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Title: SN2002es-like supernovae from different viewing angles

Journal Article · · The Astrophysical Journal (Online)
ORCiD logo [1]; ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]; ORCiD logo [4]; ORCiD logo [5]; ORCiD logo [6]
  1. California Inst. of Technology (CalTech), Pasadena, CA (United States). Astronomy Dept.
  2. Weizmann Inst. of Science, Rehovot (Israel)
  3. Stockholm Univ. (Sweden). Oskar Klein Centre, Dept. of Physics
  4. Univ. of California, Berkeley, CA (United States). Dept. of Astronomy; Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  5. California Inst. of Technology (CalTech), Pasadena, CA (United States). Infrared Processing and Analysis Center
  6. California Inst. of Technology (CalTech), Pasadena, CA (United States). Jet Propulsion Lab.
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In this letter, 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 , 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.

Research Organization:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Organization:
USDOE Office of Science (SC)
Grant/Contract Number:
AC02-05CH11231
OSTI ID:
1398441
Journal Information:
The Astrophysical Journal (Online), Vol. 832, Issue 1; ISSN 1538-4357
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 4 works
Citation information provided by
Web of Science

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Cited By (11)

A hybrid type Ia supernova with an early flash triggered by helium-shell detonation journal October 2017
A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate journal May 2017
R-band light-curve properties of Type Ia supernovae from the (intermediate) Palomar Transient Factory journal December 2018
Color Me Intrigued: The Discovery of iPTF 16fnm, an SN 2002cx–like Object journal October 2017
Type Ia Supernovae in the First Few Days: Signatures of Helium Detonation versus Interaction journal July 2018
Surface Radioactivity or Interactions? Multiple Origins of Early-excess Type Ia Supernovae and Associated Subclasses journal October 2018
Early Blue Excess from the Type Ia Supernova 2017cbv and Implications for Its Progenitor journal August 2017
K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova journal December 2018
A common-envelope wind model for Type Ia supernovae (I): binary evolution and birth rate text January 2017
Early Blue Excess from the Type Ia Supernova 2017cbv and Implications for Its Progenitor text January 2017
Type Ia Supernovae in the First Few Days: Signatures of Helium Detonation versus Interaction text January 2018

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