CoChat
Sign Up
Cited by 43

The DOI matches its Crossref record; 16 of the 16 references it cites were found in a registry or an index.

Cosmology from random entanglement

Antonini, Stefano, Sasieta, Martin, Swingle, Brian·2023·Journal of High Energy Physics
DOI 10.1007/jhep11(2023)188
Open this paper in CoChat — free account

Abstract

A bstract: We construct entangled microstates of a pair of holographic CFTs whose dual semiclassical description includes big bang-big crunch AdS cosmologies in spaces without boundaries. The cosmology is supported by inhomogeneous heavy matter and it partially purifies the bulk entanglement of two disconnected auxiliary AdS spacetimes. We show that the island formula for the fine grained entropy of one of the CFTs follows from a standard gravitational replica trick calculation. In generic settings, the cosmology is contained in the entanglement wedge of one of the two CFTs. We then investigate properties of the cosmology-to-boundary encoding map, and in particular, its non-isometric character. Restricting our attention to a specific class of states on the cosmology, we provide an explicit, and state-dependent, boundary representation of operators acting on the cosmology. Finally, under genericity assumptions, we argue for a non-isometric to approximately-isometric transition of the cosmology-to-boundary map for “simple” states on the cosmology as a function of the bulk entanglement, with tensor network toy models of our setup as a guide.

