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The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models

Journal Article · · Astrophysical Journal Letters
; ; ; ; ;  [1];  [2];  [3]; ;  [4];  [5]; ; ;  [6];  [7];  [8];  [9];  [10];  [11];  [12] more »; « less
  1. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 (United States)
  2. Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States)
  3. Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701 (United States)
  4. CIERA and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208 (United States)
  5. Department of Physics, Brandeis University, Waltham, MA 02454 (United States)
  6. Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States)
  7. Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104 (United States)
  8. Department of Physics, Syracuse University, Syracuse, NY 13224 (United States)
  9. Department of Astronomy, Indiana University, 727 E. Third Street, Bloomington, IN 47405 (United States)
  10. Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States)
  11. Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637 (United States)
  12. The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101 (United States)

We present UV, optical, and near-infrared (NIR) photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at 0.47–18.5 days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the Hubble Space Telescope (HST). The spectral energy distribution (SED) inferred from this photometry at 0.6 days is well described by a blackbody model with T≈8300 K, a radius of R≈4.5×10{sup 14} cm (corresponding to an expansion velocity of v≈0.3c), and a bolometric luminosity of L{sub bol}≈5×10{sup 41} erg s{sup −1}. At 1.5 days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set, we find that models with heating from radioactive decay of {sup 56}Ni, or those with only a single component of opacity from r-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data; the resulting “blue” component has M{sub ej}{sup blue}≈0.01 M{sub ⊙} and v{sub ej}{sup blue}≈0.3 c, and the “red” component has M{sub ej}{sup red}≈0.04 M{sub ⊙} and v{sub ej}{sup red}≈0.1 c. These ejecta masses are broadly consistent with the estimated r-process production rate required to explain the Milky Way r-process abundances, providing the first evidence that binary neutron star (BNS) mergers can be a dominant site of r-process enrichment.

OSTI ID:
22872526
Journal Information:
Astrophysical Journal Letters, Vol. 848, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
Country of Publication:
United Kingdom
Language:
English

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