SN 2013ej: A type IIL supernova with weak signs of interaction
- Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263002 (India)
- Indian Institute of Astrophysics, Block-II, Koramangala, Bangalore 560034 (India)
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A and M University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843 (United States)
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States)
- Department of Astronomy and Astrophysics and The Enrico Fermi Institute, University of Chicago, Chicago, IL 60637 (United States)
- Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
- Centre of Advance Study, Department of Physics, Kumaun University, Nainital 263001 (India)
- Carthage College, 2001 Alford Park Dr., Kenosha, WI 53140 (United States)
- Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005 (India)
We present optical photometric and spectroscopic observations of SN 2013ej. It is one of the brightest Type II supernovae (SNe II) exploded in a nearby (∼10 Mpc) galaxy, NGC 628. The light-curve characteristics are similar to SNe II, but with a relatively shorter (∼85 days) and steeper (∼1.7 mag (100 days){sup −1} in V) plateau phase. The SN shows a large drop of 2.4 mag in V-band brightness during the plateau-to-nebular transition. The absolute ultraviolet (UV) light curves are identical to SN 2012aw, showing a similar UV-plateau trend extending up to 85 days. The radioactive {sup 56}Ni mass estimated from the tail luminosity is 0.02 M{sub ⊙}, which is significantly lower than typical SNe IIP. The characteristics of spectral features and evolution of line velocities indicate that SN 2013ej is a Type II event. However, light-curve characteristics and some spectroscopic features provide strong support in classifying it as a Type IIL event. A detailed synow modeling of spectra indicates the presence of some high-velocity components in Hα and Hβ profiles, implying a possible ejecta–circumstellar medium interaction. The nebular phase spectrum shows an unusual notch in the Hα emission, which may indicate bipolar distribution of {sup 56}Ni. Modeling of the bolometric light curve yields a progenitor mass of ∼14 M{sub ⊙} and a radius of ∼450 R{sub ⊙}, with a total explosion energy of ∼2.3×10{sup 51} erg.
- OSTI ID:
- 22883042
- Journal Information:
- Astrophysical Journal, Vol. 806, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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