{"total":12,"items":[{"citing_arxiv_id":"2606.23838","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Degeneracy Distillery","primary_cat":"cs.LG","submitted_at":"2026-06-22T18:18:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A method called the degeneracy distillery uses symbolic transformations to flatten the Fisher information matrix globally from simulations alone, identifying independent parameter combinations and reducing neural posterior estimation simulation budgets by up to 10x.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20787","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Gas-induced perturbations on the gravitational wave in-spiral of live post-Newtonian LISA massive black hole binaries: 0.1 disk aspect ratio","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"3D hydro + 2.5PN simulations of an equal-mass 10^6 M_sun MBHB in a 0.1-aspect-ratio locally isothermal CBD measure a gas-induced orbital phase shift of 0.12 rad over 600 cycles, claimed detectable by LISA at z=1.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05151","ref_index":118,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27225","ref_index":32,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2026-05-26T16:09:49+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":8.0,"formal_verification":"none","one_line_summary":"GWTC-5.0 adds 161 new compact binary coalescence candidates from O4b with p_astro >= 0.5, detailed properties for 104, all binary black holes, for a cumulative total of 390.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2014; Farr et al. 2016; Vitale et al. 2017a; Abbott et al. 2016c; García- Bellido et al. 2021; Green et al. 2021; Hoy et al. 2025). The component spins of compact binaries,χ 1 andχ 2, are typ- ically poorly constrained since the leading-order spin con- tribution to the GW signal is determined by mass-weighted combinations of the components (Damour 2001; Blanchet 2014; Pürrer et al. 2016; Ng et al. 2018; Zevin et al. 2020). Here, we focus on two mass-weighted spin parameters: the effective inspiral spinχ eff and the effective precession spin χp (Abac et al. 2026a). The effective inspiral spinχ eff (Ajith et al. 2011; Santa- maría et al. 2010) is a mass-weighted combination of the components of the spin aligned with the Newtonian orbital"},{"citing_arxiv_id":"2605.27224","ref_index":68,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-5.0: Methods for Identifying and Characterizing Gravitational-wave Transients","primary_cat":"gr-qc","submitted_at":"2026-05-26T16:09:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Describes the methods for producing the fifth gravitational-wave transient catalog (GWTC-5.0) from O4b data of LIGO, Virgo and KAGRA.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"For an introduction to waveform modeling in general and definitions of our coordinate conventions, see Section 5 of Abac et al. (2026a). Several different modeling approaches have been followed in the development of CBC waveform models for the com- plete inspiral-merger-ringdown (IMR) stages of the signal. Inspiral-only models have been developed based on post- Newtonian (PN) theory (Blanchet 2014), using different PN- expansions of the energy balance equations for the two-body dynamics, under the TAYLORfamily (Buonanno et al. 2009) for non-spinning systems and the SPINTAYLORfamily (Stu- rani 2015; Isoyama et al. 2020) for spinning systems. The IMRPHENOMapproach (Ajith et al. 2007) focuses on the description of the GW signal, traditionally in Fourier do-"},{"citing_arxiv_id":"2605.26308","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nuclear Physics of Binary Neutron Star Mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-05-25T19:59:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"by interchangingf j ↔ ¯fj. Whileλ Urca generally must be evaluated numerically, analytic expressions in the degenerate regime are available that make the main scaling relations explicit not far from this limit. For neutrino-trapped matter (assuming equal neutron and proton effective massesm ∗) one finds λUrca = 1 12π3 m∗2 ˜G2T 2pF epF ν(pF p +p F e +p F ν −p F n),(34) where ˜G=G 2 F cos2 θc 1 + 3g2 A \u0001 , whereas in neutrino-transparent matter λUrca = 17 240π m∗2 ˜G2T 4pF e θ(pF p +p F e −p F n).