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REVIEW 2 major objections 3 minor 5 cited by

Complex black holes do not control low-temperature AdS thermodynamics; contour arguments show they drop out of the partition function.

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2026-08-04 20:04 UTC pith:ICI2F65P

load-bearing objection A genuine new puzzle about complex AdS-Schwarzschild saddles dominating by real action at low T in AdS5+, with a sound mini-superspace contour argument that excludes them, but the reduction to one dimension is assumed, so treat the general claim as conditional. the 2 major comments →

arxiv 2509.08883 v1 pith:ICI2F65P submitted 2025-09-10 hep-th

A Brief Note on Complex AdS-Schwarzschild Black Holes

Raghu Mahajan , Kaustubh Singhi This is my paper
classification hep-th
keywords AdS-Schwarzschildcomplex saddlesthermal AdSgravitational path integralsteepest descentHawking-Page transitionmini-superspaceholography
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper tackles a puzzle in holographic thermodynamics: at very low temperatures, AdS-Schwarzschild black holes persist as complex saddle points of the gravitational path integral, and their real on-shell action is smaller than that of thermal AdS. If those saddles contributed, the bulk would predict physics completely at odds with the dual gauge theory's confined low-temperature phase. The authors argue, using a mini-superspace reduction to a one-dimensional integral over the horizon radius, that the integration contour is the steepest-descent contour of the thermal AdS saddle, so the complex black holes do not contribute at all. The standard result—thermal AdS dominates at low temperatures—survives. The note also examines why the unstable small black hole does not genuinely contribute in the high-temperature phase, via complexifying Newton's constant and averaging steepest-descent contours.

Core claim

For beta greater than beta_max, the two AdS-Schwarzschild saddles become complex: the horizon radius r+ takes two complex values. A naive comparison of on-shell actions suggests these saddles dominate over thermal AdS at low temperature, threatening the AdS/CFT correspondence. The paper's central claim is that these complex black holes contribute nothing to the partition function, no matter how small their imaginary part. The argument reduces the gravitational path integral to a one-dimensional integral over r+ with an action S(r+)-beta E(r+); because the coefficient of the quadratic term is negative, the steepest-descent contour through the r+=0 (thermal AdS) saddle is the positive real r+

What carries the argument

The key machinery is a mini-superspace integral over the black hole horizon radius r+, Z(beta) = integral from 0 to infinity of dr+ exp[S(r+)-beta E(r+)], together with the steepest-descent analysis of that integral. The real positive r+ axis is identified as (half of) the steepest-descent contour of the thermal AdS saddle (r+=0), because the quadratic term in the action has a negative coefficient. Since the defining contour does not pass through the complex saddles, those saddles do not contribute. For the beta<beta_max case, complexifying Newton's constant G and taking a homology average of steepest-decent contours isolates and cancels the small black hole contribution.

Load-bearing premise

The entire argument relies on the reduction of the full gravitational path integral to a one-dimensional integral over r+ with the positive real axis as the contour; if the true contour in field space is different or includes other degrees of freedom, the complex saddles could contribute.

What would settle it

Directly compute the gravitational path integral in a saddle-point approximation without the mini-superspace truncation, at a beta slightly above beta_max, and check whether the result contains a contribution whose entropy scales as the area of a complex horizon; if such a contribution appears, the central claim fails.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

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If this is right

  • Thermal AdS remains the correct low-temperature saddle in asymptotically AdS gravity in five and higher dimensions, despite the existence of complex black holes with smaller real on-shell action.
  • The complex Schwarzschild black holes contribute zero to the thermal partition function for beta>beta_max, even when their imaginary part is arbitrarily small and they pass the Kontsevich-Segal criterion.
  • The same contour argument applies in any dimension and rules out even suppressed contributions from the complex black holes, contrary to earlier finite-cutoff AdS4 conclusions.
  • In the high-temperature phase, the small black hole saddle does not genuinely contribute: its steepest-descent contribution cancels under median-resummation/homology averaging, leaving thermal AdS and the big black hole as the physical saddles.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The key conceptual lesson is that dominance by on-shell action is not sufficient: a saddle contributes only if the defining contour of the path integral can be deformed onto it. This suggests similar contour analyses could decide whether other complex gravitational saddles (e.g., cosmological or rotating ones) are physical.
  • The mini-superspace reduction effectively encodes the 'real energy' condition as the choice of contour along the real r+ axis. A testable extension would be to check whether relaxing that condition—allowing complex energies—leads to contributions from the complex black holes, which would change the low-temperature physics.
  • The cancellation of the small black hole via homology averaging hints that 'unstable' saddles in gravitational path integrals should generically be interpreted through median resummation; this may clarify analogous false saddles in higher-dimensional black hole thermodynamics.
  • One could test the paper's claim against a direct Lorentzian path-integral computation of the low-temperature partition function, which should show no saddle with black-hole-like entropy at large beta, matching the confined phase of the dual gauge theory.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 3 minor

