Interplanetary Network Localizations of Konus Short Gamma-Ray Bursts

Pal'Shin, V.; Hurley, K.; Svinkin, D.; Aptekar, R.; Golenetskii, S.; Frederiks, D.; Mazets, E.; Oleynik, P.; Ulanov, M.; Cline, T.; Митрофанов, И. Г.; Golovin, D. V.; Kozyrev, A.; Litvak, M. L.; Санин, А. Б.; Boynton, W. V.; Fellows, C.; Harshman, K.; Trombka, J. I.; McClanahan, T. P.; Starr, R.; Goldsten, J.; Gold, R. E.; Rau, A.; Kienlin, A. von; Savchenko, V.; Smith, D. M.; Hajdas, W.; Barthelmy, S. D.; Cummings, J. R.; Gehrels, N.; Krimm, H. A.; Palmer, D. M.; Yamaoka, K.; Ohno, M.; Fukazawa, Yasushi; Hanabata, Y.; Takahashi, T.; Tashiro, M.; Terada, Y.; Murakami, T.; Makishima, K.; Briggs, M. S.; Kippen, R. M.; Kouveliotou, C.; Meegan, C.; Fishman, G. J.; Connaughton, V.; Boër, M.; Guidorzi, C.; Frontera, F.; Montanari, E.; Rossi, Fabrice; Feroci, M.; Amati, L.; Nicastro, L.; Orlandini, M.; Monte, E. Del; Costa, E.; Donnarumma, I.; Evangelista, Y.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Rapisarda, M.; Soffitta, P.; Cocco, G. Di; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Atteia, J. L.; Vanderspek, R.; Ricker, G.

doi:10.1088/0067-0049/207/2/38

Cited by 31 publications

(19 citation statements)

References 57 publications

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“…The AGILE onboard clock deviations from the GPS reference are of order of few μs per second and are corrected for by on‐ground data preprocessing. MCAL data are also routinely used within the third Inter‐Planetary Network (IPN, web page: http://www.ssl.berkeley.edu/ipn3/) for GRB localization by means of triangulation, see Hurley et al [] and Pal'shin et al [] for recent IPN results including MCAL data. Pal'shin et al [] used timing data for 23 precisely localized GRBs to test the accuracy of the localization algorithm.…”

Section: Instrument and Data Descriptionmentioning

confidence: 99%

“…MCAL data are also routinely used within the third Inter‐Planetary Network (IPN, web page: http://www.ssl.berkeley.edu/ipn3/) for GRB localization by means of triangulation, see Hurley et al [] and Pal'shin et al [] for recent IPN results including MCAL data. Pal'shin et al [] used timing data for 23 precisely localized GRBs to test the accuracy of the localization algorithm. In the case of the short bright GRB 090510 the difference between the observed and expected time delay between MCAL and the Konus‐WIND spacecraft is

1 . 5_{- 3.3}^{+ 1.3}

ms (1 σ error), as resulting from the cross correlation of the burst light curves (V. Pal'shin, personal communication, 2013).…”

Section: Instrument and Data Descriptionmentioning

confidence: 99%

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Properties of terrestrial gamma ray flashes detected by AGILE MCAL below 30 MeV

et al. 2014

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Citation:Marisaldi, M., et al. (2014) • latitude band and selected to have the maximum photon energy up to 30 MeV. The characteristics of the AGILE events are analyzed and compared to the observational framework established by the two other currently active missions capable of detecting TGFs from space, RHESSI and Fermi. A detailed model of the MCAL dead time is presented, which is fundamental to properly interpret our observations. The most significant contribution to dead time is due to the anticoincidence shield in its current configuration and not to the MCAL detector itself. Longitude and local time distributions are compatible with previous observations, while the duration distribution is biased toward longer values because of dead time. The intensity distribution is compatible with previous observations, when dead time is taken into account. The TGFs cumulative spectrum supports a low production altitude, in agreement with previous measurements. We also compare our sample to lightning sferics detected by the World Wide Lightning Location Network and suggest a new method to assess quantitatively the consistency of two TGF populations based on the comparison of the associated lightning activity. According to this method, AGILE and RHESSI samples are compatible with the same parent population. The AGILE TGF catalog below 30 MeV is accessible online at the website of the ASI Science Data Center http://www.asdc.asi.it/mcaltgfcat/.

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Section: Instrument and Data Descriptionmentioning

confidence: 99%

1 . 5_{- 3.3}^{+ 1.3}

ms (1 σ error), as resulting from the cross correlation of the burst light curves (V. Pal'shin, personal communication, 2013).…”

Section: Instrument and Data Descriptionmentioning

confidence: 99%

Properties of terrestrial gamma ray flashes detected by AGILE MCAL below 30 MeV

et al. 2014

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“…Of those, perhaps 10%, or 215, would display EE (Palʼshin et al 2013), bringing the sample to 1935 non-EE bursts. We would expect about 80% of them to have no optical counterpart, either because none was detected or none was searched for (this number applies only to short bursts).…”

Section: Confirmed Cosmic Bursts Which Occurred Between 1990mentioning

confidence: 99%

Investigation of Primordial Black Hole Bursts Using Interplanetary Network Gamma-Ray Bursts

Ukwatta

Hurley

MacGibbon

et al. 2016

ApJ

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The detection of a gamma-ray burst (GRB) in the solar neighborhood would have very important implications for GRB phenomenology. The leading theories for cosmological GRBs would not be able to explain such events. The final bursts of evaporating primordial black holes (PBHs), however, would be a natural explanation for local GRBs. We present a novel technique that can constrain the distance to GRBs using detections from widely separated, non-imaging spacecraft. This method can determine the actual distance to the burst if it is local. We applied this method to constrain distances to a sample of 36 short-duration GRBs detected by the Interplanetary Network (IPN) that show observational properties that are expected from PBH evaporations. These bursts have minimum possible distances in the 10 13 -10 18 cm (7-10 5 au) range, which are consistent with the expected PBH energetics and with a possible origin in the solar neighborhood, although none of the bursts can be unambiguously demonstrated to be local. Assuming that these bursts are real PBH events, we estimate lower limits on the PBH burst evaporation rate in the solar neighborhood.

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“…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). By crosscorrelating of different catalogues, we have created a list composed by 7516 distinct GRBs shown in Table 2 (here only a sample, the complete table is presented as on line material).…”

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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Interplanetary Network Localizations of Konus Short Gamma-Ray Bursts

Cited by 31 publications

References 57 publications

Properties of terrestrial gamma ray flashes detected by AGILE MCAL below 30 MeV

Properties of terrestrial gamma ray flashes detected by AGILE MCAL below 30 MeV

Investigation of Primordial Black Hole Bursts Using Interplanetary Network Gamma-Ray Bursts

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

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