#### Emergent gravity from Eguchi-Kawai reduction

Received: December
Emergent gravity from Eguchi-Kawai reduction
Santa Barbara 0
CA 0
U.S.A. 0
Open Access 0
c The Authors. 0
0 Department of Physics, University of California
Holographic theories with a local gravitational dual have a number of striking features. Here I argue that many of these features are controlled by the Eguchi-Kawai mechanism, which is proposed to be a hallmark of such holographic theories. Higherspin holographic duality is presented as a failure of the Eguchi-Kawai mechanism, and its restoration illustrates the deformation of higher-spin theory into a proper string theory with a local gravitational limit. AdS/CFT is used to provide a calculable extension of the Eguchi-Kawai mechanism to eld theories on curved manifolds and thereby introduce topological volume independence." Finally, I discuss implications for a general understanding of the extensivity of the Bekenstein-Hawking-Wald entropy.
AdS-CFT Correspondence; Gauge-gravity correspondence; Gauge Symmetry
1 Introduction
1.1 Summary of results
2 Center symmetry and Wilson loops
3 Reproducing gravitational phase structure/sparse spectra/extended
5 Higher-spin theory as a failure of the Eguchi-Kawai mechanism
6 Learning about the Eguchi-Kawai mechanism from gravity
Center symmetry stabilization and translation symmetry breaking
6.2 Extending the Eguchi-Kawai mechanism to curved backgrounds
7 Extensivity of the Bekenstein-Hawking-Wald entropy Reproducing additional features of AdS gravity Reducing or blowing up models The necessity of the Eguchi-Kawai mechanism for holographic gauge theories 28
range of validity of the Cardy formula
Extended range of validity of Cardy formula
Sparse spectra in holographic CFTs
SL(2; Z) family of black holes
3.4 SL(d; Z) family of black holes
4 Correlation functions and entanglement entropy Correlation functions Two-point functions M -point functions
4.4 Entanglement/Renyi entropies 3.1 3.2 3.3
8 Discussion Outlook
A SL(d; Z)
B Four-point function sample calculation
C Validity of gravitational description
Holographic theories with a local gravitational dual have several remarkable features that
can be read o by analyzing (semi-)classical gravity in Anti-de Sitter space (AdS). To
understand the emergence of gravity, it is important to understand precisely in the language of
eld theory what mechanism is responsible for these features. Much of the work in
this direction has focused on constraints from conformal eld theory (CFT). Conformality is
not an essential feature of holography. On the other hand, every holographic theory to date
can be understood as a large-N gauge theory. It is therefore natural to leverage whatever
power such a structure brings us. This brings us to the idea of Eguchi-Kawai reduction.
The proposal of Eguchi and Kawai was that large-N SU(N ) lattice gauge theory could
be reduced to a matrix model living on a single site of the lattice [1]. This equivalence was
postulated through an analysis of the Migdal-Makeenko loop equations (the
SchwingerDyson equations for Wilson loop correlation functions) [2, 3] and assumed the preservation
of center symmetry in the gauge theory. However, it was immediately noticed [4] that the
center symmetry is spontaneously broken at weak coupling, disallowing the consistency of
the reduction with a continuum limit. The authors of [4] further proposed the rst in a long
list of modi cations to the gauge theory in an attempt to prevent center symmetry from
spontaneously breaking. Their proposal is known as the quenched Eguchi-Kawai model,
further studied in [5], where the eigenvalues of the link matrices were frozen to a
centersymmetric distribution. Another proposed variant is known as the twisted Eguchi-Kawai
model, wherein each plaquette in Wilson's action is \twisted" (multiplied by) an element of
the center of the gauge group [6]. Numerical studies have shown these early modi cations
fail at preserving center symmetry as well [7{10].
Let us turn to the continuum. Whether or not center symmetry is preserved is often
checked analytically by pushing the theory into a weakly coupled regime and calculating the
one-loop Coleman-Weinberg potential for the Wilson loop around the compact direction.
This is an order parameter for the center symmetry, and a nonvanishing value indicates
a breaking of center symmetry. An early analytic calculation of the Coleman-Weinberg
potential indicates the center-symmetry-breaking nature of Yang-Mills theories [11].
Nevertheless, there are a few tricks that seem to work at suppressing any center-breaking phase
transitions: a variant of the original twisted Eguchi-Kawai model [12], deforming the
action by particular double-trace terms [13], or considering adjoint fermions with periodic
boundary conditions [14]. For a modern review see [15].
In this work, we will not be concerned with suppressing center-breaking phase
transitions. Instead, we will focus on implications of the Eguchi-Kawai mechanism within
centersymmetric phases. This will not be a restriction to the con ned phase since we will be
considering center symmetry with respect to spatial and thermal cycles. As we will be working
in the continuum, let us formulate the continuum version of the Eguchi-Kawai mechanism.
Consider a d-dimensional large-N gauge theory compacti ed on M
symmetry at the Lagrangian level. If translation symmetry and center symmetry are not
spontaneously broken along a given S1, then correlation functions of appropriate
singletrace, gauge-invariant operators are independent of the size of that S1 at leading order in
(S1)k with center
N . We will review these notions in the rest of the introduction and spend section 4
elaborating on which sorts of observables are \appropriate." This is often called large-N volume
independence, where \volume" in particular refers to the size of the center-symmetric S1s.
The Eguchi-Kawai mechanism is a robust, nonperturbative property of large-N gauge
theories that preserve certain symmetries. Famously, large-N gauge theories also play a
starring role in holographic duality. Curiously both contexts involve emergent spacetime
in radically di erent ways. In this work we will be interested in what predictions the
Eguchi-Kawai mechanism makes about gravity in AdS. Since the proposal concerns only
leading-in-N observables, we will be dealing exclusively with the (semi-)classical gravity
limit in AdS. A simple example illustrating the mechanism at work is the
temperatureindependence of the free energy density on M
S1 at leading order in N in the con ned
S1). In AdS/CFT, this occurs because the
thermal partition function is given by the contribution of thermal AdS below the
HawkingPage phase transition, whose on-shell action has an overall factor of inverse temperature
. When the theory decon nes, the free energy density becomes a nontrivial function
volume independence, see equation (3.1).
We will spend the next section reviewing introductory material, ending with the central
tool of this work, which is that a smooth, translation-invariant gravitational description
implies center symmetry preservation along all but one cycle. Center symmetry can
spontaneously break along a given cycle as its size is varied, but there must only ever be one
cycle which breaks the symmetry. We will refer to these transitions as
center-symmetryswapping transitions (CSSTs). The rest of the paper will leverage this structure to learn
primarily about universal features of gravity, but also to learn about the Eguchi-Kawai
mechanism in large-N gauge theories. For some previous work exploring the Eguchi-Kawai
mechanism in holography, see [16{19].
Summary of results
Our primary tool will be that a smooth, translation-invariant gravitational description of a
state or density matrix in a toroidally compacti ed CFT preserves center symmetry along
all but one cycle. We will use this to produce the following universal features of gravity in
AdS: (a) an extended range of validity of the general-dimensional Cardy formula, (b) the
exact phase structure (including thermal and quantum phase transitions) with a toroidally
compacti ed boundary, (c) a sparse spectrum of light states on the torus, (d) leading-in-N
connected correlators will be given by the method of images under smooth quotients of the
spacetime, which reproduces the behavior of tree-level Witten diagrams, and (e) extensivity
of the entropy for spherical/hyperbolic/planar black holes which dominate the canonical
ensemble; for planar black holes this implies the Bekenstein-Hawking-Wald area law.
(a)(c) are closely related and can be found in section 3, (d) can be found in section 4, and
(e) can be found in section 7. Using gravity to learn about the Eguchi-Kawai mechanism,
we will nd new center-stabilizing structures for strongly coupled holographic theories and
propose an extension of the mechanism to curved backgrounds in section 6.
Center symmetry and Wilson loops
Consider pure Yang-Mills theory on manifold Md 1
SU(N )) with nontrivial center C (for example ZN ):
This theory is invariant under the gauge symmetry
S =
F a = @ A
S1 with gauge group G (for example
S1 ! G a map from our spacetime into the gauge group. The eld strength
Let us consider the function g to be periodic along the S1 only up to an element of
the gauge group: g(x;
+ ) = g(x; )h for h 2 G. For A to remain periodic we need
h 1A (x; )h. But this requires h 2 C so we can commute it past A
h 1. So we see that we can consistently maintain twisted gauge transformations as long as
and cancel it against
we twist by an element of the center. The action above is invariant under these extended
gauge transformations. The space of physical states are constrained to be singlets under
the usual gauge group G but not under the twisted gauge transformations. In particular,
Wilson loops which wrap an S1, which will henceforth be referred to as Polyakov loops,
transform under the generalized gauge transformation. To see this, consider the
pathordered exponential, i.e. the holonomy of the connection, around the S1:
x( + ; ) = P exp
The P stands for path. We will refer to the trace of this object as the Polyakov loop, which
for ordinary gauge transformations causes g and g 1 to annihilate by cylicity. For twisted
gauge transformations, however, we are left with
The W stands for Polyakov. Thus the expectation value of a Polyakov loop can serve as
an order parameter for the spontaneous breaking of center symmetry.
We will always take our trace in the fundamental representation, since the vanishing of
the expectation value of such a loop is necessary and su cient for the preservation of center
symmetry, independent of the matter content. Contrast this with the case of rectangular
Wilson loops (traces of path-ordered exponentials where the path traces out a large
rectangle instead of wrapping an S1) where the trace needs to be evaluated in the same
representation as that of the matter content to access the energy required to decon ne the matter.
Even for matter in vectorlike representations that break center symmetry, there is
Let us now specify to gauge group SU(N ). The center of the gauge group is ZN ,
by which of the N representations of ZN it falls under. This is called the N -ality of the
representation, and it is determined by counting the number of boxes mod N of the Young
tableau of the representation. The addition of matter to our gauge theory explicitly breaks
the center symmetry of the Lagrangian unless the matter is in a representation of vanishing
N -ality [20]. Fundamental representations have N -ality 1 and therefore explicitly break
center symmetry. Adjoint representations, on the other hand, have vanishing N -ality and
therefore preserve center symmetry.
an e ective emergence of the symmetry as N ! 1 as long as the number of vectorlike
avors is kept nite. This is simply because quarks decouple at leading order and one is
left with the pure Yang-Mills theory. Interestingly, by orientifold dualities, even matrix
representations (which break center symmetry and for which the matter does not decouple)
have an emergent center symmetry at in nite N [21, 22].
Calculating Wilson loops in AdS.
There is a simple prescription for calculating the
expectation value of a Wilson loop in the fundamental representation of the gauge theory
using classical string theory. One calculates e SNG for the Nambu-Goto action SNG for
a Euclidean string worldsheet which ends on the contour of the Wilson loop C [23]. Let
us specify to Polyakov loops wrapping an S1 on the boundary. Notice that if this circle
example where this criterion distinguishes con ned and decon ned phases. The thermally
stable (i.e. large) AdS-Schwarzschild black hole, which has a thermal circle which caps o
in the interior, admits a string worldsheet and therefore gives a nonvanishing Polyakov
loop expectation value. This indicates a decon ned phase, which is appropriate as the
AdS-Schwarzschild black hole is the correct background for the gauge theory at high
temperature. Thermal global AdS, however, has a thermal circle which does not cap o in the
interior and therefore gives a vanishing Polyakov loop expectation value. This indicates
a con ned phase, which is appropriate for the theory at low temperature. Indeed, the
bulk canonical phase structure for pure gravity indicates a transition between these two
backgrounds when the inverse temperature is of order the size of the sphere. Similarly, the
entropy transitions from O(1) in the con ned phase (no black hole horizon) to O(N 2) in
the decon ned phase (yes black hole horizon).
