RAS_WEB (Page 2,340)

AstroSat-CZTI as a hard X-ray Pulsar Monitor. (arXiv:2101.08650v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Anusree_K/0/1/0/all/0/1">K.G. Anusree</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharya_D/0/1/0/all/0/1">D. Bhattacharya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_A/0/1/0/all/0/1">A.R. Rao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vadawale_S/0/1/0/all/0/1">S. Vadawale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhalerao_V/0/1/0/all/0/1">V. Bhalerao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vibhute_A/0/1/0/all/0/1">A. Vibhute</a> The Cadmium Zinc Telluride Imager (CZTI) is an imaging instrument onboard AstroSat. This instrument operates as a nearly open all-sky detector above ~60 keV, making possible long integrations irrespective of the spacecraft pointing. We present a technique based on the AstroSat-CZTI data to explore the hard X-ray characteristics of the $gamma$-ray pulsar population. We report highly significant ($sim 30sigma$) detection of hard X-ray (60–380 keV) pulse profile of the Crab pulsar using $sim$5000 ks of CZTI observationsRead More →

The final core collapse of pulsational pair instability supernovae. (arXiv:2101.06889v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Powell_J/0/1/0/all/0/1">Jade Powell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muller_B/0/1/0/all/0/1">Bernhard M&#xfc;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heger_A/0/1/0/all/0/1">Alexander Heger</a> We present 3D core-collapse supernova simulations of massive Pop-III progenitor stars at the transition to the pulsational pair instability regime. We simulate two progenitor models with initial masses of $85,mathrm{M}_{odot}$ and $100,mathrm{M}_odot$ with the LS220, SFHo, and SFHx equations of state. The $85,mathrm{M}_{odot}$ progenitor experiences a pair instability pulse coincident with core collapse, whereas the $100,mathrm{M}_{odot}$ progenitor has already gone through a sequence of four pulses $1mathord,500$ years before collapse in which it ejected its H and He envelope. The $85,mathrm{M}_{odot}$ models experience shockRead More →

SITELLE H{alpha} Imaging Spectroscopy of z~0.25 Clusters: Emission Line Galaxy Detection and Ionized Gas Offset in Abell 2390 & Abell 2465. (arXiv:2101.01887v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Q/0/1/0/all/0/1">Qing Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yee_H/0/1/0/all/0/1">Howard Yee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drissen_L/0/1/0/all/0/1">Laurent Drissen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sivanandam_S/0/1/0/all/0/1">Suresh Sivanandam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pintos_Castro_I/0/1/0/all/0/1">Irene Pintos-Castro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alcorn_L/0/1/0/all/0/1">Leo Y. Alcorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsieh_B/0/1/0/all/0/1">Bau-Ching Hsieh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_L/0/1/0/all/0/1">Lihwai Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_Y/0/1/0/all/0/1">Yen-Ting Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muzzin_A/0/1/0/all/0/1">Adam Muzzin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noble_A/0/1/0/all/0/1">Allison Noble</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Old_L/0/1/0/all/0/1">Lyndsay Old</a> Environmental effects are crucial to the understanding of the evolution of galaxies in dense environments, such as galaxy clusters. Using the large field-of-view of SITELLE, the unique imaging fourier transform spectrograph at CFHT, we are able to obtain 2D spectral information for a largeRead More →

Kilobyte Cosmic Birefringence from ALP Domain Walls. (arXiv:2012.11576v3 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Takahashi_F/0/1/0/all/0/1">Fuminobu Takahashi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Yin_W/0/1/0/all/0/1">Wen Yin</a> ALP domain walls without strings may be formed in the early Universe. We point out that such ALP domain walls lead to both isotropic and anisotropic birefringence of cosmic microwave background (CMB) polarization, which reflects spatial configuration of the domain walls at the recombination. The polarization plane of the CMB photon coming from each domain is either not rotated at all or rotated by a fixed angle. For domain walls following the scaling solution, the cosmic birefringence of CMB is characterized by $2^{N}$, i.e. $N$-bit, of information with $NRead More →

