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Title:
Search for an X-Ray Counterpart to a Gamma-Ray Burst GRB 940217 with ASCA
Authors:
Tokanai, Fuyuki; Yoshida, Atsumasa; Otani, Chiko; Kawai, Nobuyuki; Shibata, Ryo; Murakami, Toshio; Ueda, Yoshihiro; Hurley, Kevin
Affiliation:
AA(The Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-01; (FT):), AB(The Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-01; (FT):), AC(The Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-01; (FT):), AD(The Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-01; (FT):), AE(The Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-01; (FT):), AF(The Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-01; (FT):), AG(The Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229), AH(Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450, U.S.A.)
Publication:
Publ. of the Astronomical Society of Japan, v.49, p.207-212. (PASJ Homepage)
Publication Date:
04/1997
Origin:
PASJ
PASJ Keywords:
GAMMA-RAYS: BURSTS, X-RAYS: COUNTERPARTS, X-RAYS: SOURCES
Bibliographic Code:
1997PASJ...49..207T

Abstract

We report on the result of a search for an X-ray counterpart to the peculiar gamma-ray burst of 1994 February 17 (GRB 940217) detected with the ASCA satellite. This was one of the strongest bursts detected by BATSE onboard CGRO. Furthermore, it had the longest duration (90 min), and the hardest gamma-ray emission ( ~ 18 GeV) of all GRBs observed so far. Three pointed observations with ASCA were performed to cover the error region determined by the EGRET (95% confidence level), COMPTEL (3sigma confidence level), and the Interplanetary Network (IPN) localization. We detected one X-ray source (2--10 keV flux: 3.7 times 10(-13) erg s(-1) cm(-2) ) within the error region. Using the APM system at the Royal Greenwich Observatory, we found two optical sources within 1' of this source. One of the optical sources has a B-R color consistent with an AGN. The implied optical-to-X ray flux ratio is also reasonable for an AGN. If the X-ray source is an AGN with a luminosity of 10(45) erg s(-1) (4.7 Gpc; z=1) and is the source of the burst, a lower limit on the relativistic bulk Lorentz beaming factor, >~ 50, can be derived from the energy spectra and fine-time structure observed by COMPTEL.

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