THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFT AND SWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

被引：269

作者：

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

Klose, S. ^{[1
]}

Zhang, B. ^{[2
]}

Malesani, D. ^{[3
]}

Nakar, E. ^{[4
,5
]}

Pozanenko, A. ^{[6
]}

Wilson, A. C. ^{[7
]}

Butler, N. R. ^{[8
,9
]}

Jakobsson, P. ^{[10
,11
]}

Schulze, S. ^{[1
,11
]}

Andreev, M. ^{[12
,13
]}

Antonelli, L. A. ^{[14
]}

Bikmaev, I. F. ^{[15
,16
]}

Biryukov, V. ^{[17
,19
]}

Boettcher, M. ^{[18
]}

Burenin, R. A. ^{[6
]}

Castro Ceron, J. M. ^{[3
,20
]}

Castro-Tirado, A. J. ^{[21
]}

Chincarini, G. ^{[22
,23
]}

Cobb, B. E. ^{[24
,25
]}

Covino, S. ^{[22
]}

D'Avanzo, P. ^{[23
,26
]}

D'Elia, V. ^{[14
,27
]}

Della Valle, M. ^{[28
,29
,30
]}

Postigo, A. de Ugarte ^{[22
]}

Efimov, Yu. ^{[19
]}

Ferrero, P. ^{[1
,31
]}

Fugazza, D. ^{[22
]}

Fynbo, J. P. U. ^{[3
]}

Galfalk, M. ^{[32
]}

Grundahl, F. ^{[33
]}

Gorosabel, J. ^{[21
]}

Gupta, S. ^{[18
]}

Guziy, S. ^{[21
]}

Hafizov, B. ^{[34
]}

Hjorth, J. ^{[3
]}

Holhjem, K. ^{[35
,36
]}

Ibrahimov, M. ^{[34
]}

Im, M. ^{[37
]}

Israel, G. L. ^{[14
]}

Jelinek, M. ^{[21
]}

Jensen, B. L. ^{[3
]}

Karimov, R. ^{[34
]}

Khamitov, I. M. ^{[38
]}

Kiziloglu, Ue ^{[39
]}

Klunko, E. ^{[40
]}

Kubanek, P. ^{[20
]}

Kutyrev, A. S. ^{[41
]}

Laursen, P. ^{[3
]}

Levan, A. J. ^{[42
]}

机构：

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

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

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

[4] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

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

[6] Space Res Inst IKI, Moscow 117997, Russia

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

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

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

[10] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

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

[12] RAS, Terskol Branch, Inst Astron, Kabardino Balkaria Repub 361605, Russia

[13] NASU, Int Ctr Astron & Medicoecol Res, UA-03680 Kiev, Ukraine

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

[15] Kazan VI Lenin State Univ, Kazan 420008, Russia

[16] Acad Sci Tatarstan, Kazan, Russia

[17] SRI Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine

[18] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA

[19] Sternberg Astron Inst, Crimean Lab, UA-98409 Nauchnyi, Crimea, Ukraine

[20] European Space Agcy, European Space Astron Ctr, Madrid 28691, Spain

[21] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

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

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

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

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

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

[27] ASI Sci Data Ctr, I-00044 Frascati, Italy

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

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

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

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

[32] Stockholm Univ, AlbaNova Univ Ctr, Stockholm Observ, Dept Astron, S-10691 Stockholm, Sweden

[33] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

[34] Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan

[35] Nord Opt Telescope, Santa Cruz De La Palma, Spain

[36] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany

[37] Seoul Natl Univ, CEOU, Astron Program, Dept Phys & Astron, Seoul, South Korea

[38] TUBITAK Natl Observ, Antalya, Turkey

[39] Middle E Tech Univ, TR-06531 Ankara, Turkey

[40] Inst Solar Terr Phys, Irkutsk 664033, Russia

[41] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA

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

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

[44] Loyola Coll, Baltimore, MD 21210 USA

[45] Univ Complutense Madrid, Dpto Fis Atom Mol & Nucl, Madrid, Spain

[46] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

[47] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway

[48] Univ Concepcion, Astron Grp, Fac Ciencias Fis & Matemat, Concepcion, Chile

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

[50] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 720卷 / 02期

关键词：

dust; extinction; gamma-ray burst: general; HIGH-RESOLUTION SPECTROSCOPY; BAND SPECTRAL EVOLUTION; FOLLOW-UP OBSERVATIONS; STAR-FORMATION RATE; EARLY X-RAY; HOST-GALAXY; LIGHT CURVES; MG-II; DUST EXTINCTION; PROMPT EMISSION;

D O I：

10.1088/0004-637X/720/2/1513

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to 2009 September, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A, and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host-galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z = 1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, are weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) is very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at 1 day after the GRB in the z = 1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without, reveals no indication that the former are statistically significantly more luminous. Furthermore, we propose the existence of an upper ceiling on afterglow luminosities and study the luminosity distribution at early times, which was not accessible before the advent of the Swift satellite. Most GRBs feature afterglows that are dominated by the forward shock from early times on. Finally, we present the first indications of a class of long GRBs, which form a bridge between the typical high-luminosity, high-redshift events and nearby low-luminosity events (which are also associated with spectroscopic supernovae) in terms of energetics and observed redshift distribution, indicating a continuous distribution overall.

引用

页码：1513 / 1558

页数：46

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