ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914
B. P. AbbottLIGO, California Institute of Technology, Pasadena, CA 91125, USAR. AbbottLIGO, California Institute of Technology, Pasadena, CA 91125, USAT. D. AbbottLouisiana State University, Baton Rouge, LA 70803, USAM. R. AbernathyLIGO, California Institute of Technology, Pasadena, CA 91125, USAF. AcerneseINFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, ItalyK. AckleyUniversity of Florida, Gainesville, FL 32611, USAC. AdamsLIGO Livingston Observatory, Livingston, LA 70754, USAT. AdamsLaboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy-le-Vieux, FranceP. AddessoUniversità di Salerno, Fisciano, I-84084 Salerno, ItalyR. X. AdhikariLIGO, California Institute of Technology, Pasadena, CA 91125, USAV. B. AdyaAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyC. AffeldtAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyM. AgathosNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsK. AgatsumaNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsN. AggarwalLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAO. D. AguiarInstituto Nacional de Pesquisas Espaciais, 12227-010 São José, dos Campos, SP, BrazilL. AielloINFN, Gran Sasso Science Institute, I-67100 L'Aquila, ItalyA. AinInter-University Centre for Astronomy and Astrophysics, Pune 411007, IndiaP. AjithInternational Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bangalore 560012, IndiaB. AllenUniversity of Wisconsin-Milwaukee, Milwaukee, WI 53201, USAA. AlloccaINFN, Sezione di Pisa, I-56127 Pisa, ItalyP. A. AltinAustralian National University, Canberra, Australian Capital Territory 0200, AustraliaS. B. AndersonLIGO, California Institute of Technology, Pasadena, CA 91125, USAW. G. AndersonUniversity of Wisconsin-Milwaukee, Milwaukee, WI 53201, USAK. AraiLIGO, California Institute of Technology, Pasadena, CA 91125, USAM. C. ArayaLIGO, California Institute of Technology, Pasadena, CA 91125, USAC. C. ArceneauxThe University of Mississippi, Oxford, MS 38677, USAJ. S. AreedaCalifornia State University Fullerton, Fullerton, CA 92831, USAN. ArnaudLAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, Orsay, FranceK. G. ArunChennai Mathematical Institute, Chennai, IndiaS. AscenziUniversità di Roma Tor Vergata, I-00133 Roma, ItalyG. AshtonUniversity of Southampton, Southampton SO17 1BJ, UKM. AstUniversität Hamburg, D-22761 Hamburg, GermanyS. M. AstonLIGO Livingston Observatory, Livingston, LA 70754, USAP. AstoneINFN, Sezione di Roma, I-00185 Roma, ItalyP. AufmuthAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyC. AulbertAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyS. BabakAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Potsdam-Golm, GermanyP. BaconAPC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, FranceM. K. M. BaderNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsP. T. BakerMontana State University, Bozeman, MT 59717, USAF. BaldacciniINFN, Sezione di Perugia, I-06123 Perugia, ItalyG. BallardinEuropean Gravitational Observatory (EGO), I-56021 Cascina, Pisa, ItalyS. W. BallmerSyracuse University, Syracuse, NY 13244, USAJ. C. BarayogaLIGO, California Institute of Technology, Pasadena, CA 91125, USAS. E. BarclaySUPA, University of Glasgow, Glasgow G12 8QQ, UKB. C. BarishLIGO, California Institute of Technology, Pasadena, CA 91125, USAD. BarkerF. BaroneINFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, ItalyB. BarrSUPA, University of Glasgow, Glasgow G12 8QQ, UKL. BarsottiLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAM. BarsugliaAPC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, FranceD. BartaWigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklós út 29-33, HungaryJ. BartlettI. BartosColumbia University, New York, NY 10027, USAR. BassiriStanford University, Stanford, CA 94305, USAA. BastiUniversità di Pisa, I-56127 Pisa, ItalyJ. C. BatchC. BauneAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyV. BavigaddaEuropean Gravitational Observatory (EGO), I-56021 Cascina, Pisa, ItalyM. BazzanUniversità