There is one more basic geometric fact we will need. Consider an asymptotically
Euclidean AdSd+1 spacetime with toroidal boundary conditions. Preserving translation
invariance along the non-radial directions | a necessary condition for the Eguchi-Kawai
mechanism to work | gives a metric of the form
ds2 =
g (r ! 1) = r2
To avoid conical singularities (e.g. metrics which look locally like r2(d 21 + d 22)), no more
than one of the boundary circles can cap o in the interior of the spacetime. While it
may be possible that none of the boundary circles cap o in the interior (say through the
internal manifold capping o instead), I do not know of any smooth, geodesically complete
examples. We will therefore not consider this possibility, so in our context exactly one cycle
caps o and the other d
1 circles remain nite-sized. This motivates the following simple
yet extremely powerful statement. In any smooth, translation-invariant geometric
description, the expectation value of Polyakov loops in the fundamental representation vanish in
1 of the directions. For theories with an explicit center symmetry, this means that
we will have volume independence along d
1 directions as discussed in the introduction.
Appropriate observables will therefore be independent of the sizes of the circles. For the
gravitational description to be valid, the circles in the interior need to remain above string
scale. For a translation of this criterion into
eld theory language, and in particular a
discussion of Eguchi-Kawai reduction to zero size, see appendix C.
Just like the original Eguchi-Kawai example of pure Yang-Mills, our theory will of
course decon ne, as signaled by the Hawking-Page phase transition in the bulk. This is
sometimes called partial Eguchi-Kawai reduction, since the reduction only holds in the
center-symmetric phase. We will refer to the \Eguchi-Kawai mechanism" and \large-N
volume independence" to describe this state of a airs. (Large-N volume independence
refers in particular to independence of the size of center-symmetric S1s, not necessarily
the overall volume.) From our point of view, the decon nement transition is just a
centersymmetry-swapping transition (CSST) from the thermal cycle to a spatial cycle. It remains
true that d 1 of the cycles preserve center symmetry. CSSTs can also occur between spatial
cycles as they are varied. In this case, the transition is unrelated to con nement of degrees
of freedom, since the entropy is O(1) before and after the transition. It instead signals a
quantum phase transition, which can take place at zero temperature. Interestingly, this
quantum phase transition persists up to a critical temperature.
Reproducing gravitational phase structure/sparse spectra/extended
range of validity of the Cardy formula
We will now show that the semiclassical phase structure of gravity in AdS is implied by our
center symmetry structure. Consider an asymptotically AdSd+1 spacetime with toroidal
boundary conditions. The cycle lengths will be denoted L1; : : : ; Ld with
= L1. We will
pick thermal periodicity conditions for any bulk matter along all cycles and will comment
at the end about di erent periodicity conditions. Assuming a smooth and
translationinvariant description, the phase structure implied by gravity can succinctly be written in
terms of the free energy density as
log Z(L1; : : : ; Ld)
where "vac is a pure positive number (independent of any length scales) characterizing the
vacuum energy on S1
d 2 as Evac=V
"vac=Ld for spatial volume V [24], and Lmin is
the length of the smallest cycle. This is the phase structure independent of the precise bulk
theory of di eomorphism-invariant gravity, as long as we maintain translation invariance
and consider the thermal ensemble. Like in AdS3, all the data about higher curvature
terms is packaged into "vac.
Notice that the triviality of this phase structure implies highly unorthodox eld theory
behavior. The phase structure (3.1) implies thermal phase transitions as the thermal cycle
becomes the smallest cycle. There are also quantum phase transitions when two spatial
cycles are smaller than the rest of the cycles (including
), and the larger of the two is
changed to become smaller. These are quantum phase transitions because they can (and
do) occur when
! 1, so they are not driven by thermal uctuations. These quantum
phase transitions, however, persist at nite temperature. Finally, in any given phase the
functional form of the free energy density is independent of all cycle lengths except for one!
Much of [25] was focused on reproducing this structure in eld theory, and we refer the
reader to that work to see the many nuances involved.
We now turn to the gauge theory. We will see that our framework gives (3.1)
immediately, thereby locating the points where phase transitions occur and the precise functional
form of the free energy in all phases. Consider a
eld theory with our assumed center
symmetry structure, which is that all but one cycle preserve center symmetry. We also
have thermal periodicity conditions for the matter elds along all cycles, since this will give
thermal periodicity conditions for the bulk matter elds and preserve modular S
invariance between any pair of cycles. Notice that by extensivity of the free energy and modular
invariance [24, 26], we have
f (L1 ! 0; L2; : : : ; Ld) =
Since the free energy density is supposed to be independent of the center-symmetry
preserving directions, we deduce that the L1 cycle breaks center symmetry. This is consistent
with the expected decon nement of the theory. Now let us consider varying any of the cycle
sizes. As long as there is no center-symmetry-swapping transition (CSST), f (L1; : : : ; Ld)
continues to depend only on L1. Since the theory is scale invariant, this xes the L1
dependence and we continue to have the behavior (3.2). Finally, any CSST that occurs between
has to occur when L
= L
by the modular symmetry between
all cycles. So, when cycle lengths are equal, they must be symmetric: either they both
preserve the center or they are undergoing a CSST. They cannot both break the center
since only one cycle can ever break the center in our framework.
Using the above facts that f (L1; : : : ; Ld) can only change its functional form at CSSTs
and that two cycles which have equal length must have the same center-symmetry
structhe symmetry between cycles there must be a CSST between L1 and the next-smallest
cycle when they become equal. As L1 is increased further, it is a center-preserving cycle
passing other center-preserving cycles, so no more CSSTs can occur and the free energy
density remains unchanged. Starting from an arbitrary torus, with an arbitrary cycle taken
asymptotically small, this argument produces for us the entire phase structure (3.1).
What about the case where we do not preserve the symmetry between cycles? An
interesting example of this is if we pick bulk fermions to be periodic along some cycles. In
the gravitational picture these cycles are not allowed to cap o in the interior since this
would not lead to a consistent spin structure. Thus, the phase structure is just as in (3.1),
where now Lmin minimizes only over the cycles with antiperiodic bulk fermions. We will
comment more on the eld theory implications of this in section 6.1. To predict this bulk
phase structure, we need to supplement our assumption of d
1 cycles preserving center
symmetry with an assumption about which cycles preserve center symmetry for all cycle
sizes. These cycles can then never undergo CSSTs with other cycles. By repeating the
arguments above, we can reproduce this modi ed bulk phase structure.
Extended range of validity of Cardy formula
Holographic gauge theories, in addition to having the remarkable phase structure exhibited
above, have an extended range of validity of the general-dimensional Cardy formula. The
Cardy formula in higher dimensions was derived in [24, 26] and reproduces the entropy of
toroidally compacti ed black branes at asymptotically high energy:
This precisely mimics how the two-dimensional Cardy formula [27] reproduces the entropy
of BTZ black holes at asymptotically high energy [28]. Large N operates as a
thermodynamic limit that can transform our statements about the canonical partition function into
the microcanonical density of states (this is discussed for example in the appendices of [25,
29]). We nd that the Cardy formula is not valid only asymptotically, but instead is valid
down to E =
1)Evac, which in canonical variables is at a symmetric point
= Li;min
where Li;min is the smallest spatial cycle. This is precisely the energy at which the
HawkingPage phase transition between the toroidally compacti ed black brane and the toroidally
compacti ed AdS soliton occurs in the bulk! Similar arguments in the case of non-conformal
branes should give an extended range of validity for the Cardy formula of [30].
Sparse spectra in holographic CFTs
A sparse spectrum is often invoked as a fundamental requirement of holographic CFTs, and
we have several avenues of thought that lead to this conclusion. Here we will be concerned
with the sparseness necessary to reproduce the phase structure of gravity [25, 29], not with
the sparseness necessary to decouple higher-spin elds [31].
We have already reproduced the complete phase structure (3.1). By the arguments
in [25, 29] this implies a sparse low-lying spectrum
1)Evac) . exp (Li;min(E
where Li;min is the smallest spatial cycle. To roughly recap the argument of [25], modular
constraints on the vacuum energy coupled with the phase structure imply vacuum
domination along all cycles except the smallest one. But to be vacuum dominated means that
excited states do not contribute to the partition function. This leads to the constraint
above, which is really a constraint on the entire spectrum, but is written as above since for
1)Evac we have a precise functional form for the density of states: it takes the
higher-dimensional Cardy form, which trivially satis es the Hagedorn bound above.
One can also access additional sparseness data by investigating di erent boundary
conditions. To point out the simplest case, consider super Yang-Mills theory in a given
number of dimensions with fermions having periodic boundary conditions along one cycle
and antiperiodic boundary conditions along another cycle. Then modular covariance will
equate a thermal partition function ZNS;R with a twisted partition function ZR;NS (twisted
by ( 1)F ), which will access the twisted density of states
F (E). By similar
steps as performed above, one will conclude a sparseness bound for this twisted density of
states. The fact that preserving center symmetry can imply a supersymmetry-like bound
is carefully discussed in a non-supersymmetric context in [32, 33].
SL(2; Z) family of black holes
In this section and the next we will consider the case of twists between the cycles of the
torus. We will begin with three bulk dimensions, where there is an extended family of
solutions known as the SL(2; Z) family of black holes, rst discussed in [34] and elaborated upon
in [35]. They give an in nite number of phases, instead of the two we usually consider in
Lorentzian signature, and we can check volume independence in each of the phases
individually. Twists do not seem to be considered in the literature on large-N volume independence,
but we will show that volume independence continues to hold. A general SL(2; Z) black
hole has a unique contractible cycle, sometimes called an A-cycle. The non-contractible
cycle (sometimes called a B-cycle) is only additively de ned, since for any B-cycle one can
construct another B-cycle by winding around the A-cycle n times (n 2 Z) while going over
the original B cycle. The usual convention is to set this winding number to zero. Due to this
in nity is contractible in the interior [35]. Here Z acts as
+ n for modular parameter
. This data is given by two relatively prime integers (c; d) with c
0. We also need to
include the famous examples (0; 1) (thermal AdS3) and (1; 0) (BTZ). In the rest of this section
we will ignore numerical prefactors in the free energy density and will only track the
dependence on cycle lengths. Let us consider the simplest cases rst, thermal AdS3 and BTZ,
both with zero angular potential. This means
1= are pure imaginary. We have
Thermal AdS : f ( ; L)
BTZ : f ( ; L)
These exhibit volume independence for the center-symmetry preserving (i.e.
noncontractible) cycles. Let us now add an angular potential , which makes
Thermal rotating AdS :
L 2=L2 + 2=L2 =
We again get consistent results, since the lengths of the contractible cycles of thermal
rotating AdS and rotating BTZ are L and p 2 +
2, respectively.
The general SL(2; Z) black hole can be given in a frame where the modular parameter is
(a +b)=(c +d), the contractible cycle z =
z + L(a + b). Their lengths are given as
z +L(c +d) and the non-contractible
jSA1j = pd2L2 + 2cdL + c2( 2 + 2);
jSB1j = pb2L2 + 2abL + a2( 2 + 2) : (3.9)
The free energy density is found, for general
= i =L + =L, to be
d2L2 + 2cdL + c2( 2 + 2)
Notice that a and b enter into the size of the non-contractible cycle, but the condition
expected since the physically distinct states should only care about c; d by the arguments
above. We therefore
nd for the general SL(2; Z) geometry that the free energy density
exhibits volume independence.
SL(d; Z) family of black holes
There exists an unexplored analog to the SL(2; Z) family of black holes in higher dimensions,
which I will call the SL(d; Z) family of black holes. For a review of some salient points
about conformal eld theory on Td and SL(d; Z), see appendix A.
