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The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale

Journal Article · · Astrophysical Journal Letters
; ; ; ; ; ; ; ; ;  [1]; ;  [2];  [3];  [4]; ;  [5];  [6];  [7];  [8];
  1. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
  2. Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208 (United States)
  3. Department of Physics, University of Chicago, Chicago, IL 60637 (United States)
  4. Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701 (United States)
  5. Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States)
  6. Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104 (United States)
  7. Department of Physics, Syracuse University, Syracuse, NY 13224 (United States)
  8. Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States)

We present the properties of NGC 4993, the host galaxy of GW170817, the first gravitational-wave (GW) event from the merger of a binary neutron star (BNS) system and the first with an electromagnetic (EM) counterpart. We use both archival photometry and new optical/near-IR imaging and spectroscopy, together with stellar population synthesis models to infer the global properties of the host galaxy. We infer a star formation history peaked at ≳10 Gyr ago, with subsequent exponential decline leading to a low current star formation rate of 0.01 M{sub ⊙} yr{sup −1}, which we convert into a binary merger timescale probability distribution. We find a median merger timescale of 11.2{sub −1.4}{sup +0.7} Gyr, with a 90% confidence range of 6.8--13.6 Gyr. This in turn indicates an initial binary separation of ≈4.5 R{sub ⊙}, comparable to the inferred values for Galactic BNS systems. We also use new and archival Hubble Space Telescope images to measure a projected offset of the optical counterpart of 2.1 kpc (0.64r {sub e}) from the center of NGC 4993 and to place a limit of M{sub r}≳−7.2 mag on any pre-existing emission, which rules out the brighter half of the globular cluster luminosity function. Finally, the age and offset of the system indicates it experienced a modest natal kick with an upper limit of ∼200 km s{sup −1}. Future GW–EM observations of BNS mergers will enable measurement of their population delay time distribution, which will directly inform their viability as the dominant source of r-process enrichment in the universe.

OSTI ID:
22872530
Journal Information:
Astrophysical Journal Letters, Journal Name: Astrophysical Journal Letters Journal Issue: 2 Vol. 848; ISSN 2041-8205
Country of Publication:
United Kingdom
Language:
English

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