Observation of the Second LIGO/Virgo Event Connected with a Binary Neutron Star Merger S190425z in the Gamma-Ray Range

Pozanenko, A.; Minaev, P. Yu.; Гребенев, С. А.; Человеков, И. В.

doi:10.1134/s1063773719110057

Cited by 50 publications

(24 citation statements)

References 52 publications

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“…A weak Gamma Ray Burst, GRB 190425, was detected by the Anti-Coincidence Shield (ACS) of the SPI gamma-ray spectrometer onboard INTEGRAL [176], but not confirmed by Fermi-GBM [118] (see also [169], [212]). The time profile of GRB 190425 (two pulses at 0.5 and 5.9 s after the merger) is similar to that of GW170817 [200]. The absence of an optical counterpart could be explained by a large inclination of the jet axis with respect to the observer [200].…”

Section: Pos(golden2019)052mentioning

confidence: 70%

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Gravitational wave astronomy with compact binary mergers

Poggiani¹

2021

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects v — PoS(GOLDEN2019)

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Event m 1 (M) m 2 (M) M c (M) χ e f f M f (M) a f E r (M c 2) l peak (erg s −1) d L (Mpc) z ∆Ω(deg 2) GW150914 35.6 +4.7 −3.1 30.6 +3.0 −4.4 28.6 +1.7 −1.5-0.01 +0.12 −0.13 63.1 +3.4 −3.0 0.69 +0.05 −0.04 3.1 +0.4 −0.4 3.6 +0.4 −0.4 × 10 56 440 +150 −170 0.09 +0.03 −0.03 182 GW151012 23.2 +14.9 −5.5 13.6 +4.1 −4.8 15.2 +2.1 −1.2 0.05 +0.31 −0.20 35.6 +10.8 −3.8 0.67 +0.13 −0.11 1.6 +0.6 −0.5 3.2 +0.8 −1.7 × 10 56 1080 +550 −490 0.21 +0.09 −0.09 1523 GW151226 13.7 +8.8 −3.2 7.7 +2.2 −2.5 8.9 +0.3 −0.3 0.18 +0.20 −0.12 20.5 +6.4 −1.5 0.74 +0.07 −0.05 1.0 +0.1 −0.2 3.4 +0.7 −1.7 × 10 56 450 +180 −190 0.09 +0.04 −0.04 1033 GW170104 30.8 +7.3 −5.6 20.0 +4.9 −4.6 21.4 +2.2 −1.8-0.04 +0.17 −0.21 48.9 +5.1 −4.0 0.66 +0.08 −0.11 2.2 +0.5 −0.5 3.3 +0.6 −1.0 × 10 56 990 +440 −430 0.20 +0.08 −0.08 921 GW170608 11.0 +5.5 −1.7 7.6 +1.4 −2.2 7.9 +0.2 −0.2 0.03 +0.19 −0.07 17.8 +3.4 −0.7 0.69 +0.04 −0.04 0.9 +0.0 −0.1 3.5 +0.4 −1.3 × 10 56 320 +120 −110 0.07 +0.02 −0.02 392 GW170729 50.2 +16.2 −10.2 34.0 +9.1 −10.1 35.4 +6.5 −4.8 0.37 +0.21 −0.25 79.5 +14.7 −10.2 0.81 +0.07 −0.13 4.8 +1.7 −1.7 4.2 +0.9 −1.5 × 10 56 2840 +1400 −1360 0.49 +0.19 −0.21 1041 GW170809 35.0 +8.3 −5.9 23.8 +5.1 −5.2 24.9 +2.1 −1.7 0.08 +0.17 −0.17 56.3 +5.2 −3.8 0.70 +0.08 −0.09 2.7 +0.6 −0.6 3.5 +0.6 −0.9 × 10 56 1030 +320 −390 0.20 +0.05 −0.07 308 GW170814 30.6 +5.6 −3.0 25.2 +2.8 −4.0 24.1 +1.4 −1.1 0.07 +0.12 −0.12 53.2 +3.2 −2.4 0.72 +0.07 −0.05 2.7 +0.4 −0.3 3.7 +0.4 −0.5 × 10 56 600 +150 −220 0.12 +0.03 −0.04 87 GW170817 1.46 +0.12 −0.10 1.27 +0.09 −0.09 1.186 +0.001 −0.001 0.00 +0.02 −0.01 ≤ 2.8 ≤ 0.89 ≥ 0.04 ≥ 0.1 × 10 56 40 +7 −15 0.01 +0.00 −0.00 16 GW170818 35.4 +7.5 −4.7 26.7 +4.3 −5.2 26.5 +2.1 −1.7-0.09 +0.18 −0.21 59.4 +4.9 −3.8 0.67 +0.07 −0.08 2.7 +0.5 −0.5 3.4 +0.5 −0.7 × 10 56 1060 +420 −380 0.21 +0.07 −0.07 39 GW170823 39.5 +11.2 −6.7 29.0 +6.7 −7.8 29.2 +4.6 −3.6 0.09 +0.22 −0.26 65.4 +10.1 −7.4 0.72 +0.09 −0.12 3.3 +1.0 −0.9 3.6 +0.7 −1.1 × 10 56 1940 +970 −900 0.35 +0.

