Discovery of the Optical Transient of the Gamma Ray Burst 990308

• Published in: arXiv.org 1999-08
• Main Authors: Schaefer, Bradley E, Snyder, J A, Hernandez, J, Roscherr, B, Deng, M, Ellmann, N, Bailyn, C, Rengstorf, A, Smith, D, Levine, A, Barthelmy, S, Butterworth, P, Hurley, K, Cline, T, Meegan, C, Kouveliotou, C, Kippen, R, Park, H, Williams, G, Porrata, R, Bionta, R, Hartmann, D, Band, D, Frail, D, Kulkarni, S, Bloom, J, Djorgovski, S, Harris, F, Abad, C, Adams, B, Andrews, P, Baltay, C, Bongiovanni, A, Briceno, C, Bruzual, G, Coppi, P, F Della Prugna, Dubuc, A, Emmet, W, Ferrin, I, Fuenmayor, F, Gebhard, M, Herrera, D, Honeycutt, K, Magris, G, Mateu, J, Muffson, S, Musser, J, Naranjo, O, Oemler, A, Pacheco, R, Paredes, G, Rengel, M, Romero, L, Rosenzweig, P, C Sabbey et al
• Format: Article
• Language: English
• Subjects: Doppler effect; Electrons; Galaxies; Gamma ray astronomy; Interstellar; Photometry; Red shift; Schmidt telescopes; Telescopes
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.9907235

The optical transient of the faint Gamma Ray Burst 990308 was detected by the QUEST camera on the Venezuelan 1-m Schmidt telescope starting 3.28 hours after the burst. Our photometry gives \(V = 18.32 \pm 0.07\), \(R = 18.14 \pm 0.06\), \(B = 18.65 \pm 0.23\), and \(R = 18.22 \pm 0.05\) for times ranging from 3.28 to 3.47 hours after the burst. The colors correspond to a spectral slope of close to \(f_{\nu} \propto \nu^{1/3}\). Within the standard synchrotron fireball model, this requires that the external medium be less dense than \(10^{4} cm^{-3}\), the electrons contain \(> 20%\) of the shock energy, and the magnetic field energy must be less than 24% of the energy in the electrons for normal interstellar or circumstellar densities. We also report upper limits of \(V > 12.0\) at 132 s (with LOTIS), \(V > 13.4\) from 132-1029s (with LOTIS), \(V > 15.3\) at 28.2 min (with Super-LOTIS), and a 8.5 GHz flux of \(< 114 \mu Jy\) at 110 days (with the Very Large Array). WIYN 3.5-m and Keck 10-m telescopes reveal this location to be empty of any host galaxy to \(R > 25.7\) and \(K > 23.3\). The lack of a host galaxy likely implies that it is either substantially subluminous or more distant than a red shift of \(\sim 1.2\).