TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1939 SUBJECT: IPN upper limit to a GRB associated with SN2003L DATE: 03/03/19 17:38:38 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley and T. Cline, on behalf of the Ulysses, HETE, Mars Odyssey, and KONUS GRB teams, E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W. Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, A. von Kienlin, G. Lichti, and A. Rau, on behalf of the INTEGRAL SPI-ACS GRB team, I. Mitrofanov, D. Anfimov, A. Kozyrev, M. Litvak and A. Sanin, on behalf of the HEND-Odyssey GRB team, W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on behalf of the GRS-Odyssey GRB team, and G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R. Vanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R. Manchanda, G. Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, T. Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on behalf of the HETE GRB team, report: We have searched the IPN data for a gamma-ray burst that might be associated with SN2003L (Boles, IAUC 8048; Valenti et al., IAUC 8057; Kulkarni et al., IAUC 8061; Kulkarni & Fox, IAUC 8073). It has been suggested by Soderberg et al. (GCN 1834) that SN2003L is actually a hypernova, and might therefore be similar to SN1998bw/GRB980425. We have limited our search to data obtained between November 10 2002 and January 10 2003. The missions and experiments in the IPN were Ulysses, Konus-Wind, RHESSI, Mars Odyssey (HEND and GRS), HETE-2 (FREGATE), and INTEGRAL (SPI-ACS). The data on 41 bursts and candidate (unconfirmed) bursts were examined. During that period, no burst which could be localized by the IPN was found to have a source position in any way consistent with that of the supernova. That is, there was no event observed by two or more spacecraft that produced a source annulus or error box consistent with the supernova. Several events were observed each by single spacecraft in the network during this time. Most of them can be ruled out as counterparts because of the coarse localization capabilities of the experiments involved. However, two such events had positions which were not inconsistent with the position of SN2003L. One occurred on 021213 at 41739 s, and was detected only by HETE-FREGATE. Based on Earth-blocking considerations, the probability of a chance association with SN2003L is ~70%. This burst had a fluence of roughly 10^-6 erg/cm^2. The other occurred on 021228 at 53801 s and was detected only by Konus-Wind. Based on the ecliptic latitude response of the Konus detectors, the probability of a chance association is ~17%. This burst had a fluence of ~2x10^-6 erg/cm^2. Lacking any definite evidence for an association, we can give an upper limit to the fluence of a GRB from SN2003L. This limit depends on the duration, spectrum, and arrival time within the search window, all of which are unknown (see Hurley et al. GCN 1252), but can be roughly taken to be several times 10^-7 erg/cm^2 in the energy range above 25 keV. SN2003L is about 2.6 times more distant than SN1998bw. Neglecting beaming and other event-to-event variations, any associated GRB might be expected to be 7 times less intense, and possibly undetectable by IPN instruments.