Pith. sign in

REVIEW 3 major objections 4 minor 65 references

This paper forecasts how many neutron-star mergers with electromagnetic counterparts—bright sirens—the Einstein Telescope would need to detect for a gravitational-wave measurement of the Hubble constant H0 to match the precision of today's

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 09:52 UTC pith:XNMDWKOB

load-bearing objection Clean, well-scoped ET forecast that puts concrete numbers on known ideas — ~90 low-z bright sirens alone, ~20 with BAO, to reach σ_H0 ≈ 1 — and deserves peer review with requests for realization scatter and EM-selection sensitivity tests. the 3 major comments →

arxiv 2607.20413 v1 pith:XNMDWKOB submitted 2026-07-22 astro-ph.CO

The road towards precision measurements of H₀ with bright sirens in the Einstein Telescope era

Chiara De Leo , Elsa M. Teixeira , Vivian Poulin This is my paper
classification astro-ph.CO
keywords gravitational wavesbright sirensHubble constantHubble tensionEinstein Telescopebinary neutron starsbaryon acoustic oscillationscosmological forecasts
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.

This paper forecasts how many neutron-star mergers with electromagnetic counterparts—bright sirens—the Einstein Telescope would need to see for a gravitational-wave measurement of the Hubble constant H0 to match today's best cosmological precision. The central result is a set of event-count requirements: about 90 nearby bright sirens alone for σ_H0≈1 km/s/Mpc, and about 45 for 2 km/s/Mpc; when a future galaxy-survey BAO measurement is added to break the H0–Ωm degeneracy, these drop to roughly 20 and 15. The numbers matter because bright sirens measure distances directly from gravity-wave waveforms and redshifts from the counterpart, so they are calibrated by physics rather than by the distance ladder. If the forecasts hold, a future bright-siren catalogue could deliver a genuinely independent check of the Hubble tension.

Core claim

The paper shows that, in a flat ΛCDM cosmology, the constraining power of bright sirens on H0 is concentrated at low redshift when used alone: the luminosity distance becomes increasingly sensitive to Ωm and statistically noisier at higher redshift, so sources beyond z∼1 add little once Ωm is left free. This is quantified by a binned and a cumulative redshift analysis, both of which show a plateau in the H0 uncertainty around z∼1. When a mock BAO measurement is added, the H0–Ωm degeneracy is broken, the informative redshift range extends to z∼2, and far fewer events are required: roughly 20 bright sirens for σ_H0≈1 km/s/Mpc and 15 for σ_H0≈2 km/s/Mpc, compared with about 90 and 45 in the bri

What carries the argument

The carrying machinery is the mock bright-siren catalogue: binary-neutron-star mergers distributed in redshift by an assumed merger rate, with gravitational-wave luminosity distances and errors computed for an Einstein-Telescope-like triangular configuration using an SNR threshold of 20. Redshifts are assigned only to events whose electromagnetic afterglow would be detectable, modeled as an inclination cut of ι<18°. The likelihood combines each event's d_L and z in a Bayesian fit to H0 and Ωm; the H0–Ωm degeneracy in the luminosity distance is the mechanism that makes high-redshift events uninformative, and a mock BAO measurement of d_M/r_d and d_H/r_d is what breaks it.

Load-bearing premise

The forecast assumes that every binary-neutron-star merger with inclination below 18° has a detectable electromagnetic counterpart, so the number of bright sirens in each mock catalogue is fixed by that selection cut; if real counterpart recovery is rarer, all required event counts rise.

What would settle it

Take the first 20 Einstein-Telescope-era binary-neutron-star mergers with identified counterparts and measure H0 from them with a BAO prior; if the resulting 1σ uncertainty is visibly larger than 1 km/s/Mpc, the assumed counterpart-detection fraction or distance errors are too optimistic. Alternatively, count the actual fraction of ET detections with detected afterglows and compare it with the ι<18° expectation.

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

If this is right

  • If roughly 20 bright sirens with counterparts are observed in the Einstein Telescope era and combined with BAO data, the resulting H0 uncertainty would be comparable to current CMB and distance-ladder measurements, but obtained without either calibration.
  • Bright-siren-only programmes would require catalogues of about 45–90 low-redshift events, so focusing electromagnetic follow-up on z≲1 mergers is the efficient strategy when no external probe is used.
  • The H0–Ωm degeneracy, not detector sensitivity alone, sets the useful redshift reach of bright sirens; adding BAO roughly quadruples the information each event contributes to H0.
  • The results set a concrete target for the ET era: roughly 15–20 identified counterparts is the threshold at which bright sirens become a sharp test of the Hubble tension.

Where Pith is reading between the lines

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

  • [inference] If real counterpart identification is rarer than the inclination cut assumes, the required event counts scale upward; re-running the forecast with a full afterglow and kilonova detectability model would map that sensitivity.
  • [inference] The abrupt improvement near 10 events in the BAO-combined case reflects one catalogue realisation; averaging over many mock draws would give a more robust expected requirement and its scatter.
  • [inference] Because the BAO prior used here avoids sound-horizon calibration, the 15–20 event target is already independent of early-universe assumptions; adding a future sound-horizon measurement would sharpen it further.
  • [inference] A practical observing strategy follows: in the ET era, prioritise low-redshift mergers when no BAO-like prior is available, but with galaxy-survey data, intermediate-redshift counterparts also become worth chasing.

