THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS

被引：193

作者：

Kann, D. A. ^{[1
]}

Klose, S. ^{[1
]}

Zhang, B. ^{[2
]}

Covino, S. ^{[3
]}

Butler, N. R. ^{[4
,5
]}

Malesani, D. ^{[6
]}

Nakar, E. ^{[7
]}

Wilson, A. C. ^{[8
]}

Antonelli, L. A. ^{[9
,10
]}

Chincarini, G. ^{[3
,11
]}

Cobb, B. E. ^{[5
,12
,13
]}

D'Avanzo, P. ^{[3
,14
]}

D'Elia, V. ^{[3
,10
]}

Della Valle, M. ^{[15
,16
,17
]}

Ferrero, P. ^{[1
,18
]}

Fugazza, D. ^{[3
]}

Gorosabel, J. ^{[19
]}

Israel, G. L. ^{[10
]}

Mannucci, F. ^{[20
]}

Piranomonte, S. ^{[10
]}

Schulze, S. ^{[1
,21
]}

Stella, L. ^{[10
]}

Tagliaferri, G. ^{[3
]}

Wiersema, K. ^{[22
,23
]}

机构：

[1] Thuringer Landessternwarte Tautenburg, Tautenburg, Germany

[2] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA

[3] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy

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

[5] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[6] Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark

[7] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[8] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[9] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy

[10] INAF Natl Inst Astrophys, I-00136 Rome, Italy

[11] Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy

[12] Yale Univ, Dept Astron, New Haven, CT 06520 USA

[13] George Washington Univ, Dept Phys, Washington, DC 20052 USA

[14] Univ Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy

[15] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy

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

[17] Int Ctr Relativist Astrophys Network, Pescara, Abruzzo, Italy

[18] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain

[19] CSIC, IAA, E-18080 Granada, Spain

[20] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy

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

[22] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands

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

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 734卷 / 02期

基金：

以色列科学基金会; 美国国家科学基金会;

关键词：

gamma-ray burst: general; gamma-ray burst: individual (GRB 060121; GRB; 060505; 060614); stars: neutron; NEUTRON-STAR MERGERS; HIGH-ENERGY EMISSION; COMPACT OBJECT MERGERS; SHORT-DURATION; HOST GALAXIES; X-RAY; LIGHT CURVES; LOW-LUMINOSITY; PRE-SWIFT; PEAK LUMINOSITY;

D O I：

10.1088/0004-637X/734/2/96

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gamma-ray bursts (GRBs) have been separated into two classes, originally along the lines of duration and spectral properties, called "short/hard" and "long/soft." The latter have been conclusively linked to the explosive deaths of massive stars, while the former are thought to result from the merger or collapse of compact objects. In recent years, indications have been accumulating that the short/hard versus long/soft division does not map directly onto what would be expected from the two classes of progenitors, leading to a new classification scheme called Type I and Type II which is based on multiple observational criteria. We use a large sample of GRB afterglow and prompt-emission data (adding further GRB afterglow observations in this work) to compare the optical afterglows (or the lack thereof) of Type I GRBs with those of Type II GRBs. In comparison to the afterglows of Type II GRBs, we find that those of Type I GRBs have a lower average luminosity and show an intrinsic spread of luminosities at least as wide. From late and deep upper limits on the optical transients, we establish limits on the maximum optical luminosity of any associated supernova (SN), confirming older works and adding new results. We use deep upper limits on Type I GRB optical afterglows to constrain the parameter space of possible mini-SN emission associated with a compact-object merger. Using the prompt-emission data, we search for correlations between the parameters of the prompt emission and the late optical afterglow luminosities. We find tentative correlations between the bolometric isotropic energy release and the optical afterglow luminosity at a fixed time after the trigger (positive), and between the host offset and the luminosity (negative), but no significant correlation between the isotropic energy release and the duration of the GRBs. We also discuss three anomalous GRBs, GRB 060505, GRB 060614, and GRB 060121, in light of their optical afterglow luminosities.

引用

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