for threefolds defined via hypersurfaces in weighted projective spaces with (mostly) small number of complex structure moduli h 21 ≤ 2. The essential quantity of interest was the length of trajectories/geodesics in the various phases. It turned out that in the LG phases these were all finite and smaller than the Planck-length. Had we found numbers that were say an order of magnitude larger than the Planck-length, the RSDC would have been falsified. The hybrid phases were also showing a hybrid behavior with respect to the length of geodesics. For the complex two-dimensional moduli spaces that we analyzed, there was one direction of finite size and another one of infinite size that showed the same logarithmic scaling behavior as describe by the Swampland Distance Conjecture. All our findings were consistent with the RSDC.
We also analyzed the LG phase of the full 101 dimensional Kähler moduli space of the mirror quintic. Here we observed an interesting scaling of the proper field distances with the inverse of the number of moduli so that eventually the overall collected proper field distance could still remain smaller than one.
Our setting was very close to the original one by Ooguri/Vafa [21] , in the sense that we were considering a flat moduli space, where the axions, the Bfields, are compact and the only non-compact directions are saxionic. As has been clarified by recent work [19,20,[24][25][26][27], for application to axion monodromy inflation, one has to formulate an axionic version of this conjecture. Due to flux, the axions receive a well controlled potential that makes them non-compact so that now the former shift symmetry acts not only on the axions themselves but on the combination of fluxes and axions. In this case, one is not interested in a RSDC along flat directions but along axionic directions with a potential. The backreaction of such an axion excursion onto the saxionic moduli was essential for finding the same logarithmic scaling of the proper field distance. Thus, there are indications that a RSDC is at work here, too. However, more work is needed to undoubtedly establish this and come closer to a sort of no-go theorem for the existence of models of large field inflation in controllable effective field theories derived from string theory.