pith. sign in

arxiv: 2606.07173 · v1 · pith:5CMIUIGInew · submitted 2026-06-05 · 🌀 gr-qc · hep-th

Vanishing of all redshift modes in Schwarzschild ringdown

Pith reviewed 2026-06-27 21:14 UTC · model grok-4.3

classification 🌀 gr-qc hep-th
keywords redshift modesSchwarzschild ringdownquasinormal modesovertonescausalityGreen functionblack hole waveformsimpulsive contribution
0
0 comments X

The pith

All redshift-mode contributions vanish in the observable Schwarzschild ringdown waveform.

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

The paper shows that redshift modes, horizon modes, and direct waves—all contributions decaying at integer multiples of the surface gravity in waveforms from particles plunging into black holes—have exactly zero amplitude once the full signal is assembled. This occurs because causality requires the source-integrated Green function to vanish on the light cone, so that the summed contributions from all quasinormal-mode overtones are precisely cancelled by the impulsive piece of the waveform. A reader should care because the result removes apparent late-time power-law tails from the observable signal and supplies a first-principles reason why standard regularization of quasinormal-mode coefficients is needed.

Core claim

For Schwarzschild black holes, every redshift-mode, horizon-mode, and direct-wave contribution has vanishing amplitude in the observable waveform. The cancellation follows from causality, which forces the source-integrated Green function to vanish on the light cone. Individual quasinormal-mode overtones still carry non-zero redshift-mode pieces, but these cancel exactly once the sum over overtones is performed; the impulsive contribution acts precisely as the counterterm enforcing the cancellation. The result also motivates the usual regularization of quasinormal-mode excitation coefficients, since their divergences produce vanishing redshift modes.

What carries the argument

Causality-enforced vanishing of the source-integrated Green function on the light cone, which supplies the exact counterterm to summed overtone contributions.

If this is right

  • Redshift modes from every individual quasinormal overtone are non-zero before summation but sum exactly to zero.
  • The same vanishing applies to horizon modes and direct waves once the full waveform is considered.
  • The impulsive term is required to enforce the cancellation and cannot be omitted.
  • Divergences in quasinormal-mode excitation coefficients are tied to the production of these vanishing redshift modes.

Where Pith is reading between the lines

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

  • The same light-cone vanishing argument may apply to the late-time waveform of any stationary black hole whose Green function respects the same causal structure.
  • Ringdown template banks that truncate the overtone sum before adding the impulsive term will systematically omit the cancellation mechanism.
  • The result suggests that any apparent power-law tail in numerical waveforms should be checked for consistency with the full sum over modes plus impulse.

Load-bearing premise

The impulsive contribution to the waveform supplies precisely the counterterm needed to cancel the summed redshift-mode pieces from all quasinormal-mode overtones.

What would settle it

A numerical computation of the full waveform from a plunging particle that retains a non-zero redshift-mode tail after summing overtones plus the impulsive term would falsify the claim.

Figures

Figures reproduced from arXiv: 2606.07173 by Adrien Kuntz, Matteo Della Rocca.

Figure 1
Figure 1. Figure 1: Approximated value of |S1| and |S2| as a function of the highest overtone nmax accounted for in the sum. Data are publicly available at Ref. [38]. the integrand of the impulsive term contribution to the redshift mode in Eq. (15) vanishes as 1/|ω| as |ω| → ∞, and so Jordan’s lemma is no longer applicable. In or￾der to get an idea on the scaling of these integrals, let us use our QNM sum approximation and co… view at source ↗
read the original abstract

Several studies of black hole ringdown from particles plunging into black holes have identified contributions decaying at integer multiples of the surface gravity, called redshift modes, horizon modes, and direct waves. We show that, for Schwarzschild black holes, every one of these contributions has vanishing amplitude in the observable waveform. The cancellation follows from causality, which forces the source-integrated Green function to vanish on the light cone. Individual quasi-normal mode overtones still carry non-zero redshift-mode contributions, but these cancel exactly once the sum over overtones is performed; the so-called impulsive contribution to the waveform acts precisely as the counterterm enforcing this cancellation. Finally, we provide a motivation to the standard regularization of quasinormal mode excitation coefficients since divergences give rise to vanishing redshift modes.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 1 minor

Summary. The manuscript claims that for Schwarzschild black holes, all redshift modes, horizon modes, and direct waves vanish in the observable waveform. This follows from causality forcing the source-integrated Green function to vanish on the light cone. While individual QNM overtones carry non-zero redshift-mode contributions, these cancel exactly upon summation over overtones, with the impulsive contribution acting as the precise counterterm. The work also motivates the standard regularization of QNM excitation coefficients on the grounds that divergences produce vanishing redshift modes.

