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Baby de Sitter Black Holes and dS$_3$/CFT$_2$
High Energy Physics - Theory · Submitted 26 Aug 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We compute the mass and angular momentum of the dS black holes and verify that a naive application of Cardy's formula exactly reproduces the entropy of both the black hole and the cosmological horizon.
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The abstract, sentence by sentence
Unlike three-dimensional Einstein gravity, three-dimensional massive gravity admits asymptotically de Sitter space (dS) black hole solutions. These black holes present interesting features and provide us with toy models to study the dS/CFT correspondence. A remarkable property of these black holes is that they are always in thermal equilibrium with the cosmological horizon of the space that hosts them. This invites us to study the thermodynamics of these solutions within the context of dS/CFT. We study the asymptotic symmetry group of the theory and find that it indeed coincides with the local two-dimensional conformal algebra. The charge algebra associated to the asymptotic Killing vectors consists of two copies of the Virasoro algebra with non-vanishing central extension. We compute the mass and angular momentum of the dS black holes and verify that a naive application of Cardy's formula exactly reproduces the entropy of both the black hole and the cosmological horizon. By adapting the holographic renormalization techniques to the case of dS space, we define the boundary stress tensor of the dual Euclidean conformal field theory.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Unlike three-dimensional Einstein gravity, three-dimensional massive gravity admits asymptotically de Sitter space (dS) black hole solutions. | background 0.97 | 0.08 | 0.07 | asserted 1.00 |
| s1 | These black holes present interesting features and provide us with toy models to study the dS/CFT correspondence. | background 0.71 | 0.09 | 0.07 | asserted 0.97 |
| s2 | A remarkable property of these black holes is that they are always in thermal equilibrium with the cosmological horizon of the space that hosts them. | result 0.64 | 0.21 | 0.10 | asserted 1.00 |
| s3 | This invites us to study the thermodynamics of these solutions within the context of dS/CFT. | future work 0.39 | 0.15 | 0.05 | hedged possibility 0.59 |
| s4 | We study the asymptotic symmetry group of the theory and find that it indeed coincides with the local two-dimensional conformal algebra. | result 0.73 | 0.96 | 0.17 | asserted 1.00 |
| s5 | The charge algebra associated to the asymptotic Killing vectors consists of two copies of the Virasoro algebra with non-vanishing central extension. | result 0.98 | 0.85 | 0.14 | asserted 1.00 |
| s6 | We compute the mass and angular momentum of the dS black holes and verify that a naive application of Cardy's formula exactly reproduces the entropy of both the black hole and the cosmological horizon. | result 0.99 | 0.95 | 0.49 | asserted 1.00 |
| s7 | By adapting the holographic renormalization techniques to the case of dS space, we define the boundary stress tensor of the dual Euclidean conformal field theory. | method 0.51 | 0.94 | 0.12 | asserted 1.00 |
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The paper
Original abstract
Unlike three-dimensional Einstein gravity, three-dimensional massive gravity admits asymptotically de Sitter space (dS) black hole solutions. These black holes present interesting features and provide us with toy models to study the dS/CFT correspondence. A remarkable property of these black holes is that they are always in thermal equilibrium with the cosmological horizon of the space that hosts them. This invites us to study the thermodynamics of these solutions within the context of dS/CFT. We study the asymptotic symmetry group of the theory and find that it indeed coincides with the local two-dimensional conformal algebra. The charge algebra associated to the asymptotic Killing vectors consists of two copies of the Virasoro algebra with non-vanishing central extension. We compute the mass and angular momentum of the dS black holes and verify that a naive application of Cardy's formula exactly reproduces the entropy of both the black hole and the cosmological horizon. By adapting the holographic renormalization techniques to the case of dS space, we define the boundary stress tensor of the dual Euclidean conformal field theory.
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References
How the literature uses it
9 arXiv papers cite this in 9 sentences
Papers citing it · 3 sentences without a confident label
Compares with it 1 paper
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Note added : While we are preparing this paper, the preprint [ref] appeared in the arXiv which deals with the thermodynamics of the dS black holes of NMG in a different way from our approach.
Some properties of the de Sitter black holes in three dimensional spacetime · Acknowledgements · 0.83
Cites it as background 5 papers
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In [ref] , it was proposed that NMG has a dual description in terms of a CFT.[In 2013, de Buyl et al. considered the asymptotically dS case, $Λ=+1/ℓ^2>0$, within the context of dS/CFT correspondence [ref] .
Holography of 3D Asymptotically Flat Black Holes · CFT dual to NMG · 0.82
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To wit, there are no black hole solutions to three-dimensional Einstein gravity with $Λ≥0$.[Black holes in dS$_3$ have been uncovered in topologically massive theories [ref] , and “new massive gravity” [ref] , including perturbative backreaction effects [ref] .] Rather, Schwarzschild- and Kerr-(dS$_3$) geometries describe a conical defect with (possibly) a single cosmological horizon and no black hole horizon [ref] .
Nucleation of charged quantum de-Sitter$_{3}$ black holes · Introduction · 0.80
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These solutions with central charge expressions were a starting point for the warped AdS/CFT correspondence [ref] and the Kerr/CFT correspondence [ref] , which may be extended to the dS/CFT case [ref] .
Quasilocal Conserved Charges with a Gravitational Chern-Simons Term · Introduction · 0.84
What it cites · 64 sentences without a confident label
Uses the method or tool of 7 papers
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As in the case of AdS, to apply the method of [ref] one first needs to supplement the gravity action with adequate boundary terms, which eventually yield the correct boundary stress-tensor.
Mass, Entropy and Holography in Asymptotically de Sitter Spaces · Boundary stress-tensor · 0.99
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As in the case of AdS, to apply the method of [ref] one first needs to supplement the gravity action with adequate boundary terms, which eventually yield the correct boundary stress-tensor.
Les Houches Lectures on De Sitter Space · Boundary stress-tensor · 0.99
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As in the case of AdS, to apply the method of [ref] one first needs to supplement the gravity action with adequate boundary terms, which eventually yield the correct boundary stress-tensor.
Lecture Notes on Holographic Renormalization · Boundary stress-tensor · 0.99
Compares with 5 papers
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In the limit $m^2→∞$ one recovers the central charge of [ref] which differs from [ref] by a minus sign.
The dS/CFT Correspondence · Phase Space, Symmetries and Charges · 0.95
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In the limit $m^2→∞$ one recovers the central charge of [ref] which differs from [ref] by a minus sign.
Mass, Entropy and Holography in Asymptotically de Sitter Spaces · Phase Space, Symmetries and Charges · 0.95
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To this regard, it is convenient to compare our notation with that of Ref. [ref] where this special point is also considered.
More on Massive 3D Gravity · Three-dimensional Massive gravity · 0.95
Cites as background 27 papers
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The dS/CFT correspondence [ref] was proposed with the aim of extending the idea of holography to asymptotically de Sitter space.
The dS/CFT Correspondence · Introduction · 1.00
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The dS/CFT correspondence [ref] was proposed with the aim of extending the idea of holography to asymptotically de Sitter space.
Non-Gaussian features of primordial fluctuations in single field inflationary models · Introduction · 1.00
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The dS/CFT correspondence [ref] was proposed with the aim of extending the idea of holography to asymptotically de Sitter space.
Quantum Gravity In De Sitter Space · Introduction · 1.00
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