{"total":21,"items":[{"citing_arxiv_id":"2606.30504","ref_index":39,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Rapid Hubble constant inference from GW170817 using GPU-accelerated nested sampling: prior sensitivity and the limits of post-hoc reweighting","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T16:07:25+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GPU-accelerated nested sampling on GW170817 demonstrates that switching to a uniform-in-dL prior shifts the H0 tail and median far more than post-hoc reweighting captures, due to an under-sampled (dL, iota) bimodality.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23786","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Collapsar-Disk Origin for GW190814","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GW190814 is proposed to originate from a collapsar-disk fragment merging with the central black hole, potentially preceded by SN2019npv ~60 days earlier, yielding H0 = 70.5 (+9.2, -6.4) km/s/Mpc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17752","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Intrinsic handedness in O1-O4a black-hole mergers: probing orbital precession, remnant retention in dense environments and cosmological mirror asymmetry","primary_cat":"gr-qc","submitted_at":"2026-06-16T10:12:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"92% of 91 LIGO black hole mergers favor non-zero V_GW, constraining bound remnants to at most 8% and finding no cosmological handedness preference with average near zero.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17136","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Lazuli Space Observatory: Opportunities for time-domain and multi-messenger astronomy","primary_cat":"astro-ph.IM","submitted_at":"2026-06-15T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Lazuli is proposed as a space observatory combining flagship sensitivity with response times one to two orders of magnitude faster than current large facilities to enable new time-domain and multi-messenger science.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"will take up to 5 minutes (but is typically expected to be much shorter), after which photons will start being collected. These estimates yield typical response times of≲4 hours. Achieving these response times relies on several key design choices: (1) automation-first ToO processing with minimal human-in-the-loop intervention, (2) pre- validated observing templates to reduce validation over- head, (3) dynamic queue scheduling that can be re- computed on short timescales, and (4) near-continuous commanding enabled by the selected orbit and ground segment architecture. Under favorable conditions (slew distance<50 degrees with typical thermal load) and a nominal system state, best-case scenario response times approaching 60-70 minutes are expected, well below the"},{"citing_arxiv_id":"2606.05151","ref_index":50,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mapping the star formation peak with LIGO A# and Next-Generation detectors","primary_cat":"gr-qc","submitted_at":"2026-06-03T17:53:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show LIGO-A# constrains the peak redshift of binary black hole merger rate (tracing star formation) to ±0.1 in one year, improving to ±0.02 with next-generation detectors.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"T able 1.Probability distribution models and ranges for parame- ters used for simulating binaries. distribution is given by a power law that also includes the smoothing term and is given as p(q) =q βS(m1q|mmin,δm) (3) withβ= 0.76. We have distributed the component masses (mi) in the range of [2, 100]M ⊙and the mass ratio (q= m1/m2) in the range of [1, 50]. The spins of the binaries are distributed using an isotropic distribution. The probability density models for the spin mag- nitudes (ai) and spin angles (θi,ϕ12,ϕJL) are given in Ta- ble 1,3 where we have also listed the models and parameter ranges used for inclination angle (θJN), sky location angles (α,δ,Ψ), and coalescence phase (ϕc) used for simulating the"},{"citing_arxiv_id":"2605.16132","ref_index":49,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nucleosynthesis in the fast ejecta of a neutron star merger","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T16:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11474","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Secondary-Mass Features improve Spectral-Siren $H_0$ Constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T03:43:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new model emphasizing secondary mass features and pairing transitions improves spectral siren H0 constraints by ~30% using 142 GW events from GWTC-4.0.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"pendix A) to measure the Hubble constant as well as the mass distribution of GW events. 