SN2002es-like Supernovae from Different Viewing Angles
Abstract
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.
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.Attached Files
Published - Cao_2016_ApJ_832_86.pdf
Submitted - 1606.05655v1.pdf
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Additional details
- Eprint ID
- 72193
- Resolver ID
- CaltechAUTHORS:20161121-100334709
- DE-AC02-05CH11231
- Department of Energy (DOE)
- OISE-1545949
- NSF
- 307260
- European Research Council (ERC)
- Israeli Committee for Planning and Budgeting
- Israel Science Foundation
- Weizmann-UK Program
- Kimmel Award
- ARCHES Award
- NASA/JPL/Caltech
- Created
-
2016-11-21Created from EPrint's datestamp field
- Updated
-
2021-11-11Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC), Palomar Transient Factory, Division of Geological and Planetary Sciences