{"total":19,"items":[{"citing_arxiv_id":"2605.23554","ref_index":292,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Inferring the role of binary neutron star mergers in r-process nucleosynthesis with multi-messenger observations using Cosmic Explorer and Einstein Telescope","primary_cat":"astro-ph.HE","submitted_at":"2026-05-22T12:19:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new redshift-correlation technique with third-generation GW detectors can constrain the BNS contribution to cosmic r-process nucleosynthesis to 5-6% precision via Fisher forecasts on mock bright- and dark-siren data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21580","ref_index":184,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19653","ref_index":100,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Evidence for Intermediate-Mass Black Holes From Microlensing Signatures in CHIME/FRB catalog 2","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T10:43:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Two FRBs exhibit microlensing signatures consistent with intermediate-mass black holes of masses approximately 500-600 and 1500-2500 solar masses, interpreted as possible evidence for isolated primordial black holes comprising about 4% of dark matter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19241","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets","primary_cat":"astro-ph.EP","submitted_at":"2026-05-19T01:22:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11947","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Inferring host environment properties and gravitational-wave decay time from the eccentricity measurement of dynamically captured binaries","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T10:56:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Eccentricity posteriors of dynamically captured binaries can be mapped to capture parameters and compared against environment velocity distributions to constrain host and infer decay time.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"L(d|e f ) can be expressed as L(d|e f )∝ p(e f |d) Π(e f ) ,(9) whereΠ(e f ) is the eccentricity prior from the GW data anal- ysis. From the mapping relations developed in the previous section, we havee f =F(b, v ∞,M, η). Therefore, the quantity p(e f |⃗θ) in Eq. (8) is a Dirac delta function that peaks at the value ofe f determined by ⃗θ, implying p(e f |⃗θ)=δ e f −F( ⃗θ)\u0001.(10) Hence, by substituting Eqs. (9) and (10) into Eq. (8), Eq. (7) becomes p(⃗θ|d)∝Π( ⃗θ) Z p(e f |d) Π(e f ) δe f −F( ⃗θ)\u0001 de f , ∝Π( ⃗θ) p(e f |d) Π(e f ) e f =F(⃗θ) .(11) 4 0 50 100 150 200 250 300 v∞ [km/s] 0.000 0.001 0.002 0.003 0.004 0.005 104 105 b/M 0 1 2 3 4 5 1e 5 Probability density Figure 1.Inferred posteriors forv ∞ andbfor GW200105 based on the formalism in Sec."},{"citing_arxiv_id":"2605.11283","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Black Hole Binary Detection Landscape for the Laser Interferometer Lunar Antenna (LILA): Signal-to-Noise Calculations & Science Cases","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T22:09:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"numerical relativity calculations, but for the purposes of this paper, we approximate using an inspiral-merger-ringdown (IMR) phenomenological template derived from numerical relativity waveforms, written in the form of the waveform amplitude in the frequency domain (PhenomA model; Ajith et al. 2008): A∝    f −7/6 iff < f merge f −2/3 iff merge ≤f < f ring L(f;f ring, σ)iff ring ≤f < f cut, (6) where fmerge =A 0;f ring =A 1;σ=A 2;f cut =A 3 (7a) An ≡ anη2 +b nη+c n π(GM/c3)(1 +z) (7b) L(f;f ring, σ)≡ 1 2π σ (f−f ring)2 +σ 2/4 (7c) withη≡µ/Mand the parametersA n are derived from numerical relativity template fits reported in Table 1 of Ajith et al. 2008. The frequencies above are defined in the observed frame. Additionally,L(f;f ring, σ)denotes the Lorentzian function of widthσcentered aroundf ring."},{"citing_arxiv_id":"2605.10557","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Observational Properties of Nonthermal Emission from Relativistic Jets Escaping Active Galactic Nucleus Disks","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T13:32:18+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2×107 cm−3 \u0012 b 0.5 \u0013−1 ˙Mw 0.1 ˙MEdd !\u0012 R 103Rg \u0013−2\u0010 vw 109 cm s−1 \u0011−1 , (3) for a SMBH of massM= 10 7M⊙, which is consistent in magnitude with the observation (Laha et al. 2021). The corresponding vertical gas density profile above the AGN disk is modeled as (e.g., Zhou et al. 2023) 2 n=n 0 p R2 0 +r 2 p R2 0 +H 2 d !