LOTIS Upper Limits and the Prompt OT from GRB 990123.pdf

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LOTIS Upper Limits and the Prompt OT from GRB 990123.pdf

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LOTIS Upper Limits and the Prompt OT from GRB 990123

a r X i v : a s t r o - p h / 9 9 1 2 4 0 2 v 1 1 8 D e c 1 9 9 9 LOTIS Upper Limits and the Prompt OT from GRB 990123 G. G. Williams?, D. H. Hartmann?, H. S. Park?, R. A. Porrata?, E. Ables?, R. Bionta?, D. L. Band?, S. D. Barthelmy§, T. Cline§, N. Gehrels§, D. H. Ferguson?, G. Fishman?, R. M. Kippen?, C. Kouveliotou?, K. Hurley?, R. Nemiroff?, and T. Sasseen|| ?Dept. of Physics and Astronomy, Clemson University, Clemson, SC 29634 ?Lawrence Livermore National Laboratory, Livermore, CA 94550 ?Los Alamos National Laboratory, Los Alamos, NM 87545 §NASA Goddard Space Flight Center, Greenbelt, MD 20771 ?Dept. of Physics, California State University, Hayward, CA 94542 ?NASA Marshall Space Flight Center, Huntsville, AL 35812 ?Space Sciences Laboratory, University of California, Berkeley, CA 94720 ?Dept. of Physics, Michigan Technological University, Houghton, MI 49931 ||Dept. of Physics, University of California, Santa Barbara, CA 93106 Abstract. GRB 990123 established the existence of prompt optical emission from gamma-ray bursts (GRBs). The Livermore Optical Transient Imaging System (LOTIS) has been conducting a fully automated search for this kind of simultaneous low energy emission from GRBs since October 1996. Although LOTIS has obtained simultaneous, or near simultaneous, coverage of the error boxes obtained with BATSE, IPN, XTE, and BeppoSAX for several GRBs, image analysis resulted in only upper limits. The unique gamma-ray properties of GRB 990123, such as very large fluence (top 0.4%) and hard spectrum, complicate comparisons with more typical bursts. We scale and compare gamma-ray properties, and in some cases afterglow properties, from the best LOTIS events to those of GRB 990123 in an attempt to determine whether the prompt optical emission of this event is representative of all GRBs. Furthermore, using LOTIS upper limits in conjunction with the relativistic blast wave model, we weakly constrain the GRB and afterglow parameters such as density of the cir