Diversity of gamma-ray burst energetics vs. supernova homogeneity: SN 2013cq associated with GRB 130427A

被引：56

作者：

Melandri, A. ^{[1
]}

Pian, E. ^{[2
,3
,4
,6
]}

D'Elia, V. ^{[5
]}

D'Avanzo, P. ^{[1
]}

Della Valle, M. ^{[7
,8
]}

Mazzali, P. A. ^{[9
,10
,11
]}

Tagliaferri, G. ^{[1
]}

Cano, Z. ^{[12
]}

Levan, A. J. ^{[13
]}

Moller, P. ^{[14
]}

Amati, L. ^{[3
]}

Bernardini, M. G. ^{[1
]}

Bersier, D. ^{[9
]}

bufano, F. ^{[15
]}

Campana, S. ^{[1
]}

Castro-Tirado, A. J. ^{[16
]}

Covino, S. ^{[1
]}

Ghirlanda, G. ^{[1
]}

Hurley, K. ^{[17
]}

Malesani, D. ^{[18
]}

Masetti, N. ^{[3
]}

Palazzi, E. ^{[3
]}

Piranmonte, S. ^{[6
]}

Rossi, A. ^{[19
]}

Salvaterra, R. ^{[20
]}

Starling, R. L. C. ^{[21
]}

Tanaka, M. ^{[22
]}

Tanvir, N. R. ^{[21
]}

Vergani, S. D. ^{[23
]}

机构：

[1] INAF Osservatorio Astron Brera, I-23807 Merate, Italy

[2] Scuola Normale Super Pisa, I-56126 Pisa, Italy

[3] INAF Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy

[4] INFN, Sez Pisa, I-56127 Pisa, Italy

[5] ASI, Sci Data Ctr, I-00133 Rome, Italy

[6] INFN Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[7] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy

[8] ICRANET, Piazza Repubbl, I-65122 Pescara, Italy

[9] Liverpool John Moores Univ, ARI, Liverpool L3 5UX, Merseyside, England

[10] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[11] Max Planck Inst Astrophys, D-85741 Garching, Germany

[12] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland

[13] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[14] European So Observ, D-85748 Garching, Germany

[15] Univ Andres Bello, Dept Ciencias Fis, Santiago 837025, Chile

[16] Inst Astrofis Andalucia, Granada 18008, Spain

[17] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[18] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark

[19] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany

[20] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy

[21] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[22] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[23] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92195 Meudon, France

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 567卷

基金：

新加坡国家研究基金会;

关键词：

gamma-ray burst: general; supernovae: individual: SN2013cq; DIGITAL SKY SURVEY; OPTICAL AFTERGLOW; E-P; E-I-E-ISO CORRELATION; LIGHT-CURVE; HOST GALAXY; LONG; PHOTOMETRY; SPECTROSCOPY; GRB-030329; DISCOVERY;

D O I：

10.1051/0004-6361/201423572

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. Long-duration gamma-ray bursts (GRBs) have been found to be associated with broad-lined type-Ic supernovae (SNe), but only a handful of cases have been studied in detail. Prompted by the discovery of the exceptionally bright, nearby GRB 130427A (redshift z = 0.3399), we aim at characterising the properties of its associated SN 2013cq. This is the first opportunity to test the progenitors of high-luminosity GRBs directly. Methods. We monitored the field of the Swift long-duration GRB 130427A using the 3.6 m TNG and the 8.2 m VLT during the time interval between 3.6 and 51.6 days after the burst. Photometric and spectroscopic observations revealed the presence of the type Ic SN2013cq. Results. Spectroscopic analysis suggests that SN 2013cq resembles two previous GRB-SNe, SN 1998bw and SN 2010bh, associated with GRB 980425 and X-ray flash (XRF) 100316D, respectively. The bolometric light curve of SN 2013cq, which is significantly affected by the host galaxy contribution, is systematically more luminous than that of SN 2010bh (similar to 2 mag at peak), but is consistent with SN 1998bw. The comparison with the light curve model of another GRB-connected SN 2003dh indicates that SN 2013cq is consistent with the model when brightened by 20%. This suggests a synthesised radioactive Ni-56 mass of similar to 0.4M(circle dot). GRB 130427A/SN 2013cq is the first case of low-z GRB-SN connection where the GRB energetics are extreme (E-gamma,E-iso similar to 10(54) erg). We show that the maximum luminosities attained by SNe associated with GRBs span a very narrow range, but those associated with XRFs are significantly less luminous. On the other hand the isotropic energies of the accompanying GRBs span 6 orders of magnitude (10(48) erg < E-gamma.iso < 10(54) erg), although this range is reduced when corrected for jet collimation. The GRB total radiated energy is in fact a small fraction of the SN energy budget.

引用

页数：9

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