The bulk topology is that of a solid d-torus, with a unique contractible cycle. Winding
a B-cycle by an A-cycle is topologically trivial. A \small" bulk di eomorphism, i.e. one
continuously connected to the identity, can undo this winding. However, winding a
Bcycle by another B-cycle leads to a true winding number and is topologically distinct.
This corresponds to a large di eomorphism in the bulk. Thus, as in the two-dimensional
case, we only need to sum over a subgroup of the full SL(d; Z), because B-cycles are only
1, n 2 Z and V~d the xed contractible cycle vector.
As reviewed in appendix A, the V~i represent lattice vectors that de ne the quotient of the
plane that gives us the torus Td.
Our \seed" solution in three bulk dimensions was global AdS3 at nite temperature
and nite angular velocity. In higher dimensions our seed solution will be the AdS soliton,
with all spatial directions compacti ed, arbitrary twists turned on (including both twists
between spatial directions and time-space twists, interpreted as angular velocities), and the
geometry described above should give an SL(d; Z)-invariant partition function. Ignoring
the important issue of convergence of this sum, we can see that the invariance is naively
guaranteed since the seed solution and its images are independently invariant under the
Z we mod out by. In other words, the analog of Z0;1( ) from the previous section, call it
Z0(V~1; : : : V~d), and its images are invariant under shifts V~i ! V~i + nV~d.
Anyway, this restricted sum is not important for our purposes. It is su cient to show
that an arbitrary element of the SL(d; Z) family has a free energy density that depends
only on the contractible cycle. The simplest case is the AdS soliton at nite temperature
with spatial directions compacti ed, which has free energy density
where Ld is the length of the contractible cycle. This is volume-independent as required.
Twisting any of the non-contractible directions by any of the other directions by any amount
does not change this answer. Thus, the general AdS soliton with arbitrary angular
potentials and spatial twists exhibits volume independence with respect to the non-contractible
cycles. We can now consider SL(d; Z) images of this geometry.
The general SL(d; Z) image geometry has global Killing vector elds for all the
nonVol(Td) R drF (r; r~h) where r~h is a parameter xed by the size of the dth cycle and F (r; r~h)
is some function. Thus, twists can only enter into Vol(Td), but torus volumes are
invariant under twists. Higher-order corrections in the Newton constant GN will bring in
a dependence on the twists, as the momentum quantization of perturbative
torus depends on the twists. In this way we see that volume-independence will break down
density a little more carefully.
Consider a general twisted seed geometry, with the contractible direction chosen to lie
along the dth direction, speci ed by lattice vectors de ning the twists:
L2k =
j=1 i=1
= 666 ...
det(A) = +1 to give
Pid=1 a1i id
Pid=1 adi id
We can compose d(d
1)=2 rotations in the d(d
1)=2 two-planes to make this matrix
upper triangular. This will allow us to identify the new modular parameter matrix
This will not change the lengths of the cycles, which are given as
where Ld gives the length of the contractible direction. The volume of the resulting torus
Vol(ATd) = det(A
) = det(A) det( ) = Y
In particular, it is unchanged by the SL(d; Z) transformation. The free energy density is
exhibiting volume independence in the center-symmetric directions.
with the case of no twist in that direction. This is because there exists a bulk di
eomorphism, continuously connected to the identity, which induces this twist on the boundary.
Twists in non-contractible directions, however, correspond to large gauge transformations
cycle is not su cient. We still have a reduction in moduli, with d2
1) = d(d
numbers specifying distinct geometries. Interestingly, the distinct geometries obtained by
twisting non-contractible directions by other non-contractible directions do not di er in
their classical on-shell action.
Correlation functions and entanglement entropy
In this section we will discuss the implications of the Eguchi-Kawai mechanism for
correlation functions and Renyi entropies. As usual, the statements are restricted to leading order
in N , meaning tree-level Witten diagrams in the bulk. We will only consider volume
independence with respect to a single direction for conceptual clarity; generalization to multiple
directions is straightforward. For correlation functions we will see that position space
correlators must be given by the method-of-images under smooth quotients, as in (4.10). The
connection between large-N reduced correlation functions and the role of the method of
images in AdS has previously been explored in the stringy (zero 't Hooft coupling) limit
in [16, 17], although there are several points of deviation from the present work.
Correlation functions
Let us assume that we are volume-independent with respect to a single direction. Then
connected correlation functions of local, single-trace, gauge-invariant, neutral-sector
observables will be volume independent at leading order in N . Nonlocal operators like
Wilson loops can also be treated as long as they have trivial winding around the cycle.
One term that may need explanation is \neutral-sector." We will explain brie y below;
for details see [14].
Consider the theory on R
S1 as we vary the circle size from some length L to
some other length L0. A given operator in the theory of size L can be decomposed as
n= 1
On=Le2 inx=L :
sector" operators, and it is their correlation functions which are volume-independent. For
independent. While this may seem like a severe restriction, we will only be concerned with
nite-size results from in nite-size results, and all momenta in
commensurate with some momentum in in nite size.
write this precisely as
O(1=N 2(M
purely adjoint theory shows that the connected correlator of M single-trace operators is
N M 1 in front to isolate the leading contribution to the connected correlator. But the basic
point is clear: the statement is about the rst order in N that is expected to have a
nonvanishing answer by large-N counting. If it vanishes, no statements are made about the leading
nonvanishing order. This is what the limit above makes precise in a pure adjoint theory. We
will not worry about the various cases of large-N counting, because within AdS/CFT the
leading-in-N diagrams are given by tree-level diagrams in the bulk. It is only these diagrams
we wish to make a statement about. We will therefore use as our primary tool the equality
hOn1=LOn2=L : : : OnM =LiL = J M 1hOn1=LOn2=L : : : OnM =LiJL
with the caveat that this is the leading-in-N piece of a connected correlator left implicit.
To see the e ect on a general correlation function of local operators, it will su ce to
consider the two-point function. We consider the Fourier representation of the nite-size
hO(x)O(y)iL =
e 2 i(nx+my)=LhOn=LOm=LiL
e 2 i(nx+my)=LJ hOn=LOm=LiJL ;
where in the second line we used (4.3). We could immediately use translation invariance to
write the correlator as a function of only the separation x
y, but to make generalization
to higher-point correlators clear we will keep the dependence until the end.
We can now simplify this expression by transforming the momentum-space correlator
in size J L to position space and evaluating the various sums and integrals:
hO(x)O(y)iL =
dy0e 2 i(nx+my)=Le2 i(nx0+my0)=LJ hO(x0)O(y0)iJL
This generalizes to
hO(x1) : : : O(xM )iL =
hO(x1 + n1L) : : : O(xM + nM L)iJL :
The converse is also true. That is, starting from the method-of-images form of a position
space correlator above, one can show (4.3). Altogether, volume-independence of
neutralsector correlators is true if and only if nite-size correlators are obtained by the method of
images from correlators in a larger size.
Two-point functions
To focus on the simplest case, consider the equal-time two-point function in a
translationinvariant two-dimensional theory. Say we want to construct the nite-size correlator from
the in nite-size correlator. We begin from (4.10) and use translation invariance, which says
that our correlator is only a function of the distance between the two insertion points:
hO(x)O(y)iL = hO(x
y) O(0)iL =
m))L) O(0)iJL
where we used the J L-periodicity of the size-J L correlator. To compare to the in nite-size
correlator we can take J ! 1 in a particular way:
y) O(0)iL = lim
y + nL) O(0)iJL + hO(x
hO(x + nL)O(y + mL)iJL :
ni=0
= lim
n= (J 1)
e 2 i(nx+my)=Le2 i(nx0+my0)=LhO(x0)O(y0)iJL
mL)hO(x0)O(y0)iJL
Notice that taking this limit will give us the correlator on the semi-in nite line with
semiin nite periodicity. Doubling it (and picking up a factor of 2 just as in the factor of J
that comes from relating two-point functions in size L to size J L) gives us the real-line
correlator. We thus have our nal result
n= 1
y) O(0)iL =
Now we compare to gravity in AdS. Conformal eld theory correlators, at leading order
in N , are obtained by extrapolating the bulk-to-bulk propagator to the boundary. Since
the bulk-to-bulk propagator for free elds satis es a Green function equation, we can
the propagator after performing an arbitrary smooth quotient by the method of images.
This gives precisely the form of correlator above, which for example in the famous case of
the BTZ black hole takes the form [36]
hO(t; )O(0; 0)i =
n= 1 cosh 2 t
for operators of dimension
. Notice that this sums over spatial images but not thermal
images. For thermal AdS3, which is obtained instead as a quotient in the Euclidean time
direction, we would sum over thermal images but not over spatial images. In each case, the
correlator is given by a sum over images with respect to the center-preserving direction.
This is exactly what is predicted by our arguments above. Furthermore, we see that the
\free-ness" of large-N theories is not su cient by itself to imply that the correlator should
be a sum over images, since there is no sum over images in the center-breaking direction.
M -point functions
For higher-point functions, recall that we focus only on diagrams in the bulk that do not
have any loops. Any given contribution to the tree-level M -point function is constructed
out of M bulk-to-boundary propagators K and n < M bulk-to-bulk propagators G. This
means there are n + 1 interaction vertices in the bulk. An illustrative case of tree-level
(leading in N ) and loop level (subleading in N ) diagrams is depicted in
The position space correlation function can be written schematically as
hO(x1) : : : O(xM )iAdS =
AdS i=1
where boundary points are denoted by small x and bulk points by big X. From here we
hOn1=L
OnM =LiAdS= = j j
M 1hOn1=L
OnM =LiAdS :
Before we outline the proof of this we need the following facts. The bulk-to-bulk propagator
satis es a Green function equation since the bulk theory is free at this order (leading in
N ). The bulk-to-boundary propagator is obtained by a certain limit of the bulk-to-bulk
propagator where one of its points is pulled to the boundary. Thus, both propagators
There are many more diagrams contributing at this order. Right: a loop-level Witten diagram,
which contributes at rst subleading order in N to the nine-point function. It is constructed out
interaction vertices. There are again many more diagrams contributing at this order.
can be obtained on a smooth quotient of our AdS background by the method of images.
Finally, in momentum space, the integrals over spacetime give n + 1 momentum-conserving
delta functions since there are no loops in the bulk.
The general proof of (4.19) is notationally clumsy and would ruin the already regretful
aesthetics of this paper, so we will provide an outline of the general proof here and give
a sample calculation in appendix B. The left-hand-side is evaluated by an inverse Fourier
transform of the position space expression. The position space expression is written in
by those in AdS by the method of images. These propagators are then transformed into
and integrals are re-ordered at will and this expression is simpli ed down to an integral
over the bulk radial interaction vertices zi. The right-hand-side is evaluated in the same
way, except its propagators are never replaced with other propagators. This leads to (4.19).
Explicit details for a four-point function can be found in appendix B.
So we see that the behavior of tree-level perturbation theory in AdSd+1 under generic,
smooth quotients of spacetime is reproduced. Notice that bulk loops are made of
bulk-tobulk propagators as well, but their momenta are not xed and instead are integrated over.
This leads to a non-universal answer, since there are bulk-to-bulk propagators in the AdS
by the usual method of images trick, the sums are over di erent momenta and cannot be
carried out in general.
Entanglement/Renyi entropies
Another place where volume independence crops up is in the calculation of entanglement
entropy of theories dual to gravity in AdSd+1. For simplicity I will restrict to AdS3.
