On the Afterglow of the X-Ray Flash of 2003 July 23: Photometric Evidence for an Off-Axis Gamma-Ray Burst with an Associated Supernova?

• Published in: The Astrophysical journal 2004-07, Vol.609 (2), p.962-971
• Main Authors: Fynbo, J. P. U, Sollerman, J, Hjorth, J, Grundahl, F, Gorosabel, J, Weidinger, M, Møller, P, Jensen, B. L, Vreeswijk, P. M, Fransson, C, Ramirez-Ruiz, E, Jakobsson, P, Jørgensen, S. F, Vinter, C, Andersen, M. I, Cerón, J. M. Castro, Castro-Tirado, A. J, Fruchter, A. S, Greiner, J, Kouveliotou, C, Levan, A, Klose, S, Masetti, N, Pedersen, H, Palazzi, E, Pian, E, Rhoads, J, Rol, E, Sekiguchi, T, Tanvir, N. R, Tristram, P, de Ugarte Postigo, A, Wijers, R. A. M. J, van den Heuvel, E
• Format: Article
• Language: English
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; Gamma-ray sources; gamma-ray bursts; Late stages of stellar evolution (including black holes); Stars; Stellar systems. Galactic and extragalactic objects and systems. The universe; Supernovae; Unidentified sources and radiation outside the solar system
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/421260

We present optical and near-infrared follow-up observations of the X-ray flash (XRF) of 2003 July 23. Our observations in the R band cover the temporal range from 4.2 hr to 64 days after the high-energy event. We also present the results of multicolor imaging extending to the K band on three epochs. The light curve of the R-band afterglow the first week after the burst is similar to the light curve for long-duration gamma-ray bursts (GRBs), i.e. a broken power law with a late time slope of alpha ~ 2.0 (F sub( nu ) [proportional] t super(-alpha)). Furthermore, the spectral energy distribution (SED) has a power-law (F sub( nu ) [proportional] nu super(- beta )) shape with slope beta ~ 1.0. However, the decay slope at t < 1 day is shallow, consistent with zero. This is in qualitative agreement with the prediction that XRFs are off-axis classical GRBs. After the first week there is a strong bump in the light curve, which peaks at around 16 days. The SED after the peak becomes significantly redder. We discuss the possible interpretations of this bump and conclude that an underlying supernova is the most likely explanation since no other model appears consistent with the evolution of the SED. Finally, we present deep spectroscopy of the burst both in the afterglow and in the bump phase. A firm upper limit of z = 2.3 is placed on the redshift of XRF 030723 from the lack of Lyalpha forest lines in the spectrum of the afterglow. The lack of significant absorption and emission lines in either of the two spectra excludes a spectroscopic redshift determination.