The broad-lined type Ic supernova 2003jd

Creators: Valenti, S.; Benetti, S.; Cappellaro, E.; Patat, F.; Mazzali, P.; Turatto, M.; Hurley, K.; Maeda, K.; Gal-Yam, A.; Foley, R. J.; Filippenko, A. V.; Pastorello, A.; Challis, P.; Frontera, F.; Harutyunyan, A.; Iye, M.; Kawabata, K.; Kirshner, R. P.; Li, W.; Lipkin, Y. M.; Matheson, T.; Nomoto, K.; Ofek, E. O.; Ohyama, Y.; Pian, E.; Poznanski, D.; Salvo, M.; Sauer, D. N.; Schmidt, B. P.; Soderberg, A.; Zampieri, L.

Abstract

The results of a worldwide coordinated observational campaign on the broad-lined Type Ic supernova (SN Ic) 2003jd are presented. In total, 74 photometric data points and 26 spectra were collected using 11 different telescopes. SN 2003jd is one of the most luminous SN Ic ever observed. A comparison with other Type Ic supernovae (SNe Ic) confirms that SN 2003jd represents an intermediate case between broad-line events (2002ap, 2006aj) and highly energetic SNe (1997ef, 1998bw, 2003dh, 2003lw), with an ejected mass of M_ej= 3.0 ± 1 M⊙ and a kinetic energy of E_k(tot) = 7^+3_−2 × 10^51 erg. SN 2003jd is similar to SN 1998bw in terms of overall luminosity, but it is closer to SNe 2006aj and 2002ap in terms of light-curve shape and spectral evolution. The comparison with other SNe Ic suggests that the V-band light curves of SNe Ic can be partially homogenized by introducing a time-stretch factor. Finally, because of the similarity of SN 2003jd to the SN 2006aj/XRF 060218 event, we discuss the possible connection of SN 2003jd with a gamma-ray burst (GRB).

Additional Information

© 2008 The Authors. Journal compilation © 2008 RAS. Accepted 2007 October 26. Received 2007 October 26; in original form 2007 September 26. We thank D. Branch to have refereed the paper, S. Taubenberger, F. Saitta and G. Bono for helpful suggestions. We are grateful to V. Pal'shin, E. Mazets, S. Golenetskii, I. Mitrofanov, A. Sanin, W. Boynton, A. von Kienlin, G. Lichti, A. Rau, G. Ricker, D. Lamb and J.-L. Atteia for contributing Konus, Mars Odyssey, INTEGRAL and HETE data to the IPN to search for an accompanying GRB. AVF thanks the Lorentz Centre in Leiden for its hospitality during the workshop 'From Massive Stars to Supernova Remnants', when this paper was finalized. This work was supported by grant no. 2006022731 of the PRIN of Italian Ministry of University and Sci. Research. AG-Y acknowledges partial support by NASA through Hubble Fellowship grant HST-HF-01158.01-A awarded by STScI, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. AVF's group at the University of California, Berkeley, is supported by National Science Foundation (NSF) grant AST-0607485 and by the TABASGO Foundation. KAIT was made possible by generous donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California and the Sylvia & Jim Katzman Foundation.KH is grateful for IPN support under the following grants and contracts: JPL 958056 (Ulysses), MIT SC-A-293291 (HETE), NAG5-13080 (RHESSI), NAG5-12614 (INTEGRAL) and NAG5-11451 (HETE and Mars Odyssey). This paper is based on observations made with the following facilities: the European Southern Observatory telescopes (Chile) obtained from the ESO/ST-ECF Science Archive Facility (Prog ID. 074.D-0161A), the 10-m Keck I Telescope at the W. M. Keck Observatory (Hawaii), the robotic 1.5-m telescope at Palomar Observatory (California), the Italian National Telescope Galileo (La Palma), the 1.82-m Copernico Telescope of the Asiago Observatory (Italy), the 2.3-m Advanced Technology Telescope at the Siding Spring Observatory (Australia), the 1-m telescope at the Wise Observatory (Israel), the Subaru 8.2-m telescope of the National Astronomic Observatory of Japan (Hawaii), KAIT and the Shane 3-m telescope at Lick Observatory (California) and the 1.5-m telescope at the Fred Lawrence Whipple Observatory (Arizona). We are grateful to the staffs at all of the telescopes for their assistance. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

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