36 research outputs found
Dark siren cosmology with binary black holes in the era of third-generation gravitational wave detectors
Third-generation (3G) gravitational wave detectors, in particular Einstein
Telescope (ET) and Cosmic Explorer (CE), will explore unprecedented cosmic
volumes in search for compact binary mergers, providing us with tens of
thousands of detections per year. In this study, we simulate and employ binary
black holes detected by 3G interferometers as dark sirens, to extract and infer
cosmological parameters by cross-matching gravitational wave data with
electromagnetic information retrieved from a simulated galaxy catalog.
Considering a standard CDM model, we apply a suitable Bayesian
framework to obtain joint posterior distributions for the Hubble constant
and the matter energy density parameter in different scenarios.
Assuming a galaxy catalog complete up to and dark sirens detected with a
network signal-to-noise ratio greater than 300, we show that a network made of
ET and two CEs can constrain () to a promising
() at confidence interval within one year of continuous
observations. Additionally, we find that most of the information on is
contained in local, single-host dark sirens, and that dark sirens at do
not substantially improve these estimates. Our results imply that a sub-percent
measure of can confidently be attained by a network of 3G detectors,
highlighting the need for characterising all systematic effects to a higher
accuracy.Comment: 23 pages, 8 figures. Major update on results, updated figures, v2
accepted for publication in PR
Bekenstein-Hod universal bound on information emission rate is obeyed by LIGO-Virgo binary black hole remnants
Causality and the generalized laws of black hole thermodynamics imply a bound, known as the Bekenstein-Hod universal bound, on the information emission rate of a perturbed system. Using a time-domain ringdown analysis, we investigate whether remnant black holes produced by the coalescences observed by Advanced LIGO and Advanced Virgo obey this bound. We find that the bound is verified by the astrophysical black hole population with 94% probability, providing a first confirmation of the Bekenstein-Hod bound from black hole systems
Eigenvalue repulsions in the quasinormal spectra of the Kerr-Newman black hole
We study the gravito-electromagnetic perturbations of the Kerr-Newman (KN)
black hole metric and identify the two photon sphere and near-horizon
families of quasinormal modes (QNMs) of the KN black hole, computing the
frequency spectra (for all the KN parameter space) of the modes with the
slowest decay rate. We uncover a novel phenomenon for QNMs that is unique to
the KN system, namely eigenvalue repulsion between QNM families. Such a feature
is common in solid state physics where \eg it is responsible for energy
bands/gaps in the spectra of electrons moving in certain Schr\"odinger
potentials. Exploiting the enhanced symmetries of the near-horizon limit of the
near-extremal KN geometry we also develop a matching asymptotic expansion that
allows us to solve the perturbation problem using separation of variables and
provides an excellent approximation to the KN QNM spectra near extremality. The
KN QNM spectra here derived are required not only to account for the
gravitational emission in astrophysical environments, such as the ones probed
by LIGO, Virgo and LISA, but also allow to extract observational implications
on several new physics scenarios, such as mini-charged dark-matter or certain
modified theories of gravity, degenerate with the KN solution at the scales of
binary mergers.Comment: 9 pages, 2 figure
ICAROGW: A python package for inference of astrophysical population properties of noisy, heterogeneous and incomplete observations
We present icarogw 2.0, a pure CPU/GPU python code developed to infer
astrophysical and cosmological population properties of noisy, heterogeneous,
and incomplete observations. icarogw 2.0 is mainly developed for compact binary
coalescence (CBC) population inference with gravitational wave (GW)
observations. The code contains several models for masses, spins, and redshift
of CBC distributions, and is able to infer population distributions as well as
the cosmological parameters and possible general relativity deviations at
cosmological scales. We present the theoretical and computational foundations
of icarogw, and we describe how the code can be employed for population and
cosmological inference using (i) only GWs, (ii) GWs and galaxy surveys and
(iii) GWs with electromagnetic counterparts. Although icarogw 2.0 has been
developed for GW science, we also describe how the code can be used for any
physical and astrophysical problem involving observations from noisy data in
the presence of selection biases. With this paper, we also release tutorials on
Zenodo.Comment: 33 pages, code available at
(https://github.com/simone-mastrogiovanni/icarogw), tutorials available at
(https://zenodo.org/record/7846415#.ZG0l0NJBxQo
Joint population and cosmological properties inference with gravitational waves standard sirens and galaxy surveys
