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| 多个超新星/伽马暴的光学光变 |
文章信息:
- · arXiv e-print (arXiv:1104.5141)
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| Title: |
| XRF 100316D / SN 2010bh and the Nature of Gamma Ray Burst Supernovae |
| Authors: |
| Cano, Z.; Bersier, D.; Guidorzi, C.; Kobayashi, S.; Levan, A. J.; Tanvir, N. R.; Wiersema, K.; D'Avanzo, P.; Fruchter, A. S.; Garnavich, P.; Gomboc, A.; Gorosabel, J.; Kasen, D.; Kopac, D.; Margutti, R.; Mazzali, P. A.; Melandri, A.; Mundell, C. G.; Nugent, P. E.; Pian, E.; Smith, R. J.; Steele, I.; Wijers, R. A. M. J.; Woosley, S. E. |
| Publication: |
| eprint arXiv:1104.5141 |
| Publication Date: |
| 04/2011 |
| Origin: |
| ARXIV |
| Keywords: |
| Astrophysics - Solar and Stellar Astrophysics |
| Comment: |
| Sumitted to ApJ (27-April-2011). 17 pages, 11 figures and 8 tables |
| Bibliographic Code: |
| 2011arXiv1104.5141C |
Abstract
We present ground-based and HST optical and infrared observations of XRF 100316D / SN 2010bh. It is seen that the optical light curves of SN 2010bh evolve at a faster rate than the archetype GRB-SN 1998bw, but at a similar rate to SN 2006aj, a supernova that was spectroscopically linked with XRF 060218, and at a similar rate to non-GRB associated type Ic SN 1994I. We estimate the rest-frame extinction of this event from our optical data to be E(B-V)=0.18 +/- 0.08 mag. We find the V-band absolute magnitude of SN 2010bh to be M_{V}=-18.62 +/- 0.08, which is the faintest peak V-band magnitude observed to-date for a spectroscopically-confirmed GRB-SNe. When we investigate the origin of the flux at t-t_{o}=0.598 days, it is shown that the light is not synchrotron in origin, but is likely coming from the supernova shock break-out. We then use our optical and infrared data to create a quasi-bolometric light curve of SN 2010bh which we model with a simple analytical formula. The results of our modeling imply that SN 2010bh synthesized a nickel mass of M_{Ni}=0.10 +/- 0.01 M_{\odot}, ejected M_{ej}=2.24 +/- 0.08 M_{\odot} and has an explosion energy of E_{k}=1.39 +/- 0.06 x 10^{52} erg (where the quoted errors are statistical only; we discuss the potential sources of the systematic errors in the text). Finally, for a sample 20 GRB-SNe we check for a correlation between the stretch factors and luminosity factors in the R band and conclude that no statistically-significant correlation exists.
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