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

3 major / 4 minor

Summary. The paper forecasts how many bright-siren binary neutron star (BNS) detections with the Einstein Telescope, accompanied by electromagnetic counterparts, would be required to measure H0 with σ_H0 ≈ 1 and 2 km/s/Mpc in a flat ΛCDM cosmology. The authors build mock catalogues with an ET triangular configuration, SNR>20, a redshift-dependent merger rate, and GW170817 as the N=1 reference. EM detectability is modelled by an inclination cut ι<18° motivated by earlier afterglow modelling. They analyse the mocks both with bright sirens alone (restricting to 0.1<z≤1 after a saturation diagnostic) and with an SKAO-like BAO mock, sampling H0 and Ωm (and rd when BAO is added). The headline results are that ~90 and ~45 BSs suffice for σ_H0 ≈ 1 and 2 km/s/Mpc in the BS-only case, while with BAO ~20 and ~15 BSs suffice (Sections 5.2–5.3, Fig. 4).

Significance. If these numbers are robust, they provide an actionable target for ET-era bright-siren cosmology and quantify the value of combining standard sirens with BAO to break the H0–Ωm degeneracy. The paper has genuine strengths: the redshift-bin and cumulative analyses are internally consistent, the mock pipeline and analysis code (CANDI, GWFish, Cobaya) are public, and the authors are transparent about the realization-driven N=10 knee and the z>0.1 lower cut. The conclusion that low-redshift events dominate BS-only H0 constraints is physically plausible and consistent with earlier dark-siren studies. The concerns raised below concern the EM selection-function model and the statistical robustness of the exact N values; these are fixable within the scope of the paper.

major comments (3)
  1. [§3.2 and §5.3] The central BAO-improved claim (N≈20/15) relies on sources out to z≈2–3 in Fig. 3(b) and Fig. 4(b), but EM detectability is modelled as a redshift-independent inclination cut ι<18° (Section 3.2). The equivalence cited from De Leo et al. (2025) was established for the total number of detectable counterparts, not for the joint (ι,z) selection function. Real afterglow detection is flux-limited: at fixed inclination, high-redshift afterglows are fainter and harder to detect, so the adopted cut likely overestimates the high-z tail of the bright-siren catalogue — exactly the tail that drives the BAO-improved result. The paper does not test this redshift dependence. I recommend including a redshift-dependent EM detection efficiency (e.g., based on afterglowpy fluxes and an LSST-like limiting magnitude) or, at minimum, a conservative sensitivity test with the high-z catalogue truncated to z≲1.5–
  2. [§5.2, §5.3, Fig. 4] The headline N values are point estimates from a single progressive random draw from the master catalogue. The authors explicitly note that the sharp knee at N=10 in Fig. 4(b) is realization-driven, but they do not quantify how much σ_H0(N) fluctuates across realizations for any N. For small catalogues (N≈15–20), a single well-measured event can significantly shift the inferred precision, so the stated 20/15 thresholds may vary substantially from realization to realization. I recommend repeating the catalogue construction over many random draws and reporting the median and scatter (e.g., 68% interval) of σ_H0(N), so the reader can assess whether the sub-1-km/s threshold is reached robustly at N=20 or only in a particular realization.
  3. [§4] The likelihood in Eq. (12) uses a diagonal covariance matrix and explicitly neglects correlated systematic uncertainties such as a common detector-calibration error. For the target σ_H0 ≈ 1 km/s/Mpc, a percent-level common distance calibration error is comparable to the claimed statistical reach (1% in distance corresponds to ~0.7 km/s/Mpc at the fiducial H0≈67.7). The forecast should either specify the assumed calibration uncertainty, marginalize over a calibration nuisance parameter, or demonstrate that the required N is insensitive to realistic calibration errors. Without this, the absolute numbers (90 vs 45 and 20 vs 15) are not robust to a known systematic that is important at the precision the paper targets.
minor comments (4)
  1. [§5.2, abstract] The phrase 'low-redshift BSs' refers specifically to 0.1<z≤1.0 plus GW170817. Because the master catalogue has no events below z=0.1, the forecast does not sample the very local population; the text notes this limitation, but the abstract and conclusions should state the redshift range in the same sentence for clarity.
  2. [Fig. 2] The labels showing the number of events in each bin are difficult to parse with the current plot formatting. A companion table listing N per redshift bin for each catalogue would aid reproducibility.
  3. [References] There are two 'Abac et al. 2026' entries with different arXiv numbers (2605.27223 and the JCAP 2026/03/081). Disambiguate them (e.g., 'Abac, A., et al. 2026a,b') to avoid confusion.
  4. [§5.2] The paper reports σ_H0≈1 and 2 km/s/Mpc as target precisions but does not state the actual posterior σ obtained at N=90 and N=45 in Fig. 4(a), nor at N=20 and N=15 in Fig. 4(b). Reporting the measured values would make the threshold statements more quantitative.