Electroweak Phase Transition with an SU(2) Dark Sector. (arXiv:2012.09758v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Ghosh_T/0/1/0/all/0/1">Tathagata Ghosh</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Guo_H/0/1/0/all/0/1">Huai-Ke Guo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Han_T/0/1/0/all/0/1">Tao Han</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Liu_H/0/1/0/all/0/1">Hongkai Liu</a> We consider a non-Abelian dark SU(2)$_{rm D}$ model where the dark sector couples to the Standard Model (SM) through a Higgs portal. We investigate two different scenarios of the dark sector scalars with $Z_2$ symmetry, with Higgs portal interactions that can introduce mixing between the SM Higgs boson and the SM singlet scalars in the dark sector. We utilize the existing collider results of the Higgs signal rate, direct heavy Higgs searches, and electroweak precision observables to constrain the model parameters. TheRead More →

Bayesian analysis of the spin distribution of LIGO/Virgo black holes. (arXiv:2010.13811v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">Juan Garcia-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siles_J/0/1/0/all/0/1">Jose Francisco Nu&#xf1;o Siles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_E/0/1/0/all/0/1">Ester Ruiz Morales</a> Gravitational wave detection from binary black hole (BBH) inspirals has become routine thanks to the LIGO/Virgo interferometers. The nature of these back holes remains uncertain. We study here the spin distributions of LIGO/Virgo black holes from the first catalogue GWTC-1 and the first four published BBH events from run O3. We compute the Bayes evidence for several independent priors: flat, isotropic, spin-aligned and anti-aligned. We find strong evidence for low spins in all of the cases, and significant evidence forRead More →

Study of Blazar activity in 10 year Fermi-LAT data and implications for TeV neutrino expectations. (arXiv:2011.13043v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sacahui_J/0/1/0/all/0/1">J. R. Sacahui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penacchioni_A/0/1/0/all/0/1">A. V. Penacchioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marinelli_A/0/1/0/all/0/1">A. Marinelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_A/0/1/0/all/0/1">A. Sharma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castro_M/0/1/0/all/0/1">M. Castro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osorio_J/0/1/0/all/0/1">J. M. Osorio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_M/0/1/0/all/0/1">M. A. Morales</a> Blazars are the most active extragalactic gamma-ray sources. They show sporadic bursts of activity, lasting from hours to months. In this work we present a 10-year analysis of a sample of bright sources detected by Fermi-LAT (100 MeV – 300 GeV). Using 2-week binned lightcurves (LC) we estimated the Duty Cycle (DC): fraction of time that the source spends in an activeRead More →

Search for inelastic scattering of WIMP dark matter in XENON1T. (arXiv:2011.10431v2 [hep-ex] UPDATED) <a href="http://arxiv.org/find/hep-ex/1/au:+Collaboration_XENON/0/1/0/all/0/1">XENON Collaboration</a>: <a href="http://arxiv.org/find/hep-ex/1/au:+Aprile_E/0/1/0/all/0/1">E. Aprile</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Aalbers_J/0/1/0/all/0/1">J. Aalbers</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Agostini_F/0/1/0/all/0/1">F. Agostini</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Alfonsi_M/0/1/0/all/0/1">M. Alfonsi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Althueser_L/0/1/0/all/0/1">L. Althueser</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Amaro_F/0/1/0/all/0/1">F. D. Amaro</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Andaloro_S/0/1/0/all/0/1">S. Andaloro</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Angelino_E/0/1/0/all/0/1">E. Angelino</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Angevaare_J/0/1/0/all/0/1">J. R. Angevaare</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Antochi_V/0/1/0/all/0/1">V. C. Antochi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Arneodo_F/0/1/0/all/0/1">F. Arneodo</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Baudis_L/0/1/0/all/0/1">L. Baudis</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bauermeister_B/0/1/0/all/0/1">B. Bauermeister</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bellagamba_L/0/1/0/all/0/1">L. Bellagamba</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Benabderrahmane_M/0/1/0/all/0/1">M. L. Benabderrahmane</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Brown_A/0/1/0/all/0/1">A. Brown</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Brown_E/0/1/0/all/0/1">E. Brown</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bruenner_S/0/1/0/all/0/1">S. Bruenner</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bruno_G/0/1/0/all/0/1">G. Bruno</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Budnik_R/0/1/0/all/0/1">R. Budnik</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Capelli_C/0/1/0/all/0/1">C. Capelli</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cardoso_J/0/1/0/all/0/1">J. M. R. Cardoso</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cichon_D/0/1/0/all/0/1">D. Cichon</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cimmino_B/0/1/0/all/0/1">B. Cimmino</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Clark_M/0/1/0/all/0/1">M. Clark</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Coderre_D/0/1/0/all/0/1">D. Coderre</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Colijn_A/0/1/0/all/0/1">A. P. Colijn</a>, <aRead More →

