TY - JOUR
T1 - Interaction-powered supernovae
T2 - Rise-time versus peak-luminosity correlation and the shock-breakout velocity
AU - Ofek, Eran O.
AU - Arcavi, Iair
AU - Tal, David
AU - Sullivan, Mark
AU - Gal-Yam, Avishay
AU - Kulkarni, Shrinivas R.
AU - Nugent, Peter E.
AU - Ben-Ami, Sagi
AU - Bersier, David
AU - Cao, Yi
AU - Cenko, S. Bradley
AU - De Cia, Cia, Annalisa
AU - Filippenko, Alexei V.
AU - Fransson, Claes
AU - Kasliwal, Mansi M.
AU - Laher, Russ
AU - Surace, Jason
AU - Quimby, Robert
AU - Yaron, Ofer
N1 - Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of Science; I-CORE Program of the Planning and Budgeting Committee; ISF; BSF; GIF; Minerva; EU/FP7 via ERC grant [307260]; Israel Science Foundation; Israel Science Foundation, Minerva, Weizmann-UK; Hubble Fellowship; Carnegie-Princeton Fellowship; Christopher R.Redlich Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-1211916]We thank Dan Perley for obtaining some spectra. E.O.O. thanks Ehud Nakar and Orly Gnat for discussions. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva, Weizmann-UK and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. A. G-Y. acknowledge grants from the ISF, BSF, GIF, Minerva, the EU/FP7 via ERC grant (307260), and the I-CORE program of the Planning and Budgeting Committee and The Israel Science Foundation. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A.V.F
PY - 2014/6/20
Y1 - 2014/6/20
N2 - Interaction of supernova (SN) ejecta with the optically thick circumstellar medium (CSM) of a progenitor star can result in a bright, long-lived shock-breakout event. Candidates for such SNe include Type IIn and superluminous SNe. If some of these SNe are powered by interaction, then there should be a specific relation between their peak luminosity, bolometric light-curve rise time, and shock-breakout velocity. Given that the shock velocity during shock breakout is not measured, we expect a correlation, with a significant spread, between the rise time and the peak luminosity of these SNe. Here, we present a sample of 15 SNe IIn for which we have good constraints on their rise time and peak luminosity from observations obtained using the Palomar Transient Factory. We report on a possible correlation between the R-band rise time and peak luminosity of these SNe, with a false-alarm probability of 3%. Assuming that these SNe are powered by interaction, combining these observables and theory allows us to deduce lower limits on the shock-breakout velocity. The lower limits on the shock velocity we find are consistent with what is expected for SNe (i.e., ∼104 km s-1). This supports the suggestion that the early-time light curves of SNe IIn are caused by shock breakout in a dense CSM. We note that such a correlation can arise from other physical mechanisms. Performing such a test on other classes of SNe (e.g., superluminous SNe) can be used to rule out the interaction model for a class of events.
AB - Interaction of supernova (SN) ejecta with the optically thick circumstellar medium (CSM) of a progenitor star can result in a bright, long-lived shock-breakout event. Candidates for such SNe include Type IIn and superluminous SNe. If some of these SNe are powered by interaction, then there should be a specific relation between their peak luminosity, bolometric light-curve rise time, and shock-breakout velocity. Given that the shock velocity during shock breakout is not measured, we expect a correlation, with a significant spread, between the rise time and the peak luminosity of these SNe. Here, we present a sample of 15 SNe IIn for which we have good constraints on their rise time and peak luminosity from observations obtained using the Palomar Transient Factory. We report on a possible correlation between the R-band rise time and peak luminosity of these SNe, with a false-alarm probability of 3%. Assuming that these SNe are powered by interaction, combining these observables and theory allows us to deduce lower limits on the shock-breakout velocity. The lower limits on the shock velocity we find are consistent with what is expected for SNe (i.e., ∼104 km s-1). This supports the suggestion that the early-time light curves of SNe IIn are caused by shock breakout in a dense CSM. We note that such a correlation can arise from other physical mechanisms. Performing such a test on other classes of SNe (e.g., superluminous SNe) can be used to rule out the interaction model for a class of events.
KW - stars: mass-loss
KW - stars: massive
KW - supernovae: general
UR - https://www.scopus.com/pages/publications/84902204360
U2 - 10.1088/0004-637X/788/2/154
DO - 10.1088/0004-637X/788/2/154
M3 - مقالة
SN - 0004-637X
VL - 788
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 154
ER -