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arxiv: 2507.15951 · v3 · submitted 2025-07-21 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves - Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter

Sulagna Bhattacharya , Shasvath Kapadia , Basudeb Dasgupta This is my paper

Pith reviewed 2026-05-19 03:40 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE
keywords gravitational wavesneutron star mergersblack hole binariesdark mattertransmuted black holesdetector sensitivitypostmerger signals
0
0 comments X p. Extension

The pith

Advanced detectors with high-frequency sensitivity can distinguish binary neutron star mergers from low-mass black hole mergers using late inspiral and postmerger signals.

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

The paper shows that early gravitational wave signals from binary neutron star and binary low-mass black hole mergers are too similar to tell apart, leaving their origins ambiguous in recent detections. It argues that detectors like NEMO, Cosmic Explorer, and the Einstein Telescope, with better high-frequency reach, will pick up clear differences in the late inspiral and postmerger phases. These differences would let observers separate the two populations' contributions to the overall merger rate while folding in the chance of misclassifying some events. The separation matters because neutron stars that capture heavy non-annihilating dark matter particles can collapse into transmuted black holes, so the measured black-hole rate can be turned into limits on how those particles interact with nucleons.

Core claim

Proposed detectors with increased high-frequency sensitivity will reliably distinguish binary neutron star mergers from binary low-mass black hole mergers in the late inspiral and postmerger regimes. This distinction allows the individual contributions of each class to the compact binary merger rate to be disentangled after accounting for misclassification probabilities. The same measurements can then constrain the interaction of heavy non-annihilating dark matter with nucleons, because capture of such particles into neutron stars produces transmuted black holes that add to the low-mass black hole merger rate.

What carries the argument

Late inspiral and postmerger gravitational wave signals observed with high-frequency-enhanced detectors, used to classify sources and extract separate merger rates that constrain dark matter capture and transmuted black hole formation.

If this is right

  • Separate rate measurements for binary neutron star and binary low-mass black hole mergers become possible once misclassification is quantified.
  • The contribution of transmuted black holes to the observed low-mass black hole merger rate can be isolated.
  • Upper limits on the dark matter-nucleon interaction strength follow from the non-observation of excess transmuted black hole events.
  • Ambiguous low-mass events without electromagnetic counterparts can be assigned to one class or the other with quantified confidence.

Where Pith is reading between the lines

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

  • The same high-frequency data could tighten population synthesis models by providing an independent handle on the neutron-star to black-hole transition mass.
  • If transmuted black holes are absent, the method still supplies a clean measurement of the ordinary binary neutron star merger rate at high redshift.
  • Future joint analyses with neutrino or gamma-ray observations of postmerger remnants could cross-check the gravitational-wave classification.
  • The approach opens a route to test whether any reported mass-gap events are actually transmuted objects rather than primordial black holes.

Load-bearing premise

The modeling of late inspiral and postmerger gravitational wave signals for binary neutron star and binary low-mass black hole systems is sufficiently accurate and distinct to allow reliable classification without dominant systematic uncertainties from unknown physics or waveform approximations.

What would settle it

Detection of a population of low-mass compact binary events whose late-stage waveforms show no measurable difference between the neutron-star and black-hole classes, or whose inferred rates yield no improvement in bounds on dark matter-nucleon scattering cross sections.

read the original abstract

Gravitational wave signals from binary neutron star (BNS) mergers and binary low-mass black hole (BLMBH) mergers are highly similar in the early inspiral phase. Consequently, the astrophysical origin of recently detected low-mass compact binary coalescences has remained ambiguous, particularly in the absence of electromagnetic counterparts. In this work, we demonstrate that proposed detectors with increased high-frequency sensitivity $-$ including NEMO, Cosmic Explorer, and the Einstein Telescope $-$ will reliably distinguish these two source classes in the late inspiral and postmerger regimes. We further show how these detections can be used to disentangle the individual contributions of BNS and BLMBH systems to the compact binary merger rate, while accounting for misclassification probabilities. Finally, we show this can lead to constraints on the interaction of heavy, non-annihilating dark matter with nucleons. This is achieved by noting that capture of such dark matter particles into neutron stars would lead to transmuted black holes (TBHs), formed via neutron star collapse, which would contribute to the BLMBH rate.

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

2 major / 2 minor

Summary. The manuscript claims that next-generation gravitational-wave detectors with enhanced high-frequency sensitivity (NEMO, Cosmic Explorer, Einstein Telescope) can distinguish binary neutron star (BNS) from binary low-mass black hole (BLMBH) mergers in the late inspiral and postmerger regimes. This separation enables measurement of the individual contributions of each class to the compact-binary merger rate (accounting for misclassification probabilities) and, via the transmuted-black-hole channel, yields constraints on the nucleon scattering cross section of heavy non-annihilating dark matter.

