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Astron. Astrophys. Suppl. Ser. 138, 463-464

BeppoSAX detection and follow-up of GRB 980425

E. Pian1 - L. Amati1 - L.A. Antonelli2 - R.C. Butler3 - E. Costa4 - G. Cusumano5 - J. Danziger6 - M. Feroci4 - F. Fiore7 - F. Frontera1,8 - P. Giommi7 - N. Masetti1 - J.M. Muller7 - T. Oosterbroek9 - A. Owens9 - E. Palazzi1 - L. Piro4 - A. Castro-Tirado10 - A. Coletta7 - D. Dal Fiume1 - S. Del Sordo5 - J. Heise11 - L. Nicastro5 - M. Orlandini1 - A. Parmar9 - P. Soffitta4 - V. Torroni7 - J.J.M. in 't Zand11

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1 - Istituto Te.S.R.E., CNR, via Gobetti 101, I-40129 Bologna, Italy
2 - Osservatorio Astronomico di Roma, sede di Monteporzio Catone, Via Frascati 33, 00040 Monteporzio Catone, Italy
3 - Agenzia Spaziale Italiana, Viale Regina Margherita 120, Roma, Italy
4 - I.A.S., C.N.R., Via Fosso del Cavaliere, Area della Ricerca di Tor Vergata, I-00131 Rome, Italy
5 - I.F.C.A.I., CNR, via Ugo La Malfa 153, I-90146 Palermo, Italy
6 - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34131 Trieste, Italy
7 - BeppoSAX Scientific Data Center, Via Corcolle 19, I-00131 Rome, Italy
8 - Dip. di Fisica, Univ. di Ferrara, Via Paradiso 11, I-44100 Ferrara, Italy
9 - Astrophysics Division, SSD of ESA, ESTEC, P.O. Box 299, 2200 AG Noordwijk, The Netherlands
10 - IAA-CSIC, Granada, Spain and LAEFF-INTA, Madrid, Spain
11 - Space Research Organization Netherlands, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands

Received March 16; accepted July 5, 1999


We present BeppoSAX GRBM and WFC light curves of GRB 980425 and NFI follow-up data taken in 1998 April, May, and November. The first NFI observation has detected within the $8^{\prime}$ radius error box of the GRB an X-ray source positionally consistent with the supernova SN 1998bw, exploded within a day of GRB 980425, and a fainter X-ray source, not consistent with the position of the supernova. The former source is detected in the following NFI pointings and exhibits a decline of a factor of two in six months. If it is associated with SN 1998bw, this is the first detection of hard X-ray emission from a Type I supernova. The latter source exhibits only marginally significant variability. Based on these data, it is not possible to select either source as a firm candidate for the GRB counterpart.

Key words: gamma-rays: bursts

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