On the Progenitor of Binary Neutron Star Merger GW170817

被引：126

作者：

Abbott, B. P. ^{[1
]}

Abbott, R. ^{[1
]}

Abbott, T. D. ^{[2
]}

Acernese, F. ^{[3
,4
]}

Ackley, K. ^{[5
,6
]}

Adams, C. ^{[7
]}

Adams, T. ^{[8
]}

Addesso, P. ^{[9
,10
]}

Adhikari, R. X. ^{[1
]}

Adya, V. B. ^{[11
]}

Affeldt, C. ^{[11
]}

Afrough, M. ^{[12
]}

Agarwal, B. ^{[13
]}

Agathos, M. ^{[14
]}

Agatsuma, K. ^{[15
]}

Aggarwal, N. ^{[16
]}

Aguiar, O. D. ^{[17
]}

Aiello, L. ^{[18
,19
]}

Ain, A. ^{[20
]}

Ajith, P. ^{[21
]}

Allen, B. ^{[11
,22
,23
]}

Allen, G. ^{[13
]}

Allocca, A. ^{[24
,25
]}

Altin, P. A. ^{[26
]}

Amato, A. ^{[27
]}

Ananyeva, A. ^{[1
]}

Anderson, S. B. ^{[1
]}

Anderson, W. G. ^{[22
]}

Angelova, S. V. ^{[28
]}

Antier, S. ^{[29
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

Araya, M. C. ^{[1
]}

Areeda, J. S. ^{[30
]}

Arnaud, N. ^{[29
,31
]}

Arun, K. G. ^{[32
]}

Ascenzi, S. ^{[33
,34
]}

Ashton, G. ^{[11
]}

Ast, M. ^{[35
]}

Aston, S. M. ^{[7
]}

Astone, P. ^{[36
]}

Atallah, D. V. ^{[37
]}

Aufmuth, P. ^{[23
]}

Aulbert, C. ^{[11
]}

AultONeal, K. ^{[38
]}

Austin, C. ^{[2
]}

Avila-Alvarez, A. ^{[30
]}

Babak, S. ^{[39
]}

Bacon, P. ^{[40
]}

Bader, M. K. M. ^{[15
]}

机构：

[1] CALTECH, LIGO, Pasadena, CA 91125 USA

[2] Louisiana State Univ, Baton Rouge, LA 70803 USA

[3] Univ Salerno, I-84084 Salerno, Italy

[4] Ist Nazl Fis Nucl, Complesso Univ Monte S Angelo, Sez Napoli, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

[6] Monash Univ, Sch Phys Astron, OzGrav, Clayton, Vic 3800, Australia

[7] LIGO Livingston Observ, Livingston, LA 70754 USA

[8] Univ Savoie Mont Blanc, CNRS, Lab Annecy Le Vieux Phys Particules LAPP, IN2P3, F-74941 Annecy, France

[9] Univ Sannio Benevento, I-82100 Benevento, Italy

[10] INFN, Sez Napoli, I-80100 Naples, Italy

[11] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany

[12] Univ Mississippi, University, MS 38677 USA

[13] Univ Illinois, NCSA, Urbana, IL 61801 USA

[14] Univ Cambridge, Cambridge CB2 1TN, England

[15] Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands

[16] MIT, LIGO, Cambridge, MA 02139 USA

[17] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Paulo, Brazil

[18] GSSI, I-67100 Laquila, Italy

[19] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Assergi, Italy

[20] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[21] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bengaluru 560089, India

[22] Univ Wisconsin, Milwaukee, WI 53201 USA

[23] Leibniz Univ Hannover, D-30167 Hannover, Germany

[24] Univ Pisa, I-56127 Pisa, Italy

[25] INFN, Sez Pisa, I-56127 Pisa, Italy

[26] Australian Natl Univ, OzGrav, Canberra, ACT 0200, Australia

[27] CNRS, IN2P3, LMA, F-69622 Villeurbanne, France

[28] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland

[29] Univ Paris Sud, Univ Paris Saclay, CNRS IN2P3, LAL, F-91898 Orsay, France

[30] Calif State Univ Fullerton, Fullerton, CA 92831 USA

[31] EGO, I-56021 Pisa, Italy

[32] Chennai Math Inst, Madras 603103, Tamil Nadu, India

[33] Univ Roma Tor Vergata, I-00133 Rome, Italy

[34] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy

[35] Univ Hamburg, D-22761 Hamburg, Germany

[36] INFN, Sez Roma, I-00185 Rome, Italy

[37] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales

[38] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA

[39] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany

[40] Univ Paris Diderot, AstroParticule & Cosmol, CNRS IN2P3, APC,CEA Irfu,Observ Paris, F-75205 Paris, France

[41] Korea Inst Sci & Technol Informat, Daejeon 34141, South Korea

[42] West Virginia Univ, Morgantown, WV 26506 USA

[43] Univ Perugia, I-06123 Perugia, Italy

[44] INFN, Sez Perugia, I-06123 Perugia, Italy

[45] Syracuse Univ, Syracuse, NY 13244 USA

[46] Univ Minnesota, Minneapolis, MN 55455 USA

[47] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland

[48] LIGO Hanford Observ, Richland, WA 99352 USA

[49] Caltech CaRT, Pasadena, CA 91125 USA

[50] RMKI, Wigner RCP, Konkoly Thege Miklos 29-33, H-1121 Budapest, Hungary

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2017年 / 850卷 / 02期

基金：

美国国家科学基金会; 俄罗斯基础研究基金会; 匈牙利科学研究基金会; 新加坡国家研究基金会; 澳大利亚研究理事会; 英国科学技术设施理事会; 中国国家自然科学基金; 瑞士国家科学基金会; 俄罗斯科学基金会;

关键词：

binaries: general; gravitational waves; stars: kinematics and dynamics; stars: neutron; GAMMA-RAY BURSTS; MASSIVE CLOSE BINARIES; GLOBULAR-CLUSTERS; COMPACT BINARIES; CORE-COLLAPSE; HOST GALAXY; NATAL KICKS; PULSAR; EVOLUTION; AFTERGLOW;

D O I：

10.3847/2041-8213/aa93fc

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

On 2017 August 17 the merger of two compact objects with masses consistent with two neutron stars was discovered through gravitational-wave (GW170817), gamma-ray (GRB. 170817A), and optical (SSS17a/AT 2017gfo) observations. The optical source was associated with the early-type galaxy NGC 4993 at a distance of just similar to 40Mpc, consistent with the gravitational-wave measurement, and the merger was localized to be at a projected distance of similar to 2 kpc away from the galaxy's center. We use this minimal set of facts and the mass posteriors of the two neutron stars to derive the first constraints on the progenitor of GW170817 at the time of the second supernova (SN). We generate simulated progenitor populations and follow the three-dimensional kinematic evolution from binary neutron star (BNS) birth to the merger time, accounting for pre-SN galactic motion, for considerably different input distributions of the progenitor mass, pre-SN semimajor axis, and SN-kick velocity. Though not considerably tight, we find these constraints to be comparable to those for Galactic BNS progenitors. The derived constraints are very strongly influenced by the requirement of keeping the binary bound after the second SN and having the merger occur relatively close to the center of the galaxy. These constraints are insensitive to the galaxy's star formation history, provided the stellar populations are older than 1 Gyr.

引用

页数：18

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