Significance. If the central cancellation holds, the result would clarify the structure of ringdown waveforms from plunging sources by eliminating apparent non-vanishing contributions from redshift and related modes, with direct implications for modeling extreme-mass-ratio signals and the interpretation of overtone sums. The explicit link to an external causality principle and the byproduct motivation for regularization are strengths.

major comments (1)
  1. [Abstract (final paragraph)] Abstract (final paragraph): The assertion that the impulsive contribution 'acts precisely as the counterterm' enforcing exact cancellation of the summed redshift-mode pieces from all QNM overtones is load-bearing for the vanishing claim. The manuscript must supply an explicit derivation or calculation showing that the sum over overtones is exactly offset by the impulsive term (rather than relying solely on the general statement that the source-integrated Green function vanishes on the light cone), as this step is not automatic and is identified as the weakest assumption.
minor comments (1)
  1. [Abstract] The abstract would be clearer if it indicated the section or equation where the explicit summation and cancellation are demonstrated.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for identifying the need for a more explicit demonstration of the cancellation mechanism. We address the major comment below.

read point-by-point responses
  1. Referee: [Abstract (final paragraph)] Abstract (final paragraph): The assertion that the impulsive contribution 'acts precisely as the counterterm' enforcing exact cancellation of the summed redshift-mode pieces from all QNM overtones is load-bearing for the vanishing claim. The manuscript must supply an explicit derivation or calculation showing that the sum over overtones is exactly offset by the impulsive term (rather than relying solely on the general statement that the source-integrated Green function vanishes on the light cone), as this step is not automatic and is identified as the weakest assumption.

    Authors: We agree that an explicit derivation of the exact offset between the summed overtone contributions and the impulsive term would strengthen the presentation and remove any ambiguity about whether the cancellation is automatic. In the revised manuscript we will add a dedicated calculation (in a new subsection or appendix) that starts from the explicit expression for the source-integrated retarded Green function, performs the sum over QNM overtones of the redshift-mode pieces, and demonstrates term-by-term cancellation against the impulsive contribution on the light cone. This will make the argument self-contained while still grounding the result in the underlying causality principle. revision: yes

Circularity Check

0 steps flagged

Derivation self-contained via external causality principle

full rationale

The paper derives vanishing redshift-mode amplitudes from causality forcing the source-integrated Green function to vanish on the light cone—an independent physical input not defined by the result itself. The exact cancellation between summed overtone contributions and the impulsive term is presented as following from that principle rather than by construction or redefinition. No self-citations, fitted predictions, or ansatz smuggling appear in the abstract or described chain. The regularization motivation is a secondary consequence. This meets the default expectation of a non-circular derivation.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Ledger extracted from abstract only; full paper may contain additional parameters or axioms.

axioms (1)
  • domain assumption Causality forces the source-integrated Green function to vanish on the light cone.
    This premise is invoked to conclude that all listed contributions have vanishing amplitude.

pith-pipeline@v0.9.1-grok · 5649 in / 1259 out tokens · 22433 ms · 2026-06-27T21:14:22.353637+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Radial Mirror Scattering and the QNM Convergence Region

    gr-qc 2026-06 unverdicted novelty 5.0

    A reflection about a distinguished point in the tortoise coordinate maps the Regge-Wheeler problem to a mirror version with the same QNM spectrum and provides an image interpretation of the lightcone distance controll...

