X-RAY SPECTRAL COMPONENTS OBSERVED IN THE AFTERGLOW OF GRB 130925A

被引：19

作者：

Bellm, Eric C. ^{[1
]}

Barriere, Nicolas M. ^{[2
]}

Bhalerao, Varun ^{[3
]}

Boggs, Steven E. ^{[2
]}

Cenko, S. Bradley ^{[4
]}

Christensen, Finn E. ^{[5
]}

Craig, William W. ^{[2
,6
]}

Forster, Karl ^{[1
]}

Fryer, Chris L. ^{[7
]}

Hailey, Charles J. ^{[8
]}

Harrison, Fiona A. ^{[1
]}

Horesh, Assaf ^{[9
]}

Kouveliotou, Chryssa ^{[10
]}

Madsen, Kristin K. ^{[1
]}

Miller, Jon M. ^{[11
]}

Ofek, Eran O. ^{[9
]}

Perley, Daniel A. ^{[1
]}

Rana, Vikram R. ^{[1
]}

Reynolds, Stephen P. ^{[12
]}

Stern, Daniel ^{[13
]}

Tomsick, John A. ^{[2
]}

Zhang, William W. ^{[4
]}

机构：

[1] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

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

[3] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[5] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark

[6] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA

[7] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA

[8] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[9] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel

[10] NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA

[11] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[12] NC State Univ, Dept Phys, Raleigh, NC 27695 USA

[13] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2014年 / 784卷 / 02期

基金：

美国国家航空航天局;

关键词：

gamma-ray burst: individual (GRB 130925A); BURST; SUPERNOVA; SEARCH; STAR; SIGNATURES; EMISSION; OUTBURST; FALLBACK; PROMPT; EJECTA;

D O I：

10.1088/2041-8205/784/2/L19

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have identified spectral features in the late-time X-ray afterglow of the unusually long, slow-decaying GRB 130925A using NuSTAR, Swift/X-Ray Telescope, and Chandra. A spectral component in addition to an absorbed power law is required at >4 sigma significance, and its spectral shape varies between two observation epochs at 2 x 10(5) and 10(6) s after the burst. Several models can fit this additional component, each with very different physical implications. A broad, resolved Gaussian absorption feature of several keV width improves the fit, but it is poorly constrained in the second epoch. An additive blackbody or second power-law component provide better fits. Both are challenging to interpret: the blackbody radius is near the scale of a compact remnant (10(8) cm), while the second power-law component requires an unobserved high-energy cutoff in order to be consistent with the non-detection by Fermi/Large Area Telescope.

引用

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