Gravitational wave (GW) sources at cosmological distances can be used to probe the expansion rate of the Universe. GWs directly provide a distance estimation of the source but no direct information on its redshift. The optimal scenario to obtain a redshift is through the direct identification of an electromagnetic (EM) counterpart and its host galaxy. With almost 100 GW sources detected without EM counterparts (dark sirens), it is becoming crucial to have statistical techniques able to perform cosmological studies in the absence of EM emission. Currently, only two techniques for dark sirens are used on GW observations; the spectral siren method, which is based on the source-frame mass distribution to estimate conjointly cosmology and the source’s merger rate, and the galaxy survey method, which uses galaxy surveys to assign a probabilistic redshift to the source while fitting cosmology. It has been recognized, however, that these two methods are two sides of the same coin. In this paper, we present a novel approach to unify these two methods. We apply this approach to several observed GW events using the glade+ galaxy catalog discussing limiting cases. We provide estimates of the Hubble constant, modified gravity propagation effects, and population properties for binary black holes. We also estimate the binary black hole merger rate per galaxy to be 10−6–10−5 yr−1 depending on the galaxy catalog hypotheses
Cosmology with the Laser Interferometer Space Antenna
254 pags:, 44 figs.The Laser Interferometer Space Antenna (LISA) has two scientific objectives of cosmological focus: to probe the expansion rate of the universe, and to understand stochastic gravitational-wave backgrounds and their implications for early universe and particle physics, from the MeV to the Planck scale. However, the range of potential cosmological applications of gravitational-wave observations extends well beyond these two objectives. This publication presents a summary of the state of the art in LISA cosmology, theory and methods, and identifies new opportunities to use gravitational-wave observations by LISA to probe the universe.This work is partly supported by: A.G. Leventis Foundation; Academy of Finland
Grants 328958 and 345070; Alexander S. Onassis Foundation, Scholarship ID: FZO 059-1/2018-2019;
Amaldi Research Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP:
B81I18001170001); ASI Grants No. 2016-24-H.0 and No. 2016-24-H.1-2018; Atracción de Talento
Grant 2019-T1/TIC-15784; Atracción de Talento contract no. 2019-T1/TIC-13177 granted by the
Comunidad de Madrid; Ayuda ‘Beatriz Galindo Senior’ by the Spanish ‘Ministerio de Universidades’,
Grant BG20/00228; Basque Government Grant (IT-979-16); Belgian Francqui Foundation; Centre national
d’Etudes spatiales; Ben Gurion University Kreitman Fellowship, and the Israel Academy of Sciences and
Humanities (IASH) & Council for Higher Education (CHE) Excellence Fellowship Program for
International Postdoctoral Researchers; Centro de Excelencia Severo Ochoa Program SEV-2016-0597;
CERCA program of the Generalitat de Catalunya; Cluster of Excellence “Precision Physics, Fundamental
Interactions, and Structure of Matter” (PRISMA? EXC 2118/1); Comunidad de Madrid, Contrato de
Atracción de Talento 2017-T1/TIC-5520; Czech Science Foundation GAČR, Grant No. 21-16583M; Delta
ITP consortium; Department of Energy under Grant No. DE-SC0008541, DE-SC0009919 and DESC0019195; Deutsche Forschungsgemeinschaft (DFG), Project ID 438947057; Deutsche Forschungsgemeinschaft under Germany’s Excellence Strategy - EXC 2121 Quantum Universe - 390833306; European
Structural and Investment Funds and the Czech Ministry of Education, Youth and Sports (Project
CoGraDS - CZ.02.1.01/0.0/0.0/15 003/0000437); European Union’s H2020 ERC Consolidator Grant
“GRavity from Astrophysical to Microscopic Scales” (Grant No. GRAMS-815673); European Union’s
H2020 ERC, Starting Grant Agreement No. DarkGRA-757480; European Union’s Horizon 2020
programme under the Marie Sklodowska-Curie Grant Agreement 860881 (ITN HIDDeN); European
Union’s Horizon 2020 Research and Innovation Programme Grant No. 796961, “AxiBAU” (K.S.);
European Union’s Horizon 2020 Research Council grant 724659 MassiveCosmo ERC-2016-COG; FCT
through national funds (PTDC/FIS-PAR/31938/2017) and through project “BEYLA – BEYond LAmbda”
with Ref. Number PTDC/FIS-AST/0054/2021; FEDER-Fundo Europeu de Desenvolvimento Regional
through COMPETE2020 - Programa Operacional Competitividade e Internacionalização (POCI-01-0145-
FEDER-031938) and research Grants UIDB/04434/2020 and UIDP/04434/2020; Fondation CFM pour la
Recherche in France; Foundation for Education and European Culture in Greece; French ANR project
MMUniverse (ANR-19-CE31-0020); FRIA Grant No.1.E.070.19F of the Belgian Fund for Research, F.R.
S.-FNRS Fundação para a Ciência e a Tecnologia (FCT) through Contract No. DL 57/2016/CP1364/
CT0001; Fundação para a Ciência e a Tecnologia (FCT) through Grants UIDB/04434/2020, UIDP/04434/
2020, PTDC/FIS-OUT/29048/2017, CERN/FIS-PAR/0037/2019 and “CosmoTests – Cosmological tests of
gravity theories beyond General Relativity” CEECIND/00017/2018; Generalitat Valenciana Grant
PROMETEO/2021/083; Grant No. 758792, project GEODESI; Government of Canada through the
Department of Innovation, Science and Economic Development and Province of Ontario through the
Ministry of Colleges and Universities; Grants-in-Aid for JSPS Overseas Research Fellow (No.