Reference graph

Works this paper leans on

49 extracted references · 2 canonical work pages · cited by 1 Pith paper

  1. [1]

    monodromy method

    Teukolsky amplitudes The Teukolsky equation describes the response of a BH with massMand angular momentumJ=M ato a generic perturbation with spins. The MST method relies on the introduction of an additional parameter in the Teukolsky equation, the so-calledrenormalized angu- lar momentumν. This parameter enables the construc- tion of a convergent series r...

  2. [2]

    (A1) can be computed from the Teukol- sky amplitudes (withs=−2)

    The Sasaki-Nakamura amplitudes The normalized Sasaki-Nakamura amplitudeA in ap- pearing in Eq. (A1) can be computed from the Teukol- sky amplitudes (withs=−2). In the same way than for the Teukolsky amplitudes, we can defineA ref,A inc and Atrans from the expansion Xin → ( Atranse−i(ω−ma/r+)r⋆ r→r + Aref eiωr⋆ +A ince−iωr⋆ r→+∞ .(A15) 2 The Sasaki-Nakamur...

  3. [3]

    R. Abbottet al.(LIGO Scientific, Virgo), GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run, (2020), arXiv:2010.14527 [gr-qc]

  4. [4]

    Abbottet al.(KAGRA, VIRGO, LIGO Scien- tific), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run, Phys

    R. Abbottet al.(KAGRA, VIRGO, LIGO Scien- tific), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run, Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]

  5. [5]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, (2025), arXiv:2508.18082 [gr-qc]

  6. [6]

    Bertiet al., Black hole spectroscopy: from theory to experiment, (2025), arXiv:2505.23895 [gr-qc]

    E. Bertiet al., Black hole spectroscopy: from theory to experiment, (2025), arXiv:2505.23895 [gr-qc]

  7. [7]

    Lagos and L

    M. Lagos and L. Hui, Generation and propagation of non- linear quasinormal modes of a schwarzschild black hole, Physical Review D107, 10.1103/physrevd.107.044040 (2023)

  8. [8]

    Chavda, M

    A. Chavda, M. Lagos, and L. Hui, The impact of ini- tial conditions on quasi-normal modes, JCAP07, 084, arXiv:2412.03435 [gr-qc]

  9. [9]

    Kuntz, Green function of the P¨ oschl-Teller potential, SciPost Phys.20, 120 (2026), arXiv:2510.17954 [gr-qc]

    A. Kuntz, Green function of the P¨ oschl-Teller potential, SciPost Phys.20, 120 (2026), arXiv:2510.17954 [gr-qc]

  10. [10]

    Arnaudo, J

    P. Arnaudo, J. Carballo, and B. Withers, Beyond quasi- normal modes: a complete mode decomposition of black hole perturbations, (2025), arXiv:2510.18956 [gr-qc]

  11. [11]

    Arnaudo and B

    P. Arnaudo and B. Withers, Price’s law from quasinormal modes, (2025), arXiv:2511.17703 [gr-qc]

  12. [12]

    J. Su, N. Khera, M. Casals, S. Ma, A. Chowd- huri, and H. Yang, Decomposition of the Schwarzschild Green’s function, Phys. Rev. D113, 104013 (2026), arXiv:2601.22015 [gr-qc]

  13. [13]

    D. Q. Aruquipa and M. Casals, Green functions of the Regge-Wheeler and Teukolsky equations in Schwarzschild spacetime, (2026), arXiv:2603.07747 [gr- qc]

  14. [14]

    Arnaudo and B

    P. Arnaudo and B. Withers, Bouncing singularities in Schwarzschild: a geometric origin of the QNM conver- gence region, (2026), arXiv:2605.16489 [gr-qc]

  15. [15]

    De Amicis, E

    M. De Amicis, E. Cannizzaro, G. Carullo, and L. Sberna, Dynamical quasinormal mode excitation, (2025), arXiv:2506.21668 [gr-qc]

  16. [16]

    De Amicis, E

    M. De Amicis, E. Cannizzaro, G. Carullo, A. Kuntz, and L. Sberna, Dynamical quasinormal mode excitation II: propagation and convergence in Schwarzschild, (2026), arXiv:2605.16492 [gr-qc]

  17. [17]

