XRF 100316D/SN 2010bh AND THE NATURE OF GAMMA-RAY BURST SUPERNOVAE

Journal Article · Mon Oct 10 00:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/740/1/41; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21587403

Cano, Z; Bersier, D; Guidorzi, C; Kobayashi, S; Melandri, A; Mundell, C G ^[1]; Levan, A J ^[2]; Tanvir, N R; Wiersema, K ^[3]; D'Avanzo, P; Margutti, R ^[4]; Fruchter, A S ^[5]; Garnavich, P ^[6]; Gomboc, A; Kopac, D ^[7]; Gorosabel, J ^[8]; Kasen, D ^[9]; Mazzali, P A ^[10]; Nugent, P E ^[11]; Pian, E ^[12]

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1. Astrophysics Research Institute, Liverpool John Moores University, Liverpool (United Kingdom)
2. Department of Physics, University of Warwick, Coventry (United Kingdom)
3. Department of Physics and Astronomy, University of Leicester, Leicester (United Kingdom)
4. INAF-Osservatorio Astronomico di Brera, 23807 Merate, LC (Italy)
5. Space Telescope Science Institute, Baltimore, MD (United States)
6. Physics Department, University of Notre Dame, Notre Dame, IN (United States)
7. Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana (Slovenia)
8. Instituto de Astrofisica de Andalucia (IAA-CSIC), Granada (Spain)
9. Department of Astronomy and Astrophysics, UC Berkeley, Berkeley CA (United States)
10. Max-Planck-Institut fuer Astrophysik, Garching (Germany)
11. Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA (United States)
12. INAF Oss. Astron. Padova, Padova (Italy)

We present ground-based and Hubble Space Telescope optical and infrared observations of Swift XRF 100316D/SN 2010bh. It is seen that the optical light curves of SN 2010bh evolve at a faster rate than the archetype gamma-ray burst supernova (GRB-SN) 1998bw, but at a similar rate to SN 2006aj, an SN that was spectroscopically linked with XRF 060218, and at a similar rate to the 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{sub V} = -18.62 {+-} 0.08, which is the faintest peak V-band magnitude observed to date for spectroscopically confirmed GRB-SNe. When we investigate the origin of the flux at t - t{sub 0} = 0.598 days, it is shown that the light is not synchrotron in origin, but is likely coming from the SN shock breakout. 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{sub Ni} {approx} 0.1 M{sub sun}, ejected M{sub ej} {approx} 2.2 M{sub sun}, and has an explosion energy of E{sub k} {approx} 1.4 x 10{sup 52} erg. Thus, while SN 2010bh is an energetic explosion, the amount of nickel created during the explosion is much less than that of SN 1998bw and only marginally more than SN 1994I. Finally, for a sample of 22 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.

• OSTI ID: 21587403
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 740; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BINARY STARS
COSMIC GAMMA BURSTS
COSMIC RADIATION
ELEMENTS
ERUPTIVE VARIABLE STARS
EXPLOSIONS
IONIZING RADIATIONS
METALS
NICKEL
PRIMARY COSMIC RADIATION
RADIATIONS
SIMULATION
STARS
SUPERNOVAE
TRANSITION ELEMENTS
VARIABLE STARS