Observations of the First Electromagnetic Counterpart to a Gravitational-wave Source by the TOROS Collaboration

Díaz, M. C.; Macri, Lucas M.; Lambas, D. García; Oliveira, C. Mendes de; Castellón, José Luis Nilo; Ribeiro, T.; Sánchez, Bruno; Schoenell, W.; Abramo, L. Raul; Akras, S.; Alcaniz, J. S.; Artola, R.; Beroiz, Martín; Bonoli, Silvia; Cabral, Juan B.; Camuccio, Richard; Castillo, M.; Chavushyan, V.; Coelho, P.; Colazo, C.; Costa-Duarte, M. V.; Larenas, H. Cuevas; DePoy, D. L.; Romero, M. Domínguez; Dultzin, D.; Fernández, Daniela Meli; García, Javier A.; Girardini, C.; Gonçalves, Denise R.; Gonçalves, T. S.; Gurovich, S.; Jiménez-Teja, Y.; Kanaan, A.; Lares, M.; Oliveira, R. Lopes de; López-Cruz, Omar; Marshall, J. L.; Melia, R.; Molino, A.; Padilla, Nelson; Peñuela, T.; Placco, Vinicius M.; Quiñones, C.; Rivera, A. Ramírez; Renzi, Víctor; Riguccini, L.; Ríos-López, E.; Rodríguez, Horacio Adolfo; Sampedro, L.; Schneiter, M.; Sodré, L.; Starck, M.; Torres-Flores, S.; Tornatore, M.; Zadrożny, A.

doi:10.3847/2041-8213/aa9060

Cited by 117 publications

(66 citation statements)

References 22 publications

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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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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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“…As one of the best sGRB events observed ever, GW170817 is rich in new data; E-mail: hamidani.hamid@yukawa.kyoto-u.ac.jp such as, the mass of the BNS (∼ 2.7M ; Abbott et al 2017a), the viewing angle (∼ 20 • − 30 • ; Abbott et al 2017a;Troja et al 2018), and the delay between the GW and the EM signal (∼ 1.7s; Abbott et al 2017a;Abbott et al 2017c), all inferred for the first time. Superluminal motion in late radio afterglow observations (Mooley et al 2018), and macronova/kilonova (hereafter macronova) emission with a strong support for r-process nucleosynthesis (Arcavi et al 2017;Chornock et al 2017;Coulter et al 2017;Díaz et al 2017;Drout et al 2017;Kilpatrick et al 2017;Kasliwal et al 2017;Nicholl et al 2017;Pian et al 2017;Smartt et al 2017;Shappee et al 2017;Soares-Santos et al 2017;Tanaka et al 2017;Utsumi et al 2017;Valenti et al 2017) are also new revelations. This event also had impacts on the equation of state of neutron stars, relativity, cosmology, etc.…”

Section: Introductionmentioning

confidence: 93%

Jet Propagation in Neutron Star Mergers and GW170817

Hamidani

Kiuchi

Ioka

2019

Monthly Notices of the Royal Astronomical Society

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The gravitational wave event from the binary neutron star (BNS) merger GW170817 and the following multi-messenger observations present strong evidence for i) merger ejecta expanding with substantial velocities and ii) a relativistic jet which had to propagate through the merger ejecta. The ejecta's expansion velocity is not negligible for the jet head motion, which is a fundamental difference from the other systems like collapsars and active galactic nuclei. Here we present an analytic model of the jet propagation in an expanding medium. In particular, we notice a new term in the expression of the breakout time and velocity. In parallel, we perform a series of over a hundred 2D numerical simulations of jet propagation. The BNS merger ejecta is prepared based on numerical relativity simulations of a BNS merger with the highestresolution to date. We show that our analytic results agree with numerical simulations over a wide parameter space. Then we apply our analytic model to GW170817, and obtain two solid constraints on: i) the central engine luminosity as L iso,0 ∼ 3 × 10 49 − 2.5 × 10 52 erg s −1 , and on ii) the delay time between the merger and engine activation t 0 − t m < 1.3 s. The engine power implies that the apparently-faint short gamma-ray burst (sGRB) sGRB 170817A is similar to typical sGRBs if observed on-axis.

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“…The simultaneous detection of gravitational waves (GWs) from a neutron star-neutron star (NS-NS) merger (Abbott et al 2017a) and its electromagnetic (EM) counterparts opened a new window of the multimessenger astronomy. EM counterparts to GW170817 were observed over the entire wavelength range, from gamma-ray to radio wavelengths (Abbott et al 2017b;Andreoni et al 2017;Arcavi et al 2017;Coulter et al 2017;Cowperthwaite et al 2017;Díaz et al 2017;Drout et al 2017;Evans et al 2017;Hu et al 2017;Valenti et al 2017;Kasliwal et al 2017;Lipunov et al 2017;Pian et al 2017;Pozanenko et al 2018;Smartt et al 2017;Tanvir et al 2017;Troja et al 2017;Utsumi et al 2017;Mooley et al 2018;Hallinan et al 2017). In particular, a counterpart in optical and infrared wavelengths (named as SSS17a, AT 2017gfo or DLT17ck), is identified as the emission so-called a kilonova (also known as macronova).…”

Section: Introductionmentioning

confidence: 99%

Diversity of Kilonova Light Curves

Kawaguchi

Shibata

Tanaka

2020

ApJ

141

151

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We perform radiative transfer simulations for kilonova in various situations, including the cases of prompt collapse to a black hole from neutron-star mergers, high-velocity ejecta possibly accelerated by magnetars, and a black hole-neutron star merger. Our calculations are done employing ejecta profiles predicted by numerical-relativity simulations and a new line list for all the r-process elements. We found that (i) the optical emission for binary neutron stars promptly collapsing to a black hole would be fainter by 1-2 mag than that found in GW170817, while the infrared emission could be as bright as that in GW170817 if the post-merger ejecta is as massive as ≈ 0.01 M ; (ii) the kilonova would be brighter than that observed in GW170817 for the case that the ejecta is highly accelerated by the electromagnetic energy injection from the remnant, but it would decline rapidly and the magnitude would become fainter than in GW170817 within a few days; (iii) the optical emission from a black hole-neutron star merger ejecta could be as bright as that observed in GW170817 for the case that sufficiently large amount of matter is ejected ( 0.02 M ), while the infrared brightness would be brighter by 1-2 mag at the same time. We show that the difference in the ejecta properties would be imprinted in the differences in the peak brightness and time of peak. This indicates that we may be able to infer the type of the central engine for kilonovae by observation of the peak in the multiple band.

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Observations of the First Electromagnetic Counterpart to a Gravitational-wave Source by the TOROS Collaboration

Cited by 117 publications

References 22 publications

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

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

Jet Propagation in Neutron Star Mergers and GW170817

Diversity of Kilonova Light Curves

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