    Mino and J

    Y. Mino and J. Brink, Gravitational Radiation from Plunging Orbits: Perturbative Study, Phys. Rev. D78, 124015 (2008), arXiv:0809.2814 [gr-qc]

  18. [18]

    Zimmerman and Y

    A. Zimmerman and Y. Chen, New Generic Ringdown Frequencies at the Birth of a Kerr Black Hole, Phys. Rev. D84, 084012 (2011), arXiv:1106.0782 [gr-qc]. 12

  19. [19]

    Motohashi and Y

    H. Motohashi and Y. Suichi, Pole Structure of Kerr Green’s Function, (2026), arXiv:2605.01964 [gr-qc]

  20. [20]

    Oshita, S

    N. Oshita, S. Ma, Y. Chen, and H. Yang, Prob- ing Direct Waves in Black Hole Ringdowns, (2025), arXiv:2509.09165 [gr-qc]

  21. [21]

    E. W. Leaver, Spectral decomposition of the perturbation response of the Schwarzschild geometry, Phys. Rev. D34, 384 (1986)

  22. [22]

    Hadar and B

    S. Hadar and B. Kol, Post-ISCO Ringdown Amplitudes in Extreme Mass Ratio Inspiral, Phys. Rev. D84, 044019 (2011), arXiv:0911.3899 [gr-qc]

  23. [23]

    Rungta, V

    E. Berti, V. Cardoso, and C. M. Will, Gravitational-wave spectroscopy of massive black holes with the space in- terferometer lisa, Physical Review D73, 10.1103/phys- revd.73.064030 (2006)

  24. [24]

    Berti and V

    E. Berti and V. Cardoso, Quasinormal ringing of Kerr black holes. I. The Excitation factors, Phys. Rev. D74, 104020 (2006), arXiv:gr-qc/0605118

  25. [25]

    Zhang, E

    Z. Zhang, E. Berti, and V. Cardoso, Quasinormal ring- ing of Kerr black holes. II. Excitation by particles falling radially with arbitrary energy, Phys. Rev. D88, 044018 (2013), arXiv:1305.4306 [gr-qc]

  26. [26]

    Sun and R

    Y. Sun and R. H. Price, Excitation of Quasinormal Ring- ing of a Schwarzschild Black Hole, Phys. Rev. D38, 1040 (1988)

  27. [27]

    Della Rocca, L

    M. Della Rocca, L. Pezzella, E. Berti, L. Gualtieri, and A. Maselli, Quasinormal ringing of Kerr black holes. III. Excitation coefficients for equatorial inspirals from the innermost stable circular orbit, (2025), arXiv:2512.07959 [gr-qc]

  28. [28]

    Regge and J

    T. Regge and J. A. Wheeler, Stability of a Schwarzschild singularity, Phys.Rev.108, 1063 (1957)

  29. [29]

    F. J. Zerilli, Gravitational field of a particle falling in a schwarzschild geometry analyzed in tensor harmonics, Physical Review D2, 2141 (1970)

  30. [30]

    Nagar, T

    A. Nagar, T. Damour, and A. Tartaglia, Binary black hole merger in the extreme mass ratio limit, Class. Quant. Grav.24, S109 (2007), arXiv:gr-qc/0612096

  31. [31]

    E. W. Leaver, Solutions to a generalized spheroidal wave equation: Teukolsky’s equations in general relativity, and the two-center problem in molecular quantum mechanics, J. Math. Phys.27, 1238 (1986)

  32. [32]

    Maassen van den Brink, Analytic treatment of black hole gravitational waves at the algebraically special fre- quency, Phys

    A. Maassen van den Brink, Analytic treatment of black hole gravitational waves at the algebraically special fre- quency, Phys. Rev. D62, 064009 (2000), arXiv:gr- qc/0001032

  33. [33]

    Kubota and H

    K.-i. Kubota and H. Motohashi, Pole Skipping, Avoided Crossing, and Resonant Excitation in Kerr Quasinormal Modes near Algebraically Special Frequencies, (2026), arXiv:2605.17840 [gr-qc]

  34. [34]

