TY - JOUR
T1 - X-ray spectral components observed in the afterglow of GRB 130925A
AU - Bellm, Eric C.
AU - Barrière, Nicolas M.
AU - Bhalerao, Varun
AU - Boggs, Steven E.
AU - Cenko, S. Bradley
AU - Christensen, Finn E.
AU - Craig, William W.
AU - Forster, Karl
AU - Fryer, Chris L.
AU - Hailey, Charles J.
AU - Harrison, Fiona A.
AU - Horesh, Assaf
AU - Kouveliotou, Chryssa
AU - Madsen, Kristin K.
AU - Miller, Jon M.
AU - Ofek, Eran O.
AU - Perley, Daniel A.
AU - Rana, Vikram R.
AU - Reynolds, Stephen P.
AU - Stern, Daniel
AU - Tomsick, John A.
AU - Zhang, William W.
PY - 2014/4/1
Y1 - 2014/4/1
N2 - 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 >4σ significance, and its spectral shape varies between two observation epochs at 2 × 105 and 106 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 (108 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.
AB - 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 >4σ significance, and its spectral shape varies between two observation epochs at 2 × 105 and 106 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 (108 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.
KW - gamma-ray burst: individual (GRB 130925A)
UR - https://www.scopus.com/pages/publications/84896981982
U2 - 10.1088/2041-8205/784/2/L19
DO - 10.1088/2041-8205/784/2/L19
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AN - SCOPUS:84896981982
SN - 2041-8205
VL - 784
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 2
M1 - L19
ER -