The Search for Fast Transients with CZTI. (arXiv:2011.07067v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_Y/0/1/0/all/0/1">Y. Sharma</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Marathe_A/0/1/0/all/0/1">A. Marathe</a> (2 and 3), <a href="http://arxiv.org/find/astro-ph/1/au:+Bhalerao_V/0/1/0/all/0/1">V. Bhalerao</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Shenoy_V/0/1/0/all/0/1">V. Shenoy</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Waratkar_G/0/1/0/all/0/1">G. Waratkar</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Nadella_D/0/1/0/all/0/1">D. Nadella</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Page_P/0/1/0/all/0/1">P. Page</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Hebbar_P/0/1/0/all/0/1">P. Hebbar</a> (2 and 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Vibhute_A/0/1/0/all/0/1">A. Vibhute</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharya_D/0/1/0/all/0/1">D. Bhattacharya</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_A/0/1/0/all/0/1">A.R. Rao</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Vadawale_S/0/1/0/all/0/1">S. Vadawale</a> (7) ((1) Division of Physics Mathematics and Astronomy California Institute of Technology, (2) Indian Institute of Technology Bombay, (3) National Institute of Technology Karnataka, (4) University of Alberta Edmonton, (5) Inter-University Centre for Astronomy and Astrophysics India, (6) Tata Institute of FundamentalRead More →

Neutrino refractive effects during their decoupling era in the early universe. (arXiv:2011.05456v4 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Sawyer_R/0/1/0/all/0/1">R. F. Sawyer</a> There is an accepted approach to calculation of the neutrino flavor density-matrix in the halo of a supernova, in which neutrino amplitudes, not cross-sections, need to be followed carefully in the region above the region of frequent scatterings. The same reasoning and techniques, applied to the evolution of neutrino flavors and energy distributions in the early universe in the era of neutrino decoupling, leads to radical changes in the prediction of the effects of the neutrino-neutrino interaction. Predictions for the production of sterile neutrinos, should they exist,Read More →

MAGNUM survey: Compact jets causing large turmoil in galaxies — Enhanced line widths perpendicular to radio jets as tracers of jet-ISM interaction. (arXiv:2011.04677v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Venturi_G/0/1/0/all/0/1">G. Venturi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cresci_G/0/1/0/all/0/1">G. Cresci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marconi_A/0/1/0/all/0/1">A. Marconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mingozzi_M/0/1/0/all/0/1">M. Mingozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nardini_E/0/1/0/all/0/1">E. Nardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carniani_S/0/1/0/all/0/1">S. Carniani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mannucci_F/0/1/0/all/0/1">F. Mannucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marasco_A/0/1/0/all/0/1">A. Marasco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiolino_R/0/1/0/all/0/1">R. Maiolino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perna_M/0/1/0/all/0/1">M. Perna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Treister_E/0/1/0/all/0/1">E. Treister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bland_Hawthorn_J/0/1/0/all/0/1">J. Bland-Hawthorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallimore_J/0/1/0/all/0/1">J. Gallimore</a> Outflows accelerated by AGN are commonly observed in the form of coherent, mildly collimated high-velocity gas directed along the AGN ionisation cones and kinetically powerful (>$10^{44-45}$ erg/s) jets. Recent works found that outflows can also be accelerated by low-power (<$10^{44}$ erg/s)Read More →

Superconducting phases in a two-component microscale model of neutron star cores. (arXiv:2011.02873v2 [cond-mat.supr-con] UPDATED) <a href="http://arxiv.org/find/cond-mat/1/au:+Wood_T/0/1/0/all/0/1">Toby S. Wood</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Graber_V/0/1/0/all/0/1">Vanessa Graber</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Newton_W/0/1/0/all/0/1">William G. Newton</a> We identify the possible ground states for a mixture of two superfluid condensates (one neutral, the other electrically charged) using a phenomenological Ginzburg-Landau model. While this framework is applicable to any interacting condensed-matter mixture of a charged and a neutral component, we focus on nuclear matter in neutron star cores, where proton and neutron condensates are coupled via non-dissipative entrainment. We employ the Skyrme interaction to determine the neutron star’s equilibrium composition, and hence obtain realistic coefficients for our Ginzburg-LandauRead More →

