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Issue A&A
Volume 464, Number 3, March IV 2007
Page(s) L29 - L32
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20066912



A&A 464, L29-L32 (2007)
DOI: 10.1051/0004-6361:20066912

Letter

Constraining the rate of GRB visible afterglows with the CFHTLS very wide survey

F. Malacrino1, J.-L. Atteia1, M. Boër2, A. Klotz2, 3, C. Veillet4, J.-C. Cuillandre4, and the GRB RTAS collaboration

1  Laboratoire d'Astrophysique de Toulouse-Tarbes, Observatoire Midi-Pyrénées (CNRS-UMR5572/Université Paul Sabatier Toulouse III), 14 avenue Édouard Belin, 31400 Toulouse, France
    e-mail: fmalacri@ast.obs-mip.fr
2  Observatoire de Haute-Provence, 04870 Saint-Michel l'Observatoire, France
3  Centre d'Étude Spatiale des Rayonnements, Observatoire Midi-Pyrénées (CNRS/UPS), BP 4346, 31028 Toulouse Cedex 04, France
4  Canada-France-Hawaii Telescope Corp., Kamuela, HI 96743, USA

(Received 11 December 2006 / Accepted 19 January 2007 )

Abstract
Aims.We analyze images of the CFHTLS Very Wide Survey to search for visible orphan afterglows from gamma-ray bursts (GRBs).
Methods.We have searched 490 square degrees down to magnitude r'=22.5 for visible transients similar to GRB afterglows. We translate our observations into constraints on the number of GRB visible afterglows in the sky, by measuring the detection efficiency of our search with a simulation reproducing the characteristics of our observational strategy and the properties of on-axis GRB afterglows.
Results.We have found only three potential candidates, of which two are most probably variable stars, and one presents similarities to an orphan afterglow. We constrain the number of visible afterglows to be less than 220 down to r'=22.5 in the whole sky at any time. Our observations are marginally consistent with the most optimistic model, which predicts orphan afterglows to be about 10 times more frequent than GRBs.
Conclusions.This search has led to the detection of one possible GRB afterglow, and provides the strongest constraints on the rate of GRB visible afterglows as well as an estimation of the observing time required to detect a significant number of GRB afterglows.


Key words: gamma rays: bursts -- methods: data analysis



© ESO 2007


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