Prompt, early, and afterglow optical observations of five gamma-ray bursts (GRBs 100901A, 100902A, 100905A, 100906A, and 101020A)
astro-ph.HE
/ Authors
E. S. Gorbovskoy, G. V. Lipunova, V. M. Lipunov, V. G. Kornilov, A. A. Belinski, N. I. Shatskiy, N. V. Tyurina, D. A. Kuvshinov, P. V. Balanutsa, V. V. Chazov
and 28 more authors
A. Kuznetsov, D. S. Zimnukhov, M. V. Kornilov, A. V. Sankovich, A. Krylov, K. I. Ivanov, O. Chvalaev, V. A. Poleschuk, E. N. Konstantinov, O. A. Gress, S. A. Yazev, N. M. Budnev, V. V. Krushinski, I. S. Zalozhnich, A. A. Popov, A. G. Tlatov, A. V. Parhomenko, D. V. Dormidontov, V. Sennik, V. V. Yurkov, Yu. P. Sergienko, D. Varda, I. P. Kudelina
/ Abstract
We present results of the prompt, early, and afterglow optical observations of five gamma-ray bursts, GRBs 100901A, 100902A, 100905A, 100906A, and 101020A, made with the Mobile Astronomical System of TElescope-Robots in Russia (MASTER-II net), the 1.5-m telescope of Sierra-Nevada Observatory, and the 2.56-m Nordic Optical Telescope. For two sources, GRB 100901A and GRB 100906A, we detected optical counterparts and obtained light curves starting before cessation of gamma-ray emission, at 113 s and 48 s after the trigger, respectively. Observations of GRB 100906A were conducted with two polarizing filters. Observations of the other three bursts gave the upper limits on the optical flux; their properties are briefly discussed. More detailed analysis of GRB 100901A and GRB 100906A supplemented by Swift data provides the following results and indicates different origins of the prompt optical radiation in the two bursts. The light curves patterns and spectral distributions suggest a common production site of the prompt optical and high-energy emission in GRB 100901A. Results of spectral fits for GRB 100901A in the range from the optical to X-rays favor power-law energy distributions with similar values of the optical extinction in the host galaxy. GRB 100906A produced a smoothly peaking optical light curve suggesting that the prompt optical radiation in this GRB originated in a front shock. This is supported by a spectral analysis. We have found that the Amati and Ghirlanda relations are satisfied for GRB 100906A. An upper limit on the value of the optical extinction on the host of GRB 100906A is obtained.