(35) Thus, close to the degenerate limit the trapped-matter rate scales asλ Urca ∝T 2, while the transparent-matter rate scales asλ Urca ∝T 4. The step function in the latter expression encodes the direct-Urca threshold: in neutrino-"},{"citing_arxiv_id":"2605.16132","ref_index":299,"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":"2605.05300","ref_index":22,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"No model-independent evidence for a peak in binary black hole spin (mis)alignments","primary_cat":"astro-ph.HE","submitted_at":"2026-05-06T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"No model-independent evidence for a peak in binary black hole spin tilts is found in GWTC-4; mass-spin magnitude correlation is confirmed but mass-tilt correlation is not.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"best the effective spin of the binary (S. Vitale et al. 2017a; F. H. Shaik et al. 2020; G. Pratten et al. 2020; R. Green et al. 2021; S. Biscoveanu et al. 2021; N. V. Kr- ishnendu & F. Ohme 2022; S. J. Miller et al. 2025), i.e., the mass-weighted projection of the component spin vec- tors along the orbital angular momentum (T. Damour 2001; E. Racine 2008; L. Blanchet 2014). In principle, population inference should be able to make a meaning- ful measurement of spin tilts from the combination of many poorly measured examples (S. Vitale et al. 2017b; C. Talbot & E. Thrane 2017; S. J. Miller et al. 2024). In practice and given current GW datasets, population constraints on spin tilts are: sensitive to modeling as- sumptions (S."},{"citing_arxiv_id":"2604.09788","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Even a precessing clock is right twice per orbit -- The super-periods of eRO-QPE2 and challenges for quasi-periodic eruption orbital models","primary_cat":"astro-ph.HE","submitted_at":"2026-04-10T18:11:56+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-mission O-C data on eRO-QPE2 reveal hierarchical super-periods consistent with apsidal precession at a~140 Rg but no robust EMRI solution due to sparse sampling and narrow likelihood peaks.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The main difference withQPE-FITis that the preces- sion period is linked to the MBH spin and the disk prop- erties, providing a stronger constraint to the spin value during the parameter inference. Following Franchini et al. (2023), the EMRI trajectory is evolved by integrat- ing the equations of motion within the post-Newtonian framework up to 3.5PN order (Boh' e et al. 2013; Blanchet 2014), thereby accounting for dissipative effects due to gravitational-wave emission. The equations are numer- ically integrated over the full temporal baseline of the T able C.1.Prior ranges for variousQPE-FITruns with two/one flares per orbit (QF-2coll/QF-1collrespectively). Parameter Two-flare One-flare One-flare (wide) (narrow) a/Rg U(50,1000)U(50,1000)U(136,187)"},{"citing_arxiv_id":"2604.08679","ref_index":63,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Tidal Response of Compact Objects","primary_cat":"gr-qc","submitted_at":"2026-04-09T18:10:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"This review summarizes tidal Love numbers and dissipation effects for black holes, neutron stars, and exotic objects, noting vanishing static bosonic Love numbers for black holes in GR but nonzero values for fermions and exotic objects, with implications for gravitational-wave astronomy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.19077","ref_index":38,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The First Model-Independent Upper Bound on Micro-lensing Signature of the Highest Mass Binary Black Hole Event GW231123","primary_cat":"gr-qc","submitted_at":"2025-12-22T06:37:44+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"No definitive lensing is detected in GW231123, though a potential microlensing feature with modulation amplitude up to 0.8 at 95% confidence is noted, limited by large waveform systematics in short signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.12611","ref_index":52,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"banks (Sathyaprakash & Dhurandhar 1991; Blanchet et al. 1995; Owen 1996; Owen & Sathyaprakash 1999; Damour et al. 2001; Blanchet et al. 2005; Cokelaer 2007; Harry et al. 2009; Brown et al. 2013; Ajith et al. 2014; Harry et al. 2014; Capano et al. 2016b; Roy et al. 2017, 2019; Indik et al. 2018) of modeled gravi- tational waveforms (Buonanno & Damour 1999; Arun et al. 2009; Blanchet 2014; Boh' e et al. 2017; P¨ urrer 2016) as filter templates. A Notice was issued through NASA's Gamma-ray Coordinates Network (GCN) 20 min later (LIGO Scientific Collaboration, Virgo Col- laboration 2019a) with a two-detector source local- ization computed using the rapid Bayesian algorithm BAYESTAR (Singer & Price 2016) that is shown in Figure 2. The event was initially classified as \"Mass-"}],"limit":50,"offset":0}