双黑洞合并GW150914的特性
Properties of the Binary Black Hole Merger GW150914.
作者信息
Abbott B P, Abbott R, Abbott T D, Abernathy M R, Acernese F, Ackley K, Adams C, Adams T, Addesso P, Adhikari R X, Adya V B, Affeldt C, Agathos M, Agatsuma K, Aggarwal N, Aguiar O D, Aiello L, Ain A, Ajith P, Allen B, Allocca A, Altin P A, Anderson S B, Anderson W G, Arai K, Araya M C, Arceneaux C C, Areeda J S, Arnaud N, Arun K G, Ascenzi S, Ashton G, Ast M, Aston S M, Astone P, Aufmuth P, Aulbert C, Babak S, Bacon P, Bader M K M, Baker P T, Baldaccini F, Ballardin G, Ballmer S W, Barayoga J C, Barclay S E, Barish B C, Barker D, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Bartos I, Bassiri R, Basti A, Batch J C, Baune C, Bavigadda V, Bazzan M, Behnke B, Bejger M, Bell A S, Bell C J, Berger B K, Bergman J, Bergmann G, Berry C P L, Bersanetti D, Bertolini A, Betzwieser J, Bhagwat S, Bhandare R, Bilenko I A, Billingsley G, Birch J, Birney R, Birnholtz O, Biscans S, Bisht A, Bitossi M, Biwer C, Bizouard M A, Blackburn J K, Blair C D, Blair D G, Blair R M, Bloemen S, Bock O, Bodiya T P, Boer M, Bogaert G, Bogan C, Bohe A, Bojtos P, Bond C, Bondu F, Bonnand R, Boom B A, Bork R, Boschi V, Bose S, Bouffanais Y, Bozzi A, Bradaschia C, Brady P R, Braginsky V B, Branchesi M, Brau J E, Briant T, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks A F, Brown D A, Brown D D, Brown N M, Buchanan C C, Buikema A, Bulik T, Bulten H J, Buonanno A, Buskulic D, Buy C, Byer R L, Cadonati L, Cagnoli G, Cahillane C, Calderón Bustillo J, Callister T, Calloni E, Camp J B, Cannon K C, Cao J, Capano C D, Capocasa E, Carbognani F, Caride S, Casanueva Diaz J, Casentini C, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cepeda C B, Cerboni Baiardi L, Cerretani G, Cesarini E, Chakraborty R, Chalermsongsak T, Chamberlin S J, Chan M, Chao S, Charlton P, Chassande-Mottin E, Chen H Y, Chen Y, Cheng C, Chincarini A, Chiummo A, Cho H S, Cho M, Chow J H, Christensen N, Chu Q, Chua S, Chung S, Ciani G, Clara F, Clark J A, Cleva F, Coccia E, Cohadon P-F, Colla A, Collette 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J, Hall B R, Hall E D, Hammond G, Haney M, Hanke M M, Hanks J, Hanna C, Hannam M D, Hanson J, Hardwick T, Harms J, Harry G M, Harry I W, Hart M J, Hartman M T, Haster C-J, Haughian K, Healy J, Heidmann A, Heintze M C, Heitmann H, Hello P, Hemming G, Hendry M, Heng I S, Hennig J, Heptonstall A W, Heurs M, Hild S, Hoak D, Hodge K A, Hofman D, Hollitt S E, Holt K, Holz D E, Hopkins P, Hosken D J, Hough J, Houston E A, Howell E J, Hu Y M, Huang S, Huerta E A, Huet D, Hughey B, Husa S, Huttner S H, Huynh-Dinh T, Idrisy A, Indik N, Ingram D R, Inta R, Isa H N, Isac J-M, Isi M, Islas G, Isogai T, Iyer B R, Izumi K, Jacqmin T, Jang H, Jani K, Jaranowski P, Jawahar S, Jiménez-Forteza F, Johnson W W, Johnson-McDaniel N K, Jones D I, Jones R, Jonker R J G, Ju L, K Haris, Kalaghatgi C V, Kalogera V, Kandhasamy S, Kang G, Kanner J B, Karki S, Kasprzack M, Katsavounidis E, Katzman W, Kaufer S, Kaur T, Kawabe K, Kawazoe F, Kéfélian F, Kehl M S, Keitel D, Kelley D B, Kells W, Kennedy R, Key J S, Khalaidovski A, Khalili F Y, Khan I, Khan S, Khan Z, Khazanov E A, Kijbunchoo N, Kim C, Kim J, Kim K, Kim Nam-Gyu, Kim Namjun, Kim Y-M, King E