Overview

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Integrity signals

Registry

Crossref · 10.1007/jhep11(2023)188

Cites

16 of 16 references verified0 citation errors · 0 not checkable

Statistics

Figures

Figure 1 Semiclassical state prepared by the gravitational path integral at low preparation temperatures. The geometry of the Euclidean section X consists of two thermal AdS spaces. Each space has topology D d ˆ S 1 , where D d is a d -dimensional ball, and S 1 is the additional non-contractible thermal circle. The two solutions are glued together along the trajectory of the thin shell (red line). The Euclidean manifold X is homotopic to a pair of pants. The semiclassical state is prepared on the time reflection-symmetric slice Σ (blue slice), which contains the initial data of two global AdS timeslices Σ l and Σ r , and a third closed universe Σ c supported by the thin shell. In the Loretzian section, obtained from analytic continuation along Σ , the universe crunches towards the future.
Figure 1 Semiclassical state prepared by the gravitational path integral at low preparation temperatures. The geometry of the Euclidean section X consists of two thermal AdS spaces. Each space has topology D d ˆ S 1 , where D d is a d -dimensional ball, and S 1 is the additional non-contractible thermal circle. The two solutions are glued together along the trajectory of the thin shell (red line). The Euclidean manifold X is homotopic to a pair of pants. The semiclassical state is prepared on the time reflection-symmetric slice Σ (blue slice), which contains the initial data of two global AdS timeslices Σ l and Σ r , and a third closed universe Σ c supported by the thin shell. In the Loretzian section, obtained from analytic continuation along Σ , the universe crunches towards the future.CC-BY · From the PDF
Figure 2 Schematic representation of the semiclassical state. The lines connecting the cosmology to the left and right AdS spacetimes represent entanglement between bulk fields. The green line cutting the entanglement lines represents the dominant RT surface for the whole CFT L , which is geometrically empty. The cosmology c is contained within the entanglement wedge of CFT L .
Figure 2 Schematic representation of the semiclassical state. The lines connecting the cosmology to the left and right AdS spacetimes represent entanglement between bulk fields. The green line cutting the entanglement lines represents the dominant RT surface for the whole CFT L , which is geometrically empty. The cosmology c is contained within the entanglement wedge of CFT L .CC-BY · From the PDF
Figure 3 TN model of our setup defining the cosmology-to-boundary map V ψ .
Figure 3 TN model of our setup defining the cosmology-to-boundary map V ψ .CC-BY · From the PDF
Figure 4 Euclidean path integral on the flat cylinder preparing | Ψ O y .
Figure 4 Euclidean path integral on the flat cylinder preparing | Ψ O y .CC-BY · From the PDF
Figure 5 Semiclassical state prepared by the gravitational path integral at high preparation temperatures. The Euclidean section X consists of two Euclidean black holes of masses M L and M R . Each solution is topologically D 2 ˆ S d ´ 1 , where D 2 is a two dimensional disk (each point in the figure corresponds to a transverse S d ´ 1 ). The two solutions are glued together along the worldvolume of the thin shell W , in red. The semiclassical bulk state is prepared at the time reflection-symmetric slice Σ (blue slice), which contains a long Einstein-Rosen bridge supported by the shell. In the Lorentzian section, the shell hides behind the horizon of the two-sided black hole.
Figure 5 Semiclassical state prepared by the gravitational path integral at high preparation temperatures. The Euclidean section X consists of two Euclidean black holes of masses M L and M R . Each solution is topologically D 2 ˆ S d ´ 1 , where D 2 is a two dimensional disk (each point in the figure corresponds to a transverse S d ´ 1 ). The two solutions are glued together along the worldvolume of the thin shell W , in red. The semiclassical bulk state is prepared at the time reflection-symmetric slice Σ (blue slice), which contains a long Einstein-Rosen bridge supported by the shell. In the Lorentzian section, the shell hides behind the horizon of the two-sided black hole.CC-BY · From the PDF
Figure 6 Half of the Euclidean manifold X in the limit of large mass for the thin shell operator. In this illustration, the trajectory of the shell pinches off to the asymptotic region, ∆ τ ˘ Ñ 0 , and the physical preparation time becomes β L , R ' ˜ β L , R . The slice Σ c Ă Σ corresponds to the initial data of a very large closed universe.
Figure 6 Half of the Euclidean manifold X in the limit of large mass for the thin shell operator. In this illustration, the trajectory of the shell pinches off to the asymptotic region, ∆ τ ˘ Ñ 0 , and the physical preparation time becomes β L , R ' ˜ β L , R . The slice Σ c Ă Σ corresponds to the initial data of a very large closed universe.CC-BY · From the PDF
