Mind the peak: improving cosmological constraints from GWTC-4.0 spectral sirens using semiparametric mass models
Università di Bologna（博洛尼亚大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚天文物理与空间科学研究所）；INFN - Sezione di Bologna（博洛尼亚意大利国家核物理研究所）
Gravitational wave spectral sirens can provide cosmological constraints by using the shape of the binary black hole (BBH) mass distribution (MD). However, the precision and accuracy of these constraints depends critically on the capturing all the MD features. In this work, we analyze 137 BBH events from the latest GWTC-4.0 with a novel data-driven semiparametric approach based on \textsc{Bspline} that adaptively places knots around the most informative structures in the MD, while keeping the dimensionality of the parameter space moderate. Our flexible models resolve three distinct peaks at $\sim10$, $18$, and $33\,\mathrm{M}_\odot$ and are statistically preferred over standard parametric models, with Bayes factors up to 226. Because these features are correlated with $H_0$, the semiparametric model yields, under different prior assumptions, 12%-21% improvement in the precision of $H_0$ relative to parametric models, providing $H_0 = 57.8^{+21.9}_{-20.6}\,\mathrm{km/s/Mpc}$ in the best case. Our results demonstrate that capturing the full complexity of the BBH mass distribution is essential for realizing the cosmological potential of spectral sirens as gravitational wave catalogs continue to grow.
We present the latest measurements of the Hubble parameter and of the parameter $Ξ_0$ describing modified gravitational wave propagation, obtained from the third gravitational wave transient catalog, GWTC-3, using the correlation with galaxy catalogs and information from the source-frame mass distribution of binary black holes. The latter leads to the tightest bound on $Ξ_0$ so far, i.e. $Ξ_0 = 1.2^{+0.7}_{-0.7}$ with a flat prior on $Ξ_0$, and $Ξ_0 = 1.0^{+0.4}_{-0.8}$ with a prior uniform in $\logΞ_0$ (Max posterior and $68\%$ HDI). The measurement of $H_0$ is dominated by the single bright …
We show that the gravitational waves measurements have raised the opportunity to measure $H_0$ with dark sirens to within 2$σ$, the accuracy required to resolve the \hubble tension. There are two principal reasons for our results: (1) upgrades to GW LIGO-Virgo transient catalogues GWTC-1 and GWTC-2 enhance their sensitive with only 10\% of contamination fraction, and (2) new dark sirens should help to constrain our dynamical EoS. In conjunction, sensitivity upgrades and a new dark energy model will facilitate an accurate inference of the \hubble constant $H_0$ to better with an $\pm 0.077$ err…
The study of current gravitational waves (GW) catalogues provide an interesting model independent way to understand further the nature of dark energy. In this work, we present an update of the constrains related to dynamical dark energy parametrisations using recent Gravitational-Wave Transient catalogues (GWTC-1 and GWTC-2) along with Type Ia supernova (SNeIa) and Cosmic Chronometers (CC) catalogues. According to our Bayesian results using the full SNeIa+CC+GW database, the $Λ$CDM model shows a strong preference against two dark energy parameterisation known as Barboza-Alcaniz (BA) and the Lo…
We present a detailed study of the methodology for correlating `dark sirens' (compact binaries coalescences without electromagnetic counterpart) with galaxy catalogs. We propose several improvements on the current state of the art, and we apply them to the GWTC-2 catalog of LIGO/Virgo gravitational wave (GW) detections, and the GLADE galaxy catalog, performing a detailed study of several sources of systematic errors that, with the expected increase in statistics, will eventually become the dominant limitation. We provide a measurement of $H_0$ from dark sirens alone, finding as the best result…
The use of gravitational wave standard sirens for cosmological analyses is becoming well known, with particular interest in measuring the Hubble constant, $H_0$, and in shedding light on the current tension between early- and late-time measurements. The current tension is over $4σ$ and standard sirens will be able to provide a completely independent measurement. Dark sirens (binary black hole or neutron star mergers with no electromagnetic counterparts) can be informative if the missing redshift information is provided through the use of galaxy catalogues to identify potential host galaxies of…
