8th HEAD Meeting, 8-11 September, 2004
Session 18 Gamma-ray Bursts
Poster, Thursday, September 9, 2004, 9:00am-10:00pm

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[18.10] The Interplanetary Network Supplement to the BATSE Catalogs of Untriggered Cosmic Gamma-Ray Bursts

K. Hurley (UC Berkeley Space Sciences Laboratory), B. Stern (Institute for Nuclear Research, Moscow, Russia), J. Kommers (MIT Lincoln Laboratory, Lexington, MA), T. Cline, E Mazets (NASA Goddard Space Flight Center), S. Golenetskii, J. Trombka (Ioffe Physico-Technical Institute, St. Petersburg, Russia), T. McClanahan (NASA Goddard Space Flight Center), R. Starr (Catholic University of America, Washington DC), J. Goldsten (The Johns Hopkins University, Applied Physics Laboratory, Laurel, MD), M Feroci (IAS, Rome, Italy), F Frontera (University of Ferrara, Ferrara, and IASFC, Bologna, Italy), C Guidorzi (ARI, Liverpool, UK, and IASFC, Bologna, Italy), E. Montanari (University of Ferrara, Ferrara, Italy), W. Lewin, C. Kouveliotou, C. Meegan (MIT Center for Space Research, Cambridge, MA), G. Fishman (NASA Marshall Space Flight Center, Huntsville, AL)

We present Interplanetary Network (IPN) detection and localization information for 211 gamma-ray bursts (GRBs) observed as untriggered events by the Burst and Transient Source Experiment (BATSE), and published in catalogs by Kommers et al. (2001) and Stern et al. (2001). IPN confirmations have been obtained by analyzing the data from 11 experiments. For any given burst observed by BATSE and one other distant spacecraft, arrival time analysis (or ``triangulation'') results in an annulus of possible arrival directions whose half-width varies between 14 arcseconds and 5.6 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. This annulus generally intersects the BATSE error circle, resulting in a reduction of the area of up to a factor of ~ 650. When three widely separated spacecraft observed a burst, the result is an error box whose area is as much as 30000 times smaller than that of the BATSE error circle.

Because the IPN instruments are considerably less sensitive than BATSE, they generally did not detect the weakest untriggered bursts, but did detect the more intense ones which failed to trigger BATSE when the trigger was disabled. In some cases, we have been able to identify the probable origin of bursts as soft gamma repeaters. The vast majority of the IPN-detected events, however, are GRBs, and the confirmation of them validates many of the procedures utilized to detect BATSE untriggered bursts.

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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.