Summary. This note addresses the low-temperature (β>β_max) phase of asymptotically AdS gravitational saddle points. The authors observe that complex AdS-Schwarzschild black holes, obtained by analytically continuing the horizon radius r_+(β), have a real on-shell action smaller than that of thermal AdS in AdS5 (and, they claim, higher dimensions), which would naively make them the dominant saddles and contradict the dual CFT. To resolve this, they propose a mini-superspace path integral over the horizon radius, Eq. (9), with the integration contour taken along the positive real r_+ axis (corresponding to real energy). They show that for β>β_max this contour is (half of) the steepest-descent contour of the r_+=0 thermal AdS saddle and does not pass through the complex saddles, so the latter do not contribute. They also analyze the unstable small black hole for β<β_max by complexifying Newton's constant and taking a homology average, concluding that it does not contribute. The authors contrast their argument with the Kontsevich–Segal criterion and with Ref. [9].

Significance. If the reduction to Eq. (9) is accepted, the paper gives a simple and elegant resolution of a genuine puzzle, showing that a naive on-shell-action comparison is misleading and that steepest-descent/thimble methods provide a more refined criterion. The treatment of the small black hole is also a nice illustration of Stokes phenomena and median resummation. However, the central result is conditional on an unproven mini-superspace reduction; the authors acknowledge this limitation in the text. As it stands, the note is a useful toy-model resolution, but it does not establish the claim for the full gravitational path integral.

major comments (2)
  1. The central claim—that complex AdS-Schwarzschild saddles do not contribute to Z(β) for β>β_max—is established only inside the one-dimensional model (9). The reduction from the full gravitational path integral to this integral is assumed: the text says 'We approximate the full path integral as just a one-dimensional integral over r+' and footnote 5 drops Jacobian factors. In particular, the integration contour in the full field-space path integral is not derived; the 'reasonable assumption' that it corresponds to the positive real r_+ axis is precisely the assumption that excludes the complex saddles. Without a derivation of the mini-superspace reduction from a Lorentzian/Euclidean definition of the path integral, or an argument that the omitted modes do not affect the thimble decomposition, the statement that these complex black holes 'do not actually contribute' is not established for t
  2. [Abstract and d=4 specialization] The abstract says that the puzzle arises in AdS5 and higher dimensions and the text later states that the non-contribution holds 'in any dimension,' but the explicit calculation is only for d=4 (AdS5). Equations (6)–(9) are specialized to that case. For d>5 the effective action has different powers of r_+, and the sign of the quadratic coefficient and the contour analysis need to be rechecked. As written, the general claim is an extrapolation. Please either provide the d-dimensional version of Eq. (9) or explicitly state that the detailed analysis is for d=4 and only comment on higher dimensions heuristically.
minor comments (3)
  1. [Fig. 3] The steepest-descent contours are drawn schematically. It would be helpful to indicate the direction of flow and to clarify the role of the endpoint r_+=0, since the defining contour is half of a thimble rather than a complete thimble.
  2. [Small black hole discussion] The conclusion that the small black hole does not contribute for β<β_max is based on a homology average over Im G>0 and Im G<0. This is a natural choice, but the statement 'does not contribute' depends on this resummation convention; the text partly acknowledges this, but it would be clearer to state that the conclusion is convention-dependent.
  3. [References and Eq. (9)] Ref. [29] (Marolf) is cited as a source of the mini-superspace approximation, but the connection between that derivation and Eq. (9) is not explained. A sentence clarifying how Eq. (9) follows from that work, or where it deviates from it, would strengthen the presentation.

Circularity Check

0 steps flagged

No significant circularity; the central result is a steepest-descent statement within an explicitly assumed mini-superspace integral, and the principal limitation is the assumed real-r+ contour, not a definitional or self-citation circularity.