Circularity Check

0 steps flagged

No significant circularity; the forecast is a self-contained simulation study with only a mild reliance on prior work for the EM selection function.

full rationale

The central claim (N≈90/45 BS-only and ≈20/15 with BAO) is obtained by generating mock catalogues from explicit assumptions—merger rate, ET sensitivity, SNR threshold, inclination cut, fiducial Planck+BAO cosmology—and then running an MCMC likelihood analysis. The precision target is not an input to the simulation; it is read off the posterior width as a function of N. The only self-citation entering the pipeline is De Leo et al. (2025), used to justify replacing full afterglow detectability with an inclination cut ι<18° based on the total number of detectable counterparts. That equivalence is conditional and does not encode the H0 precision target, so the forecast numbers are not forced by construction. The paper itself flags the main limitations of the cut (z>0.1 lower bound, N=10 knee, redshift-independent EM selection), further indicating that the results are conditional assumptions rather than circular reductions. No fitted parameter is renamed as a prediction, and no uniqueness theorem is imported to forbid alternatives.

Axiom & Free-Parameter Ledger

7 free parameters · 6 axioms · 0 invented entities

The forecast introduces no invented physics. Its event-count targets depend on several chosen inputs: EM counterpart selection (inclination cut), ET sensitivity/SNR threshold, merger rate, neutron-star mass, and the BAO noise model. These are the quantities a reader would need to vary to test whether the 90/20 numbers hold.

free parameters (7)
  • Fiducial H0 and Ωm (mock injection cosmology) = H0=67.66 km/s/Mpc, Ωm=0.3111
    Taken from Planck+BAO; used to generate every mock event. Posterior widths can depend on these through noise realization, although the forecast is mainly about widths.
  • Fiducial sound-horizon scale rd in BAO mock = sampled with uniform prior [100,200] Mpc
    BAO distance ratios are generated using a chosen rd and then rd is sampled; the assumed rd affects the BAO likelihood normalization.
  • EM counterpart inclination cut = ι < 18°
    Calibrated to LSST afterglow detectability in De Leo et al. (2025); directly sets how many GW detections become bright sirens.
  • SNR detection threshold = SNR > 20
    Conservative ET detectability threshold from Branchesi et al. (2023); changes the detected catalogue.
  • Merger-rate function R(z) = 1+2z (z≤1); 3/4(5−z) (1<z<5); 0 (z≥5)
    From Cutler & Holz/Hogg et al.; sets the redshift distribution of simulated events.
  • Monochromatic neutron-star mass = 1.4 M_sun
    Assumed for all injections; affects distance uncertainty and SNR.
  • Redshift range of master catalogue = 0.1 < z < 3.5; BS-only restricted to 0.1 < z ≤ 1
    Chosen to match ET BNS range; excludes very local population except GW170817.
axioms (6)
  • domain assumption Flat ΛCDM expansion history (Eqs. 1 and 9).
    All mocks and likelihoods assume no curvature and no beyond-ΛCDM physics; central to the H0–Ωm degeneracy statement.
  • domain assumption Gaussian, diagonal likelihood for GW distances; no common calibration systematics.
    Section 4; if detector calibration errors are correlated, the forecast precision is overestimated.
  • ad hoc to paper EM detectability is equivalent to an inclination cut ι<18°.
    Section 3.2; based on afterglowpy+LSST modeling in De Leo et al. (2025); kilonovae and other counterpart channels are ignored.
  • domain assumption Merger rate R(z) from Cutler & Holz with source-frame to observer-frame conversion.
    Section 3.2; adopted from astrophysical population synthesis, not fit here.
  • domain assumption Gaussian approximation for GW170817 distance uncertainty despite published asymmetric errors.
    Section 3.2 note; relevant for the smallest catalogues.
  • domain assumption BAO mock errors follow the optimistic SKA2 configuration from Bull (2016).
    Section 3.3; if SKAO performs worse, the N=20 number degrades.

pith-pipeline@v1.3.0-alltime-deepseek · 14410 in / 12431 out tokens · 96760 ms · 2026-08-01T09:52:41.281918+00:00 · methodology