Recall that the Ryu-Takayanagi prescription dictates that the entanglement entropy
is given by the regularized area of a minimal surface that is anchored on the entangling
surface on the AdS boundary [37]. Consider a spatial interval of size ` on a spatial circle of
size L at temperature T . For entangling surfaces at xed time for static states or density
matrices, the minimal surface will lie on a constant bulk time slice. This makes it clear
that in the con ned phase, which is thermal AdS3, the Ryu-Takayanagi answer will be
independent of the center-preserving thermal circle of size T :
SEE =
. Note that it is not given as a sum over thermal images like in the case of
correlation functions. It is instead completely independent of the thermal cycle size.
In the decon ned phase, i.e. above the Hawking-Page CSST, we get an answer
independent of the center-preserving spatial circle of size L:
SEE =
The minimization inherent in the Ryu-Takayanagi prescription is the reason why we do
not sum over images and so get exact volume independence. (There is a proposal that
the image minimal surfaces instead contribute to entanglement between internal degrees
of freedom, coined \entwinement" [38].)
Apparently, single-interval entanglement entropy is an appropriate neutral-sector
\observable" that obeys large-N volume independence. As shown by a bulk calculation in [39],
volume-dependence appears at rst subleading order in the central charge c (the proxy for
N in two-dimensional theories). Volume-dependence also appears at leading order in the
central charge in the Renyi entropies, but not in any trivial way as in the local correlators
of the previous section. The Renyi entropies must not be neutral-sector observables. The
Renyi entropy in this context is related to the free energy on higher-genus handlebodies; the
analytic continuation connecting to the original torus to de ne the entanglement entropy
is therefore special.
It is interesting that in the cases where we have a volume-independent object, it is the
entanglement entropy and not any of the higher Renyi entropies. This may be related to
the fact that it is the entanglement entropy that naturally geometrizes in the bulk, or to
the fact that it is a good ensemble observable (or these two could be the same thing).
Higher-spin theory as a failure of the Eguchi-Kawai mechanism
We have presented large-N volume independence along all but one cycle of toroidal
compacti cations as a necessary condition for a eld theory to have a local gravitational dual.
This is discussed further in section 8.3. Higher-spin theories are a good example of how
things go wrong if this does not occur, and provide additional evidence for this conjecture.
Higher-spin theories in AdS are nonlocal on the scale of the AdS curvature.
There are a zoo of higher-spin theories, so let us analyze one of the simplest cases.
Consider the parity-invariant Type-A non-minimal Vasiliev theory with Neumann
boundary conditions for the bulk scalar eld [40{42]. This is a theory that can be expanded
around an AdS4 background and has elds of all non-negative integer spin. It is proposed
to be dual to the three-dimensional, free U(N ) vector model of a scalar eld restricted to
the singlet sector [43]. The singlet projection is performed by weakly gauging the U(N )
symmetry with a Chern-Simons gauge eld.
The Chern-Simons-matter theory does not enjoy large-N volume independence. In
fact, given that the matter is in the fundamental representation, it does not even have center
symmetry at the Lagrangian level. However, there is a simple procedure for deforming such
theories into close cousins with explicit center symmetry at the Lagrangian level. This is
discussed for example in [14]. First we add a global U(Nf ) avor symmetry to the boundary
theory, and then we weakly gauge it and change the representation of the matter to be in
the bifundamental. Such a theory has explicit center symmetry at the Lagrangian level
now exist single-trace, gauge-invariant operators made up of arbitrarily long strings of the
bifundamental elds, which did not exist in the previous theory. These are the objects
associated to the string states in the bulk.
This procedure, with some more bells and whistles (the bells and whistles being an
appropriate amount of supersymmetry), is precisely what takes these vector models into
the more mature ABJ theory [44, 45]. The bulk interpretation of this procedure is also
straightforward and deforms the higher-spin theory into its more mature cousin, string
theory. The addition of the global avor symmetry is the addition of Chan-Paton factors
to the higher-spin theory, which implies upgrading the spin-1 bulk gauge eld to a
nonabelian U(Nf ) gauge eld, with all other elds transforming in the adjoint of U(Nf ). The
gauging is then a familiar procedure in AdS/CFT whereby the boundary conditions of this
bulk gauge eld are changed. In fact, this entire story is just that of the ABJ triality
beautifully painted in [46], whereby the higher-spin \bits" are conjectured to bind together
into the strings of ABJ theory. All I would like to highlight is that the deformations that
were necessary to connect to a theory with a local gravitational limit included deforming
to a theory with an explicitly center-symmetric Lagrangian and center-symmetric phases
leads to a lifting [47] of the light states present in vector models [48].
It may be interesting to explore what other deformations of the vector models can
introduce center symmetry and the particular center symmetry structure that is a hallmark
of classical gravity. This may shed light on how to deform the set of proposed higher-spin
dualities for de Sitter space [49{51] to an Einstein-like dual. In the context of de Sitter, the
deformation discussed above leads to a \tachyonic catastrophe" in the bulk, as discussed
in [52], and does not seem to give a viable option.
Learning about the Eguchi-Kawai mechanism from gravity
In this section, we will shift our focus and analyze what gravity teaches us about the
Eguchi-Kawai mechanism.
Center symmetry stabilization and translation symmetry breaking
Although this was discussed in previous sections, we would like to emphasize that the bulk
gravitational description gives us a way to predict whether volume independence is upheld
in particular holographic gauge theories.
rst nontrivial statement is that center
symmetry can be broken along at most one cycle for any given con guration of cycle sizes.
The second nontrivial statement is that there are simple ways to preserve center symmetry
along a given cycle for any cycle size which remains larger than string scale in the bulk.
In particular, periodic bulk fermions and antiperiodic bulk scalars prevent cycles from
capping o in the bulk, as this is an inconsistent spin structure. These cases therefore
preserve center symmetry beyond the CSST points which correspond to gravitational
Hawking-Page transitions. This argument does not explicitly rely on the representation
theory, where the fermions are in the adjoint and the bifundamental, respectively). The
bulk matter is made of gauge-invariant combinations of the boundary
periodicity conditions of the bulk matter will be correlated with the periodicity conditions
of the boundary elds. For example, bulk fermions are constructed by taking single-trace
gauge-invariant operators consisting of an odd number of boundary fermionic elds (e.g.
]). Therefore, bulk fermions with periodic spin structure imply boundary fermions
with periodic spin structure. A similar statement is true for antiperiodic bulk scalars.
Higher-spin dualities, however, o er an interesting case where the bulk theory is purely
bosonic while the boundary theory can be purely fermionic.
The quantum-mechanically generated potentials for the gauge eld holonomies can be
straightforwardly calculated at weak coupling, see for example [11, 53]. From the weakly
coupled point of view, for (3 + 1)-dimensional SU(N ) Yang-Mills theories, preserving center
symmetry with non-adjoint periodic fermions or antiperiodic scalars of any representation
is not possible. The only choice that works is periodic adjoint fermions. Interestingly, for
periodic adjoint fermions (which we will have for super Yang-Mills theories) we seem to
preserve center symmetry at strong coupling as well. But there is a small catch. At weak
coupling, one would need to make the fermions periodic along all k cycles of Tk
At strong coupling, however, this will not give us a background well-described by gravity
alone, since it will be the toroidally compacti ed Poincare patch with circles shrinking to
substringy scales near the horizon. To have a proper gravitational description, we would
need to make the fermions antiperiodic along one of the cycles (or the scalars periodic).
In this case, we will still preserve center symmetry along all the cycles that have periodic
fermions, but this does not match what happens at weak coupling.
1A calculation of the Casimir energy in N = 4 super Yang-Mills on T2
R2 [54], for example, shows
that we lose volume independence along both cycles if the fermion is periodic along only one cycle.
We have not made any comments about operator expectation values and correlation
functions within a grand canonical ensemble, say for turning on a chemical potential for
some global symmetry. In this case, one can spontaneously break translation invariance,
in which case the Eguchi-Kawai mechanism fails [55]. There exist holographic examples of
such spatially modulated phases [56{58].
Extending the Eguchi-Kawai mechanism to curved backgrounds
An important question about the Eguchi-Kawai mechanism is whether it extends to curved
backgrounds. The original Eguchi-Kawai mechanism, and most modern proofs of
largeN volume independence, rely on a lattice regularization which we do not have on curved
backgrounds (although see [59] for some progress in the case of spherical backgrounds).
We will set this aside for the moment as a technical issue. We will see that the natural
uplift of volume independence to curved backgrounds is what I will call \topological volume
independence." We will make this notion precise by de ning an order parameter (which will
again be the expectation value of a Polyakov loop) and checking in gravitational examples
that \topological volume independence" is indeed realized.
eld theory. We already have some hints from
eld theory about what
the Eguchi-Kawai mechanism on curved manifolds should look like. The rst hint comes
from the perturbative intuition for volume independence on torus compacti cations. In
particular, mesons and glueballs form the con ned phase degrees of freedom (baryons have
masses that scale with N and can be ignored for our purposes), and interactions between
theory behaves as if it is free. The con ned phase degrees of freedom are therefore incapable
of communicating with their images to discover they are in a toroidal box. This intuition,
however, is valid even in a curved box. This seems to suggest the size of the manifold should
again not be relevant even if it is curved. But curved backgrounds have local curvature
which can vary as you change the overall size of the background, e.g. increasing the radius
of a sphere. There is no reason the mesons and glueballs cannot feel this local curvature
at leading order in N and thereby (for maximally symmetric manifolds like a sphere of
hyperboloid) would know the overall size of the compact manifold on which they live. So
it seems we should not expect a totally general uplift to curved backgrounds.
The second hint comes from thinking about volume independence in toroidal
compacti cations as a generalized orbifold projection, where one orbifolds by a discrete translation
group [14]. (The language of orbifolds here is conventional but everything is really a
smooth quotient.) Generic changes in the overall size of curved backgrounds cannot be
thought of this way, so we again see that we cannot expect a totally general uplift to
Combining the two hints above provides a compelling case for what kind of setup has
a chance of maintaining a useful notion of volume independence. One begins with a curved
background and considers smooth quotients that change the volume of the manifold. Such
operations do not change the local curvature and maintain the picture of volume-changing
as an orbifold procedure. This therefore utilizes the two hints above. We can now check that
gravity provides a calculable setup where this proposal for the Eguchi-Kawai mechanism
on curved backgrounds can be checked to be valid. The simplest case to analyze is the
conformal eld theory on any simply connected manifold, like the sphere or the hyperboloid.
As an illustrative example, we will investigate the family of lens spaces formed by smooth
quotients of S3, although our results are general. For any smooth quotients of simply
connected manifolds, we will see that the Polyakov loop expectation value continues to
serve as an order parameter for center symmetry.
Holographic realization of the Eguchi-Kawai mechanism on curved manifolds.
Holographic gauge theories in the gravitational limit realize all of the intuition of the
above. They explicitly show that naive volume-independence on curved backgrounds does
not hold. Furthermore, they show that topological volume independence does hold when
interpreted in the above sense!
To see that naive volume independence on curved backgrounds does not hold, we can
consider an observable as basic as the zero-point function, or the free energy density. We
saw that for torus-compacti ed holographic theories, the free energy density was
volumeindependent due to the thermodynamics of black branes. For holographic theories on a
sphere or the hyperboloid, this is no longer the case. The relevant bulk geometries are the
spherical and hyperbolic black holes. The key di erence between these geometries and the
black brane is that the horizon radius is not proportional to the Hawking temperature.
