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
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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 approximate to 8300 K, a radius of R approximate to 4.5 x 10(14) cm (corresponding to an expansion velocity of v approximate to 0.3c), and a bolometric luminosity of L-bol approximate to 5 x 10(41) erg s(-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 Ni-56, 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-ej(blue) approximate to 0.01 M-circle dot and v(ej)(blue) approximate to 0.3c, and the "red" component has M-cj(red) approximate to 0.04 M-circle dot and v(cj)(red) approximate to 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.
NSF AST-1411763 AST-1714498 DGE 1144152 PHY-1707954 AST-1518052 NASA NNX15AE50G NNX16AC22G National Science Foundation Kavli Foundation Danish National Research Foundation Niels Bohr International Academy DARK Cosmology Centre Gordon & Betty Moore Foundation Heising-Simons Foundation UCSC Alfred P. Sloan Foundation David and Lucile Packard Foundation European Research Council ERC-StG-335936 Gordon and Betty Moore Foundation GBMF5076 DOE (USA) NSF (USA) MISE (Spain) STFC (UK) HEFCE (UK) NCSA (UIUC) KICP (U. Chicago) CCAPP (Ohio State) MIFPA (Texas AM) MINECO (Spain) DFG (Germany) CNPQ (Brazil) FAPERJ (Brazil) FINEP (Brazil) Argonne Lab UC Santa Cruz University of Cambridge CIEMAT-Madrid University of Chicago University College London DES-Brazil Consortium University of Edinburgh ETH Zurich Fermilab University of Illinois ICE (IEEC-CSIC) IFAE Barcelona Lawrence Berkeley Lab LMU Munchen Excellence Cluster Universe University of Michigan NOAO University of Nottingham Ohio State University University of Pennsylvania University of Portsmouth SLAC National Lab Stanford University University of Sussex Texas AM University Gemini Observatory GS-2017B-Q-8 GS-2017B-DD-4
Artículo de publicación ISI
Quote ItemThe Astrophysical Journal Letters, 848: L17 (10pp), 2017
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