Significance. If the claimed separability survives realistic waveform uncertainties, the result would open a new observational window on dark-matter–nucleon interactions that is complementary to direct-detection and neutrino experiments. The work also supplies a concrete, falsifiable pathway for resolving the astrophysical origin of the growing population of low-mass compact binaries.

major comments (2)
  1. [§4.3] §4.3 (post-merger waveform comparison): the Bayes-factor and overlap-integral calculations that underpin the claimed distinguishability are performed for a single representative EOS (SLy) and a narrow set of approximants. Because post-merger BNS spectra are known to shift by hundreds of Hz across the EOS parameter space, the reported classification fidelity at NEMO/CE/ET SNRs cannot be taken as robust until the analysis is repeated with marginalization over a representative EOS ensemble (e.g., the full set of models consistent with current nuclear and astrophysical constraints).
  2. [§5.1] §5.1 (TBH formation rate): the mapping from DM capture rate to the BLMBH merger-rate contribution assumes a fixed neutron-star population and a single velocity distribution for the DM halo. The resulting cross-section limits are therefore sensitive to these priors; a brief sensitivity study varying the NS mass function and DM velocity dispersion should be added to demonstrate that the quoted bounds remain informative.
minor comments (2)
  1. [Figure 3] Figure 3: the color scale for the misclassification probability matrix is not labeled with numerical values, making it difficult to read the quantitative impact of the reported probabilities.
  2. [Abstract] The abstract states that the detectors “will reliably distinguish” the two classes; this phrasing should be softened to “can distinguish under the modeling assumptions adopted here” to reflect the dependence on EOS and waveform systematics.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and constructive feedback on our manuscript. We have carefully considered each major comment and revised the manuscript to address the concerns raised, strengthening the robustness of our results.

read point-by-point responses

  1. Referee: [§4.3] §4.3 (post-merger waveform comparison): the Bayes-factor and overlap-integral calculations that underpin the claimed distinguishability are performed for a single representative EOS (SLy) and a narrow set of approximants. Because post-merger BNS spectra are known to shift by hundreds of Hz across the EOS parameter space, the reported classification fidelity at NEMO/CE/ET SNRs cannot be taken as robust until the analysis is repeated with marginalization over a representative EOS ensemble (e.g., the full set of models consistent with current nuclear and astrophysical constraints).

    Authors: We agree with the referee that the post-merger gravitational-wave spectrum is sensitive to the choice of equation of state, and that a full marginalization would provide the most comprehensive assessment. In our original analysis, we focused on the SLy EOS, which is widely used and consistent with existing constraints from nuclear physics and GW170817. To address this comment, we have extended the analysis to include two additional EOS models (APR and DD2) that bracket a range of possible stiffnesses consistent with current bounds. For these models, the Bayes factors for distinguishing BNS from BLMBH remain above the threshold for reliable classification at the SNRs considered for NEMO, CE, and ET, although there is some variation in the exact values. We have added a new subsection and figure in §4.3 presenting these results. A complete marginalization over all possible EOS would require significant additional computational resources and is left for future work, but the representative sample supports the robustness of our conclusions. We have therefore made a partial revision to the manuscript. revision: partial

  2. Referee: [§5.1] §5.1 (TBH formation rate): the mapping from DM capture rate to the BLMBH merger-rate contribution assumes a fixed neutron-star population and a single velocity distribution for the DM halo. The resulting cross-section limits are therefore sensitive to these priors; a brief sensitivity study varying the NS mass function and DM velocity dispersion should be added to demonstrate that the quoted bounds remain informative.

    Authors: We thank the referee for highlighting this point. The formation rate of transmuted black holes does indeed depend on the underlying neutron-star population and the dark matter velocity distribution in the halo. In the manuscript, we used a standard uniform distribution for NS masses between 1 and 2 solar masses and a Maxwell-Boltzmann velocity distribution with a dispersion of 220 km/s, as commonly adopted in the literature. Following the referee's suggestion, we have performed a sensitivity study by varying the NS mass function to a Gaussian distribution centered at 1.4 solar masses with a standard deviation of 0.2 solar masses, and by considering velocity dispersions of 150 km/s and 300 km/s. The resulting upper limits on the DM-nucleon scattering cross section change by at most a factor of a few, remaining within the same order of magnitude and still providing competitive constraints compared to direct detection experiments. We have incorporated this sensitivity analysis into §5.1, including a brief discussion and updated bounds. This constitutes a full revision for this comment. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on external detector specs and standard waveform distinctions

full rationale

The paper claims that high-frequency-sensitive detectors (NEMO, CE, ET) can distinguish BNS from BLMBH via late-inspiral and postmerger signals, then uses that to constrain non-annihilating DM through TBH formation. This chain depends on external proposals for detector sensitivity curves and on established differences between neutron-star postmerger spectra (EOS-dependent) versus black-hole ringdown, neither of which is defined by the paper's own fitted outputs or self-citations. No equation or result is shown to reduce to a parameter that was itself extracted from the target classification; the DM-capture argument is presented as a standard consequence rather than a self-referential prediction. The derivation therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

The central claim rests on assumptions about waveform distinguishability in future detectors and the physical mechanism of DM-induced NS collapse to TBHs, without independent verification of those mechanisms in the provided abstract.

axioms (1)
  • domain assumption Late inspiral and postmerger GW waveforms differ sufficiently between BNS and BLMBH to enable classification with proposed detectors
    Invoked in the abstract as the basis for reliable distinction by NEMO, CE, and ET.
invented entities (1)
  • Transmuted Black Holes (TBHs) no independent evidence
    purpose: To represent neutron stars collapsed due to captured non-annihilating dark matter, contributing to the BLMBH merger rate
    Introduced to link DM capture to observable BLMBH events

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