Instead, we have
This means that the Bekenstein-Hawking area law, which scales as rd 1 and gives the
thermal entropy of the CFT, is not extensive in eld theory variables (i.e. does not scale
as T d 1). Here it is important to keep in mind that the theories we are considering are
xing the temperature dependence xes the volume dependence. Moreover
changing the radius of the sphere or hyperboloid can equally well be regarded as changing
we do not have extensivity of the thermal entropy or the free energy, unless rh ! 1 which
pushes us into the black brane limit. Furthermore, correlation functions in these
backgrounds have nontrivial volume-dependence. While the ideas of large-N volume
independence do not apply, there may still be a lower-dimensional matrix model description of the
higher-dimensional theory, see e.g. [60{62]
Both of these problems are solved by considering the smooth orbifolds suggested in
the previous section. The entropy density (or free energy density) becomes appropriately
volume-independent because smooth orbifolds of the spatial manifold cannot be interpreted
as changes in the temperature. Thus, the nonlinear relation between horizon radius and
temperature is not a problem. Said another way, we consider a setup where our eld theory
is on a manifold M
d 1 and its thermal ensemble at high temperature (i.e. the decon ned
theory) is dominated by a black object with horizon topology M
for the eld theory on a sphere, plane, or hyperboloid. The quotient of the manifold Md 1
d 1. This is what happens
by some freely acting group
changes the Bekenstein-Hawking entropy as follows:
SBH =
We see from this formula that the eld theory's entropy density and free energy density is
appropriately independent of such changes in volume, as long as no CSST occurs (more on
this possibility below).
How about correlation functions? As we saw before, these are constructed by bulk
Witten diagrams, whose atoms are bulk-to-bulk and bulk-to-boundary propagators. These
objects again obey a Green function equation in the bulk, meaning any orbifold of the
background geometry can be dealt with by summing over orbifold images. As long as we remain
at leading order in N , meaning we do not consider bulk loops, the correlator will pick up a
trivial volume dependence fully determined by the volume-dependence before quotienting.
We have analyzed volume independence in the decon ned phase of the theory, where
the relevant bulk geometries which dominate the thermal ensemble are given by black holes
with some horizon topology. Uplifting the intuition from our torus-compacti ed theories,
we should expect to nd nontrivial volume-dependence and temperature-independence in
the con ned phase of the theory. We will address this in the next section.
It is interesting that the gravitational description and the
eld theory description
give the same hints as to what sort of generalization to curved backgrounds should work.
In particular, we discussed how from the
eld theory point of view we should expect
volume-changing orbifolds to be the natural uplift of the Eguchi-Kawai mechanism to
curved backgrounds. Gravity gives the exact same intuition, and furthermore it explicitly
demonstrates that it works, at least for the types of observables considered above.
Order parameter on curved manifolds and testing topological volume
independence. For any simply connected manifold M
d 1, the quotient by some freely acting
gives a manifold with nontrivial fundamental group isomorphic to . This means
that we can wrap a Polyakov loop on the existing nontrivial cycle and could reasonably
expect that its expectation value continues to serve as a good order parameter. We will
see in a concrete example that this is the case.
To illustrate the point, consider the family of lens spaces L(p; 1) which have
< 4 =p : (6.3)
d 23=p =
Volume independence for lens spaces can now be stated in terms very close to that of the
generalized orbifold projections used to discuss volume independence for torus
compacti cations. Just as we vary the size of a circle in a torus compacti cation by shifting its
periodicity, in this case we move between lens spaces by changing the periodicity of the
coordinate. To maintain a smooth quotient we need p 2 Z+ so these are discrete changes.
by the change in the
circle. We can wrap a Polyakov loop around the
circle due to the
nontrivial homotopy, and it is again the expectation value of this loop which we propose
serves as our order parameter.
Let us turn to the gravity picture. In the decon ned phase, the orbifolded circle is
non-contractible in the bulk, which implies a vanishing Polyakov loop expectation value
and therefore volume independence:
ds2 =
+ r2d 23=p :
As we showed in the previous section, topological volume independence is indeed realized
in the free energy density and correlation functions. How about the con ned phase? The
naive geometry for the con ned phase is obtained by taking a quotient of global AdS. This
geometry has a conical singularity at the origin which is not well-described within gravity.
For antiperiodic fermions along the orbifolded circle (with even p > 2), it has been proposed
that closed string tachyon condensation regularizes the geometry into what is called the
Eguchi-Hanson-AdS soliton [63, 64]. This geometry has the orbifolded circle smoothly
capping o in the interior, giving a nonvanishing expectation value to the Polyakov loop.
There is a decon ning CSST at inverse temperature
c = 2
8p2 + 20)3=2
(This corrects the expression given in (4.14) of [65].) In the con ned phase, an analysis
of the Eguchi-Hanson soliton shows that we have topological volume-dependence with
respect to the spatial manifold and volume-independence with respect to the thermal circle!
This picture of topological volume independence is also found in ABJM theory through a
nontrivial calculation utilizing supersymmetric localization on lens spaces [66].
An intuitive way to understand the absence of nite-size e ects is to transmute the
connections along the orbifolded circle is discussed in e.g. [67].
The topological volume independence that we discuss seems to be controlling the
relaon S2, as discussed on the gravity side in [68] and the eld theory side in [69]. An important
distinction we draw here from previous work is that the precise pattern of center symmetry
breaking/preservation in the gravitational picture is not realized at weak coupling.
It would be fascinating to carry out weakly coupled tests of our proposal for topological
volume independence of gauge theory on quotients of simply connected manifolds. A simple
case to analyze is that of (3 + 1)-dimensional gauge theory on a lens space. In particular,
our arguments (and weakly coupled intuition from an ordinary circle compacti cation of
at space) suggest that periodic adjoint fermions along the Hopf ber of the lens space
should lead to topological volume independence at weak coupling.
Extensivity of the Bekenstein-Hawking-Wald entropy
The Bekenstein-Hawking area law is a universal formula in Einstein gravity that applies to
black hole horizons, cosmological horizons, and in a certain sense to spacetime itself. Let us
restrict the discussion to black hole horizons and focus on the scaling with area, ignoring the
AdS, since this corresponds to the asymptotically high-temperature limit of the eld theory
where the entropy should become extensive [70]. As discussed in the previous section, in
this limit the scaling of the eld theory entropy with the spatial volume maps directly to
the scaling with the area of the horizon in the bulk. The Eguchi-Kawai mechanism, when
manifested as the volume-independence of entropy density, seems to be exactly the sort
of tool necessary to provide a general mechanism for the area law. But there are several
puzzling and ultimately insurmountable features in trying to pinpoint an exact scaling with
area purely from the Eguchi-Kawai mechanism (except for large toroidally compacti ed
black branes in AdS). We will instead see that the mechanism explains a more general
\area" law: the extensivity of the Bekenstein-Hawking-Wald entropy.2 Before considering
higher curvature corrections, however, let us investigate how the Bekenstein-Hawking area
law is at least consistent with the Eguchi-Kawai mechanism, even if not predicted by it.
In AdSd+1/CFTd, we may ask why toroidally compacti ed black branes above the
Hawking-Page phase transition have no subextensive piece in their classical entropy. Fixing
to a spatial torus, as
! 0 we expect to get an entropy scaling of the conformal eld theory
. Since the bulk Hawking temperature scales as T
rh, this gives S
d 1Vd 1 in bulk variables, which is precisely the Bekenstein-Hawking area law. However,
h
as the temperature is lowered we should generically expect subextensive corrections to the
thermal entropy, which would spoil the universal area law in the bulk since T
tained for black branes at any temperature. However, the Eguchi-Kawai mechanism saves
the day, and implies that no such corrections can appear until one undergoes a CSST, whose
location can be determined as discussed in section 3. This uses the Eguchi-Kawai
mechanism to generalize Witten's explanation of the Bekenstein-Hawking area law to all toroidally
compacti ed black branes above the Hawking-Page transition. Of course, if a periodic spin
structure is chosen for the fermions along all spatial cycles, then no such transition appears
in the gravitational regime and we can explain the area law for arbitrary toroidally
compacti ed black branes. This is just a recap of what was shown more carefully in section 3.
What about the Bekenstein-Hawking area law for black hole horizons with
curvature, like the spherical or hyperbolic black holes in AdS? Again adopting center-symmetry
preservation along the orbifolding cycle (up to any CSST) as our working assumption, we
deduce that the entropy density in the eld theory is volume-independent in the
orbifold2The language here and in the literature is very confusing. We refer to the Bekenstein-Hawking entropy
as extensive even though it is very famously subextensive. By this we mean extensive in horizon area
not volume. Also, the Wald entropy is sometimes referred to as providing subextensive corrections to the
Bekenstein-Hawking area law, by which it is meant terms that do not scale with the area of the event
horizon. When we refer to the extensivity of the Wald or Bekenstein-Hawking-Wald entropy, we mean the
fact that it can be written as an integral of a local quantity over the horizon of the black hole. We will
discuss this further below.
ing direction. The orbifolding direction is a discrete direction, indexed by an integer p in
the previous section. Any potential analytic continuation to complex p is on very shaky
ground, but the Bekenstein-Hawking area law for the original spherical or hyperbolic black
hole may be understood by analytic continuation from the discrete family of quotiented
geometries. This is akin to understanding entanglement entropy through the discrete Renyi
family, although there the analytic continuation is on much rmer footing.
If these ideas are correct, then they provide a mechanism for the area law for large
black holes with horizon topology
which dominate the canonical ensemble for some dual
eld theory on background
. What about small black holes? Here the interpretation in
terms of plasma balls in the dual large-N gauge theory may be useful [71]. It may then
be true that the Eguchi-Kawai mechanism applies to this decon ned plasma ball in a way
which maps to the area law in the bulk, as we saw for large black holes above.
Stringy corrections and extensivity of the Wald entropy.
We can ask about
subleading order in the 't Hooft coupling , which should correspond to bulk stringy
corrections. One way these stringy corrections manifest themselves is as higher-curvature
corrections to the bulk Einstein gravity. The Polyakov loop analysis remains the same and
continues to indicate center symmetry preservation along d 1 cycles. Thus a center-symmetry
analysis in the eld theory predicts that for any planar/spherical/hyperbolic black holes,
the entropy density should be volume-independent in any smooth orbifolding direction.
To check this, we can look at zero-point functions like the entropy density. Since we
have higher-curvature corrections we need to use the Wald formula for black hole entropy.
For toroidally compacti ed black branes, the area law is maintained although the coe cient
can change. For spherical or hyperbolic black holes, we have corrections to the
BekensteinHawking area law which do not scale with the area of the horizon. This seems to be in
contradiction with the Eguchi-Kawai mechanism. To address this, let us step back for a
There is a spiritually correct but technically incorrect holographic explanation of the
Bekenstein-Hawking area law that is often given. It says that the scaling with area is
because there is a holographic dual theory in one lower dimension with the same entropy,
and its entropy is scaling with volume as it should be. This captures the holographic spirit,
but in general it is technically incorrect as can be seen in many ways. If the area maps to a
eld theory volume, does the 1/GN map to temperature? This is of course wrong. Even in
the cases where the area does map rigorously to volume, like toroidally compacti ed black
branes, why does the eld theory not exhibit any subextensive corrections to its entropy?
This we explained within our framework of large-N volume independence. Finally, what
about higher curvature corrections? In the bulk the entropy picks up what are sometimes
confusingly called \subextensive corrections to the Bekenstein-Hawking area law" from the
Wald entropy formula. This ruins the Bekenstein-Hawking area law. Interpreted as bulk
stringy corrections and therefore as corrections in the gauge coupling of a dual eld theory,
why should going to weaker coupling ruin extensivity?
These issues are clari ed by recalling that the Wald entropy is an integral over the
event horizon and is therefore extensive. Consider a black hole with metric ansatz
ds2 =
is independent of r and t. This does not capture the most general case but
will su ce for the argument. The Wald entropy for a general di eomorphism-invariant
higher-curvature theory of gravity with Lagrangian density L is given as an integral along
is the binormal to the horizon. The corrections implied by the Wald entropy are
terms that do not scale as rhd 1, which is the scaling of the Bekenstein-Hawking entropy.