Figure 7 Each one of the locally AdS patches c l and c r (shaded in red) is bounded by the collapsing shell (red solid line) and contained within the t ' 0 Wheeler-DeWitt patch (bounded by the solid blue line) in the corresponding pure AdS spacetime without cutoff. The gray lines represent constant t c slices in the hyperbolic foliation described by the metric (2.24). In our setup, each slice is cut off when it intersects the shell and glued to an analogous slice of the other cosmological component. A curvature singularity arises at the tips of the shell's trajectory. In this figure we represent the full Lorentzian geometry obtained by evolving the initial state for c l or c r at t ' 0 backwards and forward in time.
Figure 7 Each one of the locally AdS patches c l and c r (shaded in red) is bounded by the collapsing shell (red solid line) and contained within the t ' 0 Wheeler-DeWitt patch (bounded by the solid blue line) in the corresponding pure AdS spacetime without cutoff. The gray lines represent constant t c slices in the hyperbolic foliation described by the metric (2.24). In our setup, each slice is cut off when it intersects the shell and glued to an analogous slice of the other cosmological component. A curvature singularity arises at the tips of the shell's trajectory. In this figure we represent the full Lorentzian geometry obtained by evolving the initial state for c l or c r at t ' 0 backwards and forward in time.CC-BY · From the PDF
Figure 8 Global AdS time elapsed during the shell's trajectory from r ' R ˚ to r ' 0 as a function of the shell's mass m for d ' 3 . We set here ℓ ' 1 , so the x axis is measured in units of the AdS radius. t f ă πℓ { 2 for all values of m , and t f Ñ πℓ { 2 in the large m limit: the shell is always contained within the t ' 0 Wheeler-DeWitt patch.
Figure 8 Global AdS time elapsed during the shell's trajectory from r ' R ˚ to r ' 0 as a function of the shell's mass m for d ' 3 . We set here ℓ ' 1 , so the x axis is measured in units of the AdS radius. t f ă πℓ { 2 for all values of m , and t f Ñ πℓ { 2 in the large m limit: the shell is always contained within the t ' 0 Wheeler-DeWitt patch.CC-BY · From the PDF
Figure 9 Preparation of the excited state | ψ y from local operator insertions along X . The radial slices correspond to constant Euclidean time slices, evolved with the action of the time-independent Hamiltonians H l , r b . Note that here and in all the following figures, we add probe operator insertions in the bulk manifold X that do not backreact on the geometry. These local operators are inserted at different points on the S d ´ 1 (which is suppressed in the figures).
Figure 9 Preparation of the excited state | ψ y from local operator insertions along X . The radial slices correspond to constant Euclidean time slices, evolved with the action of the time-independent Hamiltonians H l , r b . Note that here and in all the following figures, we add probe operator insertions in the bulk manifold X that do not backreact on the geometry. These local operators are inserted at different points on the S d ´ 1 (which is suppressed in the figures).CC-BY · From the PDF
Figure 10 Euclidean CFT path integral computing the unnormalized purity Tr p ˆ ρ 2 L q . Each point represents a spatial sphere S d ´ 1 . The two replicas are glued together across the dashed axis of Z 2 symmetry, which cuts the Hilbert space of the L subsystems.
Figure 10 Euclidean CFT path integral computing the unnormalized purity Tr p ˆ ρ 2 L q . Each point represents a spatial sphere S d ´ 1 . The two replicas are glued together across the dashed axis of Z 2 symmetry, which cuts the Hilbert space of the L subsystems.CC-BY · From the PDF
Figure 11 The saddle point geometry X e consist of thin shell contractions between each replica. The center of replica symmetry corresponds to an AdS space of physical inverse temperature β L , 2 ' 2 ˜ β L ` 2∆ τ ` . Here and in all the following figures we consider generic saddles in which additional operator insertions ϕ I are present (represented by the crosses), see Sec. 2.2.
Figure 11 The saddle point geometry X e consist of thin shell contractions between each replica. The center of replica symmetry corresponds to an AdS space of physical inverse temperature β L , 2 ' 2 ˜ β L ` 2∆ τ ` . Here and in all the following figures we consider generic saddles in which additional operator insertions ϕ I are present (represented by the crosses), see Sec. 2.2.CC-BY · From the PDF
Figure 12 The replica wormhole X η consist of thin shell contractions between replicas. The center of replica symmetry corresponds to an AdS space of temperature β R , 2 ' 2 ˜ β R ` 2∆ τ ` . On the right, the large mass limit of the shell, where the geometry becomes effectively composed of disconnected Euclidean AdS spaces, with β R , 2 ' 2 β R . Each of these spaces contributes with a factor of Z l p kβ L q or Z r p kβ R q .
Figure 12 The replica wormhole X η consist of thin shell contractions between replicas. The center of replica symmetry corresponds to an AdS space of temperature β R , 2 ' 2 ˜ β R ` 2∆ τ ` . On the right, the large mass limit of the shell, where the geometry becomes effectively composed of disconnected Euclidean AdS spaces, with β R , 2 ' 2 β R . Each of these spaces contributes with a factor of Z l p kβ L q or Z r p kβ R q .CC-BY · From the PDF