201960698); I?D Grant PID2020-118159GB-C41 of the Spanish Ministry of Science and Innovation;
INFN iniziativa specifica TEONGRAV; Israel Science Foundation (Grant No. 2562/20); Japan Society for
the Promotion of Science (JSPS) KAKENHI Grant Nos. 20H01899 and 20H05853; IFT Centro de
Excelencia Severo Ochoa Grant SEV-2; Kavli Foundation and its founder Fred Kavli; Minerva
Foundation; Ministerio de Ciencia e Innovacion Grant PID2020-113644GB-I00; NASA Grant
80NSSC19K0318; NASA Hubble Fellowship grants No. HST-HF2-51452.001-A awarded by the Space
Telescope Science Institute with NASA contract NAS5-26555; Netherlands Organisation for Science and
Research (NWO) Grant Number 680-91-119; new faculty seed start-up grant of the Indian Institute of
Science, Bangalore, the Core Research Grant CRG/2018/002200 of the Science and Engineering; NSF
Grants PHY-1820675, PHY-2006645 and PHY-2011997; Polish National Science Center Grant 2018/31/D/
ST2/02048; Polish National Agency for Academic Exchange within the Polish Returns Programme under
Agreement PPN/PPO/2020/1/00013/U/00001; Pró-Reitoria de Pesquisa of Universidade Federal de Minas
Gerais (UFMG) under Grant No. 28359; Ramón y Cajal Fellowship contract RYC-2017-23493; Research
Project PGC2018-094773-B-C32 [MINECO-FEDER]; Research Project PGC2018-094773-B-C32
[MINECO-FEDER]; ROMFORSK Grant Project. No. 302640; Royal Society Grant URF/R1/180009
and ERC StG 949572: SHADE; Shota Rustaveli National Science Foundation (SRNSF) of Georgia (Grant
FR/18-1462); Simons Foundation/SFARI 560536; SNSF Ambizione grant; SNSF professorship Grant
(No. 170547); Spanish MINECO’s “Centro de Excelencia Severo Ochoa” Programme Grants SEV-2016-
0597 and PID2019-110058GB-C22; Spanish Ministry MCIU/AEI/FEDER Grant (PGC2018-094626-BC21); Spanish Ministry of Science and Innovation (PID2020-115845GB-I00/AEI/10.13039/
501100011033); Spanish Proyectos de I?D via Grant PGC2018-096646-A-I00; STFC Consolidated
Grant ST/T000732/1; STFC Consolidated Grants ST/P000762/1 and ST/T000791/1; STFC Grant ST/
S000550/1; STFC Grant ST/T000813/1; STFC Grants ST/P000762/1 and ST/T000791/1; STFC under the
research Grant ST/P000258/1; Swiss National Science Foundation (SNSF), project The Non-Gaussian
Universe and Cosmological Symmetries, Project Number: 200020-178787; Swiss National Science
Foundation Professorship Grants No. 170547 and No. 191957; SwissMap National Center for Competence
in Research; “The Dark Universe: A Synergic Multi-messenger Approach” Number 2017X7X85K under
the MIUR program PRIN 2017; UK Space Agency; UKSA Flagship Project, Euclid.Peer reviewe
Observation of gravitational waves from the coalescence of a 2.5−4.5 M⊙ compact object and a neutron star
Search for gravitational-lensing signatures in the full third observing run of the LIGO-Virgo network
Gravitational lensing by massive objects along the line of sight to the source causes distortions of gravitational wave-signals; such distortions may reveal information about fundamental physics, cosmology and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO--Virgo network. We search for repeated signals from strong lensing by 1) performing targeted searches for subthreshold signals, 2) calculating the degree of overlap amongst the intrinsic parameters and sky location of pairs of signals, 3) comparing the similarities of the spectrograms amongst pairs of signals, and 4) performing dual-signal Bayesian analysis that takes into account selection effects and astrophysical knowledge. We also search for distortions to the gravitational waveform caused by 1) frequency-independent phase shifts in strongly lensed images, and 2) frequency-dependent modulation of the amplitude and phase due to point masses. None of these searches yields significant evidence for lensing. Finally, we use the non-detection of gravitational-wave lensing to constrain the lensing rate based on the latest merger-rate estimates and the fraction of dark matter composed of compact objects
Search for eccentric black hole coalescences during the third observing run of LIGO and Virgo
Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that were already identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total mass M>70 M⊙) binaries covering eccentricities up to 0.3 at 15 Hz orbital frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place an upper limit for the merger rate density of high-mass binaries with eccentricities 0<e≤0.3 at 0.33 Gpc−3 yr−1 at 90\% confidence level