0 comments
read the original abstract

Gravitational-wave standard sirens provide an independent probe of cosmic expansion since their luminosity distances are inferred directly from the gravitational-wave signal and, for bright sirens (BSs), the source redshifts are obtained through the identification of electromagnetic counterparts. In this work, we forecast the constraining power of future bright siren catalogues on the Hubble constant using simulated binary-neutron-star mergers detected by the Einstein Telescope with associated electromagnetic counterparts. We construct mock catalogues with different numbers of events and redshift distributions, with GW170817 as a reference BS, and analyse the resulting constraints within a flat $\Lambda$CDM cosmology. We find that, when bright sirens are used as a standalone probe, most of the information on $H_0$ is provided by low-redshift events, with the improvement in precision saturating for sources above $z \sim 1$; beyond that redshift, the constraining power of BSs is increasingly limited by the degeneracy with $\Omega_m$, which prevents further gains in precision on $H_0$. In this case, approximately $90$ low-redshift BSs are required to reach $\sigma_{H_0} \sim 1\,{\rm km\,s^{-1}\,Mpc^{-1}}$, while about $45$ are sufficient for $\sigma_{H_0} \sim 2\,{\rm km\,s^{-1}\,Mpc^{-1}}$. When external BAO information is included to reduce the $H_0 - \Omega_m$ degeneracy, intermediate-redshift sirens become more informative and the required number of events decreases substantially, to roughly $20$ and $15$ BSs for $\sigma_{H_0} \sim 1\,{\rm km\,s^{-1}\,Mpc^{-1}}$ and $\sigma_{H_0} \sim 2\,{\rm km\,s^{-1}\,Mpc^{-1}}$, respectively. These results highlight the importance of both electromagnetic counterpart identification and complementary background probes in making BSs a competitive, distance-ladder-independent test of the Hubble tension.

Figures

Figures reproduced from arXiv: 2607.20413 by Chiara De Leo, Elsa M. Teixeira, Vivian Poulin.

Figure 1
Figure 1. Figure 1: — Posterior probability distribution of H0 inferred from GW170817, compared with the SH0ES-calibrated Pantheon+ H0 (purple) measurement, the value constrained from Planck under a ΛCDM cosmology (blue) and the posterior obtained using 20 mock bright-siren events alone (dashed orange) and analysed with external BAO information (dashed green). The mocks are generated following the prescriptions described in S… view at source ↗
Figure 2
Figure 2. Figure 2: — Variance of the inferred H0 posterior as a function of redshift bin for three mock bright siren catalogues containing N = 30, N = 45, and N = 60 events. The events are divided into six equally spaced redshift bins centred at zcent and the labels indicate the number of events in each bin. Panel (a) shows the results obtained when only BS data are included, while panel (b) shows the corresponding results w… view at source ↗
Figure 3
Figure 3. Figure 3: — Marginalised uncertainty on H0 as a function of the maximum catalogue redshift threshold zmax, for catalogues containing N = 30 and N = 60 events. Each point includes all events with z ≤ zmax. Panel (a) shows the results obtained when only BS data are analysed, while panel (b) shows the corresponding results when complementary BAO information is included. 1 2 5 20 30 45 75 90 Number of BS 65 70 75 80 85 … view at source ↗
Figure 4
Figure 4. Figure 4: — Constraints on H0 as a function of the total number of bright sirens, including GW170817. Panel (a) uses bright siren catalogues restricted to the redshift range 0.1 < z ≤ 1.0, with both H0 and Ωm being sampled. Panel (b) combines catalogues extending to z ≤ 3 with external information from the SKAO BAO mock catalogue, while varying H0, Ωm and rd. The purple bands show the SH0ES-Pantheon+ constraint, wit… view at source ↗
Figure 5
Figure 5. Figure 5: — Two-dimensional constraints in the H0–Ωm plane obtained from BS catalogues containing NBS = 1, 20, 45, and 90 events, together with the constraint from the NBS = 20 catalogue combined with BAO measurements. The darker and lighter coloured contours refer to the 1σ and 2σ intervals, respectively. The NBS = 1 case corresponds to GW170817, while the remaining catalogues are constructed by progressively addin… view at source ↗

discussion (0)

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

Reference graph

Works this paper leans on

65 extracted references · 1 canonical work pages

  1. [1]

    De Leo, Chiara and Martinelli, Matteo and D'Agostino, Rocco and Gianfagna, Giulia and Martins, Carlos J. A. P. Distinguishing Distance Duality breaking models using electromagnetic and gravitational waves measurements. 2025. arXiv:2505.13613

    arXiv 2025

  2. [2]

    The Local Distance Network: A community consensus report on the measurement of the Hubble constant at 1 \

    Casertano, Stefano and others. The Local Distance Network: A community consensus report on the measurement of the Hubble constant at 1 \. Astron. Astrophys. 2026. doi:10.1051/0004-6361/202557993. arXiv:2510.23823

    Pith/arXiv arXiv 2026

  3. [3]

    and Daniel, Richard and Frusciante, Noemi and van de Bruck, Carsten

    Teixeira, Elsa M. and Daniel, Richard and Frusciante, Noemi and van de Bruck, Carsten. Forecasts on interacting dark energy with standard sirens. Phys. Rev. D. 2023. doi:10.1103/PhysRevD.108.084070. arXiv:2309.06544

    Pith/arXiv arXiv 2023

  4. [4]

    Current and future constraints on the expansion history of the GREA model

    Graziotti, Irene and De Leo, Chiara and Martinelli, Matteo. Current and future constraints on the expansion history of the GREA model. 2026. arXiv:2603.01934