Figure 13 The Euclidean wormhole X 2 contributing to the square of the norm of the state. In the space transverse to the spheres, X 2 is homotopic to a sphere with four punctures. The asymptotic boundary B X 2 contains two disconnected components, corresponding to Euclidean CFT path integrals computing the normalization Z 1 . The wormhole is deconstructed in a pair of thermal AdS spaces at inverse temperatures β R , 2 ' 2 β R ` 2∆ τ ` and β L , 2 ' 2 β L ` 2∆ τ ` , glued along the trajectories of two thin shells.
Figure 13 The Euclidean wormhole X 2 contributing to the square of the norm of the state. In the space transverse to the spheres, X 2 is homotopic to a sphere with four punctures. The asymptotic boundary B X 2 contains two disconnected components, corresponding to Euclidean CFT path integrals computing the normalization Z 1 . The wormhole is deconstructed in a pair of thermal AdS spaces at inverse temperatures β R , 2 ' 2 β R ` 2∆ τ ` and β L , 2 ' 2 β L ` 2∆ τ ` , glued along the trajectories of two thin shells.CC-BY · From the PDF
Figure 14 The operator insertions with propagate into X in the probe worldline approximation. There are three types of insertions, depending on the Euclidean time τ i of the corresponding operator insertion: type I creates a particle on c , type II creates a linear superposition of a particle on c and a particle on l or r , and type III creates a particle on l or r .
Figure 14 The operator insertions with propagate into X in the probe worldline approximation. There are three types of insertions, depending on the Euclidean time τ i of the corresponding operator insertion: type I creates a particle on c , type II creates a linear superposition of a particle on c and a particle on l or r , and type III creates a particle on l or r .CC-BY · From the PDF
Figure 15 The overlap G ij ' g ij , computed gravitationally by the overlap between two bulk states with two different particles, vanishes from the orthogonality of the bulk overlaps between the state of the particle i I and the particle j I .
Figure 15 The overlap G ij ' g ij , computed gravitationally by the overlap between two bulk states with two different particles, vanishes from the orthogonality of the bulk overlaps between the state of the particle i I and the particle j I .CC-BY · From the PDF
Figure 16 Euclidean wormhole geometry X 2 contributing semiclassically to the second moment of the overlap | G ij | 2 in eq. (4.12). It consists of two Euclidean AdS spaces, glued by the trajectories of two thin shells, where the shells on the left and right are identified. Each of the two states | Ψ I i y , ∣ ∣ Ψ I j D contains a different type I and a type III insertion (additional type II insertions that prepare the reference state have been omitted). The type I and type III operator insertions correspond to different primaries, even if they are labeled by the same i and j , which corresponds to the label of the bra and the ket in the overlap.
Figure 16 Euclidean wormhole geometry X 2 contributing semiclassically to the second moment of the overlap | G ij | 2 in eq. (4.12). It consists of two Euclidean AdS spaces, glued by the trajectories of two thin shells, where the shells on the left and right are identified. Each of the two states | Ψ I i y , ∣ ∣ Ψ I j D contains a different type I and a type III insertion (additional type II insertions that prepare the reference state have been omitted). The type I and type III operator insertions correspond to different primaries, even if they are labeled by the same i and j , which corresponds to the label of the bra and the ket in the overlap.CC-BY · From the PDF
Figure 17 Saddle point geometry X contributing to the semiclassical normalization of the CFT state | Ψ I i y , Z I i ' z I i . The state contains a type I insertion on the left, and a type III insertion on the right (additional type II insertions that prepare the reference state have been omitted). The Euclidean time elapsed by type I geodesics is identical to that one elapsed in the wormhole geometry X 2 in Fig. 16. Contrarily, the Euclidean time elapsed by type III geodesics is smaller than that one elapsed in the wormhole geometry X 2 in Fig. 16. In this case, both Euclidean times are related by 2 τ i,X 2 ˚ ' 2 ´ β R 2 ´ τ i,X ˚ ¯ in the large shell's mass limit. This discrepancy causes the type III overlaps to be suppressed.
Figure 17 Saddle point geometry X contributing to the semiclassical normalization of the CFT state | Ψ I i y , Z I i ' z I i . The state contains a type I insertion on the left, and a type III insertion on the right (additional type II insertions that prepare the reference state have been omitted). The Euclidean time elapsed by type I geodesics is identical to that one elapsed in the wormhole geometry X 2 in Fig. 16. Contrarily, the Euclidean time elapsed by type III geodesics is smaller than that one elapsed in the wormhole geometry X 2 in Fig. 16. In this case, both Euclidean times are related by 2 τ i,X 2 ˚ ' 2 ´ β R 2 ´ τ i,X ˚ ¯ in the large shell's mass limit. This discrepancy causes the type III overlaps to be suppressed.CC-BY · From the PDF
