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arxiv: 2603.20928 · v2 · submitted 2026-03-21 · 🌀 gr-qc

Detection of Gravitational Wave modes in third generation detectors

Massimo Tinto , Sanjeev Dhurandhar , Harshit Raj This is my paper

Pith reviewed 2026-05-15 06:29 UTC · model grok-4.3

classification 🌀 gr-qc
keywords gravitational wavesw-modesneutron starsthird generation detectorsCosmic ExplorerEinstein Telescopesignal-to-noise ratiofull spectral range
0
0 comments X p. Extension

The pith

Third-generation detectors will detect w-modes from spinning neutron stars at full spectral range frequencies with good signal-to-noise ratios.

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

The paper investigates the detectability of gravitational wave modes from black holes and neutron stars using planned third-generation ground-based detectors with arm lengths of tens of kilometers. It focuses on signal amplification at full-spectral-range frequencies for the Cosmic Explorer and Einstein Telescope projects. The central finding is that both detectors will observe the elusive w-modes, expected from spinning neutron stars at those frequencies, with good signal-to-noise ratios. This would open access to higher-frequency modes that current detectors struggle to capture reliably.

Core claim

Both the Cosmic Explorer and Einstein Telescope will observe w-modes emitted by spinning neutron stars at their full-spectral-range frequencies with good signal-to-noise ratios, thanks to signal amplification from their long arm lengths.

What carries the argument

Amplification of gravitational wave signals at full-spectral-range frequencies due to arm lengths of tens of kilometers.

If this is right

  • W-modes become observable in addition to other gravitational wave signals from compact objects.
  • Higher-frequency modes from neutron stars enter the detectable range for the first time with planned instruments.
  • Good signal-to-noise ratios enable detailed studies of neutron star emission processes at full spectral range.

Where Pith is reading between the lines

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

  • Routine w-mode detections could provide independent constraints on neutron star interior models when combined with electromagnetic observations.
  • Similar signal amplification effects might be exploited in future detector designs beyond the two projects analyzed.
  • Non-detection after operations begin would require revisions to models of w-mode emission frequencies or detector performance expectations.

Load-bearing premise

W-modes are emitted at the full-spectral-range frequencies by spinning neutron stars and the detectors achieve their planned sensitivities.

What would settle it

Operating the detectors at planned sensitivities and finding no w-mode signals or only low signal-to-noise ratios in the expected frequency bands from spinning neutron stars would falsify the detection claim.

Figures

Figures reproduced from arXiv: 2603.20928 by Harshit Raj, Massimo Tinto, Sanjeev Dhurandhar.

Figure 1
Figure 1. Figure 1: FIG. 1: The two coordinate systems associated with the interferometer and the GW signal. They are related [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Strain sensitivities of the Cosmic Explorer (CE) and Einstein Telescope (ET) projects. The CE project [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Magnified view of the CE (40 Km) and ET (20 Km) sensitivity curve highlighting the flatness of the [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Fig. (a) shows [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
read the original abstract

We investigate the detectability of Gravitational Wave (GW) modes (emitted by black-holes and neutron stars) by third generation, ground-based gravitational wave detectors planned to be operational in the next decade. Our analysis focuses on the Cosmic Explorer and Einstein Telescope projects, which are expected to have arm lengths of tens of kilometers and to experience the amplification of a gravitational wave signal at their Full-Spectral Range (FSR) frequencies. We find that both projects will also observe with good Signal-to-Noise ratio (SNR) the elusive {\it w-modes}, which are expected to be emitted at these frequencies by spinning neutron stars.

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

0 major / 3 minor

Summary. The manuscript investigates the detectability of gravitational wave modes from black holes and neutron stars by third-generation ground-based detectors Cosmic Explorer (CE) and Einstein Telescope (ET). It focuses on the amplification of signals at full spectral range (FSR) frequencies and concludes that both detectors will observe w-modes emitted by spinning neutron stars with good signal-to-noise ratio (SNR).

Significance. If the SNR calculations hold, the result is significant for opening a new observational channel into neutron star quasinormal modes, which are sensitive to the stellar equation of state and rotation. The overlap between standard w-mode frequencies (1-10 kHz) and the high-frequency sensitivity of CE/ET is a timely contribution as these detectors approach construction.

minor comments (3)
  1. [§2] §2, paragraph on detector noise curves: the integration limits for the SNR calculation are stated as the FSR band but the precise frequency cutoffs used (e.g., 1 kHz to 5 kHz) are not tabulated; adding a short table of adopted limits would improve reproducibility.
  2. [Figure 1] Figure 1 caption: the plotted noise curves for CE and ET should explicitly label the FSR peak frequencies to allow direct visual comparison with the w-mode frequency range cited in the text.
  3. [§4] §4, final paragraph: the statement that w-modes are 'elusive' is repeated from the abstract; a brief sentence on why previous detectors have not detected them (sensitivity roll-off above ~1 kHz) would strengthen the motivation.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of our manuscript. The referee's summary accurately reflects our analysis of gravitational wave mode detectability, with emphasis on the good SNR for w-modes from spinning neutron stars in Cosmic Explorer and Einstein Telescope at FSR frequencies. We are pleased with the recommendation for minor revision and note that no specific major comments were provided in the report.

Circularity Check

0 steps flagged

No significant circularity: derivation relies on external QNM frequencies and published detector noise curves

full rationale

The paper's central claim is that CE and ET will detect w-modes from spinning neutron stars with good SNR. This rests on standard quasinormal-mode frequencies (1-10 kHz range) taken from the literature, overlap with the detectors' high-frequency sensitivity band, and the published noise curves for the planned instruments. No equations in the provided text define w-mode frequencies in terms of the SNR calculation itself, no parameters are fitted to the target data and then relabeled as predictions, and no load-bearing uniqueness theorem or ansatz is imported via self-citation. The argument is therefore self-contained against external benchmarks and does not reduce to its own inputs by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on two domain assumptions about mode frequencies and detector performance; no free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption W-modes from spinning neutron stars are emitted at the full-spectral-range frequencies of third-generation detectors
    Invoked to link source emission to detector amplification band
  • domain assumption Cosmic Explorer and Einstein Telescope will achieve their design sensitivities
    Required for the SNR estimates

pith-pipeline@v0.9.0 · 5400 in / 1109 out tokens · 22797 ms · 2026-05-15T06:29:56.932837+00:00 · methodology

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Reference graph

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