    Pith/arXiv arXiv 2026

  5. [5]

    Illuminating the dark sector: understanding modified gravity signatures with cross-correlations of Gravitational Waves and Large-Scale Structure

    De Leo, Chiara and Ca \ n as-Herrera, Guadalupe and Balaudo, Anna and Martinelli, Matteo and Silvestri, Alessandra and Baker, Tessa. Illuminating the dark sector: understanding modified gravity signatures with cross-correlations of Gravitational Waves and Large-Scale Structure. JCAP. 2026. doi:10.1088/1475-7516/2026/05/038. arXiv:2512.19186

    Pith/arXiv arXiv 2026

  6. [6]

    Model-Independent Test of Prerecombination New Physics: Measuring the Sound Horizon with Gravitational Wave Standard Sirens and the Baryon Acoustic Oscillation Angular Scale

    Giar \`e , William and Betts, Jonathan and van de Bruck, Carsten and Di Valentino, Eleonora. Model-Independent Test of Prerecombination New Physics: Measuring the Sound Horizon with Gravitational Wave Standard Sirens and the Baryon Acoustic Oscillation Angular Scale. Phys. Rev. Lett. 2025. doi:10.1103/k6mg-g23d. arXiv:2406.07493

    Pith/arXiv arXiv 2025

  7. [7]

    Dark siren cosmology with binary black holes in the era of third-generation gravitational wave detectors

    Muttoni, Niccol \`o and Laghi, Danny and Tamanini, Nicola and Marsat, Sylvain and Izquierdo-Villalba, David. Dark siren cosmology with binary black holes in the era of third-generation gravitational wave detectors. Phys. Rev. D. 2023. doi:10.1103/PhysRevD.108.043543. arXiv:2303.10693

    Pith/arXiv arXiv 2023

  8. [8]

    and Tanvir, Nial R

    Hjorth, Jens and Levan, Andrew J. and Tanvir, Nial R. and Lyman, Joe D. and Wojtak, Radosław and Schrøder, Sophie L. and Mandel, Ilya and Gall, Christa and Bruun, Sofie H. , year=. The Distance to NGC 4993: The Host Galaxy of the Gravitational-wave Event GW170817 , volume=. The Astrophysical Journal , publisher=. doi:10.3847/2041-8213/aa9110 , number=

    doi:10.3847/2041-8213/aa9110 2041

  9. [9]

    and Giar \`e , William and Hogg, Natalie B

    Teixeira, Elsa M. and Giar \`e , William and Hogg, Natalie B. and Montandon, Thomas and Poudou, Ad \`e le and Poulin, Vivian. Implications of distance duality violation for the H0 tension and evolving dark energy. Phys. Rev. D. 2025. doi:10.1103/zzmp-rxrh. arXiv:2504.10464

    Pith/arXiv arXiv 2025

  10. [10]

    and Kunz, Martin

    Bassett, Bruce A. and Kunz, Martin. Cosmic distance-duality as a probe of exotic physics and acceleration. Phys. Rev. D. 2004. doi:10.1103/PhysRevD.69.101305. arXiv:astro-ph/0312443

    Pith/arXiv arXiv 2004

  11. [11]

    and Martinelli, Matteo and Nesseris, Savvas

    Renzi, Fabrizio and Hogg, Natalie B. and Martinelli, Matteo and Nesseris, Savvas. Strongly lensed supernovae as a self-sufficient probe of the distance duality relation. Phys. Dark Univ. 2021. doi:10.1016/j.dark.2021.100824. arXiv:2010.04155

    arXiv 2021

  12. [12]

    and Verde, Licia and Jimenez, Raul

    Avgoustidis, A. and Verde, Licia and Jimenez, Raul. Consistency among distance measurements: transparency, BAO scale and accelerated expansion. JCAP. 2009. doi:10.1088/1475-7516/2009/06/012. arXiv:0902.2006

    Pith/arXiv arXiv 2009

  13. [13]

    Constraints on cosmic opacity and beyond the standard model physics from cosmological distance measurements

    Avgoustidis, Anastasios and Burrage, Clare and Redondo, Javier and Verde, Licia and Jimenez, Raul. Constraints on cosmic opacity and beyond the standard model physics from cosmological distance measurements. JCAP. 2010. doi:10.1088/1475-7516/2010/10/024. arXiv:1004.2053

    Pith/arXiv arXiv 2010

  14. [14]

    and Li, Zhengxiang

    Liao, Kai and Avgoustidis, A. and Li, Zhengxiang. Is the Universe Transparent?. Phys. Rev. D. 2015. doi:10.1103/PhysRevD.92.123539. arXiv:1512.01861

    Pith/arXiv arXiv 2015

  15. [15]

    and others

    Martinelli, M. and others. Euclid: Forecast constraints on the cosmic distance duality relation with complementary external probes. Astron. Astrophys. 2020. doi:10.1051/0004-6361/202039078. arXiv:2007.16153

    Pith/arXiv arXiv 2020

  16. [16]

