On the progenitor of binary neutron star merger GW170817

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dc.contributor.authorAbbott, B.
dc.contributor.authorAbbott, R.
dc.contributor.authorAbbott, T.
dc.contributor.authorAcernese, F.
dc.contributor.authorAckley, K.
dc.contributor.authorAdams, C.
dc.contributor.authorAdams, T.
dc.contributor.authorAddesso, P.
dc.contributor.authorAdhikari, R.
dc.contributor.authorAdya, V.
dc.contributor.authorAffeldt, C.
dc.contributor.authorAfrough, M.
dc.contributor.authorAgarwal, B.
dc.contributor.authorAgathos, M.
dc.contributor.authorAgatsuma, K.
dc.contributor.authorAggarwal, N.
dc.contributor.authorAguiar, O.
dc.contributor.authorAiello, L.
dc.contributor.authorAin, A.
dc.contributor.authorAjith, P.
dc.contributor.authoret al.
dc.date.issued2017
dc.description.abstractOn 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.
dc.description.statementofresponsibilityB. P. Abbott … Miftar Ganija … Won Kim … Jesper Munch … David J Ottaway … Peter J Veitch … et al. (LIGO Scientific Collaboration and Virgo Collaboration)
dc.identifier.citationLetters of the Astrophysical Journal, 2017; 850(2)
dc.identifier.doi10.3847/2041-8213/aa93fc
dc.identifier.issn2041-8205
dc.identifier.issn2041-8213
dc.identifier.orcidBrown, D.D. [0000-0001-7851-3939]
dc.identifier.orcidCao, H. [0000-0001-6583-6907]
dc.identifier.orcidGanija, M.R. [0000-0002-6882-3930]
dc.identifier.orcidOttaway, D.J. [0000-0001-6794-1591]
dc.identifier.orcidVeitch, P. [0000-0002-2597-435X]
dc.identifier.urihttp://hdl.handle.net/2440/111234
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.relation.grantARC
dc.rights© 2017. The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
dc.source.urihttps://doi.org/10.3847/2041-8213/aa93fc
dc.subjectBinaries: general - gravitational waves - stars: kinematics and dynamics - stars: neutron
dc.titleOn the progenitor of binary neutron star merger GW170817
dc.typeJournal article
pubs.publication-statusPublished

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