Figure 18 Suppression factor α given by eq. (4.16) as a function of the Euclidean time difference between the insertion point of the operators and the time reflection-symmetric slice, where we set for simplicity τ i,X ˚ ' τ j,X ˚ ' τ ˚ . We chose ℓ ' 1 , β R ' 1 , m i ' 50 , m j ' 40 in eq. (4.16). Insertions to the right of the dashed red line at τ ˚ ' β 4 ´ ϵ with ϵ ' 1 { m j « 1 { ∆ j are type II and therefore are not relevant for our analysis. For all relevant values of the insertion point τ ˚ P p 0 , β R 4 ´ ϵ q , the suppression factor is very small and drops rapidly as we decrease τ ˚ (see the inset). This implies that the overlap computed by the gravitational Euclidean path integral for CFT states corresponding to (orthogonal) bulk EFT states with different particles in the AdS regions is very small. In this case, the bulk-to-boundary map is expected to be isometric.
Figure 18 Suppression factor α given by eq. (4.16) as a function of the Euclidean time difference between the insertion point of the operators and the time reflection-symmetric slice, where we set for simplicity τ i,X ˚ ' τ j,X ˚ ' τ ˚ . We chose ℓ ' 1 , β R ' 1 , m i ' 50 , m j ' 40 in eq. (4.16). Insertions to the right of the dashed red line at τ ˚ ' β 4 ´ ϵ with ϵ ' 1 { m j « 1 { ∆ j are type II and therefore are not relevant for our analysis. For all relevant values of the insertion point τ ˚ P p 0 , β R 4 ´ ϵ q , the suppression factor is very small and drops rapidly as we decrease τ ˚ (see the inset). This implies that the overlap computed by the gravitational Euclidean path integral for CFT states corresponding to (orthogonal) bulk EFT states with different particles in the AdS regions is very small. In this case, the bulk-to-boundary map is expected to be isometric.CC-BY · From the PDF
Image 19
CC-BY · From the PDF
Figure 20 Left: unnormalized purity Tr p ˆ ρ 2 L q for the TN state before gaussian average. Note that the contracted isometries on the left and right sides of the figure yield identities. Right: 'replica wormhole' contribution to the average unnormalized purity, where the non-trivial Wick contraction of the random operator (depicted here by dashed red lines) amounts for the shell's propagation between different replicas. The outer isometries I l and I r do not play a role in this computation.
Figure 20 Left: unnormalized purity Tr p ˆ ρ 2 L q for the TN state before gaussian average. Note that the contracted isometries on the left and right sides of the figure yield identities. Right: 'replica wormhole' contribution to the average unnormalized purity, where the non-trivial Wick contraction of the random operator (depicted here by dashed red lines) amounts for the shell's propagation between different replicas. The outer isometries I l and I r do not play a role in this computation.CC-BY · From the PDF
Figure 21 TN for the cosmology-to-boundary map V ψ . | ψ i y P H ψ is a state on all bulk DOF in the class of our interest. Here we only represented the DOF | l | , | r | of the AdS regions which are entangled with the cosmology, omitting the unentangled ones.
Figure 21 TN for the cosmology-to-boundary map V ψ . | ψ i y P H ψ is a state on all bulk DOF in the class of our interest. Here we only represented the DOF | l | , | r | of the AdS regions which are entangled with the cosmology, omitting the unentangled ones.CC-BY · From the PDF
Figure 22 Upper bound for the probability of non-isometric encoding-given by the minimum between 1 and the righthand side of eq. (5.26) with C given by eq. (5.28)-as a function of the entanglement S l ` S r between cosmology and AdS regions. We chose here d ' 3 , k ' 5 , γ ' 0 . 25 , | c | ' 1000 . For S l ` S r ' O p log 2 log 2 | c |q a sharp non-isometric to approximately-isometric transition takes place. In particular, with the parameters of our choice the right hand side of eq. (5.30) is ' 16 . 6 .
Figure 22 Upper bound for the probability of non-isometric encoding-given by the minimum between 1 and the righthand side of eq. (5.26) with C given by eq. (5.28)-as a function of the entanglement S l ` S r between cosmology and AdS regions. We chose here d ' 3 , k ' 5 , γ ' 0 . 25 , | c | ' 1000 . For S l ` S r ' O p log 2 log 2 | c |q a sharp non-isometric to approximately-isometric transition takes place. In particular, with the parameters of our choice the right hand side of eq. (5.30) is ' 16 . 6 .CC-BY · From the PDF
Figure 23 In the symmetric case ˜ β L ' ˜ β R ' ˜ β in AdS 5 ( d ' 4 ), the exchange in dominance between the Euclidean black hole saddle X BH | BH and the Euclidean AdS saddle X AdS | AdS occurs at the inverse preparation temperature ˜ β « 0 . 70 β HP « 1 . 47 ℓ for a shell of mass m ' ℓ 2 { G , where β HP « 2 πℓ { 3 .
Figure 23 In the symmetric case ˜ β L ' ˜ β R ' ˜ β in AdS 5 ( d ' 4 ), the exchange in dominance between the Euclidean black hole saddle X BH | BH and the Euclidean AdS saddle X AdS | AdS occurs at the inverse preparation temperature ˜ β « 0 . 70 β HP « 1 . 47 ℓ for a shell of mass m ' ℓ 2 { G , where β HP « 2 πℓ { 3 .CC-BY · From the PDF