di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, ItalyB. BehnkeAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Potsdam-Golm, GermanyM. BejgerKrzysztof BelczyńskiAstronomical Observatory Warsaw University, 00-478 Warsaw, PolandA. S. BellSUPA, University of Glasgow, Glasgow G12 8QQ, UKC. BellSUPA, University of Glasgow, Glasgow G12 8QQ, UKB. K. BergerLIGO, California Institute of Technology, Pasadena, CA 91125, USAJ. BergmanG. BergmannAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyC. P. L. BerryUniversity of Birmingham, Birmingham B15 2TT, UKD. BersanettiINFN, Sezione di Genova, I-16146 Genova, ItalyA. BertoliniNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsJ. BetzwieserLIGO Livingston Observatory, Livingston, LA 70754, USAS. BhagwatSyracuse University, Syracuse, NY 13244, USAR. BhandareRRCAT, Indore MP 452013, IndiaI. A. BilenkoFaculty of Physics, Lomonosov Moscow State University, Moscow 119991, RussiaG. BillingsleyLIGO, California Institute of Technology, Pasadena, CA 91125, USAJ. BirchLIGO Livingston Observatory, Livingston, LA 70754, USAR. BirneySUPA, University of the West of Scotland, Paisley PA1 2BE, UKS. BiscansLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAA. BishtLeibniz Universität Hannover, D-30167 Hannover, GermanyM. BitossiEuropean Gravitational Observatory (EGO), I-56021 Cascina, Pisa, ItalyC. BiwerSyracuse University, Syracuse, NY 13244, USAM. A. BizouardLAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, Orsay, FranceJ. K. BlackburnLIGO, California Institute of Technology, Pasadena, CA 91125, USAC. D. BlairUniversity of Western Australia, Crawley, Western Australia 6009, AustraliaD. G. BlairUniversity of Western Australia, Crawley, Western Australia 6009, AustraliaR. M. BlairS. BloemenDepartment of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The NetherlandsO. BockAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyT. P. BodiyaLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAM. BoërArtemis, Université Côte d'Azur, CNRS, Observatoire Côte d'Azur, CS F-34229, Nice cedex 4, FranceG. BogaertArtemis, Université Côte d'Azur, CNRS, Observatoire Côte d'Azur, CS F-34229, Nice cedex 4, FranceC. BoganAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, GermanyA. BohéAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Potsdam-Golm, GermanyP. BojtosMTA Eötvös University, "Lendulet" Astrophysics Research Group, Budapest 1117, HungaryC. BondUniversity of Birmingham, Birmingham B15 2TT, UKF. BonduInstitut de Physique de Rennes, CNRS, Université de Rennes 1, F-35042 Rennes, FranceR. BonnandLaboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy-le-Vieux, FranceB. A. BoomNikhef, Science Park, 1098 XG Amsterdam, The Netherlands
2016en
ABI
Аннотация
ABSTRACT The discovery of the gravitational-wave (GW) source GW150914 with the Advanced LIGO detectors provides the first observational evidence for the existence of binary black hole (BH) systems that inspiral and merge within the age of the universe. Such BH mergers have been predicted in two main types of formation models, involving isolated binaries in galactic fields or dynamical interactions in young and old dense stellar environments. The measured masses robustly demonstrate that relatively “heavy” BHs ( ) can form in nature. This discovery implies relatively weak massive-star winds and thus the formation of GW150914 in an environment with a metallicity lower than about 1/2 of the solar value. The rate of binary-BH (BBH) mergers inferred from the observation of GW150914 is consistent with the higher end of rate predictions ( Gpc −3 yr −1 ) from both types of formation models. The low measured redshift ( ) of GW150914 and the low inferred metallicity of the stellar progenitor imply either BBH formation in a low-mass galaxy in the local universe and a prompt merger, or formation at high redshift with a time delay between formation and merger of several Gyr. This discovery motivates further studies of binary-BH formation astrophysics. It also has implications for future detections and studies by Advanced LIGO and Advanced Virgo, and GW detectors in space.
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