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Section: Pos(golden2019)052mentioning

confidence: 70%

“…The time profile of GRB 190425 (two pulses at 0.5 and 5.9 s after the merger) is similar to that of GW170817 [200]. The absence of an optical counterpart could be explained by a large inclination of the jet axis with respect to the observer [200].…”

Section: Pos(golden2019)052mentioning

confidence: 70%

Gravitational wave astronomy with compact binary mergers

Poggiani¹

2021

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects v — PoS(GOLDEN2019)

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“…The secondary component of the GW190521 binary was inferred to have m 2 = 66 +0. 28 −0.34 M , which means that this was the heaviest system detected by LIGO-Virgo to date, with a total mass M = m 1 + m 2 = 150 +29 −17 M . The remnant formed in this merger had a correspondingly large mass of m f = 142 +28 −16 M , making it the first confirmed intermediate-mass black hole (IMBH), i.e., a hole in the range 10 2 −10 5 M .…”

Section: Gw190521mentioning

confidence: 87%

“…9 Unlike for that first BNS detection, however, there was no confirmed electromagnetic counterpart associated with this GW trigger (although see Ref. [28]). Although both LIGO Livingston and Virgo were collecting data at the time, GW190425's network signal-to-noise ratio (SNR) of 12.9 was overwhelmingly a Unless otherwise noted, all quantities reported in this review consist of the median and the symmetric 90%-credible interval around it.…”

Section: Gw190425mentioning

confidence: 94%

Recent LIGO-Virgo discoveries

Isi

2021

Mod. Phys. Lett. A

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The LIGO and Virgo gravitational-wave detectors carried out the first half of their third observing run from April through October 2019. During this period, they detected 39 new signals from the coalescence of black holes or neutron stars, more than quadrupling the total number of detected events. These detections included some unprecedented sources, like a pair of black holes with unequal masses (GW190412), a massive pair of neutron stars (GW190425), a black hole potentially in the supernova pair-instability mass gap (GW190521), and either the lightest black hole or the heaviest neutron star known to date (GW190814). Collectively, the full set of signals provided astrophysically valuable information about the distributions of compact objects and their evolution throughout cosmic history. It also enabled more constraining and diverse tests of general relativity, including new probes of the fundamental nature of black holes. This review summarizes the highlights of these results and their implications.

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“…In this observing period, two merger events possibly involving neutron stars were reported by the LIGO-Virgo consortium: GW190425, caused by the coalescence of two compact objects of masses each in the range 1.12-2.52 M ⊙ , at ∼ 160 Mpc (Abbott et al, 2020a), and GW190814, caused by a 23 M ⊙ black hole merging with a compact object of 2.6 M ⊙ at ∼ 240 Mpc (Abbott et al, 2020b). In neither case did the search for an optical or infrared counterpart return a positive result (Coughlin et al, 2019;Gomez et al, 2019;Ackley et al, 2020;Andreoni et al, 2020;Antier et al, 2020;, owing presumably to the large distance and sky error areas, although a short GRB may have been detected by the INTEGRAL SPI-ACS simultaneously with GW190425 (Pozanenko et al, 2019). Note that all coalescing stars may have been black holes, as the neutron star nature of the binary members lighter than 3 M ⊙ could not be confirmed.…”

Section: Summary and Future Prospectsmentioning

confidence: 98%

Mergers of Binary Neutron Star Systems: A Multimessenger Revolution

Pian

2021

Front. Astron. Space Sci.

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On August 17, 2017, less than two years after the direct detection of gravitational radiation from the merger of two∼30 M⊙ black holes, a binary neutron star merger was identified as the source of a gravitational wave signal of ∼100 s duration that occurred at less than 50 Mpc from Earth. A short gamma-ray burst was independently identified in the same sky area by the Fermi and INTEGRAL satellites for high energy astrophysics, which turned out to be associated with the gravitational event. Prompt follow-up observations at all wavelengths led first to the detection of an optical and infrared source located in the spheroidal Galaxy NGC4993 and, with a delay of ∼10 days, to the detection of radio and X-ray signals. This article revisits these observations and focusses on the early optical/infrared source, which was thermal in nature and powered by the radioactive decay of the unstable isotopes of elements synthesized via rapid neutron capture during the merger and in the phases immediately following it. The far-reaching consequences of this event for cosmic nucleosynthesis and for the history of heavy elements formation in the Universe are also illustrated.

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Observation of the Second LIGO/Virgo Event Connected with a Binary Neutron Star Merger S190425z in the Gamma-Ray Range

Cited by 50 publications

References 52 publications

Gravitational wave astronomy with compact binary mergers

Gravitational wave astronomy with compact binary mergers

Recent LIGO-Virgo discoveries

Mergers of Binary Neutron Star Systems: A Multimessenger Revolution

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