Verification

Claims the paper makes

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Claims other papers make about this one

Each is checked against this paper’s own text: does it say what the citing paper says it does?

Self-check

Percentages, sums and reported differences re-computed from the paper’s own numbers.

The self-check needs the paper’s full text.

Citations

Cites

Show all 16 references

Research works printed but not linked: 90

  1. G. ’t Hooft, Dimensional reduction in quantum gravity, Conf. Proc. C 930308 (1993) 284 [gr-qc/9310026] [INSPIRE]. · arXiv
  2. L. Susskind, The world as a hologram, J. Math. Phys. 36 (1995) 6377 [hep-th/9409089] [INSPIRE]. · DOI · Paper page
  3. J.M. Maldacena, The large N limit of superconformal field theories and supergravity, Adv. Theor. Math. Phys. 2 (1998) 231 [hep-th/9711200] [INSPIRE]. · DOI · Paper page
  4. S. Ryu and T. Takayanagi, Aspects of Holographic Entanglement Entropy, JHEP 08 (2006) 045 [hep-th/0605073] [INSPIRE]. · DOI · Paper page
  5. B. Swingle, Entanglement Renormalization and Holography, Phys. Rev. D 86 (2012) 065007 [arXiv:0905.1317] [INSPIRE]. · DOI · Paper page
  6. M. Van Raamsdonk, Building up spacetime with quantum entanglement, Gen. Rel. Grav. 42 (2010) 2323 [arXiv:1005.3035] [INSPIRE]. · DOI · Paper page
  7. A. Lewkowycz and J. Maldacena, Generalized gravitational entropy, JHEP 08 (2013) 090 [arXiv:1304.4926] [INSPIRE]. · DOI · Paper page
  8. T. Faulkner, A. Lewkowycz and J. Maldacena, Quantum corrections to holographic entanglement entropy, JHEP 11 (2013) 074 [arXiv:1307.2892] [INSPIRE]. · DOI · Paper page
  9. D. Stanford and L. Susskind, Complexity and Shock Wave Geometries, Phys. Rev. D 90 (2014) 126007 [arXiv:1406.2678] [INSPIRE]. · DOI
  10. J. Maldacena, S.H. Shenker and D. Stanford, A bound on chaos, JHEP 08 (2016) 106 [arXiv:1503.01409] [INSPIRE]. · DOI
  11. F. Pastawski, B. Yoshida, D. Harlow and J. Preskill, Holographic quantum error-correcting codes: Toy models for the bulk/boundary correspondence, JHEP 06 (2015) 149 [arXiv:1503.06237] [INSPIRE]. · DOI · Paper page
  12. A.R. Brown et al., Holographic Complexity Equals Bulk Action?, Phys. Rev. Lett. 116 (2016) 191301 [arXiv:1509.07876] [INSPIRE]. · DOI
  13. P. Hayden et al., Holographic duality from random tensor networks, JHEP 11 (2016) 009 [arXiv:1601.01694] [INSPIRE]. · DOI · Paper page
  14. A. Almheiri, N. Engelhardt, D. Marolf and H. Maxfield, The entropy of bulk quantum fields and the entanglement wedge of an evaporating black hole, JHEP 12 (2019) 063 [arXiv:1905.08762] [INSPIRE]. · DOI · Paper page
  15. J.B. Hartle, S.W. Hawking and T. Hertog, Accelerated Expansion from Negative Λ, arXiv:1205.3807 [INSPIRE]. · arXiv
  16. P.J.E. Peebles and B. Ratra, Cosmology with a Time Variable Cosmological Constant, Astrophys. J. Lett. 325 (1988) L17 [INSPIRE]. · DOI · Paper page
  17. B. Ratra and P.J.E. Peebles, Cosmological Consequences of a Rolling Homogeneous Scalar Field, Phys. Rev. D 37 (1988) 3406 [INSPIRE]. · DOI · Paper page
  18. S. Tsujikawa, Quintessence: A Review, Class. Quant. Grav. 30 (2013) 214003 [arXiv:1304.1961] [INSPIRE]. · DOI
  19. S. Antonini, P. Simidzija, B. Swingle and M. Van Raamsdonk, Accelerating Cosmology from a Holographic Wormhole, Phys. Rev. Lett. 130 (2023) 221601 [arXiv:2206.14821] [INSPIRE]. · DOI
  20. S. Antonini et al., Accelerating cosmology from Λ < 0 gravitational effective field theory, JHEP 05 (2023) 203 [arXiv:2212.00050] [INSPIRE]. · DOI
  21. M. Van Raamsdonk and C. Waddell, Possible hints of decreasing dark energy from supernova data, arXiv:2305.04946 [INSPIRE]. · arXiv
  22. A. Strominger, The dS / CFT correspondence, JHEP 10 (2001) 034 [hep-th/0106113] [INSPIRE]. · DOI
  23. M. Alishahiha, A. Karch, E. Silverstein and D. Tong, The dS/dS correspondence, AIP Conf. Proc. 743 (2004) 393 [hep-th/0407125] [INSPIRE]. · DOI
  24. X. Dong, E. Silverstein and G. Torroba, De Sitter Holography and Entanglement Entropy, JHEP 07 (2018) 050 [arXiv:1804.08623] [INSPIRE]. · DOI · Paper page
  25. V. Gorbenko, E. Silverstein and G. Torroba, dS/dS and $$ T\overline{T} $$, JHEP 03 (2019) 085 [arXiv:1811.07965] [INSPIRE]. · DOI
  26. E. Coleman et al., De Sitter microstates from $$ T\overline{T} $$ + Λ2 and the Hawking-Page transition, JHEP 07 (2022) 140 [arXiv:2110.14670] [INSPIRE]. · DOI
  27. L. Susskind, Black Holes Hint towards De Sitter Matrix Theory, Universe 9 (2023) 368 [arXiv:2109.01322] [INSPIRE]. · DOI
  28. L. Susskind, De Sitter Holography: Fluctuations, Anomalous Symmetry, and Wormholes, Universe 7 (2021) 464 [arXiv:2106.03964] [INSPIRE]. · DOI
  29. L. Susskind, Entanglement and Chaos in De Sitter Space Holography: An SYK Example, JHAP 1 (2021) 1 [arXiv:2109.14104] [INSPIRE]. · arXiv