2.1.Cosmological model We adopt a flat ΛCDM cosmological model and as- sume a constant dark energy density throughout cosmic expansion. The luminosity distanceD L as a function of redshiftzis then given by (R. Abbott et al. 2023c; The LIGO Scientific Collaboration et al. 2025b) DL(z) = c(1 +z) H0 Z z 0 [Ωm(1 +x) 3 + 1−Ω m]−1/2dx = F(z|H0,Ω m), (1) where Ωm denotes the present-day dimensionless matter density, andH 0 is the Hubble constant. Gravitational- wave signals allow measurements of the detector-frame masses of BBHs and the luminosity distance (i.e.,M 1, M2,D L). Given the cosmological parametersH 0 and Ω m, the source-frame masses can be obtained via the relationm 1,2 =M 1,2/(1 +z(D L)) =M 1,2/(1 +"},{"citing_arxiv_id":"2605.11437","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Revisiting GW170817 at milliarcsecond scale: high-precision constraints on jet geometry and $H_0$","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T02:39:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new Bayesian analysis of VLBI observations of GW170817's jet afterglow constrains the viewing angle to 16.8-19.2 degrees and measures H0 = 65.5 ± 4.4 km s^{-1} Mpc^{-1}, closer to Planck than SH0ES values.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Govreen-Segal & Nakar (2023) and is calibrated using simulations withθ v up to 0.75 radians. 22 Fit parameter Bayesian model average mean value Bayesian model average 68% credible interval F0 (Jy) 5.074×10 −5 [4.573×10 −5,5.582×10 −5] δF,1 0.003 [−0.081,0.089] δF,2 -0.033 [−0.122,0.057] δF,3 0.024 [−0.067,0.114] PA (degrees) 87.7 [80.2,95.4] RAoff (mas)−7.28 [−7.40,−7.16] Decoff (mas)−0.82 [−0.98,−0.66] δra,1 (mas) 0.2 [−0.1,0.3] δdec,1 (mas)−0.14 [−0.50,0.22] δra,2 (mas)−0.02 [−0.15,0.10] δdec,2 (mas) 0.01 [−0.44,0.46] δra,3 (mas)−0.06 [−0.18,0.06] δdec,3 (mas) 0.06 [−0.35,0.48] θv θcp 6.4 [4.3,8.5] θv −θ cp (radians) 0.260 [0.241,0.278] tp (days) 154.7 [150.8,158.7] dL (Mpc) 44.0 [42.5,45.6] cz(km s −1) 3002 [2938,3061] H0 (km s−1Mpc−1) 65.5 [61.1,69.9] Table 4.Bayesian model average posterior means and 68% credible intervals."},{"citing_arxiv_id":"2605.10940","ref_index":259,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T17:59:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10584","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An agentic framework for gravitational-wave counterpart association in the multi-messenger era","primary_cat":"astro-ph.IM","submitted_at":"2026-05-11T13:58:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GW-Eyes is a new LLM-powered agent framework that autonomously associates gravitational-wave events with electromagnetic counterparts by integrating specialized tools and supporting natural-language interaction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10102","ref_index":231,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"From Large Telescopes to the MUltiplexed Survey Telescope (MUST)","primary_cat":"astro-ph.IM","submitted_at":"2026-05-11T07:18:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MUST is a new 6.5 m telescope designed to deliver simultaneous optical spectra for over 20,000 targets across a 5 deg² field, enabling the largest 3D spectroscopic map of the Universe with redshifts for more than 100 million objects over an 8-year survey.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06783","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dark siren cross-correlations and the sensitivity of $H_0$ to methodological choices","primary_cat":"astro-ph.CO","submitted_at":"2026-05-07T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Methodological choices in dark siren cross-correlations can mitigate biases in H0 inference when selection effects are built into the model and samples of precise events are sufficiently large.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Several techniques have been developed to use gravitational waves to measureH0, using eitherbright sirensordark sirens. In the former case, the identification of an electromagnetic counterpart to the gravitational wave event enables a direct measurement of the source redshift, allowing for an inference ofH0 through the luminosity distance-redshift relation [1]. In the latter, the redshift is inferred statistically by associating the gravitational wave localisation area with galaxies in existing catalogues. These redshifts are then combined with the inferred luminosity distance to construct a Hubble diagram and constrain H0 [3, 13, 19, 23, 24, 26, 30, 32, 47]. Another complementary approach, known as the spectral"},{"citing_arxiv_id":"2605.06769","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Origins of Extreme Emission-Line Ratios in z > 3 Galaxies: Insights from the Lumen Model","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Lumen modeling of IllustrisTNG50 shows that high ionization parameters from massive star clusters plus enhanced nitrogen abundances are needed to reproduce the extreme [OIII]/Hβ, [OIII]/[OII], and [NII]/Hα ratios seen in z>3 galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05563","ref_index":4,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"How do the LIGO-Virgo-KAGRA's Heavy Black Holes Form? No evidence for core-collapse Intermediate-mass black holes in GWTC-4","primary_cat":"astro-ph.HE","submitted_at":"2026-05-07T01:12:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No evidence for core-collapse formed low-spin IMBHs in GWTC-4, with 90% upper limit on merger rate of 0.077 Gpc^{-3} yr^{-1}, low-spin BH mass truncation at 65 solar masses consistent with pair-instability gap lower edge, and high-spin IMBHs from hierarchical mergers.