J, King P J, Kinzel D L, Kissel J S, Kleybolte L, Klimenko S, Koehlenbeck S M, Kokeyama K, Koley S, Kondrashov V, Kontos A, Korobko M, Korth W Z, Kowalska I, Kozak D B, Kringel V, Krishnan B, Królak A, Krueger C, Kuehn G, Kumar P, Kuo L, Kutynia A, Lackey B D, Landry M, Lange J, Lantz B, Lasky P D, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lebigot E O, Lee C H, Lee H K, Lee H M, Lee K, Lenon A, Leonardi M, Leong J R, Leroy N, Letendre N, Levin Y, Levine B M, Li T G F, Libson A, Littenberg T B, Lockerbie N A, Logue J, Lombardi A L, London L T, Lord J E, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough J D, Lousto C O, Lovelace G, Lück H, Lundgren A P, Luo J, Lynch R, Ma Y, MacDonald T, Machenschalk B, MacInnis M, Macleod D M, Magaña-Sandoval F, Magee R M, Mageswaran M, Majorana E, Maksimovic I, Malvezzi V, Man N, Mandel I, Mandic V, Mangano V, Mansell G L, Manske M, Mantovani M, Marchesoni F, Marion F, Márka S, Márka Z, Markosyan A S, Maros E, Martelli F, Martellini L, Martin I W, Martin R M, Martynov D V, Marx J N, Mason K, Masserot A, Massinger T J, Masso-Reid M, Matichard F, Matone L, Mavalvala N, Mazumder N, Mazzolo G, McCarthy R, McClelland D E, McCormick S, McGuire S C, McIntyre G, McIver J, McManus D J, McWilliams S T, Meacher D, Meadors G D, Meidam J, Melatos A, Mendell G, Mendoza-Gandara D, Mercer R A, Merilh E, Merzougui M, Meshkov S, Messenger C, Messick C, Meyers P M, Mezzani F, Miao H, Michel C, Middleton H, Mikhailov E E, Milano L, Miller J, Millhouse M, Minenkov Y, Ming J, Mirshekari S, Mishra C, Mitra S, Mitrofanov V P, Mitselmakher G, Mittleman R, Moggi A, Mohan M, Mohapatra S R P, Montani M, Moore B C, Moore C J, Moraru D, Moreno G, Morriss S R, Mossavi K, Mours B, Mow-Lowry C M, Mueller C L, Mueller G, Muir A W, Mukherjee Arunava, Mukherjee D, Mukherjee S, Mukund N, Mullavey A, Munch J, Murphy D J, 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机构信息
LIGO, California Institute of Technology, Pasadena, California 91125, USA.
Louisiana State University, Baton Rouge, Louisiana 70803, USA.
出版信息
Phys Rev Lett. 2016 Jun 17;116(24):241102. doi: 10.1103/PhysRevLett.116.241102. Epub 2016 Jun 14.
On September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36_{-4}^{+5}M_{⊙} and 29_{-4}^{+4}M_{⊙}; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be <0.7 (at 90% probability). The luminosity distance to the source is 410_{-180}^{+160} Mpc, corresponding to a redshift 0.09_{-0.04}^{+0.03} assuming standard cosmology. The source location is constrained to an annulus section of 610 deg^{2}, primarily in the southern hemisphere. The binary merges into a black hole of mass 62_{-4}^{+4}M_{⊙} and spin 0.67_{-0.07}^{+0.05}. This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.
2015年9月14日，激光干涉引力波天文台（LIGO）探测到一个引力波瞬变事件（GW150914）；我们对该源的性质及其参数进行了表征。利用一套精确的波形模型，对事件发生时刻前后LIGO网络的数据进行了连贯分析，这些模型描述了广义相对论中致密双星系统产生的引力波。GW150914由质量分别为36_{-4}^{+5}M_{⊙}和29_{-4}^{+4}M_{⊙}的近乎等质量双黑洞产生；对于每个参数，我们报告其中位数以及90%可信区间的范围。质量更大的黑洞的无量纲自旋大小必定小于0.7（概率为90%）。到该源的光度距离为410_{-180}^{+160} 兆秒差距，假设标准宇宙学，对应红移0.09_{-0.04}^{+0.03}。源的位置被限制在610平方度的环形区域内，主要位于南半球。双星合并形成一个质量为62_{-4}^{+4}M_{⊙}、自旋为0.67_{-0.07}^{+0.05}的黑洞。这个黑洞比恒星质量范围内通过电磁观测推断出的任何其他黑洞都要重得多。
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