Spectral sirens cosmology from binary black holes populations with sharper mass features
L2IT, Université de Toulouse, CNRS/IN2P3（图卢兹大学）；Laboratoire de Physique de l’ENS, Université Paris Cité, Ecole Normale Supérieure, Université PSL, Sorbonne Université, CNRS（巴黎综合理工学院）
The localization and distance inference of gravitational waves are two crucial factors for dark sirens as precise probes of cosmology, astrophysics, and fundamental physics. In this Letter, for the first time we investigate the parameter estimation of gravitational waves emitted by the eccentric compact binaries in the mid-frequency (0.1--10 Hz) band. Based on the configuration of one cluster of DECIGO (B-DECIGO), we simulate five types of typical compact binaries in GWTC-3 with component mass ranging from $\mathcal{O}(1\sim100)~M_{\odot}$. For each type of binaries, we assign discrete eccentr…
Secondary-Mass Features improve Spectral-Siren $H_0$ Constraints
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Institute for Theoretical Physics and Cosmology, Zhejiang University of Technology（浙江工业大学理论物理与宇宙学研究所）；School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
Consistency between cosmological and standard siren observations in evolving dark energy
Institute of Astrophysics, Department of Physics and Astronomy, Universidad Andrés Bello（安第斯贝尔托大学天体物理研究所）；Department of Physics, University of Oxford（牛津大学物理系）
Calibrating spectral siren cosmology with synthetic catalogs of binary black hole mergers
INFN, Sezione di Roma（意大利国家核物理研究所罗马分部）；Gran Sasso Science Institute（格兰萨索科学研究所）；INFN, Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所格兰萨索国家实验室）；INAF, Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）
Measurement of the Hubble constant using the Dark Energy Survey Year 6 Gold galaxy catalogue and the fourth Gravitational-Wave Transient Catalogue
Physik-Institut, University of Zürich（苏黎世大学物理研究所）；Department of Physics, University of Warwick（华威大学物理系）；L2IT, Laboratoire des 2 Infinis – Toulouse, Université de Toulouse, CNRS/IN2P3, UPS（图卢兹双无穷大实验室（L2IT），图卢兹大学，法国国家科学研究中心/法国国家粒子物理研究所）；HUN-REN–ELTE Extragalactic Astrophysics Research Group（匈牙利研究网络-厄特沃什·罗兰大学河外天体物理学研究组）；Institute for Gravitational Wave Astronomy & School of Physics and Astronomy, University of Birmingham（伯明翰大学引力波天文研究所与物理与天文学学院）；SUPA, University of Glasgow（格拉斯哥大学苏格兰物理与天文学联盟）
Gravitational Wave Propagation in K-essence Cosmology: Theory and Observational Constraints
University of Calcutta（加尔各答大学）；Ben-Gurion University of the Negev（内盖夫本-古里安大学）；Frankfurt Institute for Advanced Studies (FIAS)（法兰克福高等研究所）；Bahamas Advanced Study Institute and Conferences（巴哈马高级研究院与会议）；Sister Nivedita University（尼维蒂达修女大学）；Pontificia Universidad Católica de Valparaíso（瓦爾帕萊索天主教大學）；Prabhat Kumar College（普拉巴特庫瑪學院）；Institute of Astronomy, Space and Earth Science（天文、太空與地球科學研究所）
First measurement of the Hubble constant from gravitational wave-galaxy cross-correlations
Institute of Cosmology and Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）；ICTP South American Institute for Fundamental Research（国际理论物理中心南美基础研究所）；Institut Philippe Meyer, Département de Physique, École Normale Supérieure (ENS), Université PSL（巴黎高等师范学校物理系菲利普·迈耶研究所，PSL大学）；Queen Mary University of London（伦敦玛丽女王大学）；Instituto de Física, Universidade de São Paulo（圣保罗大学物理研究所）；Centro Brasileiro de Pesquisas Físicas（巴西物理研究中心）；Observatório do Valongo, Universidade Federal do Rio de Janeiro（里约热内卢联邦大学瓦隆戈天文台）；PPGCosmo, Universidade Federal do Espírito Santo（圣灵联邦大学宇宙学研究生项目）
首次利用引力波-星系交叉相关性测量哈勃常数，得到H₀=67±18 km s⁻¹Mpc⁻¹及引力波偏置约束。
Eccentricity of compact binaries can improve the parameter estimation of gravitational waves (GWs). In this paper, we first investigate the parameter estimation of eccentric GWs with decihertz observatory. We consider two scenarios for the configuration of DECIGO, i.e., the one cluster of DECIGO with its design sensitivity and B-DECIGO which also has one cluster but with inferior sensitivity as a comparison. We adopt the Fisher matrix to estimate the parameter errors. By mocking up the typical binaries in GWTC-3, we find a nonvanishing eccentricity can significantly improve the estimation for …