    , keywords =

    Determining the Hubble constant from gravitational wave observations. , keywords =. doi:10.1038/323310a0 , adsurl =

    doi:10.1038/323310a0

  17. [17]

    , keywords =

    Using Gravitational-Wave Standard Sirens. , keywords =. doi:10.1086/431341 , archivePrefix =. astro-ph/0504616 , primaryClass =

    Pith/arXiv arXiv

  18. [18]

    , keywords =

    Missing Link: Bayesian detection and measurement of intermediate-mass black-hole binaries. , keywords =. doi:10.1103/PhysRevD.92.022002 , archivePrefix =. 1504.04766 , primaryClass =

    Pith/arXiv arXiv

  19. [19]

    Measuring the Hubble Constant with Neutron Star Black Hole Mergers , volume=

    Vitale, Salvatore and Chen, Hsin-Yu , year=. Measuring the Hubble Constant with Neutron Star Black Hole Mergers , volume=. Physical Review Letters , publisher=. doi:10.1103/physrevlett.121.021303 , number=

    doi:10.1103/physrevlett.121.021303

  20. [20]

    and Abbott, T

    Abbott, R. and Abbott, T. D. , year=. GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object , volume=. The Astrophysical Journal Letters , publisher=. doi:10.3847/2041-8213/ab960f , number=

    doi:10.3847/2041-8213/ab960f 2041

  21. [21]

    Abbott, B. P. and others , title =. Nature , volume =. 2017 , doi =. 1710.05835 , archivePrefix =

    Pith/arXiv arXiv 2017

  22. [22]

    , keywords =

    GW150914: First results from the search for binary black hole coalescence with Advanced LIGO. , keywords =. doi:10.1103/PhysRevD.93.122003 , archivePrefix =. 1602.03839 , primaryClass =

    Pith/arXiv arXiv

  23. [23]

    , keywords =

    Observation of Gravitational Waves from a Binary Black Hole Merger. , keywords =. doi:10.1103/PhysRevLett.116.061102 , archivePrefix =. 1602.03837 , primaryClass =

    Pith/arXiv arXiv

  24. [24]

    , keywords =

    Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A. , keywords =. doi:10.3847/2041-8213/aa920c , archivePrefix =. 1710.05834 , primaryClass =

    Pith/arXiv arXiv 2041

  25. [25]

    Abac, A. G. and others. 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

    Pith/arXiv arXiv 2025

  26. [26]

    GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog

    Abac, None and others. GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog. 2026. arXiv:2605.27223

    Pith/arXiv arXiv 2026

  27. [27]

    and Yuan, Wenlong and Macri, Lucas M

    Riess, Adam G. and Yuan, Wenlong and Macri, Lucas M. and Scolnic, Dan and Brout, Dillon and Casertano, Stefano and Jones, David O. and Murakami, Yukei and Anand, Gagandeep S. and Breuval, Louise and Brink, Thomas G. and Filippenko, Alexei V. and Hoffmann, Samantha and Jha, Saurabh W. and D’arcy Kenworthy, W. and Mackenty, John and Stahl, Benjamin E. and Z...

    2041

  28. [28]

    and Akrami, Y

    Aghanim, N. and Akrami, Y. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Ballardini, M. and Banday, A. J. and Barreiro, R. B. and Bartolo, N. and Basak, S. and Battye, R. and Benabed, K. and Bernard, J.-P. and Bersanelli, M. and Bielewicz, P. and Bock, J. J. and Bond, J. R. and Borrill, J. and Bouchet, F. R. and Boulanger, F. and Bucher, M. and B...

    2018

  29. [29]

    , keywords =

    The Science of the Einstein Telescope. , keywords =. doi:10.1088/1475-7516/2026/03/081 , archivePrefix =. 2503.12263 , primaryClass =

    Pith/arXiv arXiv 2026

  30. [30]

    , keywords =

    Science with the Einstein Telescope: a comparison of different designs. , keywords =. doi:10.1088/1475-7516/2023/07/068 , archivePrefix =. 2303.15923 , primaryClass =

    Pith/arXiv arXiv 2023

  31. [31]

    , keywords =

    Ultrahigh precision cosmology from gravitational waves. , keywords =. doi:10.1103/PhysRevD.80.104009 , archivePrefix =. 0906.3752 , primaryClass =

    Pith/arXiv arXiv

  32. [32]

    , keywords =

    Constraints on the distance duality relation with standard sirens. , keywords =. doi:10.1088/1475-7516/2020/12/019 , archivePrefix =. 2007.14335 , primaryClass =

    Pith/arXiv arXiv 2020

  33. [33]

    , keywords =

    Dancing in the dark: detecting a population of distant primordial black holes. , keywords =. doi:10.1088/1475-7516/2022/08/006 , archivePrefix =. 2205.02639 , primaryClass =

    Pith/arXiv arXiv 2022

  34. [34]

