On the progenitor of binary neutron star merger GW170817

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On the progenitor of binary neutron star merger GW170817. / Abbott, B. P.; Birney, R.; Jawahar, S.; Lockerbie, N. A.; Reid, S.; Tokmakov, K. V.; LIGO Scientific Collaboration; Virgo Collaboration.

In: Astrophysical Journal Letters, Vol. 850, No. 2, 01.12.2017, p. 1-18.

Research output: Contribution to journalArticle

Harvard

Abbott, BP, Birney, R, Jawahar, S, Lockerbie, NA, Reid, S, Tokmakov, KV, LIGO Scientific Collaboration & Virgo Collaboration 2017, 'On the progenitor of binary neutron star merger GW170817' Astrophysical Journal Letters, vol 850, no. 2, pp. 1-18. DOI: 10.3847/2041-8213/aa93fc

APA

Abbott, B. P., Birney, R., Jawahar, S., Lockerbie, N. A., Reid, S., Tokmakov, K. V., ... Virgo Collaboration (2017). On the progenitor of binary neutron star merger GW170817. Astrophysical Journal Letters, 850(2), 1-18. DOI: 10.3847/2041-8213/aa93fc

Vancouver

Abbott BP, Birney R, Jawahar S, Lockerbie NA, Reid S, Tokmakov KV et al. On the progenitor of binary neutron star merger GW170817. Astrophysical Journal Letters. 2017 Dec 1;850(2):1-18. Available from, DOI: 10.3847/2041-8213/aa93fc

Author

Abbott, B. P.; Birney, R.; Jawahar, S.; Lockerbie, N. A.; Reid, S.; Tokmakov, K. V.; LIGO Scientific Collaboration; Virgo Collaboration / On the progenitor of binary neutron star merger GW170817.

In: Astrophysical Journal Letters, Vol. 850, No. 2, 01.12.2017, p. 1-18.

Research output: Contribution to journalArticle

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@article{edf3860bfad74aad82ffa96e5d366e43,
title = "On the progenitor of binary neutron star merger GW170817",
abstract = "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 ~40 Mpc, consistent with the gravitational-wave measurement, and the merger was localized to be at a projected distance of ~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.",
keywords = "binaries, gravitational waves, stars, kinematics, dynamics, neutrons, GW170817",
author = "Abbott, {B. P.} and R. Birney and S. Jawahar and Lockerbie, {N. A.} and S. Reid and Tokmakov, {K. V.} and {LIGO Scientific Collaboration} and {Virgo Collaboration}",
year = "2017",
month = "12",
doi = "10.3847/2041-8213/aa93fc",
volume = "850",
pages = "1--18",
journal = "Astrophysics Journal Letters",
issn = "2041-8205",
number = "2",

}

RIS (suitable for import to EndNote) - Download

TY - JOUR

T1 - On the progenitor of binary neutron star merger GW170817

AU - Abbott,B. P.

AU - Birney,R.

AU - Jawahar,S.

AU - Lockerbie,N. A.

AU - Reid,S.

AU - Tokmakov,K. V.

AU - LIGO Scientific Collaboration

AU - Virgo Collaboration

PY - 2017/12/1

Y1 - 2017/12/1

N2 - 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 ~40 Mpc, consistent with the gravitational-wave measurement, and the merger was localized to be at a projected distance of ~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.

AB - 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 ~40 Mpc, consistent with the gravitational-wave measurement, and the merger was localized to be at a projected distance of ~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.

KW - binaries

KW - gravitational waves

KW - stars

KW - kinematics

KW - dynamics

KW - neutrons

KW - GW170817

UR - http://iopscience.iop.org/journal/2041-8205

U2 - 10.3847/2041-8213/aa93fc

DO - 10.3847/2041-8213/aa93fc

M3 - Article

VL - 850

SP - 1

EP - 18

JO - Astrophysics Journal Letters

T2 - Astrophysics Journal Letters

JF - Astrophysics Journal Letters

SN - 2041-8205

IS - 2

ER -

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