MASTER Optical Detection of the First LIGO/Virgo Neutron Star Binary Merger GW170817

Lipunov, V.; Gorbovskoy, E.; Корнилов, В. Г.; Tyurina, N.; Balanutsa, P.; Kuznetsov, A.; Vlasenko, D.; Kuvshinov, D.; Gorbunov, I.; Buckley, D.; Krylov, A.; Подеста, Р.; López, Carlos; Подеста, Ф.; Levato, H.; Saffe, C.; Mallamachi, C.; Potter, S.; Буднев, Н. М.; Gress, O.; Ishmuhametova, Yu. V.; Vladimirov, V.; Zimnukhov, D.; Yurkov, V.; Sergienko, Y.; Gabovich, A.; Rebolo, R.; Serra-Ricart, M.; Israelyan, G.; Chazov, V.; Wang, Xiaofeng; Tlatov, A.; Panchenko, M. I.

doi:10.3847/2041-8213/aa92c0

Cited by 243 publications

(141 citation statements)

References 43 publications

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“…The broadband counterparts also confirmed the existence of a relativistic jet (e.g., Mooley et al 2018b,a;Troja et al 2018b;Ghirlanda et al 2019;Lamb et al 2019b), which is consistent with an SGRB observed from an off-axis angle (e.g., Troja et al 2018a;Ioka & Nakamura 2019). The UV/optical/IR counterparts (Coulter et al 2017;Lipunov et al 2017;Soares-Santos et al 2017;Valenti et al 2017;Utsumi et al 2017;Smartt et al 2017;Evans et al 2017;Pian et al 2017;Tanvir et al 2017) also verified that a BNS merger produces fast and massive ejecta consisting of r-process elements (e.g., Kasliwal et al 2017;Kasen et al 2017;Murguia-Berthier et al 2017;Shibata et al 2017;Tanaka et al 2017). Gamma-rays above GeV energies and neutrinos are not detected from GW170817 (Ajello et al 2018;Abdalla et al 2017;Albert et al 2017), although they are expected (e.g., Gao et al 2013;Kimura et al 2017;Fang & Metzger 2017;Murase et al 2018;Kimura et al 2018).…”

Section: Introductionsupporting

confidence: 69%

Upscattered Cocoon Emission in Short Gamma-Ray Bursts as High-energy Gamma-Ray Counterparts to Gravitational Waves

Kimura

Murase

Ioka³

et al. 2019

ApJL

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We investigate prolonged engine activities of short gamma-ray bursts (SGRBs), such as extended and/or plateau emissions, as high-energy gamma-ray counterparts to gravitational waves (GWs). Binary neutron-star mergers lead to relativistic jets and merger ejecta with r-process nucleosynthesis, which are observed as SGRBs and kilonovae/macronovae, respectively. Long-term relativistic jets may be launched by the merger remnant as hinted in X-ray light curves of some SGRBs. The prolonged jets may dissipate their kinetic energy within the radius of the cocoon formed by the jet-ejecta interaction. Then the cocoon supplies seed photons to non-thermal electrons accelerated at the dissipation region, causing high-energy gamma-ray production through the inverse Compton scattering process. We numerically calculate high-energy gamma-ray spectra in such a system using a one-zone and steadystate approximation, and show that GeV-TeV gamma-rays are produced with a duration of 10 2 − 10 5 seconds. They can be detected by Fermi/LAT or CTA as gamma-ray counterparts to GWs.