    Astronomy and Computing , keywords =

    GWFISH: A simulation software to evaluate parameter-estimation capabilities of gravitational-wave detector networks. Astronomy and Computing , keywords =. doi:10.1016/j.ascom.2022.100671 , archivePrefix =. 2205.02499 , primaryClass =

    arXiv 2022

  35. [35]

    Contribution to Gravitational-Wave Astronomy beyond LIGO

    Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO. Bulletin of the American Astronomical Society , year = 2019, volume =. doi:10.48550/arXiv.1907.04833 , archivePrefix =. 1907.04833 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1907.04833 2019

  36. [36]

    Annals of Physics , keywords =

    Lessons from the light of a neutron star merger. Annals of Physics , keywords =. doi:10.1016/j.aop.2019.167923 , adsurl =

    arXiv 2019

  37. [37]

    , keywords =

    What is the Most Promising Electromagnetic Counterpart of a Neutron Star Binary Merger?. , keywords =. doi:10.1088/0004-637X/746/1/48 , archivePrefix =. 1108.6056 , primaryClass =

    Pith/arXiv arXiv

  38. [38]

    Gamma-Ray Burst Afterglows in the Multimessenger Era: Numerical Models and Closure Relations , volume=

    Ryan, Geoffrey and Eerten, Hendrik van and Piro, Luigi and Troja, Eleonora , year=. Gamma-Ray Burst Afterglows in the Multimessenger Era: Numerical Models and Closure Relations , volume=. The Astrophysical Journal , publisher=. doi:10.3847/1538-4357/ab93cf , number=

    doi:10.3847/1538-4357/ab93cf

  39. [39]

    and Fong, W

    Rouco Escorial, A. and Fong, W. and Berger, E. and Laskar, T. and Margutti, R. and Schroeder, G. and Rastinejad, J. C. and Cornish, D. and Popp, S. and Lally, M. and Nugent, A. E. and Paterson, K. and Metzger, B. D. and Chornock, R. and Alexander, K. and Cendes, Y. and Eftekhari, T. , title =. 2023 , month =. doi:10.3847/1538-4357/acf830 , url =

    doi:10.3847/1538-4357/acf830 2023

  40. [40]

    and Berger, E

    Fong, W. and Berger, E. and Margutti, R. and Zauderer, B. A. , title =. 2015 , month =. doi:10.1088/0004-637X/815/2/102 , url =

    doi:10.1088/0004-637x/815/2/102 2015

  41. [41]

    The Astrophysical Journal Supplement Series , keywords =

    Optimization of the Observing Cadence for the Rubin Observatory Legacy Survey of Space and Time: A Pioneering Process of Community-focused Experimental Design. The Astrophysical Journal Supplement Series , keywords =. doi:10.3847/1538-4365/ac3e72 , archivePrefix =. 2108.01683 , primaryClass =

    Pith/arXiv arXiv

  42. [42]

    , keywords =

    Extending Cosmological Tests of General Relativity with the Square Kilometre Array. , keywords =. doi:10.3847/0004-637X/817/1/26 , archivePrefix =. 1509.07562 , primaryClass =

    Pith/arXiv arXiv

  43. [43]

    , keywords =

    Cosmology with Phase 1 of the Square Kilometre Array Red Book 2018: Technical specifications and performance forecasts. , keywords =. doi:10.1017/pasa.2019.51 , archivePrefix =. 1811.02743 , primaryClass =

    Pith/arXiv arXiv 2018

  44. [44]

    Cobaya: code for Bayesian analysis of hierarchical physical models , volume=

    Torrado, Jesús and Lewis, Antony , year=. Cobaya: code for Bayesian analysis of hierarchical physical models , volume=. Journal of Cosmology and Astroparticle Physics , publisher=. doi:10.1088/1475-7516/2021/05/057 , number=

    doi:10.1088/1475-7516/2021/05/057 2021

  45. [45]

    The Astrophysical Journal , keywords =

    Efficient Computation of Cosmic Microwave Background Anisotropies in Closed Friedmann-Robertson-Walker Models. The Astrophysical Journal , keywords =. doi:10.1086/309179 , archivePrefix =. astro-ph/9911177 , primaryClass =

    Pith/arXiv arXiv

  46. [46]

    2017 , eprint=

    Bayesian Methods in Cosmology , author=. 2017 , eprint=

    2017

  47. [47]

    JCAP , keywords =

    CMB power spectrum parameter degeneracies in the era of precision cosmology. JCAP , keywords =. doi:10.1088/1475-7516/2012/04/027 , archivePrefix =. 1201.3654 , primaryClass =

    Pith/arXiv arXiv 2012

  48. [48]

    Efficient sampling of fast and slow cosmological parameters

    Lewis, Antony. Efficient sampling of fast and slow cosmological parameters. Phys. Rev. D. 2013. doi:10.1103/PhysRevD.87.103529. arXiv:1304.4473

    Pith/arXiv arXiv 2013

  49. [49]

    Cosmological parameters from CMB and other data: A Monte Carlo approach

    Lewis, Antony and Bridle, Sarah. Cosmological parameters from CMB and other data: A Monte Carlo approach. Phys. Rev. D. 2002. doi:10.1103/PhysRevD.66.103511. arXiv:astro-ph/0205436

    Pith/arXiv arXiv 2002

  50. [50]

    , keywords =

    Measurements of the Hubble Constant: Tensions in Perspective. , keywords =. doi:10.3847/1538-4357/ac0e95 , archivePrefix =. 2106.15656 , primaryClass =

    Pith/arXiv arXiv

  51. [51]

    To H0 or not to H0?