full rationale

The paper's central claim is derived within an explicit model. Eq. (9) is built from the standard Gibbons-Hawking on-shell action and energy (Eqs. 6-8); no parameter is fitted to force the conclusion. Within that model, the statement that complex black holes do not contribute follows from standard steepest-descent logic: the defining contour is chosen to be the positive real r+ axis, this contour is (half of) the steepest descent contour of the r+=0 thermal AdS saddle, and the complex saddles are off this contour. This is a valid conditional result. The important caveat is that the reduction to the one-dimensional integral over real r+ is assumed, not derived from the full gravitational path integral. The paper flags this explicitly: 'We approximate the full path integral as just a one-dimensional integral over r+.' and 'we are making the reasonable assumption that the contour of integration in the r+ plane is along the real axis.' Thus the exclusion of the complex saddles is contingent on that assumed contour; if the true contour were different, the puzzle would remain. This is a scope limitation and an unsupported premise, but it is not a circularity: the paper does not define the contour in terms of the conclusion, nor does it fit a parameter to the desired answer. The self-citations ([31], [36]) are not load-bearing: [31] is cited only as an example where Kontsevich-Segal-excluded geometries are essential, and [36] is an announced future work. The cited steepest-descent fact [30] is a standard external result. Consequently, the circularity burden is low; the appropriate score is 2 for minor non-load-bearing self-citations.

Axiom & Free-Parameter Ledger

0 free parameters · 4 axioms · 0 invented entities

The central claim rests on two modeling assumptions: the mini-superspace reduction to Eq. (9) and the real-axis contour for r+. No free parameters are introduced by the paper: G and L are fixed inputs, beta is the external variable, and the action coefficients in Eq. (9) are derived rather than fitted. Complex black holes are complexified versions of known AdS-Schwarzschild solutions, not new postulated entities.

axioms (4)
  • ad hoc to paper The full gravitational path integral may be approximated by the one-dimensional integral over r+ in Eq. (9).
    The paper states 'We approximate the full path integral as just a one-dimensional integral over r+' without deriving this reduction from the full metric path integral; the validity of this truncation is the main load-bearing modeling assumption.
  • ad hoc to paper The contour of integration in the r+ plane is along the positive real axis, corresponding to real energy.
    Stated as 'a reasonable assumption' after Eq. (9). The steepest-descent conclusion that complex saddles do not contribute depends on this contour choice; a different contour could in principle include them.
  • standard math If the defining contour is the steepest descent contour of one saddle and contains no other saddles, only that saddle contributes.
    Standard saddle-point/steepest-descent theorem, cited to Witten's Chern-Simons lectures [30]. Used to conclude only thermal AdS contributes.
  • standard math The on-shell action and energy expressions (7)-(8) for the black hole saddles are correct after holographic renormalization.
    Derived from Gibbons-Hawking with boundary counterterms [7,8]; these expressions define the integrand in Eq. (9).

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Cite this review

Pith. "Pith review of A Brief Note on Complex AdS-Schwarzschild Black Holes." pith.science (2026). https://pith.science/paper/ICI2F65P

@misc{pith2026250908883,
  author       = {Pith},
  title        = {Pith review of: A Brief Note on Complex AdS-Schwarzschild Black Holes},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ICI2F65P}},
  note         = {Machine review of arXiv:2509.08883}
}
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read the original abstract

In the context of thermodynamics of asymptotically anti-de Sitter spaces, it is often stated that at very low temperatures, there is only one saddle point available-namely, thermal AdS-and hence this sole saddle dictates the low-temperature behavior. However, AdS-Schwarzschild black holes continue to exist at low temperatures as complex saddle points. We point out that the real part of the on-shell action of these complex black holes is smaller than that of thermal AdS at the lowest temperatures, in AdS$_5$ and higher dimensions. So, na\"ively, they should be the "dominant" saddles. This raises a puzzle: if these complex black holes were indeed the relevant saddle points, the physics of the bulk and that of the dual gauge theory would completely disagree at low temperatures. Using a mini-superspace approximation and contour arguments, we argue that these complex black holes do not actually contribute to the gravitational path integral, regardless of the value of their on-shell action. So the standard conclusion that thermal AdS is the correct saddle at the lowest temperatures continues to hold. We also comment on two related matters: whether the Kontsevich-Segal criterion is useful in this setting, and whether the unstable small black hole contributes to the path integral in the high-temperature phase.

Figures

Figures reproduced from arXiv: 2509.08883 by Kaustubh Singhi, Raghu Mahajan.

Figure 1
Figure 1. Figure 1: A plot showing the thermal AdS and the Schwarzschild black hole saddles in the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The trajectory r`pβq in the complex r` plane upon varying β. The small black hole saddle (red) and the big black hole saddle (blue), which exist for β ă βmax merge at β “ βmax. For β ą βmax, the two possible values of r`pβq are complex. These complex AdS Schwarzschild black holes are shown in orange. values of r` have a complex metric, but that does not a priori mean that we should discard them. Indeed, by… view at source ↗
Figure 3
Figure 3. Figure 3: The steepest descent contours of the two complex black hole saddles, which exist for [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The steepest contours through the three saddle points with [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗

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Forward citations

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