But notice that the general theory will still scale with the volume of : SW
Vol( ). This
is what we mean by extensivity, which as before can be thought of in terms of quotients of
SW =
! Md 1=
=)
SW ! SW =j j :
In this sense the general Wald entropy | therefore the entropy in an arbitrary
di eomorphism-invariant theory of classical gravity | is just as extensive as the
Bekenstein-Hawking entropy.
For black branes this means that the Wald entropy
To bring this extensivity of curved horizons into clearer focus, consider quantum
(subleading in GN , i.e. subleading in N ) corrections to the Bekenstein-Hawking-Wald entropy.
At rst order, these are logarithmic in the area of the event horizon:
SW + log(SW ) + : : : :
The correction neither scales with the area of the horizon nor with Vol( ). It is truly
This discussion should make clear that the gravity that emerges from our center
symmetry analysis is not necessarily Einstein gravity. Nevertheless, it would be fascinating
if somehow the stringency of this center symmetry structure necessitated a CFT with
an Einstein gravity dual. One way this could occur is by requiring a sparse higher spin
spectrum [31] | recently shown to give c
a for the anomaly coe cients c and a in
four-dimensional CFTs [72] | just as it required a sparse spectrum of low-lying states to
reproduce the extended range of validity of the general-dimensional Cardy formula. In this
spirit, it is encouraging that restoration of a center symmetry plays an important role in
deforming higher-spin theory (within which the higher spin elds cannot be made sparse)
into ABJ theory (within which they can).
Reproducing additional features of AdS gravity
We have shown that several universal features of AdS gravity can be reproduced with the
starting assumption of center symmetry preservation along all but one cycle in a large-N
theory (and the suitable generalization of this statement to curved backgrounds as discussed
before). However, there are still several features that we would like to explain.
A powerful technical assumption in the context of reproducing universal features of
gravity in AdS3/CFT2 is that of Virasoro vacuum block domination of the four-point
function on the sphere. This is expected to be a valid assumption in large-c theories with a
sparse light spectrum and sparse low-lying operator-product-expansion (OPE) coe cients.
This suggests that it might be implied by our framework. More precisely, consider a
fourpoint function hO1(1); O2(z)O3(1)O4(0)i, which can be decomposed into representations
of the Virasoro algebra (i.e. into Virasoro blocks) by inserting a complete set of states. It
is believed that taking c ! 1 with external and internal operator dimensions scaling with
c leads to an exponentiation of the Virasoro block [73, 74]:
i = 1; 2; 3; 4 ;
where hp is the internal operator dimension. Now taking z ! 0 leads to vacuum block
leading OPE singularity from bringing together O2 and O4:
F (c; hp; hi; z) = zhp h2 h4 (1 + O(z)) :
In holographic theories, vacuum block dominance | like the Cardy formula we discussed
in (3) | seems to have an extended range of validity, which in this case means for a
range of z beyond the asymptotic limit z ! 0. This requires a sparseness bound both on
the spectrum of states and on the operator product expansion coe cients. Our framework
requires large c to begin with and reproduces a sparse light spectrum as discussed in
section 3. Data about the OPE coe cients is also accessible in this framework since
treelevel Witten diagrams have bulk interactions. Concretely, one may hope to analyze more
carefully volume independence for the blocks between the sphere and the torus, possibly
using the tools of [75{79]. An orthogonal clue that vacuum block dominance may be implied
by this framework is a calculation of the entanglement entropy in a heavy microstate on a
circle [80{82], which gives an answer independent of the size of the circle!
Accessing some quantity or feature which directly exhibits the smooth, geometric
nature of the bulk is another natural goal for this framework. The singularities of [83] are
one such feature that indicate a sharp geometric structure.
Reducing or blowing up models
The strong coupling description of holographic theories makes manifest that one can achieve
full volume-independence (i.e. preserve center symmetry for all cycle sizes) along directions
with periodic (antiperiodic) boundary conditions for fermions (bosons), as long as one
direction has the opposite boundary conditions and caps o
in the interior.
then perform a large-N reduction of these theories down to matrix quantum mechanical
theories, i.e. (0 + 1)-dimensional theories. For a discussion of the validity of the reduction
down to zero size, see appendix C. This captures physics in both con ned and decon ned
phases. When describing thermal physics in the gravitational limit, there will always be
one direction that does not reduce, prohibiting the reduction to a matrix model description,
i.e. a (0 + 0)-dimensional theory. (See [84] for a discussion of subtleties in dimensionally
reducing volume-independent theories.)
Blowing up low-dimensional models is another interesting direction to pursue,
especially in light of recent developments in low-dimensional models like the Sachdev-Ye-Kitaev
(SYK) model, which captures some features of AdS2 gravity. The addition of avor to the
SYK model [85] gives it the necessary ingredient to be blown up into a higher-dimensional
model by the methods of [86, 87]. (See also [88, 89] for a di erent kind of blow-up.)
The necessity of the Eguchi-Kawai mechanism for holographic gauge
theI have intermittently referred to the Eguchi-Kawai mechanism as a necessary feature of
holographic gauge theories. In a certain sense, this is obviously ridiculous. Center
symmetal matter eld, although we still have a controlled gravitational description of the infrared
physics. In this case, what I really mean is that there exists a theory which at large N is
equivalent to the one with a single fundamental eld, but which has center symmetry at
the Lagrangian level. More simply, the fundamental matter decouples at leading order in
N , so the center symmetry is emergent at in nite N . As explored heavily in the literature
on large-N volume independence and mentioned in the introduction, orbifold/orientifold
dualities in many cases imply an emergent center symmetry at in nite N , even when
centerbreaking matter does not naively decouple [21, 22]. It is this generalized emergent sense in
which the Eguchi-Kawai mechanism is necessary. In other words, there is a possibility that
center symmetry (whether existing explicitly or emergent) is playing an indispensable role
in realizing the precise form of volume independence necessary to admit a gravitational
description. Absent conclusive evidence to the contrary, I conjecture this to be the case.
It would be nice to have a formalism centered around center symmetry that does not use
the crutch of gauge theory, which may be an unnecessary redundancy of description.3
Interesting cases to study, which may teach us about large-N equivalences, are that
of the D1-D5 system and of attempts at describing unquenched
avor in AdS/CFT. At
the orbifold point, the D1-D5 theory can be thought of as a free symmetric orbifold CFT.
It is a gauge theory, but the gauge group is SN which has a trivial center. Nevertheless,
this theory seems to have at least some aspects of large-N volume independence. It
realizes the phase structure of gravity, and certain correlators can be written as a sum
over images [91]. Indeed, the physics of long strings/short strings and sharp transitions
(see for example [92, 93]). The case of unquenched
avor requires keeping Nf =N
N ! 1, which means the avor does not decouple at leading order in N . If there is a
3It was pointed out to me by Brian Willett that center symmetry can be discussed in the language of
one-form global symmetries, without the need for a Lagrangian, as developed in [90].
smooth gravitational description in AdS (or some similarly warped spacetime), then the
nature of nite-size e ects should be analyzed.
There are many directions to pursue with these ideas in the context of AdS/CFT, only
some of which were addressed above. Taking a broader view of the subject, it is clear that
holographic dualities which have rules like those of AdS/CFT will have similar
volumeindependent structure in correlation functions and phase structures. It is remarkable that
rst introduced by Eguchi and Kawai is relevant only in the context of
largeN gauge theories, and even then only at leading order in N . It is as if it was tailor-made
to explain classical gravity, whether within AdS or with some other asymptotia. Indeed,
one universal feature of classical gravity we can hang our hats on, robust against changes
in asymptotia, is the extensivity of the Bekenstein-Gibbons-Hawking-Wald entropy. The
universality of this simple formula only exists at leading order in GN , and we saw that in
the context of AdS/CFT it maps to universal volume-independence at leading order in N
for certain black holes. It is natural to conjecture that the same mechanism is controlling
the entropy for all black holes, although as discussed in the main text this statement should
be interpreted with care. The capability of these ideas in addressing classical gravity more
this is a useful and technically accurate perspective beyond AdS/CFT remains to be seen.
I am greatly indebted to Aleksey Cherman for his many patient explanations of modern
developments regarding the Eguchi-Kawai mechanism. I would like to thank Tarek Anous,
Aleksey Cherman, and Raghu Mahajan for useful conversations and comments on a draft.
I would also like to thank Dionysios Anninos, David Berenstein, William Donnelly, David
Gross, Gary Horowitz, Nabil Iqbal, Zohar Komargodski, Don Marolf, Mark Srednicki,
Tomonori Ugajin, Mithat Unsal and Brian Willett for useful conversations.
In this section we will review some basic points about SL(d; Z), the mapping class group of
Td. When d is even, we will want to consider PSL(d; Z) instead, obtained by quotienting
by the center f1; 1g. For simplicity we will just refer to the group as SL(d; Z) with this
Naively, the torus is parameterized by d arbitrary real vectors V1; : : : ; Vd in
ddimensional space. However, we can use global rotational invariance to eliminate Pd 1
overall size modulus. The torus now has d2
1 = (d
1)(d + 2)=2 real moduli.
Calling the coordinates x1; : : : ; xd, we have a twist modulus ij between xi and all xj with
i=1 i =
i < j, and a size modulus ii for d
1 of the cycles xi. Keeping the overall size modulus
explicit, we can arrange the moduli in terms of the following lattice vectors:
2 V~1 3
6 V~2 77
u1 = 66
U1 = 660 1
U2 = 660 0 1
Generators. In this section we will list four sets of generators of SL(d; Z) and show them
to be equivalent. Our rst two sets of generators of SL(d; Z) can be written as
u2 = 660 0 1
d matrices. The small u's can be shown to generate the big U 's and vice
versa. The relations for e.g. d = 4 are
U1 = u1 1;
U2 = u1 1u2u1 2u2u1u2u1 1u2 1u1u2 1u1u2 1u1 1u2u1 1u2u1u2 1u 1
Generating the small u's by the big U 's is obtained by swapping u $ U . We will henceforth
stick with the big U 's. U1 cyclically permutes all the entries of a vector while U2 twists the
rst vector by an integer amount in the direction of the second vector. The power d + 1 on
Another set of generators can be given by a simple generalization of the usual S and T
generators familiar from SL(2; Z). In this case, we simply have Sij and Tij along any pair
of directions i < j. Beware the notation: Sij is a d
d matrix for any given i; j, not the
fi; jgth element of a matrix S. Confusingly, S Transposes and T Shears! Better to think of
it as S Swaps and T Twists. So we have the elementary row switching (with a minus sign,
conventionally placed in the upper triangular part) and upper-triangular row addition (with
integer entry) transformations. To see their action more explicitly as matrix multiplication,
imagine arranging the lattice vectors row by row into a d-dimensional matrix. Then, for
example, T25 twists direction two by an integer in direction
transposes lattice vectors as V~1 !
are more diagrams contributing at this order, including the one with the four bulk-to-boundary
propagators meeting at a single interaction vertex in the interior.
twists in any direction. These include the upper-triangular Tij from the previous section
and upper-twists can also generate U1 and U2 as U1 = (S12)(S23)
(Sd 1;d) and U2 = T12.