−2 ≃n 0 \" 1 + \u0012 r R0 \u00132#−1 , r > H d (4) whereR 0 is the radius of the AGN disk where the jet launches,n 0 =n w( p R2 0 +H 2 d)∼10 8 cm−3 forM= 107M⊙ andR 0 = 10 3Rg. When the jet propagation distance is much smaller thanR 0, the ambient density remains approximately constant, i.e.,n∼n 0; at a large distance, the density approaches a wind-like profile, i.e., n∝r −2. In this work, we neglect the ambient cloud"},{"citing_arxiv_id":"2605.09351","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"High-Spin BBH Subpopulation from AGN Accretion","primary_cat":"astro-ph.HE","submitted_at":"2026-05-10T06:02:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mixture model analysis of LIGO data identifies a ~10% high-spin subpopulation with a1 ≈ 0.9 matching AGN accretion predictions, disfavoring hierarchical mergers at a1 ≈ 0.7 for that group.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"05 to 0.30, the accretion fraction ranges from 8% to 12% and lnB(M 1/M0) from 5.5 to 6.3, all within the canonical 90% credible interval. Flexible standard component.Replacing the stan- dard Beta(1,β low) with a two-parameter Beta(α,β) distribution gives a slightly elevated accretion fraction (facc = 10.3%, lnB= 7.6). The data weakly prefer α≈2.7 (90% CI [1.2,4.7]), indicating a non-monotonic low-spin distribution with a small non-zero mode. Waveform systematics.Using mixed-approximant samples for all events instead of the hybrid NRSurrogate selection givesf acc = 8.2% and lnB= 5.0. Using SEOB- NRv5/v4PHM as the preferred waveform where NRSur- rogate is unavailable givesf acc = 8.2% and lnB= 4.3. Both are consistent with the main analysis."},{"citing_arxiv_id":"2605.07027","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nuclear Constraints on $^{12}$C$(\\alpha,\\gamma)^{16}$O and Their Impact on Black-Hole Mass Predictions","primary_cat":"astro-ph.HE","submitted_at":"2026-05-07T23:15:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Updated ANC constraints on the 12C(alpha,gamma)16O S-factor favor lower values than prior evaluations and imply a black-hole mass-gap lower edge of 61-75 solar masses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"lower edge of the pair-instability mass gap is shifted to about64M ⊙, while the upper edge is shifted to about 161M ⊙. Rapid rotation can raise the lower edge further, to approximately70M ⊙. The relevance of this issue has increased because gravitational-wave observations have reported BHs with masses up to about85M ⊙, as well as numerous BHs in the60-70M⊙ range [9, 10]. More recently, Ref. [4] reported the discovery of new low-spin BHs in the mass interval50-70M⊙. It is important to emphasize that gravitational-wave observations alone cannot uniquely determine the BH mass gap or the underlying BH mass spectrum. The in- ference depends on the adopted stellar-evolution model, including nuclear reaction rates, rotation, mass loss,"},{"citing_arxiv_id":"2605.05563","ref_index":5,"ref_count":1,"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":"background","top_context_polarity":"background","context_text":"fines the lower edge of the gap. In this model, we adopt a gap width of 80±8M ⊙ based on simulations (Farmer et al. 2020), which found the width to remain approxi- mately constant at 83 +5 −8 M⊙, while the individual lower and upper edges are only weakly constrained. The the- oretically motivated mass function is then written as Pm,1(m|Λ1)∝ PS(m|Λ 1)f Gap(m|glow, gwide),(5) with f(m|g low, gwide) =    1,form < g low, 0,forg low < m < g low +g wide, 1,form > g low +g wide (6) 2.3.mass-only model Even if the mass range of the PIMG in the first- generation black hole mass function is partly filled by higher-generation black holes from hierarchical mergers, a corresponding dip or deficit may still be imprinted on the overall binary black hole mass distribution."},{"citing_arxiv_id":"2604.18676","ref_index":271,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Binary Evolution Can Mimic the Pair-Instability Mass Gap in Black Hole Mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-04-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.03163","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological Constraints from GW-FRB Associations without Redshift Measurements for LIGO-Virgo and Cosmic Explorer","primary_cat":"astro-ph.CO","submitted_at":"2026-04-03T16:36:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations demonstrate that Cosmic Explorer can robustly constrain cosmology and host galaxy parameters from GW-FRB associations using luminosity distance-dispersion measure relations without spectroscopic redshifts, unlike the current LIGO-Virgo network.