The spectral catalogue of INTEGRAL gamma-ray bursts

Bošnjak, Ž.; Götz, D.; Bouchet, L.; Schanne, S.; Cordier, B.

doi:10.1051/0004-6361/201322256

Cited by 31 publications

(54 citation statements)

References 43 publications

(70 reference statements)

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“…Although the number of correspondingly significant reported detections is relatively small (about ten detections a year for IBIS; Mereghetti 2012), the high INTEGRAL sensitivity in the hard X-ray domain efficiently probes a population of particularly faint and soft γ-ray bursts, with 20-200 keV fluences down to a few 10 −8 erg cm −2 (Bošnjak et al 2014). If at least a fraction of the LIGO/Virgo localization area for the future GW triggers overlap with the IBIS and/or SPI FoV, INTEGRAL observations could be used to localize and characterize in fairly good detail the corresponding electromagnetic counterparts, or at least put tight constraints on their hard X-ray/γ-ray emission (as is done in the present paper for LVT151012).…”

Section: Discussionmentioning

confidence: 99%

INTEGRAL IBIS, SPI, and JEM-X observations of LVT151012

Savchenko

Bazzano

Bozzo

et al. 2017

A&A

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During the first observing run of LIGO, two gravitational wave events and one lower-significance trigger (LVT151012) were reported by the LIGO/Virgo collaboration. At the time of LVT151012, the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was pointing at a region of the sky coincident with the high localization probability area of the event and thus permitted us to search for its electromagnetic counterpart (both prompt and afterglow emission). The imaging instruments on board INTEGRAL (IBIS/ISGRI, IBIS/PICsIT, SPI, and the two JEM-X modules) have been exploited to attempt the detection of any electromagnetic emission associated with LVT151012 over three decades in energy (from 3 keV to 8 MeV). The omni-directional instruments on board the satellite, i.e., the SPI-ACS and the IBIS/Veto, complemented the capabilities of the IBIS/ISGRI and IBIS/PICsIT for detections outside their imaging field of view in order to provide an efficient monitoring of the entire LVT151012 localization region at energies above 75 keV. We did not find any significant transient source that was spatially and/or temporally coincident with LVT151012, obtaining tight upper limits on the associated hard X-ray and γ-ray radiation. For typical spectral models, the upper limits on the fluence of the emission from any 1 s counterpart of LVT151012 ranges from F γ = 3.5 × 10 −8 erg cm −2 (20-200 keV), within the field of view of the imaging instruments, to F γ = 7.1 × 10 −7 erg cm −2 (75-2000 keV), considering the least favorable location of the counterpart for a detection by the omni-directional instruments. These results can be interpreted as a tight constraint on the ratio of the isotropic equivalent energy released in the electromagnetic emission to the total energy of the gravitational waves: E 75−2000 keV /E GW < 4.4 × 10 −5 . Finally, we provide an exhaustive summary of the capabilities of all instruments on board INTEGRAL to hunt for γ-ray counterparts of gravitational wave events, exploiting both serendipitous and pointed follow-up observations. This will serve as a reference for all future searches.

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Section: Discussionmentioning

confidence: 99%

INTEGRAL IBIS, SPI, and JEM-X observations of LVT151012

Savchenko

Bazzano

Bozzo

et al. 2017

A&A

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“…Despite this progress, still in the Fermi era it is found that the "Band" function provides reasonable fits to the vast majority of GRBs. [79][80][81][82][83][84] Many of these fits differ than earlier fits by the use of time-resolved analysis. Still, as explained above, in these fits "Band" model template was a-priori assumed, implying that "wiggles" could not be detected.…”

Section: Direct Evidencementioning

confidence: 99%

Photospheric emission in gamma-ray bursts

Pe’er

Ryde

2017

Int. J. Mod. Phys. D

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A major breakthrough in our understanding of gamma-ray bursts (GRB) prompt emission physics occurred in the last few years, with the realization that a thermal component accompanies the over-all non-thermal prompt spectra. This thermal part is important by itself, as it provides direct probe of the physics in the innermost outflow regions. It further has an indirect importance, as a source of seed photons for inverse-Compton scattering, thereby it contributs to the non-thermal part as well. In this short review, we highlight some key recent developments. Observationally, although so far it was clearly identified only in a minority of bursts, there are indirect evidence that thermal component exists in a very large fraction of GRBs, possibly close to 100%. Theoretically, the existence of thermal component have a large number of implications as a probe of underlying GRB physics. Some surprising implications include its use as a probe of the jet dynamics, geometry and magnetization.