  30. E. Shaghoulian and L. Susskind, Entanglement in De Sitter space, JHEP 08 (2022) 198 [arXiv:2201.03603] [INSPIRE]. · DOI
  31. P. McFadden and K. Skenderis, Holography for Cosmology, Phys. Rev. D 81 (2010) 021301 [arXiv:0907.5542] [INSPIRE]. · DOI
  32. N. Afshordi, E. Gould and K. Skenderis, Constraining holographic cosmology using Planck data, Phys. Rev. D 95 (2017) 123505 [arXiv:1703.05385] [INSPIRE]. · DOI
  33. H. Nastase, Solution of the cosmological constant problem within holographic cosmology, Phys. Lett. B 801 (2020) 135168 [arXiv:1812.07597] [INSPIRE]. · DOI
  34. H. Nastase and K. Skenderis, Holography for the very early Universe and the classic puzzles of Hot Big Bang cosmology, Phys. Rev. D 101 (2020) 021901 [arXiv:1904.05821] [INSPIRE]. · DOI
  35. J.M. Maldacena and L. Maoz, Wormholes in AdS, JHEP 02 (2004) 053 [hep-th/0401024] [INSPIRE]. · DOI · Paper page
  36. B. McInnes, Answering a basic objection to bang/crunch holography, JHEP 10 (2004) 018 [hep-th/0407189] [INSPIRE]. · DOI
  37. B. McInnes, Pre-inflationary spacetime in string cosmology, Nucl. Phys. B 748 (2006) 309 [hep-th/0511227] [INSPIRE]. · DOI
  38. B. Freivogel et al., Inflation in AdS/CFT, JHEP 03 (2006) 007 [hep-th/0510046] [INSPIRE]. · DOI
  39. N. Engelhardt, T. Hertog and G.T. Horowitz, Holographic Signatures of Cosmological Singularities, Phys. Rev. Lett. 113 (2014) 121602 [arXiv:1404.2309] [INSPIRE]. · DOI
  40. S. Cooper et al., Black hole microstate cosmology, JHEP 07 (2019) 065 [arXiv:1810.10601] [INSPIRE]. · DOI
  41. S. Antonini and B. Swingle, Cosmology at the end of the world, Nature Phys. 16 (2020) 881 [arXiv:1907.06667] [INSPIRE]. · DOI
  42. Y. Chen, V. Gorbenko and J. Maldacena, Bra-ket wormholes in gravitationally prepared states, JHEP 02 (2021) 009 [arXiv:2007.16091] [INSPIRE]. · DOI
  43. M. Van Raamsdonk, Comments on wormholes, ensembles, and cosmology, JHEP 12 (2021) 156 [arXiv:2008.02259] [INSPIRE]. · DOI
  44. M. Van Raamsdonk, Cosmology from confinement?, JHEP 03 (2022) 039 [arXiv:2102.05057] [INSPIRE]. · DOI
  45. S. Antonini, P. Simidzija, B. Swingle and M. Van Raamsdonk, Cosmology from the vacuum, arXiv:2203.11220 [INSPIRE]. · arXiv
  46. S. Fallows and S.F. Ross, Constraints on cosmologies inside black holes, JHEP 05 (2022) 094 [arXiv:2203.02523] [INSPIRE]. · DOI
  47. S.F. Ross, Cosmologies inside hyperbolic black holes, JHEP 11 (2022) 168 [arXiv:2209.11620] [INSPIRE]. · DOI
  48. A. Sahu, P. Simidzija and M. Van Raamsdonk, Bubbles of cosmology in AdS/CFT, JHEP 11 (2023) 010 [arXiv:2306.13143] [INSPIRE]. · DOI
  49. C. Akers, T. Faulkner, S. Lin and P. Rath, The page curve for reflected entropy, JHEP 06 (2022) 089 [arXiv:2201.11730] [INSPIRE]. · DOI
  50. T. Hartman, Y. Jiang and E. Shaghoulian, Islands in cosmology, JHEP 11 (2020) 111 [arXiv:2008.01022] [INSPIRE]. · DOI
  51. V. Balasubramanian, A. Kar and T. Ugajin, Islands in de Sitter space, JHEP 02 (2021) 072 [arXiv:2008.05275] [INSPIRE]. · DOI
  52. V. Balasubramanian, A. Kar and T. Ugajin, Entanglement between two disjoint universes, JHEP 02 (2021) 136 [arXiv:2008.05274] [INSPIRE]. · DOI
  53. V. Balasubramanian, A. Kar and T. Ugajin, Entanglement between two gravitating universes, Class. Quant. Grav. 39 (2022) 174001 [arXiv:2104.13383] [INSPIRE]. · DOI
  54. R. Bousso and E. Wildenhain, Islands in closed and open universes, Phys. Rev. D 105 (2022) 086012 [arXiv:2202.05278] [INSPIRE]. · DOI
  55. N. Engelhardt, G. Penington and A. Shahbazi-Moghaddam, A world without pythons would be so simple, Class. Quant. Grav. 38 (2021) 234001 [arXiv:2102.07774] [INSPIRE]. · DOI · Paper page
  56. N. Engelhardt, G. Penington and A. Shahbazi-Moghaddam, Finding pythons in unexpected places, Class. Quant. Grav. 39 (2022) 094002 [arXiv:2105.09316] [INSPIRE]. · DOI
  57. C. Akers et al., The black hole interior from non-isometric codes and complexity, arXiv:2207.06536 [INSPIRE]. · arXiv
  58. C.J. Cao, W. Chemissany, A. Jahn and Z. Zimborás, Overlapping qubits from non-isometric maps and de Sitter tensor networks, arXiv:2304.02673 [INSPIRE]. · arXiv
  59. V. Balasubramanian, A. Lawrence, J.M. Magan and M. Sasieta, Microscopic origin of the entropy of black holes in general relativity, arXiv:2212.02447 [INSPIRE]. · arXiv
  60. M. Sasieta, Wormholes from heavy operator statistics in AdS/CFT, JHEP 03 (2023) 158 [arXiv:2211.11794] [INSPIRE]. · DOI · Paper page
  61. J.A. Wheeler, Geometrodynamics and the issue of final state, in the proceedings of the Les Houches Summer Shcool of Theoretical Physics: Relativity, Groups and Topology, Les Houches, France, July 1 – 24 August (1963), p. 317–522. [INSPIRE].
  62. Z. Fu and D. Marolf, Bag-of-gold spacetimes, Euclidean wormholes, and inflation from domain walls in AdS/CFT, JHEP 11 (2019) 040 [arXiv:1909.02505] [INSPIRE]. · DOI