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Pm,1(m|Λ1) =PS(m|Λ 1) (1−r IM)+ PL(m|α IM, mmin,IM, mmax,IM)r IM, (3) wherePLis a truncated power-law distribution (Abbott et al. 2021), designed to capture the possible low-spin IMBH population formed via stellar collapse. The IMBH3 The overall population model is π(λ|Λ)∝π(m 1, χ1,|Λ)π(m 2, χ2,|Λ)F pair(m1, m2|β) × GU(cosθ 1,cosθ 2|ζ, µt, σt)Pz(z|γ), (4) whereF pair(m1, m2|β) = (m 2/m1)β is the pair- ing function,GU(cosθ 1,cosθ 2|ζ, µt, σt) = (1− ζ)U(cosθ 1,cosθ 2| −1,1) +ζG [−1,1](cosθ 1,cosθ 2|µt, σt) is for spin orientation distribution, which is the mixture of isotropic and nearly aligned assemblies.P z(z|γ) is for the redshift distribution, where we assume the merger rate density evolving with redshift asR(z) =R 0(1+z) γ,"},{"citing_arxiv_id":"2602.17267","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Illuminating the Mass Gap Through Deep Optical Constraint on a Neutron Star Merger Candidate S250206dm","primary_cat":"astro-ph.HE","submitted_at":"2026-02-19T11:15:27+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Non-detection of kilonova from S250206dm excludes AT 2017gfo-like events and disfavors NS-BH mergers with mass ratio Q >= 3.2, reaching GW-comparable precision on the mass gap candidate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.21729","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Golden and Silver Dark Sirens for precise H0 measurement with HETDEX","primary_cat":"astro-ph.CO","submitted_at":"2025-12-25T16:24:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Forecasts that golden and silver dark sirens with HETDEX VIRUS follow-up can constrain H0 to a few percent using one year of LIGO-A# observations for z < 0.2 events.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2502.14164","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Implementing a Robust Test of Galaxy Catalogue Completeness for Dark Siren Measurements of the Hubble Constant","primary_cat":"astro-ph.CO","submitted_at":"2025-02-20T00:16:17+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2109.09882","ref_index":158,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Horizon Study for Cosmic Explorer: Science, Observatories, and Community","primary_cat":"astro-ph.IM","submitted_at":"2021-09-20T23:34:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cosmic Explorer is described as a next-generation gravitational-wave observatory aiming for tenfold sensitivity improvement over Advanced LIGO to observe signals from the edge of the observable universe at z~100.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.12611","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GW190814: Gravitational Waves from the Coalescence of a 23 M$_\\odot$ Black Hole with a 2.6 M$_\\odot$ Compact Object","primary_cat":"astro-ph.HE","submitted_at":"2020-06-22T20:56:34+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.00714","ref_index":197,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Bayesian inference for compact binary coalescences with BILBY: Validation and application to the first LIGO--Virgo gravitational-wave transient catalogue","primary_cat":"astro-ph.IM","submitted_at":"2020-06-01T04:46:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"BILBY is validated on simulated compact binary signals and reproduces the eleven GWTC-1 results with configuration and output files provided for reproduction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"0805.2366","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"LSST: from Science Drivers to Reference Design and Anticipated Data Products","primary_cat":"astro-ph","submitted_at":"2008-05-15T18:10:13+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LSST will image 18,000 square degrees of sky about 800 times across six bands over 10 years to a coadded depth of r~27.5, producing a public database of 40 billion objects and 32 trillion observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"from the joint analysis of LSST LSS and WL (galaxy-galaxy, galaxy-shear, and shear-shear power spectra) with a conser- vative level of systematic uncertainties in the photometric redshift error distribution and additive and multiplicative errors in the shear and galaxy power spectra. The maximum multipole used for WL is 2000, and that for LSS is 3000 [with the additional requirement that ∆ 2 δ(ℓ/DA;z) < 0.4]. The growth parameters are evenly spaced in log(1 + z) be- tween z = 0 and 5, and the distance parameters start at z1 = 0.14. The error of each distance (growth) parameter is marginalized over all the other parameters including growth (distance) parameters. The joint constraints on distance are relatively insensitive to the assumed systematics (Zhan et al."}],"limit":50,"offset":0}