Searching for the host galaxy of GRB 920925C

Pozanenko, A.; Rumyantsev, V.; Loznikov, V. M.; Volnova, A.; Shulga, A. P.

doi:10.1134/s1063773708030018

Cited by 12 publications

(10 citation statements)

References 12 publications

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“…Using the measured redshift of this burst (Troja et al 2016) and the γ-ray fluence by , the isotropic-equivalent gamma-ray energy is E iso ∼ 0.04 × 10 51 erg (20 to 10 4 keV, rest-frame). As a part of the present work, ISON-Kislovodsk SANTEL-400A optical telescope started observations ∼ 0.141d after the burst and did not see any afterglow down to a limiting magnitude of ∼ 18.6 mag (Pozanenko et al 2014). To search further for the optical afterglow or for any possible "kilonova" emission for this nearby sGRB, we observed the field of GRB 140903A with the 1.5 m AZT-22 telescope of Maidanak astronomical observatory on 2014 September 4, 6, 7, and 13, taking 12-15 images of 60 s exposure in the R-filter.…”

Section: A5 Sgrb 140903amentioning

confidence: 75%

A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

Pandey

Castro-Tirado

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the prompt emission and the afterglow properties of short-duration gamma-ray burst (sGRB) 130603B and another eight sGRB events during 2012–2015, observed by several multiwavelength facilities including the Gran Canarias Telescope 10.4 m telescope. Prompt emission high energy data of the events were obtained by INTEGRAL-SPI-ACS, Swift-BAT, and Fermi-GBM satellites. The prompt emission data by INTEGRAL in the energy range of 0.1–10 MeV for sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A, and sGRB 151228A do not show any signature of the extended emission or precursor activity and their spectral and temporal properties are similar to those seen in case of other short bursts. For sGRB 130603B, our new afterglow photometric data constrain the pre-jet-break temporal decay due to denser temporal coverage. For sGRB 130603B, the afterglow light curve, containing both our new and previously published photometric data is broadly consistent with the ISM afterglow model. Modeling of the host galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software supports a scenario in which the environment of the burst is undergoing moderate star formation activity. From the inclusion of our late-time data for eight other sGRBs we are able to: place tight constraints on the non-detection of the afterglow, host galaxy, or any underlying ‘kilonova’ emission. Our late-time afterglow observations of the sGRB 170817A/GW170817 are also discussed and compared with the sub-set of sGRBs.

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Section: A5 Sgrb 140903amentioning

confidence: 75%

A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

Pandey

Castro-Tirado

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Lü et al 2010;Zhang et al 2012;Qin & Chen 2013;Zhang et al 2018b;Shahmoradi & Nemiroff 2015;Zou et al 2018;Pozanenko et al 2018). More over, in Pozanenko et al (2019b) the Amati relation was used to estimate the E p,i value for the second LIGO/Virgo event S190425z connected with binary neutron star merger, which was observed in gamma-ray domain by SPI-ACS/INTEGRAL experiment. Hardness -fluence (E p -F tot ) correlation, constructed for GRBs with no redshift, also demonstrated bimodal nature (e.g.…”

Section: Introductionmentioning

confidence: 99%

The Ep,i–Eiso correlation: type I gamma-ray bursts and the new classification method

Minaev

Pozanenko

2019

Monthly Notices of the Royal Astronomical Society

103

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We present the most extensive sample of 45 type I (short) and 275 type II (long) gamma-ray bursts (GRB) with known redshift to investigate the correlation between the rest frame peak energy, E p,i and the total isotropic equivalent energy, E iso of the prompt emission (Amati relation). The E p,i -E iso correlation for type I bursts is found to be well-distinguished from the one constructed for type II bursts and has a similar power-law index value, E p,i ∼ E 0.4 iso , which possibly indicates the same emission mechanism of both GRB types. We show that the initial pulse complex (IPC) of type I bursts with an extended emission and regular type I bursts follow the same correlation. We obtain similar results for type II bursts associated with Ic supernovae and for regular type II bursts.

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“…The sparse optical data constrain the break time to be t b > 0.64 d (Pavlenko et al 2005). More recently Yost et al (2007), suggested the presence of a break occurring at 0.6 ± 0.1 d in the optical light curve.…”

Section: Sample Selectionmentioning

confidence: 99%

AreSwiftgamma-ray bursts consistent with the Ghirlanda relation?

Campana¹,

Guidorzi

Tagliaferri³

et al. 2007

A&A

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A few tight correlations linking several properties of gamma-ray bursts (GRBs), namely the spectral peak energy, the total radiated energy, and the afterglow break time, have been discovered with pre-Swift GRBs. They were used to constrain the cosmological parameters, together with type-Ia supernovae. However, the tightness of these correlations is a challenge to GRB models. We explore the effect of adding Swift bursts to the Ghirlanda and Liang-Zhang relations. Although they are both still valid, they become somewhat weakened mostly due to the presence of significant outliers, which otherwise are apparently normal GRBs so difficult to distinguish. The increased dispersion of the relations makes them less reliable for purposes of precision cosmology.

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Searching for the host galaxy of GRB 920925C

Cited by 12 publications

References 12 publications

A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

The Ep,i–Eiso correlation: type I gamma-ray bursts and the new classification method

AreSwiftgamma-ray bursts consistent with the Ghirlanda relation?

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