  63. A. Hamilton, D.N. Kabat, G. Lifschytz and D.A. Lowe, Local bulk operators in AdS/CFT: A boundary view of horizons and locality, Phys. Rev. D 73 (2006) 086003 [hep-th/0506118] [INSPIRE]. · DOI
  64. A. Hamilton, D.N. Kabat, G. Lifschytz and D.A. Lowe, Holographic representation of local bulk operators, Phys. Rev. D 74 (2006) 066009 [hep-th/0606141] [INSPIRE]. · DOI · Paper page
  65. A. Goel, H.T. Lam, G.J. Turiaci and H. Verlinde, Expanding the Black Hole Interior: Partially Entangled Thermal States in SYK, JHEP 02 (2019) 156 [arXiv:1807.03916] [INSPIRE]. · DOI
  66. H.W. Lin, J. Maldacena, L. Rozenberg and J. Shan, Holography for people with no time, SciPost Phys. 14 (2023) 150 [arXiv:2207.00407] [INSPIRE]. · DOI
  67. H.W. Lin, J. Maldacena, L. Rozenberg and J. Shan, Looking at supersymmetric black holes for a very long time, SciPost Phys. 14 (2023) 128 [arXiv:2207.00408] [INSPIRE]. · DOI
  68. J. Chandra, Euclidean wormholes for individual 2d CFTs, arXiv:2305.07183 [INSPIRE]. · arXiv
  69. I. Kourkoulou and J. Maldacena, Pure states in the SYK model and nearly-AdS2 gravity, arXiv:1707.02325 [INSPIRE]. · arXiv
  70. J. Chandra and T. Hartman, Coarse graining pure states in AdS/CFT, JHEP 10 (2023) 030 [arXiv:2206.03414] [INSPIRE]. · DOI
  71. V. Balasubramanian, A. Lawrence, J.M. Magan and M. Sasieta, Microscopic origin of the entropy of astrophysical black holes, arXiv:2212.08623 [INSPIRE]. · arXiv
  72. T. Anous, T. Hartman, A. Rovai and J. Sonner, Black Hole Collapse in the 1/c Expansion, JHEP 07 (2016) 123 [arXiv:1603.04856] [INSPIRE]. · DOI · Paper page
  73. S. de Haro, S.N. Solodukhin and K. Skenderis, Holographic reconstruction of space-time and renormalization in the AdS / CFT correspondence, Commun. Math. Phys. 217 (2001) 595 [hep-th/0002230] [INSPIRE]. · DOI · Paper page
  74. K. Skenderis, Lecture notes on holographic renormalization, Class. Quant. Grav. 19 (2002) 5849 [hep-th/0209067] [INSPIRE]. · DOI
  75. G. Darmois, Les équations de la gravitation einsteinienne, Mémorial des sciences mathématiques 25 (1927) 58.
  76. W. Israel, Singular hypersurfaces and thin shells in general relativity, Nuovo Cim. B 44S10 (1966) 1 [Erratum ibid. 48 (1967) 463] [INSPIRE]. · DOI · Paper page
  77. M. Sasieta, Ergodic equilibration of Rényi entropies and replica wormholes, JHEP 08 (2021) 014 [arXiv:2103.09880] [INSPIRE]. · DOI
  78. T. Takayanagi, Holographic Dual of BCFT, Phys. Rev. Lett. 107 (2011) 101602 [arXiv:1105.5165] [INSPIRE]. · DOI · Paper page
  79. M. Fujita, T. Takayanagi and E. Tonni, Aspects of AdS/BCFT, JHEP 11 (2011) 043 [arXiv:1108.5152] [INSPIRE]. · DOI · Paper page
  80. D.N. Page, Average entropy of a subsystem, Phys. Rev. Lett. 71 (1993) 1291 [gr-qc/9305007] [INSPIRE]. · DOI · Paper page
  81. E. Witten, A Note On Complex Spacetime Metrics, arXiv:2111.06514 [INSPIRE]. · arXiv
  82. M. Kontsevich and G. Segal, Wick Rotation and the Positivity of Energy in Quantum Field Theory, Quart. J. Math. Oxford Ser. 72 (2021) 673 [arXiv:2105.10161] [INSPIRE]. · DOI
  83. H. Geng et al., Inconsistency of islands in theories with long-range gravity, JHEP 01 (2022) 182 [arXiv:2107.03390] [INSPIRE]. · DOI
  84. H. Geng and A. Karch, Massive islands, JHEP 09 (2020) 121 [arXiv:2006.02438] [INSPIRE]. · DOI · Paper page
  85. J. Chandra and T. Hartman, Toward random tensor networks and holographic codes in CFT, JHEP 05 (2023) 109 [arXiv:2302.02446] [INSPIRE]. · DOI
  86. A. Kar, Non-isometric quantum error correction in gravity, JHEP 02 (2023) 195 [arXiv:2210.13476] [INSPIRE]. · DOI · Paper page
  87. C. Akers and G. Penington, Quantum minimal surfaces from quantum error correction, SciPost Phys. 12 (2022) 157 [arXiv:2109.14618] [INSPIRE]. · DOI · Paper page
  88. V. Balasubramanian and P. Kraus, A stress tensor for Anti-de Sitter gravity, Commun. Math. Phys. 208 (1999) 413 [hep-th/9902121] [INSPIRE]. · DOI · Paper page
  89. S.W. Hawking, Zeta Function Regularization of Path Integrals in Curved Space-Time, Commun. Math. Phys. 55 (1977) 133 [INSPIRE]. · DOI · Paper page
  90. M. Srednicki, Chaos and Quantum Thermalization, cond-mat/9403051 [https://doi.org/10.1103/PhysRevE.50.888] [INSPIRE]. · DOI · Paper page

Cited by

Sorted by citations

Metadata

Authors
Antonini, S., Sasieta, M., & Swingle, B.
Venue
Journal of High Energy Physics
Publisher
Springer Science and Business Media LLC
Published
2023-11-27
Volume
2023
Issue
11
ISSN
1029-8479
DOI
10.1007/jhep11(2023)188
Cited by
43
References
16
Language
en
Licence

About these checks

Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

Statistics and arithmetic are recomputed, not judged.

Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.

What counts as a claim ›How we measure confidence ›How we check this ›

Are you an author, or do you see a problem with this page? Request a review