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Section: Introductionsupporting

confidence: 69%

Upscattered Cocoon Emission in Short Gamma-Ray Bursts as High-energy Gamma-Ray Counterparts to Gravitational Waves

Kimura

Murase

Ioka³

et al. 2019

ApJL

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“…This multimessenger data provided convincing answers to many outstanding questions. For instance, the detection of a short gamma ray burst (GRB) 1.7 seconds after GW170817 [24][25][26], and subsequent kilonova [27][28][29][30][31][36][37][38][39][40][41][42][43][44], confirmed that BNS mergers are a progenitor of these events. Lanthanide signatures in the kilonova light curves also showed BNS mergers to be a major site for nucleosynthesis of elements heavier than iron [40,44,47,48].…”

Section: Introductionmentioning

confidence: 78%

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

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The observation of gravitational wave signals from binary black hole and binary neutron star mergers has established the field of gravitational wave astronomy. It is expected that future networks of gravitational wave detectors will possess great potential in probing various aspects of astronomy. An important consideration for successive improvement of current detectors or establishment on new sites is knowledge of the minimum number of detectors required to perform precision astronomy. We attempt to answer this question by assessing the ability of future detector networks to detect and localize binary neutron stars mergers on the sky. Good localization ability is crucial for many of the scientific goals of gravitational wave astronomy, such as electromagnetic follow-up, measuring the properties of compact binaries throughout cosmic history, and cosmology. We find that although two detectors at improved sensitivity are sufficient to get a substantial increase in the number of observed signals, at least three detectors of comparable sensitivity are required to localize majority of the signals, typically to within around 10 deg 2 -adequate for follow-up with most wide field of view optical telescopes.

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“…By the combined detection of GW170817, AT2017gfo, and GRB170817A, the field of multi-messenger astronomy was ushered into a new era in which gravitationalwave (GW) and electromagnetic (EM) signatures are simultaneously measured and analyzed, e.g., Abbott B. P. (2017); Abbott et al (2017b); Arcavi et al (2017); Coulter et al (2017); Lipunov et al (2017); Mooley et al (2017); Savchenko et al (2017); Soares-Santos et al (2017); Tanvir et al (2013); Troja et al (2017); Valenti et al (2017). Joint analyses allow a better understanding of the supranuclear-dense matter inside neutron stars (NSs) (e.g.…”

Section: Introductionmentioning

confidence: 99%

Implications of the search for optical counterparts during the first six months of the Advanced LIGO’s and Advanced Virgo’s third observing run: possible limits on the ejecta mass and binary properties

Coughlin

Dietrich

Antier

et al. 2019

Monthly Notices of the Royal Astronomical Society

103

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GW170817 showed that neutron star mergers not only emit gravitational waves but also can release electromagnetic signatures in multiple wavelengths. Within the first half of the third observing run of the Advanced LIGO and Virgo detectors, there have been a number of gravitational wave candidates of compact binary systems for which at least one component is potentially a neutron star. In this article, we look at the candidates S190425z, S190426c, S190510g, S190901ap, and S190910h, predicted to have potentially a non-zero remnant mass, in more detail. All these triggers have been followed up with extensive campaigns by the astronomical community doing electromagnetic searches for their optical counterparts; however, according to the released classification, there is a high probability that some of these events might not be of extraterrestrial origin. Assuming that the triggers are caused by a compact binary coalescence and that the individual source locations have been covered during the EM follow-up campaigns, we employ three different kilonova models and apply them to derive possible constraints on the matter ejection consistent with the publicly available gravitational-wave trigger information and the lack of a kilonova detection. These upper bounds on the ejecta mass can be related to limits on the maximum mass of the binary neutron star candidate S190425z and to constraints on the mass-ratio, spin, and NS compactness for the potential black hole-neutron star candidate S190426c. Our results show that deeper electromagnetic observations for future gravitational wave events near the horizon limit of the advanced detectors are essential.

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MASTER Optical Detection of the First LIGO/Virgo Neutron Star Binary Merger GW170817

Cited by 243 publications

References 43 publications

Upscattered Cocoon Emission in Short Gamma-Ray Bursts as High-energy Gamma-Ray Counterparts to Gravitational Waves

Upscattered Cocoon Emission in Short Gamma-Ray Bursts as High-energy Gamma-Ray Counterparts to Gravitational Waves

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Implications of the search for optical counterparts during the first six months of the Advanced LIGO’s and Advanced Virgo’s third observing run: possible limits on the ejecta mass and binary properties

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