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“…In addition, the complete table reported on line will make faster the searches for given GRBs. The following satellite missions and the associated catalogues have been taken into account: Agile by Galli, M. et al (2013);Pal'shin et al (2013); Longo, F. et al (2012); Hurley et al (2013), BeppoSAX by Frontera et al (2009), CGRO by Stern et al (2001); Kommers et al (2001);Schönfelder et al (2000) and the batsegrb catalogue Meegan et al 1996) in HEASARC web site 3 , Fermi with Paciesas et al (2012);von Kienlin et al (2014) and the fermigbrst catalogue in HEASARC archive 4 von Kienlin et al 2014;Goldstein et al 2012;Paciesas et al 2012), GRANAT, HETE-2, INTEGRAL by Minaev et al (2014); Bošnjak,Ž. et al (2014); Mereghetti (2013), Konus/Wind by Pal'shin et al (2013), Swift by Sakamoto et al (2011) and the "Swift GRB Table and Lookup" 5 ; ULYSSES by Hurley et al (1999).…”

Section: The Sample Selectionmentioning

confidence: 99%

“…In fact, we have matched various catalogues (i.e., Minaev et al (2014), Bošnjak,Ž. et al (2014), Mereghetti (2013), Pal'shin et al (2013)), in order to identify single different objects with respective coordinates, and to have a reasonable list for each of these missions.…”

Section: The Sample Selectionmentioning

confidence: 99%

Possible gamma-ray burst radio detections by the Square Kilometre Array. New perspectives

Ruggeri¹,

Capozziello²

2016

Astrophys Space Sci

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The next generation interferometric radio telescope, the Square Kilometre Array (SKA), which will be the most sensitive and largest radio telescope ever constructed, could greatly contribute to the detection, survey and characterization of Gamma Ray Bursts (GRBs). By the SKA, it will be possible to perform the follow up of GRBs even for several months. This approach would be extremely useful to extend the Spectrum Energetic Distribution (SED) from the gamma to the to radio band and would increase the number of radio detectable GRBs. In principle, the SKA could help to understand the physics of GRBs by setting constraints on theoretical models. This goal could be achieved by taking into account multiple observations at different wavelengths in order to obtain a deeper insight of the sources. Here, we present an estimation of GRB radio detections, showing that the GRBs can really be observed by the SKA. The approach that we present consists in determining blind detection rates derived by a very large sample consisting of merging several GRB catalogues observed by current missions as Swift, Fermi, Agile and INTEGRAL and by previous missions as BeppoSAX, CGRO, GRANAT, HETE-2, Ulysses and Wind. The final catalogue counts 7516 distinct sources. We compute the fraction of GRBs that could be observed by the SKA at high and low frequencies, above its observable sky. Considering the planned SKA sensitivity and through an extrapolation Alan Cosimo Ruggeri Salvatore Capozziello 1 Dipartimento di Fisica, Università di Napoli "Federico II", Compl. Univ. Monte S. Angelo, Via Cinthia 9, I -80126, Napoli, Italy. 2 I.N.F.N., Sez. di Napoli, Compl. Univ. Monte S. Angelo, Edificio G, Via Cintia, Napoli, Italy. 3 Gran Sasso Science Institute (INFN), Viale F. Crispi, 7, I-67100, L'Aquila, Italy. * acruggeri@na.infn.it; capozziello@na.infn.it based on previous works and observations, we deduce the minimum fluence in the range 15 -150 keV. This is the energy interval where a GRB should emit to be detectable in the radio band by the SKA. Results seem consistent with observational capabilities.

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The spectral catalogue of INTEGRAL gamma-ray bursts

Cited by 31 publications

References 43 publications

INTEGRAL IBIS, SPI, and JEM-X observations of LVT151012

INTEGRAL IBIS, SPI, and JEM-X observations of LVT151012

Photospheric emission in gamma-ray bursts

Possible gamma-ray burst radio detections by the Square Kilometre Array. New perspectives

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