Ghirlanda 2013 Swift亮暴的射电余辉统计

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不同波段的峰值时间和峰值流量

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Title:		Radio afterglows of a complete sample of bright Swift GRBs: predictions from present days to the SKA era
Authors:		Ghirlanda, G.; Salvaterra, R.; Burlon, D.; Campana, S.; Melandri, A.; Bernardini, M. G.; Covino, S.; D'Avanzo, P.; D'Elia, V.; Ghisellini, G.; Nava, L.; Prandoni, I.; Sironi, L.; Tagliaferri, G.; Vergani, S. D.; Wolter, A.
Affiliation:		AA(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy; giancarlo.ghirlanda@brera.inaf.it), AB(INAF - IASF Milano, via E. Bassini 15, I-20133 Milano, Italy), AC(Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006, Australia; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), The University of Sydney, NSW 2006, Australia), AD(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AE(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AF(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AG(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AH(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AI(ASI - Science Data Center, via Galileo Galilei, I-00044 Frascati, Italy; INAF-OAR Via Frascati 33, I-00040 Monteporzio Catone, Italy), AJ(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AK(APC Université Paris Diderot, 10 rue Alice Domon et Leonie Duquet, F-75205 Paris Cedex 13, France; INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AL(INAF - Istituto di Radioastronomia, via P. Gobetti, 101, I-40129 Bologna, Italy), AM(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AN(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AO(GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, 5 place Jules Janssen, F-92190 Meudon, France; INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy), AP(INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 435, Issue 3, p.2543-2551 (MNRAS Homepage)
Publication Date:		11/2013
Origin:		OUP
Astronomy Keywords:		radiation mechanisms: non thermal, radio continuum: general
Abstract Copyright:		2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:		10.1093/mnras/stt1466
Bibliographic Code:		2013MNRAS.435.2543G

Abstract

Radio observations of Gamma-Ray Bursts (GRBs) afterglows are fundamental in providing insights into their physics and environment, and in constraining the true energetics of these sources. Nonetheless, radio observations of GRB afterglows are presently sparse in the time/frequency domain. Starting from a complete sample of 58 bright Swift long bursts (BAT6), we constructed a homogeneous sub-sample of 38 radio detections/upper limits which preserves all the properties of the parent sample. One half of the bursts have detections between 1 and 5 d after the explosion with typical fluxes F ≳ 100 μJy at 8.4 GHz. Through a Population SYnthesis Code coupled with the standard afterglow Hydrodynamical Emission model, we reproduce the radio flux distribution of the radio sub-sample. Based on these results, we study the detectability in the time/frequency domain of the entire long GRB population by present and future radio facilities. We find that the GRBs that typically trigger Swift can be detected at 8.4 GHz by Jansky Very Large Array within few days with modest exposures even at high redshifts. The final Square Kilometre Array (SKA) can potentially observe the whole GRB population provided that there will be a dedicated GRB gamma-ray detector more sensitive than Swift. For a sizeable fraction (50 per cent) of these bursts, SKA will allow us to perform radio calorimetry, after the trans-relativistic transition (occurring ˜100 d), providing an estimate of the true (collimation corrected) energetics of GRBs.

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