Abstract
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 dL = 156 ± 41 Mpc, while S190426c is possibly the first NS-black hole (BH) merger ever detected, at dL = 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 γ-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 γ-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 deg2 are likely essential.
Original language | English |
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Article number | L4 |
Journal | Astrophysical Journal Letters |
Volume | 880 |
Issue number | 1 |
DOIs | |
Publication status | Published - 18 Jul 2019 |
Funding
G. Hosseinzadeh P. S. Cowperthwaite S. Gomez V. A. Villar M. Nicholl R. Margutti E. Berger R. Chornock K. Paterson W. Fong V. Savchenko P. Short K. D. Alexander P. K. Blanchard J. Braga M. L. Calkins R. Cartier D. L. Coppejans T. Eftekhari T. Laskar C. Ly L. Patton I. Pelisoli D. E. Reichart G. Terreran P. K. G. Williams G. Hosseinzadeh P. S. Cowperthwaite S. Gomez V. A. Villar M. Nicholl R. Margutti E. Berger R. Chornock K. Paterson W. Fong V. Savchenko P. Short K. D. Alexander P. K. Blanchard J. Braga M. L. Calkins R. Cartier D. L. Coppejans T. Eftekhari T. Laskar C. Ly L. Patton I. Pelisoli D. E. Reichart G. Terreran P. K. G. Williams Center for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA Observatories of the Carnegie Institute for Science, 813 Santa Barbara Street, Pasadena, CA 91101-1232, USA Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill EH9 3HJ, UK Birmingham Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK Center for Interdisciplinary Exploration and Research in Astrophysics and Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208-3112, USA Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701-2942, USA ISDC, Department of Astronomy, University of Geneva, Chemin d’�cogia, 16 CH-1290 Versoix, Switzerland Instituto Nacional de Pesquisas Espaciais, Avenida dos Astronautas 1758, 12227-010, S�o Jos� dos Campos—SP, Brazil Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile Department of Physics, University of Bath, Claverton Down, Bath BA2 7AY, UK MMT and Steward Observatories, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA Institut f�r Physik und Astronomie, Universit�t Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany Department of Physics and Astronomy, University of North Carolina, 120 East Cameron Avenue, Chapel Hill, NC 27599, USA American Astronomical Society, 1667 K�Street NW, Suite 800, Washington, DC 20006-1681, USA These authors contributed equally to this work. LSSTC Data Science Fellow. Hubble Fellow. Einstein Fellow. G. Hosseinzadeh, P. S. Cowperthwaite, S. Gomez, V. A. Villar, M. Nicholl, R. Margutti, E. Berger, R. Chornock, K. Paterson, W. Fong, V. Savchenko, P. Short, K. D. Alexander, P. K. Blanchard, J. Braga, M. L. Calkins, R. Cartier, D. L. Coppejans, T. Eftekhari, T. Laskar, C. Ly, L. Patton, I. Pelisoli, D. E. Reichart, G. Terreran and P. K. G. Williams 2019-07-20 2019-07-18 08:37:43 cgi/release: Article released bin/incoming: New from .zip National Science Foundation AST-1714498 AST-1814782 National Aeronautics and Space Administration HST-HF-51404.001-A HST-HF2-51403.001-A Deutsche Forschungsgemeinschaft GE2506/12-1 yes 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 γ -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 γ -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. � 2019. The American Astronomical Society. All rights reserved. Ahumada T., Coughlin M. W., Staats K. et al 2019b GCN 24343 1 Ahumada T., Coughlin M. W., Staats K. et al GCN 0147-0728 24343 2019 1 Ahumada T., Coughlin M. W., Staats K. and Dekany R. G. 2019a GCN 24198 1 Ahumada T., Coughlin M. W., Staats K. and Dekany R. G. GCN 0147-0728 24198 2019 1 Alexander K. 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Keywords
- binaries: close
- gravitational waves
- methods: observational
- stars: black holes
- stars: neutron
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science