    Casals, S

    M. Casals, S. R. Dolan, A. C. Ottewill, and B. Wardell, Self-Force Calculations with Matched Expansions and Quasinormal Mode Sums, Phys. Rev. D79, 124043 (2009), arXiv:0903.0395 [gr-qc]

  35. [35]

    Casals, S

    M. Casals, S. Dolan, A. C. Ottewill, and B. Wardell, Self- Force and Green Function in Schwarzschild spacetime via Quasinormal Modes and Branch Cut, Phys. Rev. D88, 044022 (2013), arXiv:1306.0884 [gr-qc]

  36. [36]

    Casals, B

    M. Casals, B. C. Nolan, A. C. Ottewill, and B. Wardell, Regularized calculation of the retarded Green function in a Schwarzschild spacetime, Phys. Rev. D100, 104037 (2019), arXiv:1910.02567 [gr-qc]

  37. [37]

    D. Q. Aruquipa, M. Casals, and B. C. Nolan, Cal- culation of a regularized Teukolsky Green function in Schwarzschild spacetime, (2026), arXiv:2604.21219 [gr- qc]

  38. [38]

    R. F. Rosato, M. De Amicis, and P. Pani, Singular struc- tures and causality of the Schwarzschild Green’s function in the frequency domain, (2026), arXiv:2603.20490 [gr- qc]

  39. [39]

    Andersson, Evolving test fields in a black-hole geom- etry, Phys

    N. Andersson, Evolving test fields in a black-hole geom- etry, Phys. Rev. D55, 468 (1997)

  40. [40]

    Della Rocca and A

    M. Della Rocca and A. Kuntz, Table of quasinor- mal modes and excitation factors,https://github.com/ matteodellarocca/ExcitationFactors(2026)

  41. [41]

    M. J. Rodr´ ıguez, L. Santoni, and A. R. Solomon, Love numbers of black holes and compact objects, (2026), arXiv:2604.08653 [gr-qc]

  42. [42]

    Sasaki and H

    M. Sasaki and H. Tagoshi, Analytic black hole pertur- bation approach to gravitational radiation, Living Rev. Rel.6, 6 (2003), arXiv:gr-qc/0306120

  43. [43]

    S. Mano, H. Suzuki, and E. Takasugi, Analytic solutions of the Teukolsky equation and their low frequency ex- pansions, Prog. Theor. Phys.95, 1079 (1996), arXiv:gr- qc/9603020

  44. [44]

    S. Mano, H. Suzuki, and E. Takasugi, Analytic solutions of the Regge-Wheeler equation and the postMinkowskian expansion, Prog. Theor. Phys.96, 549 (1996), arXiv:gr- qc/9605057

  45. [45]

    Casals and A

    M. Casals and A. C. Ottewill, High-order tail in Schwarzschild spacetime, Phys. Rev. D92, 124055 (2015), arXiv:1509.04702 [gr-qc]

  46. [46]

    Sasaki, Post-newtonian expansion of the ingoing-wave regge-wheeler function, Prog.Theor.Phys.92, 17 (1994)

    M. Sasaki, Post-newtonian expansion of the ingoing-wave regge-wheeler function, Prog.Theor.Phys.92, 17 (1994)

  47. [47]

    Abramowitz and I

    M. Abramowitz and I. A. Stegun,Handbook of Mathe- matical Functions, New York: Dover, 1972, edited by Abramowitz, M. & Stegun, I. A. (Dover, New York, 1972)

  48. [48]

    Nasipak, Connecting scattering, monodromy, and MST’s renormalized angular momentum for the Teukol- sky equation in Kerr spacetime, Class

    Z. Nasipak, Connecting scattering, monodromy, and MST’s renormalized angular momentum for the Teukol- sky equation in Kerr spacetime, Class. Quant. Grav.42, 165001 (2025), arXiv:2412.06503 [gr-qc]

  49. [49]

    Nagar and L

    A. Nagar and L. Rezzolla, Gauge-invariant non-spherical metric perturbations of Schwarzschild black-hole space- times, Class. Quant. Grav.22, R167 (2005), [Erratum: Class. Quant. Grav.23,4297(2006)], arXiv:gr-qc/0502064 [gr-qc]