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"In this low-redshift regime, we focus on the comparison between current and next-generation detector sensitivities. The quantitative results for all considered scenarios, including bothD L −DM diff andD L −DM ext relations for the LIGO-Virgo (LV) and Cosmic Explorer (CE) networks, are summarized in Table 2. 12 T able 2.Summary of MCMC constraints for low-redshift events (z <0.2) Data DetectorH 0 [km/s/Mpc] Ω m wexp(µ) [pc/cm 3]σ host DL −DM diff LV 73.975 +3.833 −3.469 0.404+0.358 −0.279 −1.146+0.687 −0.586 - - DL −DM diff CE 70.968 +2.708 −2.657 0.556+0.297 −0.331 −0.878+0.603 −0.688 - - DL −DM ext LV 79.269 +7.925 −7.285 0.443+0.358 −0.308 −1.116+0.665 −0.613 145.532+18.646 −18.234 0.516+0.090 −0.078 DL −DM ext CE 71.774 +4.730 −4.234 0.528+0.320 −0.321 −0.941+0.645 −0."},{"citing_arxiv_id":"2604.02631","ref_index":72,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Proca-Maxwell System in an Infinite Tower of Higher-Derivative Gravity","primary_cat":"gr-qc","submitted_at":"2026-04-03T01:46:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Higher-order terms in an infinite tower of higher-derivative gravity regularize a 5D Proca-Maxwell system, creating frozen regular cores that mimic extremal black holes and satisfy all energy conditions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"19, 194003 doi:10.1088/1361-6382/ac1fd0 [arXiv:2103.15705 [gr-qc]]. [70] A. Masó-Ferrando, N. Sanchis-Gual, J. A. Font and G. J. Olmo, Phys. Rev. D109(2024) no.4, 044042 doi:10.1103/PhysRevD.109.044042 [arXiv:2309.14912 [gr-qc]]. [71] S. Ilijić and M. Sossich, Phys. Rev. D102 (2020) no.8, 084019 doi:10.1103/PhysRevD.102.084019 [arXiv:2007.12451 [gr-qc]]. [72] V. Baibhav and D. Maity, Phys. Rev. D95 (2017) no.2, 024027 doi:10.1103/PhysRevD.95.024027 [arXiv:1609.07225 [gr-qc]]. [73] B. Hartmann, J. Riedel and R. Suciu, Phys. Lett. B 726(2013), 906-912 doi:10.1016/j.physletb.2013.09.050 [arXiv:1308.3391 [gr-qc]]. [74] L. J. Henderson, R. B. Mann and S. Sto- tyn, Phys. Rev. D91(2015) no.2, 024009 doi:10.1103/PhysRevD."},{"citing_arxiv_id":"2510.07174","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Archival Inference for Eccentric Stellar-Mass Binary Black Holes in Space-Based Gravitational Wave Observations","primary_cat":"astro-ph.HE","submitted_at":"2025-10-08T16:15:55+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Ground-triggered Bayesian analysis enables detection and tight constraints on eccentricity and chirp mass for a GW190521-like eccentric binary black hole in one year of LISA or TianQin data at SNR ~7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.08219","ref_index":57,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\\odot}$","primary_cat":"astro-ph.HE","submitted_at":"2025-07-10T23:52:46+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":9.0,"formal_verification":"none","one_line_summary":"A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2412.20169","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Effective Field Theory Calculation of LIGO-like Compton Scattering","primary_cat":"gr-qc","submitted_at":"2024-12-28T14:52:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper computes the graviton-scalar Compton scattering cross section via EFT at ~30 PeV center-of-mass energy and derives an impact parameter that, after coherence enhancement, scales with the known LIGO GW strain and mirror recoil.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2411.10590","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"McFACTS II: Mass Ratio--Effective Spin Relationship of Black Hole Mergers in the AGN Channel","primary_cat":"astro-ph.HE","submitted_at":"2024-11-15T21:28:40+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Monte Carlo simulations of AGN-disk black hole mergers identify dense, moderately short-lived disks, a steep initial mass function, and mostly prograde orbits as the parameter combination that reproduces the observed (q, χ_eff) anti-correlation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2109.09882","ref_index":86,"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":"2006.00714","ref_index":216,"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}],"limit":50,"offset":0}