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TwitterA&A 460, 415-424 (2006)
DOI: 10.1051/0004-6361:20065010
Multi-wavelength afterglow observations of the high redshift GRB 050730
S. B. Pandey1, A. J. Castro-Tirado1, S. McBreen2, 3, M. D. Pérez-Ramírez4, M. Bremer5, M. A. Guerrero1, A. Sota6, B. E. Cobb7, M. Jelínek1, A. de Ugarte Postigo1, J. Gorosabel1, S. Guziy1, 8, C. Guidorzi9, C. D. Bailyn7, T. Muñoz-Darias10, A. Gomboc9, 11, A. Monfardini9, C. G. Mundell9, N. Tanvir12, A. J. Levan12, B. C. Bhatt13, 14, D. K. Sahu13, 14, S. Sharma15, O. Bogdanov8, and J. A. Combi41 Instituto de Astrofísica de Andalucía, PO Box 03004, 18080 Granada, Spain
e-mail: sbp2@mssl.ucl.ac.uk
2 European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
3 Max-Planck-Institut für extraterrestrische Physik, 85748 Garching, Germany
4 Departamento de Física (EPS), Universidad de Jaén, Campus Las Lagunillas s/n (Ed-A3), 23071 Jaén, Spain
5 Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 Saint Martin d'Hères, France
6 IAA-CSIC and Space Telescope Science Institute, St. Martin Dr., Baltimore, MA, USA
7 Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520, USA
8 Nikolaev State University, Nikolska 24, Nikolaev 54030, Ukraine
9 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK
10 Instituto de Astrofísica de Canarias, C/. Vía Láctea, s/n, 38200 La Laguna, Tenerife, Spain
11 Faculty of Mathematics and Physics, University of Ljubljana, Jadranska 19, 1000 Ljubljana, Slovenia
12 Center for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
13 Center for Research & Education in Science & Technology, Hosakote, Bangalore 562 114, India
14 Indian Institute of Astrophysics, Bangalore 560 034, India
15 Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Naini Tal 263129, Uttaranchal, India
(Received 11 February 2006 / Accepted 2 August 2006)
Abstract
Context.GRB 050730 is a long duration high-redshift burst (z=3.967)
that was
discovered by Swift. The
afterglow shows variability and was well monitored over a wide wavelength range.
We present comprehensive temporal and spectral analysis of the afterglow of GRB 050730
including observations covering the wavelength range from the millimeter to X-rays.
Aims.We use multi-wavelength afterglow data to understand the complex temporal and spectral decay properties
of this high redshift burst.
Methods.Five telescopes were used to study the decaying afterglow of GRB 050730 in the
B, V, r', R, i', I, J and K photometric pass bands. A spectral energy distribution was
constructed at 2.9 h post-burst in the
B, V, R, I, J and K bands.
X-ray data from the satellites Swift and XMM-Newton were used to study the
afterglow evolution at higher energies.
Results.The early afterglow shows variability at early times and
the slope steepens at 0.1 days (8.6 ks)
in the
B, V, r', R, i', I, J and K passbands. The early afterglow light curve decayed with
a powerlaw slope index
and
subsequently steepened to
based on the R and I band data.
A millimeter detection of the afterglow around 3 days after the burst shows
an excess in comparison to theoretical predictions. The early X-ray light curve observed by Swift
is complex and contains flares. At late times the X-ray light curve can be fit by a powerlaw
decay with
which is steeper than the optical light curve.
A spectral energy distribution (SED) was constructed at ~2.9 h after the
burst. An electron energy index, p, of ~2.3 was calculated using the SED and
the photon index from the X-ray afterglow spectra and implies that the
synchrotron cooling frequency
is above the X-ray band.
Key words: gamma ray: bursts -- techniques: photometric
© ESO 2006