Measuring the Mass of Missing Baryons in the Halo of Andromeda Galaxy with Gamma-Ray Observations. (arXiv:2010.15477v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Y/0/1/0/all/0/1">Yi Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_R/0/1/0/all/0/1">Ruo-Yu Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hui Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shao_S/0/1/0/all/0/1">Shi Shao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_H/0/1/0/all/0/1">Huirong Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_X/0/1/0/all/0/1">Xiang-Yu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_X/0/1/0/all/0/1">Xiao-Na Sun</a> One of the biggest mysteries in the modern cosmology and galaxy formation is the hideout of the “missing baryons”. The leading theory of galaxy formation predicts that a huge amount of baryons resides around galaxies extending out to their virial radii in the form of diffuse and hot gas of $10^6-10^7,$K, which is also known as the major component of the circumgalactic medium (CGM). Studies byRead More →

Population Properties of Compact Objects from the Second LIGO-Virgo Gravitational-Wave Transient Catalog. (arXiv:2010.14533v2 [astro-ph.HE] UPDATED) The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_LIGO_Scientific/0/1/0/all/0/1">LIGO Scientific Collaboration</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Virgo/0/1/0/all/0/1">Virgo Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_R/0/1/0/all/0/1">R. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. D. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_S/0/1/0/all/0/1">S. Abraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Acernese_F/0/1/0/all/0/1">F. Acernese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ackley_K/0/1/0/all/0/1">K. Ackley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_A/0/1/0/all/0/1">A. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_C/0/1/0/all/0/1">C. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_R/0/1/0/all/0/1">R. X. Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adya_V/0/1/0/all/0/1">V. B. Adya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Affeldt_C/0/1/0/all/0/1">C. Affeldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agathos_M/0/1/0/all/0/1">M. Agathos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agatsuma_K/0/1/0/all/0/1">K. Agatsuma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aggarwal_N/0/1/0/all/0/1">N. Aggarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguiar_O/0/1/0/all/0/1">O. D. Aguiar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiello_L/0/1/0/all/0/1">L. Aiello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ain_A/0/1/0/all/0/1">A. Ain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ajith_P/0/1/0/all/0/1">P. Ajith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_G/0/1/0/all/0/1">G. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allocca_A/0/1/0/all/0/1">A. Allocca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altin_P/0/1/0/all/0/1">P. A. Altin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amato_A/0/1/0/all/0/1">A. Amato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anand_S/0/1/0/all/0/1">S. Anand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ananyeva_A/0/1/0/all/0/1">A. Ananyeva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_S/0/1/0/all/0/1">S. B. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_W/0/1/0/all/0/1">W. G.Read More →

GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run. (arXiv:2010.14527v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Abbott_R/0/1/0/all/0/1">R. Abbott</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Abbott_T/0/1/0/all/0/1">T. D. Abbott</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Abraham_S/0/1/0/all/0/1">S. Abraham</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Acernese_F/0/1/0/all/0/1">F. Acernese</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ackley_K/0/1/0/all/0/1">K. Ackley</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Adams_A/0/1/0/all/0/1">A. Adams</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Adams_C/0/1/0/all/0/1">C. Adams</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Adhikari_R/0/1/0/all/0/1">R. X. Adhikari</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Adya_V/0/1/0/all/0/1">V. B. Adya</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Affeldt_C/0/1/0/all/0/1">C. Affeldt</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Agathos_M/0/1/0/all/0/1">M. Agathos</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Agatsuma_K/0/1/0/all/0/1">K. Agatsuma</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Aggarwal_N/0/1/0/all/0/1">N. Aggarwal</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Aguiar_O/0/1/0/all/0/1">O. D. Aguiar</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Aiello_L/0/1/0/all/0/1">L. Aiello</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ain_A/0/1/0/all/0/1">A. Ain</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ajith_P/0/1/0/all/0/1">P. Ajith</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Akcay_S/0/1/0/all/0/1">S. Akcay</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Allen_G/0/1/0/all/0/1">G. Allen</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Allocca_A/0/1/0/all/0/1">A. Allocca</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Altin_P/0/1/0/all/0/1">P. A. Altin</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Amato_A/0/1/0/all/0/1">A. Amato</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Anand_S/0/1/0/all/0/1">S. Anand</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ananyeva_A/0/1/0/all/0/1">A. Ananyeva</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Anderson_S/0/1/0/all/0/1">S. B. Anderson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Anderson_W/0/1/0/all/0/1">W. G.Read More →