Issue |
A&A
Volume 451, Number 3, June I 2006
|
|
---|---|---|
Page(s) | 777 - 787 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20053913 | |
Published online | 04 May 2006 |
Swift and XMM-Newton observations of the dark GRB 050326
1
INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy e-mail: moretti@merate.mi.astro.it
2
INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, via E. Bassini 15, 20133 Milano Italy
3
International School for Advanced Studies (SISSA/ISAS), via Beirut 2-4, 34014 Trieste, Italy
4
Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
5
NASA/Goddard Space Flight Center, Greenbelt Road, Greenbelt, MD20771, USA
6
Università degli studi di Milano-Bicocca, Dipartimento di Fisica, piazza delle Scienze 3, 20126 Milano, Italy
7
ASI Science Data Center, via G. Galilei, 00044 Frascati (Roma), Italy
8
INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, via U. La Malfa 153, 90146 Palermo, Italy
9
X-Ray Observational Astronomy Group, Department of Physics and Astronomy, University of Leicester, LE1 7RH, UK
10
Universities Space Research Association, 10211 Wincopin Circle, Suite 500, Columbia, MD, 21044-3432, USA
11
Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
12
Department Physics, University of Nevada, Las Vegas, Nevada, 89154-4002, USA
13
Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
14
Department of Physics and Astronomy, Sonoma State University, Rohnert Park, California 94928, USA
Received:
26
July
2005
Accepted:
14
December
2005
We present Swift and XMM-Newton observations of the bright gamma-ray
burst GRB 050326, detected by the Swift Burst Alert Telescope. The Swift
X-Ray Telescope (XRT) and XMM-Newton discovered the X-ray afterglow
beginning 54 min and 8.5 h after the burst, respectively. The prompt
GRB 050326 fluence was erg cm-2
(20–150 keV), and its spectrum was hard, with a power law photon index
. The X-ray afterglow was quite bright, with a flux of
erg cm-2 s-1 (0.3–8 keV), 1 h after the burst. Its
light curve did not show any break nor flares between
h and
d after the burst, and decayed with a slope
. The
afterglow spectrum is well fitted by a power-law model, suffering absorption
both in the Milky Way and in the host galaxy. The rest-frame hydrogen column
density is significant,
cm-2, and the
redshift of the absorber was constrained to be
. There was good
agreement between the spatial, temporal, and spectral parameters as derived by
Swift-XRT and XMM-Newton. By comparing the prompt and afterglow fluxes, we found
that an early break probably occurred before the beginning of the XRT
observation, similarly to many other cases observed by Swift. However, the
properties of the GRB 050326 afterglow are well described by a spherical
fireball expanding in a uniform external medium, so a further steepening
is expected at later times. The lack of such a break allowed us to
constrain the jet half-opening angle
. Using the
redshift constraints provided by the X-ray analysis, we also estimated that the
beaming-corrected gamma-ray energy was larger than
erg, at
the high end of GRB energies. Despite the brightness in X rays, only deep
limits could be placed by Swift-UVOT at optical and ultraviolet wavelengths.
Thus, this GRB was a “truly dark” event, with the optical-to-X-ray spectrum
violating the synchrotron limit. The optical and X-ray observations are
therefore consistent either with an absorbed event or with a high-redshift one.
To obey the Ghirlanda relation, a moderate/large redshift
is
required.
Key words: gamma rays: bursts / gamma rays: observations / X-rays: bursts
© ESO, 2006
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