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SN2002es-like Supernovae from Different Viewing Angles

Cao, Yi and Kulkarni, S. R. and Gal-Yam, Avishay and Papadogiannakis, S. and Nugent, P. E. and Masci, Frank J. and Bue, Brian D. (2016) SN2002es-like Supernovae from Different Viewing Angles. Astrophysical Journal, 832 (1). Art. No. 86. ISSN 0004-637X.

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In this article, we compare optical light curves of two SN2002es-like Type Ia supernovae (SNe), iPTF14atg and iPTF14dpk, from the intermediate Palomar Transient Factory. Although the two light curves resemble each other around and after maximum, they show distinct early-phase rise behavior in the r-band. On the one hand, iPTF14atg revealed a slow and steady rise that lasted for 22 days with a mean rise rate of 0.2–0.3 mag day^(-1), before it reached the R-band peak (−18.05 mag). On the other hand, iPTF14dpk rose rapidly to −17 mag within a day of discovery with a rise rate > 1.8 mag day^(-1) , and then rose slowly to its peak (−18.19 mag) with a rise rate similar to iPTF14atg. The apparent total rise time of iPTF14dpk is therefore only 16 days. We show that emission from iPTF14atg before −17 days with respect to its maximum can be entirely attributed to radiation produced by collision between the SN and its companion star. Such emission is absent from iPTF14dpk probably because of an unfavored viewing angle, provided that SN2002es-like events arise from the same progenitor channel. We further show that an SN2002es-like SN may experience a dark phase after the explosion but before its radioactively powered light curve becomes visible. This dark phase may be lit by radiation from supernova–companion interaction.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Cao, Yi0000-0002-8036-8491
Kulkarni, S. R.0000-0001-5390-8563
Gal-Yam, Avishay0000-0002-3653-5598
Papadogiannakis, S.0000-0003-0783-3323
Nugent, P. E.0000-0002-3389-0586
Masci, Frank J.0000-0002-8532-9395
Bue, Brian D.0000-0002-7856-3570
Additional Information:© 2016 The American Astronomical Society. Received 2016 June 17; revised 2016 September 11; accepted 2016 September 12; published 2016 November 18. Y.C. and P.E.N. acknowledge support from the DOE under grant DE-AC02-05CH11231, Analytical Modeling for Extreme-Scale Computing Environments. Y.C. also acknowledges support by the GROWTH project funded by the National Science Foundation under Grant No 1545949. A.G.-Y. is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I-Core programme by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK "making connections" programme; and by Kimmel and ARCHES awards. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC), Palomar Transient Factory
Funding AgencyGrant Number
Department of Energy (DOE)DE-AC02-05CH11231
European Research Council (ERC)307260
Israeli Committee for Planning and BudgetingUNSPECIFIED
Israel Science FoundationUNSPECIFIED
Weizmann-UK ProgramUNSPECIFIED
Subject Keywords:supernovae: general – supernovae: individual (SN2002es, iPTF14atg, iPTF14dpk)
Issue or Number:1
Record Number:CaltechAUTHORS:20161121-100334709
Persistent URL:
Official Citation:Yi Cao et al 2016 ApJ 832 86
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72193
Deposited By: Tony Diaz
Deposited On:21 Nov 2016 19:13
Last Modified:21 Nov 2019 23:24

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