    Efstathiou, George. To H0 or not to H0?. Mon. Not. Roy. Astron. Soc. 2021. doi:10.1093/mnras/stab1588. arXiv:2103.08723

    Pith/arXiv arXiv 2021

  52. [52]

    Nature Astronomy , keywords =

    Tensions between the early and late Universe. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0902-0 , archivePrefix =. 1907.10625 , primaryClass =

    Pith/arXiv arXiv 1907

  53. [53]

    Classical and Quantum Gravity , keywords =

    In the realm of the Hubble tension-a review of solutions. Classical and Quantum Gravity , keywords =. doi:10.1088/1361-6382/ac086d , archivePrefix =. 2103.01183 , primaryClass =

    Pith/arXiv arXiv

  54. [54]

    Physics of the Dark Universe , keywords =

    The Ups and Downs of Early Dark Energy solutions to the Hubble tension: A review of models, hints and constraints circa 2023. Physics of the Dark Universe , keywords =. doi:10.1016/j.dark.2023.101348 , archivePrefix =. 2302.09032 , primaryClass =

    arXiv 2023

  55. [55]

    2025 , eprint=

    Gravitational wave cosmology : an introduction , author=. 2025 , eprint=

    2025

  56. [56]

    de Mattia, Arnaud and others. The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the BAO and growth rate of structure of the emission line galaxy sample from the anisotropic power spectrum between redshift 0.6 and 1.1. Mon. Not. Roy. Astron. Soc. 2021. doi:10.1093/mnras/staa3891. arXiv:2007.09008

    Pith/arXiv arXiv 2021

  57. [57]

    and others

    Abdul Karim, M. and others. DESI DR2 results. II. Measurements of baryon acoustic oscillations and cosmological constraints. Phys. Rev. D. 2025. doi:10.1103/tr6y-kpc6. arXiv:2503.14738

    Pith/arXiv arXiv 2025

  58. [58]

    Gravitational Wave Cosmology

    Palmese, Antonella and Mastrogiovanni, Simone. Gravitational Wave Cosmology. 2025. arXiv:2502.00239

    Pith/arXiv arXiv 2025

  59. [59]

    doi:10.1093/oso/9780198570899.001.0001 , adsurl =

    Gravitational Waves: Volume 2: Astrophysics and Cosmology. doi:10.1093/oso/9780198570899.001.0001 , adsurl =

    arXiv

  60. [60]

    The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models. , keywords =. doi:10.3847/2041-8213/aa8fc7 , archivePrefix =. 1710.05840 , primaryClass =

    Pith/arXiv arXiv 2041

  61. [61]

    A two per cent Hubble constant measurement from standard sirens within five years

    Chen, Hsin-Yu and Fishbach, Maya and Holz, Daniel E. A two per cent Hubble constant measurement from standard sirens within five years. Nature. 2018. doi:10.1038/s41586-018-0606-0. arXiv:1712.06531

    Pith/arXiv arXiv 2018

  62. [62]

    European Physical Journal C , year = 2019, month = feb, volume =

    Low-redshift constraints on the Hubble constant from the baryon acoustic oscillation ``standard rulers'' and the gravitational wave ``standard sirens''. European Physical Journal C , year = 2019, month = feb, volume =. doi:10.1140/epjc/s10052-019-6664-0 , adsurl =

    work page doi:10.1140/epjc/s10052-019-6664-0 2019

  63. [63]

    , keywords =

    Improving cosmological parameter estimation with the future gravitational-wave standard siren observation from the Einstein Telescope. , keywords =. doi:10.1103/PhysRevD.99.063510 , archivePrefix =. 1804.08379 , primaryClass =

    Pith/arXiv arXiv

  64. [64]

    and Peiris, Hiranya V

    Feeney, Stephen M. and Peiris, Hiranya V. and Williamson, Andrew R. and Nissanke, Samaya M. and Mortlock, Daniel J. and Alsing, Justin and Scolnic, Dan. Prospects for resolving the Hubble constant tension with standard sirens. Phys. Rev. Lett. 2019. doi:10.1103/PhysRevLett.122.061105. arXiv:1802.03404

    Pith/arXiv arXiv 2019

  65. [65]

    Cosmography with standard sirens from the Einstein Telescope

    de Souza, Josiel Mendon c a Soares and Sturani, Riccardo and Alcaniz, Jailson. Cosmography with standard sirens from the Einstein Telescope. JCAP. 2022. doi:10.1088/1475-7516/2022/03/025. arXiv:2110.13316

    Pith/arXiv arXiv 2022