期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 880, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/2041-8213/ab271c
关键词
binaries: close; gravitational waves; methods: observational; stars: black holes; stars: neutron
资金
- NSF [AST-1009863, AST-1714498]
- NASA [NNX10AF62G, NNX15AE50G]
- LSSTC, NSF [1829740]
- Brinson Foundation
- Moore Foundation
- NASA through the NASA Hubble Fellowship [HST-HF2-51403.001-A]
- Space Telescope Science Institute [NAS 5-26555]
- Royal Astronomical Society Research Fellowship
- National Science Foundation [AST-1814782]
- Deutsche Forschungsgemeinschaft [GE2506/12-1]
- National Aeronautics and Space Administration through Chandra award [DD8-19101A, DDT-18096A]
- National Aeronautics Space Administration [NAS8-03060]
- Office of the Provost
- Office for Research
- Northwestern University Information Technology
- University of Arizona
- Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MCTIC) do Brasil
- Michigan State University (MSU)
On 2019 April 25.346 and 26.640 UT the Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo gravitational-wave (GW) observatory announced the detection of the first candidate events in Observing Run 3 that contained at least one neutron star (NS). S190425z is a likely binary neutron star (BNS) merger at d(L) = 156 +/- 41 Mpc, while S190426c is possibly the first NS-black hole (BH) merger ever detected, at d(L) = 377 +/- 100 Mpc, although with marginal statistical significance. Here we report our optical follow-up observations for both events using the MMT 6.5 m telescope, as well as our spectroscopic follow-up of candidate counterparts (which turned out to be unrelated) with the 4.1 m SOAR telescope. We compare to publicly reported searches, explore the overall areal coverage and depth, and evaluate those in relation to the optical/near-infrared (NIR) kilonova emission from the BNS merger GW170817, to theoretical kilonova models, and to short gamma-ray burst (SGRB) afterglows. We find that for a GW170817-like kilonova, the partial volume covered spans up to about 40% for S190425z and 60% for S190426c. For an on-axis jet typical of SGRBs, the search effective volume is larger, but such a configuration is expected in at most a few percent of mergers. We further find that wide-field gamma-ray and X-ray limits rule out luminous on-axis SGRBs, for a large fraction of the localization regions, although these searches are not sufficiently deep in the context of the gamma-ray emission from GW170817 or off-axis SGRB afterglows. The results indicate that some optical follow-up searches are sufficiently deep for counterpart identification to about 300 Mpc, but that localizations better than 1000 deg(2) are likely essential.
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