Four-point function sample calculation
Here we calculate the tree-level contribution to the four-point function illustrated in
gure 2. We will calculate it in an AdS background where one direction has size L and another
AdS background where the same direction has size J L for J 2 Z+. We will suppress all
We rst calculate the correlator in size J L. We have
O(x4)iJL =
Fourier transforming gives
K(s1=J L)
K(s4=J L)G(s5=J L);
where i = 1; : : : ; 5. Evaluating the x5 and x6 integrals gives
s1+s2;s5 s3+s4; s5 e 2JLi (s1x1+ +s4x4)K(s1=J L)
K(s4=J L)G(s5=J L) :
X J 2L2 s1+s2+s3+s4;0e 2JLi (s1x1+ +s4x4)K(s1=JL)
K(s4=JL)G((s1+s2)=JL) ;
transform with respect to the variables xi. Recall that the discrete transforms in nite size
hO(n1=L) : : : O(n4=L)iJL =
X e 2JLi (s1x1+:::s4x4)+ 2Li (n1x1+ +n4x4)K(s1=JL)
K(s4=JL)G((s1 + s2)=JL) :
Evaluating the integrals and then the sum gives
dz5 dz6K(n1=L) : : : K(n4=L)G((n1 + n2)=L) n1+n2+n3+n4;0 :
f (x) = X e2 inx=Lf (n=L) =) f (n=L) =
dx e 2 inx=Lf (x) :
1 Z L
e 2JLi (n01(x1 x5)+ +n04(x4 x6)+n05(x5 x6))K(n01=JL)
K(n04=JL)G(n05=JL) (B.14)
Now we consider the correlator in size L, where we replace the bulk-to-bulk propagator
and the bulk-to-boundary propagators with those of size JL by the method of images:
O(x4)iL =
ni=0
x5)K(x2 + n2L
x6)K(x4 + n4L
x6)G(x5 + n5L
ni=0 n0i= 1
e 2JLi (n01(x1+n1L x5)+ +n04(x4+n4L x6)+n05(x5+n5L x6))K(n01=JL)
K(n04=JL)G(n05=JL) :
Switching the two sums and evaluating the sums over ni gives
n0i= 1
for arbitrary integer si. Evaluating the sums over n0i gives
si= 1
e 2Li (s1(x1 x5)+ +s4(x4 x6)+s5(x5 x6))K(s1=L)
K(s4=L)G(s5=L) :
s1+s2;s5 s3+s4; s5 e 2Li (s1x1+ +s4x4+s5x5)K(s1=L)
K(s4=L)G(s5=L) :
s1+s2+s3+s4;0 e 2Li (s1x1+ +s4x4)K(s1=L)
K(s4=L)G((s1 + s2)=L) :
Performing the x5 and x6 integrals gives
si= 1
Performing the sum over s5 gives
si= 1
= J L
1 Z L
hO(n1=L)
O(n4=L)iL =
dz5 dz6K(n1=L)
K(n4=L)G((n1 + n2)=L) n1+n2+n3+n4;0 : (B.20)
This is our nal answer for the correlator in size L. Comparing this answer to (B.8) gives us
hO(n1=L)
O(n4=L)iL = J 3hO(n1=L)
O(n4=L)iJL
as predicted by (4.19).
This calculation should make clear that (4.19) is correct diagram-by-diagram in the
bulk. Moreover, any bulk-to-bulk propagator with momenta that need to be integrated
over, as would be the case for loop diagrams, would ruin this structure. This is expected
since the presence of such propagators signals a subleading-in-N Witten diagram, for which
volume-independence does not apply.
Validity of gravitational description
For our gravitational description to be valid, we need to deal with smooth geometries and
keep cycle sizes larger than string scale. The rst criterion is simply because singularities
are not well-described within gravity. The second criterion is because stringy excitations
(e.g. strings that wrap the cycles) will become important for cycles that are string scale.
In this case, one needs to T-dualize along the small cycle to blow it up. The language here
is a bit confusing, as T-dualizing takes us from a valid IIB gravity description to a valid
IIA gravity description, but we are concerned with maintaining a valid gravity description
in the same frame throughout.
Maintaining validity of the gravitational description depends on the periodicity
conditions chosen for the matter elds. To be very concrete, let us consider the duality between
Type IIB string theory in AdS5
pacti ed on a spatial three-torus of cycle lengths Li. First consider the case where the
matter elds are given supersymmetry-preserving boundary conditions along the spatial
cycles. In this case the ground state geometry is given by the Poincare patch with periodic
identi cations in the spatial directions. But this means that the cycles become arbitrarily
small as the horizon is approached, necessitating a breakdown of the IIB gravity description.
This was the case analyzed in [18]. However, nite temperature is di erent and necessitates
a discussion of the order of limits taken. The Euclidean geometry is that of the black brane:
ds2 =
f (r) = r2(1 (rh=r))4;
rh, the S5 is suppressed, and tE
gives the inverse temperature. The
minimum proper size of a given cycle i occurs at rh. This size must be bigger than the
string scale `s, which gives us the condition
`s =)
Here we have brought in the 't Hooft coupling . We see that we can make Li arbitrarily
small and maintain validity of the gravitational description as long as we take
rst. In other words, we do not scale any cycle sizes with the 't Hooft coupling as we take
the strong coupling limit
The case we were more preoccupied with in the text, especially in section 3, is that of
modular U1-invariant boundary conditions. This means supersymmetry-breaking boundary
conditions along all cycles. As we saw, this implies that when a cycle size is the smallest,
it caps o in the interior. The geometry that dominates is either the black brane or the
AdS soliton, whose Euclidean continuations are identical. The condition above therefore
where L ;min is the minimum cycle size. By de nition we have L ;min < 1, so this condition
is satis ed trivially. Any time a cycle tries to become substringy, it instead caps o .
Mixed boundary conditions which preserve some subgroup of the full modular U1
invariance are analyzed similarly. The nal conclusion is that the gravitational description
will remain valid for all cycle sizes as long as at least one cycle has supersymmetry-breaking
boundary conditions and remains
nite sized in the CFT. The one caveat is that any
supersymmetry-preserving cycles are not taken to zero size as an inverse power of the 't
Hooft coupling .
This article is distributed under the terms of the Creative Commons
Attribution License (CC-BY 4.0), which permits any use, distribution and reproduction in
any medium, provided the original author(s) and source are credited.
113 (1982) 47 [INSPIRE].
Phys. B 206 (1982) 440 [INSPIRE].
theory, Phys. Rev. Lett. 48 (1982) 1063 [INSPIRE].
Phys. Lett. B 88 (1979) 135 [Erratum ibid. B 89 (1980) 437] [INSPIRE].
B 188 (1981) 269 [Sov. J. Nucl. Phys. 32 (1980) 431] [Yad. Fiz. 32 (1980) 838] [INSPIRE].
[hep-th/0608072] [INSPIRE].
B 652 (2007) 359 [hep-th/0612097] [INSPIRE].
large-N lattice gauge theory, Phys. Rev. D 27 (1983) 2397 [INSPIRE].
U(1) non-commutative gauge theory: the fate of one-loop instability, JHEP 10 (2006) 042
Eguchi-Kawai model, JHEP 01 (2008) 025 [arXiv:0711.1925] [INSPIRE].
gauge theories, Phys. Rev. D 78 (2008) 034507 [arXiv:0805.2146] [INSPIRE].
Mod. Phys. 53 (1981) 43 [INSPIRE].
JHEP 07 (2010) 043 [arXiv:1005.1981] [INSPIRE].
volume independence, Phys. Rev. D 78 (2008) 065035 [arXiv:0803.0344] [INSPIRE].
theories, JHEP 06 (2007) 019 [hep-th/0702021] [INSPIRE].
[arXiv:1210.4997] [INSPIRE].
[hep-th/0505148] [INSPIRE].
[hep-th/0506183] [INSPIRE].
(2010) 066002 [arXiv:1005.3519] [INSPIRE].
(2014) 030 [arXiv:1404.0225] [INSPIRE].
International Conference on Supersymmetry and Uni cation of Fundamental Interactions,
Karlsruhe Germany, 26 July{1 August 2007, pg. 148 [arXiv:0708.0632] [INSPIRE].
[hep-th/9803002] [INSPIRE].
[arXiv:1512.06855] [INSPIRE].
B 270 (1986) 186 [INSPIRE].
[hep-th/9712251] [INSPIRE].
sparse d > 2 conformal eld theory at large-N , arXiv:1610.06186 [INSPIRE].
Rev. D 93 (2016) 126005 [arXiv:1508.02728] [INSPIRE].
the large c limit, JHEP 09 (2014) 118 [arXiv:1405.5137] [INSPIRE].
(2015) 081 [arXiv:1504.02094] [INSPIRE].
theory, JHEP 10 (2009) 079 [arXiv:0907.0151] [INSPIRE].
[arXiv:1306.2960] [INSPIRE].
JHEP 07 (2015) 016 [arXiv:1409.1617] [INSPIRE].
JHEP 12 (1998) 005 [hep-th/9804085] [INSPIRE].
[34] J.M. Maldacena and A. Strominger, AdS3 black holes and a stringy exclusion principle,
emergence of spacetime, JHEP 01 (2015) 048 [arXiv:1406.5859] [INSPIRE].
elds, Phys. Lett. B 189 (1987) 89 [INSPIRE].
550 (2002) 213 [hep-th/0210114] [INSPIRE].
classical gravity, JHEP 09 (2013) 109 [arXiv:1306.4682] [INSPIRE].
elds, Nucl. Phys. B 291 (1987) 141 [INSPIRE].
Chern-Simons-matter theories, M 2-branes and their gravity duals, JHEP 10 (2008) 091
[arXiv:0806.1218] [INSPIRE].
[arXiv:0807.4924] [INSPIRE].
strings, J. Phys. A 46 (2013) 214009 [arXiv:1207.4485] [INSPIRE].
06 (2014) 168 [arXiv:1308.2077] [INSPIRE].
coupled to fundamental matter, JHEP 03 (2013) 097 [arXiv:1207.4195] [INSPIRE].
correspondence, Class. Quant. Grav. 34 (2017) 015009 [arXiv:1108.5735] [INSPIRE].
arXiv:1309.7413 [INSPIRE].
de Sitter space, JHEP 01 (2015) 074 [arXiv:1405.1424] [INSPIRE].
holography from functional determinants, JHEP 02 (2014) 007 [arXiv:1305.6321] [INSPIRE].
S1: a smooth journey from small to
[arXiv:0802.1232] [INSPIRE].
Rev. D 60 (1999) 046002 [hep-th/9903203] [INSPIRE].
theories, JHEP 08 (2010) 030 [arXiv:1006.2101] [INSPIRE].
[56] S. Nakamura, H. Ooguri and C.-S. Park, Gravity dual of spatially modulated phase, Phys.
[57] A. Donos and J.P. Gauntlett, Holographic striped phases, JHEP 08 (2011) 140
[arXiv:1106.2004] [INSPIRE].
[62] M. Honda and Y. Yoshida, Localization and large-N reduction on S3 for the planar and
M-theory limit, Nucl. Phys. B 865 (2012) 21 [arXiv:1203.1016] [INSPIRE].
[66] L.F. Alday, M. Fluder and J. Sparks, The large-N limit of M 2-branes on lens spaces, JHEP
correspondence, JHEP 01 (2002) 013 [hep-th/0112131] [INSPIRE].
from conformal eld theory, arXiv:1610.09378 [INSPIRE].
eld theory, Nucl. Phys. B 241 (1984) 333 [INSPIRE].
[74] Al.B. Zamolodchikov, Conformal symmetry in two-dimensional space: recursion
representation of conformal block, Theor. Math. Phys. 73 (1987) 1088 [Teor. Mat. Fiz. 73
[75] A.L. Fitzpatrick, J. Kaplan and M.T. Walters, Universality of long-distance AdS physics
from the CFT bootstrap, JHEP 08 (2014) 145 [arXiv:1403.6829] [INSPIRE].
