Searching for Optical Counterparts of LIGO/Virgo Events in O2 Run

Mazaeva, E.; Pozanenko, A.; Volnova, A.; Minaev, P. Yu.; Belkin, S.; Inasaridze, R.; Klunko, E.; Kusakin, A.; Reva, I.; Rumyantsev, V.; Novichonok, A.; Москвитин, А. С.; Paronyan, G. M.; Schmalz, S.; Tungalag, N.

doi:10.1007/978-3-030-51913-1_9

Cited by 3 publications

(2 citation statements)

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“…The count rate variations in the BDRG/Lomonosov gammaquanta channels are illustrated by the curves in the upper panel of Figure 3, in which count rates of three BDRG1 NaI detector channels 10-35, 35-170, 170-650 keV shown with the time resolution of 0.1 s are plotted. The middle panel of Figure 3 shows data from the spectrometer SPI on board INTEGRAL obtained for the same time period (Mazaeva et al 2016). The GRB was detected with the anticoincidence system (ACS), which provides integral counts of gamma quanta with energies of more than about 50 keV.…”

Section: Lomonosov Observationsmentioning

confidence: 99%

Three-stage Collapse of the Long Gamma-Ray Burst from GRB 160625B Prompt Multiwavelength Observations

Lipunov

Sadovnichy

Panasyuk

et al. 2023

ApJ

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This article presents the early results of synchronous multiwavelength observations of one of the brightest gamma-ray bursts (GRBs) GRB 160625B with the detailed continuous fast optical photometry of its optical counterpart obtained by MASTER and with hard X-ray and gamma-ray emission, obtained by the Lomonosov and Konus-Wind spacecraft. The detailed photometry led us to detect the quasi-periodical emission components in the intrinsic optical emission. As a result of our analysis of synchronous multiwavelength observations, we propose a three-stage collapse scenario for this long and bright GRB. We suggest that quasiperiodic fluctuations may be associated with forced precession of a self-gravitating rapidly rotating superdense body (spinar), whose evolution is determined by a powerful magnetic field. The spinar’s mass allows it to collapse into a black hole at the end of evolution.

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Section: Lomonosov Observationsmentioning

confidence: 99%

Three-stage Collapse of the Long Gamma-Ray Burst from GRB 160625B Prompt Multiwavelength Observations

Lipunov

Sadovnichy

Panasyuk

et al. 2023

ApJ

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“…The Swift BAT and XRT observations were obtained from the web interface provided by the Leicester University (Evans et al 2009); the BAT data were binned to a signal-to-noise ratio of 7, and the absorbed 0.3−10 keV XRT light curve was converted to the observed flux density at 1 keV. For completeness, we include the optical observations and upper limits reported in the Gamma-ray Coordination Network (GCN) from the MASTER II (Tyurina et al 2018), Tien Shan Astronomical Observatory (Mazaeva et al 2018), andXinglong-2.16 m (Zhu et al 2018). Note that the GCN observations do not include filter corrections.…”

Section: Ultraviolet and Optical Light Curvesmentioning

confidence: 99%

A Short Gamma-Ray Burst from a Protomagnetar Remnant

Jordana-Mitjans

Mundell

Guidorzi

et al. 2022

ApJ

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The contemporaneous detection of gravitational waves and gamma rays from GW170817/GRB 170817A, followed by kilonova emission a day after, confirmed compact binary neutron star mergers as progenitors of short-duration gamma-ray bursts (GRBs) and cosmic sources of heavy r-process nuclei. However, the nature (and life span) of the merger remnant and the energy reservoir powering these bright gamma-ray flashes remains debated, while the first minutes after the merger are unexplored at optical wavelengths. Here, we report the earliest discovery of bright thermal optical emission associated with short GRB 180618A with extended gamma-ray emission—with ultraviolet and optical multicolor observations starting as soon as 1.4 minutes post-burst. The spectrum is consistent with a fast-fading afterglow and emerging thermal optical emission 15 minutes post-burst, which fades abruptly and chromatically (flux density F ν ∝ t −α , α = 4.6 ± 0.3) just 35 minutes after the GRB. Our observations from gamma rays to optical wavelengths are consistent with a hot nebula expanding at relativistic speeds, powered by the plasma winds from a newborn, rapidly spinning and highly magnetized neutron star (i.e., a millisecond magnetar), whose rotational energy is released at a rate L th ∝ t −(2.22±0.14) to reheat the unbound merger-remnant material. These results suggest that such neutron stars can survive the collapse to a black hole on timescales much larger than a few hundred milliseconds after the merger and power the GRB itself through accretion. Bright thermal optical counterparts to binary merger gravitational wave sources may be common in future wide-field fast-cadence sky surveys.

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