The rapid decay of the optical emission from GRB 980326 and its possible implications

被引:69
作者
Groot, PJ
Galama, TJ
Vreeswijk, PM
Wijers, RAMJ
Pian, E
Palazzi, E
van Paradijs, J
Kouveliotou, C
in't Zand, JJM
Heise, J
Robinson, C
Tanvir, N
Lidman, C
Tinney, C
Keane, M
Briggs, M
Hurley, K
Gonzalez, JF
Hall, P
Smith, MG
Covarrubias, R
Jonker, PG
Casares, J
Masetti, N
Frontera, F
Feroci, M
Piro, L
Costa, E
Smith, R
Jones, B
Windridge, D
Bland-Hawthorn, J
Veilleux, S
Garcia, M
Brown, WR
Stanek, KZ
Castro-Tirado, AJ
Gorosabel, J
Greiner, J
Jäger, K
Böhm, A
Fricke, KJ
机构
[1] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands
[2] Natl Inst Nucl & High Energy Phys, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands
[3] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[4] CNR, I-40129 Bologna, Italy
[5] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA
[6] Univ Space Res Assoc, Washington, DC USA
[7] NASA, MSFC, Huntsville, AL 35812 USA
[8] SRON, Utrecht, Netherlands
[9] European So Observ, Santiago 19, Chile
[10] Anglo Australian Observ, Epping, NSW 2121, Australia
[11] Cerro Tololo Interamer Observ, La Serena, Chile
[12] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA
[13] Univ Toronto, Dept Astron, Toronto, ON M5S 3H8, Canada
[14] Inst Astrofis Canarias, Tenerife, Spain
[15] CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy
[16] Univ Wales Coll Cardiff, Cardiff CF1 3NS, S Glam, Wales
[17] Univ Bristol, Bristol, Avon, England
[18] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[19] Ctr Astrophys, Cambridge, MA 02138 USA
[20] INTA, LAEFF, E-28080 Madrid, Spain
[21] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain
[22] Astrophys Inst Potsdam, D-14482 Potsdam, Germany
[23] Univ Sternwarte Gottingen, D-37083 Gottingen, Germany
关键词
gamma rays : bursts; gamma rays : observations; radiation mechanisms : nonthermal;
D O I
10.1086/311509
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report the discovery of the optical counterpart to GRB 980326. Its rapid optical decay can be characterized by a power law with exponent -2.10 +/- 0.13 and a constant underlying source at R-c = 25.5 +/- 0.5. Its optical colors 2.1 days after the burst imply a spectral slope of -0.66 +/- 0.70. The gamma-ray spectrum as observed with BATSE shows that it is among the 4% softest bursts ever recorded. We argue that the rapid optical decay may be a reason for the nondetection of some low-energy afterglows of GRBs.
引用
收藏
页码:L123 / L127
页数:5
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