JHEP 08 (2015) 049 [arXiv:1504.05943] [INSPIRE].
JHEP 07 (2016) 123 [arXiv:1603.04856] [INSPIRE].
equivalences of large-Nc orbifold gauge theories, JHEP 07 (2005) 008 [hep-th/0411177]
Sachdev-Ye-Kitaev models, arXiv:1609.07832 [INSPIRE].
SYK model, JHEP 01 (2017) 138 [arXiv:1610.02422] [INSPIRE].
02 (2015) 172 [arXiv:1412.5148] [INSPIRE].
string theory and gravity, Phys. Rept. 323 (2000) 183 [hep-th/9905111] [INSPIRE].
[1] T. Eguchi and H. Kawai , Reduction of dynamical degrees of freedom in the large -N gauge [2] Yu . M. Makeenko and A.A. Migdal , Exact equation for the loop average in multicolor QCD , [3] Yu . Makeenko and A.A. Migdal , Quantum chromodynamics as dynamics of loops, Nucl . Phys.
[4] G. Bhanot , U.M. Heller and H. Neuberger , The quenched Eguchi-Kawai model , Phys. Lett . B [5] D.J. Gross and Y. Kitazawa , A quenched momentum prescription for large-N theories , Nucl.
[6] A. Gonzalez-Arroyo and M. Okawa , The twisted Eguchi-Kawai model: a reduced model for [7] W. Bietenholz , J. Nishimura , Y. Susaki and J. Volkholz , A non-perturbative study of 4D [8] M. Teper and H. Vairinhos , Symmetry breaking in twisted Eguchi-Kawai models , Phys. Lett.
[9] T. Azeyanagi , M. Hanada , T. Hirata and T. Ishikawa , Phase structure of twisted [10] B. Bringoltz and S.R. Sharpe , Breakdown of large-N quenched reduction in SU(N ) lattice [11] D.J. Gross , R.D. Pisarski and L.G. Ya e, QCD and instantons at nite temperature , Rev.
[12] A. Gonzalez-Arroyo and M. Okawa , Large-N reduction with the twisted Eguchi-Kawai model , [14] P. Kovtun , M. U nsal and L.G. Ya e, Volume independence in large-Nc QCD-like gauge [15] B. Lucini and M. Panero , SU(N ) gauge theories at large-N , Phys. Rept. 526 ( 2013 ) 93 [16] K. Furuuchi , From free elds to AdS: thermal case , Phys. Rev. D 72 (2005) 066009 [17] K. Furuuchi , Large-N reductions and holography, Phys. Rev. D 74 (2006) 045027 [18] E. Poppitz and M. Unsal, AdS/CFT and large-N volume independence, Phys. Rev. D 82 [19] D. Young and K. Zarembo , Holographic dual of the Eguchi-Kawai mechanism , JHEP 06 [20] J. Greensite , An introduction to the con nement problem , Lect. Notes Phys . 821 ( 2011 ) 1 [21] A. Armoni , M. Shifman and M. Unsal, Planar limit of orientifold eld theories and emergent center symmetry , Phys. Rev. D 77 ( 2008 ) 045012 [arXiv:0712.0672] [INSPIRE].
[22] M. Shifman , Some theoretical developments in SUSY , in SUSY 2007 Proceedings , 15th [23] J.M. Maldacena , Wilson loops in large-N eld theories , Phys. Rev. Lett . 80 ( 1998 ) 4859 [24] E. Shaghoulian , Black hole microstates in AdS , Phys. Rev . D 94 ( 2016 ) 104044 [25] A. Belin , J. de Boer , J. Krutho , B. Michel , E. Shaghoulian and M. Shyani , Universality of [26] E. Shaghoulian , Modular forms and a generalized Cardy formula in higher dimensions , Phys.
[27] J.L. Cardy , Operator content of two-dimensional conformally invariant theories, Nucl . Phys.
[28] A. Strominger, Black hole entropy from near horizon microstates, JHEP 02 (1998) 009 [29] T. Hartman, C.A. Keller and B. Stoica, Universal spectrum of 2d conformal eld theory in [30] E. Shaghoulian, A Cardy formula for holographic hyperscaling-violating theories, JHEP 11 [31] I. Heemskerk, J. Penedones, J. Polchinski and J. Sully, Holography from conformal eld [32] G. Basar, A. Cherman, D. Dorigoni and M. U nsal, Volume independence in the large-N limit and an emergent fermionic symmetry, Phys. Rev. Lett. 111 (2013) 121601 [33] G. Basar, A. Cherman and D.A. McGady, Bose-Fermi degeneracies in large-N adjoint QCD, [35] R. Dijkgraaf, J.M. Maldacena, G.W. Moore and E.P. Verlinde, A black hole Farey tail, [36] E. Keski-Vakkuri, Bulk and boundary dynamics in BTZ black holes, Phys. Rev. D 59 (1999) [37] S. Ryu and T. Takayanagi, Aspects of holographic entanglement entropy, JHEP 08 (2006) [38] V. Balasubramanian, B.D. Chowdhury, B. Czech and J. de Boer, Entwinement and the [40] E.S. Fradkin and M.A. Vasiliev, Cubic interaction in extended theories of massless higher [41] E.S. Fradkin and M.A. Vasiliev, On the gravitational interaction of massless higher spin [42] M.A. Vasiliev, Higher spin gauge theories: star product and AdS space, hep-th/9910096 [43] I.R. Klebanov and A.M. Polyakov, AdS dual of the critical O(N ) vector model, Phys. Lett. B [44] O. Aharony, O. Bergman, D.L. Ja eris and J. Maldacena, N = 6 superconformal [45] O. Aharony, O. Bergman and D.L. Ja eris, Fractional M 2-branes, JHEP 11 (2008) 043 [46] C.-M. Chang, S. Minwalla, T. Sharma and X. Yin, ABJ triality: from higher spin elds to [47] S. Banerjee and D. Radicevic, Chern-Simons theory coupled to bifundamental scalars, JHEP [48] S. Banerjee, S. Hellerman, J. Maltz and S.H. Shenker, Light states in Chern-Simons theory [49] D. Anninos, T. Hartman and A. Strominger, Higher spin realization of the dS/CFT [50] C.-M. Chang, A. Pathak and A. Strominger, Non-minimal higher-spin DS4/CF T3, [51] D. Anninos, R. Mahajan, D. Radicevic and E. Shaghoulian, Chern-Simons-ghost theories and [52] D. Anninos, F. Denef, G. Konstantinidis and E. Shaghoulian, Higher spin de Sitter [53] M. Shifman and M. Unsal, QCD-like theories on R3 large r(S1) with double-trace deformations, Phys. Rev. D 78 (2008) 065004 [54] R.C. Myers, Stress tensors and Casimir energies in the AdS/CFT correspondence, Phys.
[55] M. Unsal and L.G. Ya e, Large-N volume independence in conformal and con ning gauge [58] D. Anninos , T. Anous , F. Denef and L. Peeters , Holographic vitri cation , JHEP 04 ( 2015 ) [59] R.C. Brower , G.T. Fleming and H. Neuberger , Lattice radial quantization: 3D Ising , Phys.
[60] T. Ishii , G. Ishiki , S. Shimasaki and A. Tsuchiya , N = 4 super Yang-Mills from the plane wave matrix model , Phys. Rev. D 78 ( 2008 ) 106001 [arXiv:0807.2352] [INSPIRE].
[61] H. Kawai , S. Shimasaki and A. Tsuchiya , Large-N reduction on group manifolds, Int . J.
[63] R. Clarkson and R.B. Mann , Eguchi-Hanson solitons in odd dimensions, Class. Quant. Grav.
[64] R. Clarkson and R.B. Mann , Soliton solutions to the Einstein equations in ve dimensions , [65] Y. Hikida , Phase transitions of large-N orbifold gauge theories , JHEP 12 ( 2006 ) 042 [68] H. Lin and J.M. Maldacena , Fivebranes from gauge theory , Phys. Rev. D 74 (2006) 084014 [69] G. Ishiki , S. Shimasaki , Y. Takayama and A. Tsuchiya , Embedding of theories with SU(2j4) symmetry into the plane wave matrix model , JHEP 11 ( 2006 ) 089 [hep-th /0610038] [70] E. Witten , Anti-de Sitter space, thermal phase transition and con nement in gauge theories, Adv . Theor. Math. Phys. 2 ( 1998 ) 505 [hep-th /9803131] [INSPIRE].
[71] O. Aharony , S. Minwalla and T. Wiseman , Plasma-balls in large-N gauge theories and localized black holes , Class. Quant. Grav . 23 ( 2006 ) 2171 [hep-th /0507219] [INSPIRE].
[72] N. Afkhami-Jeddi , T. Hartman , S. Kundu and A. Tajdini , Einstein gravity 3-point functions [73] A.A. Belavin , A.M. Polyakov and A.B. Zamolodchikov , In nite conformal symmetry in [76] E. Hijano , P. Kraus and R. Snively , Worldline approach to semi-classical conformal blocks , [77] E. Hijano , P. Kraus , E. Perlmutter and R. Snively , Witten diagrams revisited: the AdS geometry of conformal blocks , JHEP 01 ( 2016 ) 146 [arXiv:1508.00501] [INSPIRE].
[78] E. Hijano , P. Kraus , E. Perlmutter and R. Snively , Semiclassical Virasoro blocks from AdS3 gravity , JHEP 12 ( 2015 ) 077 [arXiv:1508.04987] [INSPIRE].
[79] K.B. Alkalaev and V.A. Belavin , Classical conformal blocks via AdS/CFT correspondence, [80] C.T. Asplund , A. Bernamonti , F. Galli and T. Hartman , Holographic entanglement entropy from 2d CFT: heavy states and local quenches , JHEP 02 ( 2015 ) 171 [arXiv:1410.1392] [81] P. Caputa , J. Simon , A. Stikonas and T. Takayanagi , Quantum entanglement of localized excited states at nite temperature , JHEP 01 ( 2015 ) 102 [arXiv:1410.2287] [INSPIRE].
[82] T. Anous , T. Hartman , A. Rovai and J. Sonner , Black hole collapse in the 1=c expansion , [83] J. Maldacena , D. Simmons-Du n and A. Zhiboedov , Looking for a bulk point , JHEP 01 [84] A. Cherman and D. Dorigoni , Large-N and bosonization in three dimensions , JHEP 10 [85] D.J. Gross and V. Rosenhaus , A generalization of Sachdev-Ye-Kitaev , JHEP 02 ( 2017 ) 093 [86] P. Kovtun , M. Unsal and L.G. Ya e, Nonperturbative equivalences among large-Nc gauge theories with adjoint and bifundamental matter elds , JHEP 12 ( 2003 ) 034 [87] P. Kovtun , M. Unsal and L.G. Ya e, Necessary and su cient conditions for non-perturbative [88] Y. Gu , X.-L. Qi and D. Stanford , Local criticality, di usion and chaos in generalized [89] M. Berkooz , P. Narayan , M. Rozali and J. Simon , Higher dimensional generalizations of the [90] D. Gaiotto , A. Kapustin , N. Seiberg and B. Willett , Generalized global symmetries , JHEP [91] V. Balasubramanian , P. Kraus and M. Shigemori , Massless black holes and black rings as e ective geometries of the D1-D5 system , Class. Quant. Grav. 22 ( 2005 ) 4803 [92] O. Aharony , S.S. Gubser , J.M. Maldacena , H. Ooguri and Y. Oz , Large-N [93] D. Birmingham , I. Sachs and S.N. Solodukhin , Relaxation in conformal eld theory, Hawking-Page transition and quasinormal normal modes , Phys. Rev. D 67 (2003) 104026