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|Title:||SN 2013ej in M74: A Luminous and Fast-declining Type II-P Supernova||Authors:||Huang, Fang
Brown, Peter J.
PUMO, MARIA LETIZIA
|Issue Date:||2015||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||807||Issue:||1||First Page:||59||Abstract:||We present extensive ultraviolet, optical, and near-infrared observations of the Type IIP supernova (SN IIP) 2013ej in the nearby spiral galaxy M74. The multicolor light curves, spanning from ̃8-185 days after explosion, show that it has a higher peak luminosity (i.e., M<SUB>V</SUB> ̃ -17.83 mag at maximum light), a faster post-peak decline, and a shorter plateau phase (i.e., ̃50 days) compared to the normal Type IIP SN 1999em. The mass of <SUP>56</SUP>Ni is estimated as 0.02 ± 0.01 M<SUB>☉</SUB> from the radioactive tail of the bolometric light curve. The spectral evolution of SN 2013ej is similar to that of SN 2004et and SN 2007od, but shows a larger expansion velocity (i.e., v<SUB>Fe ii</SUB> ̃ 4600 km s<SUP>-1</SUP> at t ̃ 50 days) and broader line profiles. In the nebular phase, the emission of the Hα line displays a double-peak structure, perhaps due to the asymmetric distribution of <SUP>56</SUP>Ni produced in the explosion. With the constraints from the main observables such as bolometric light curve, expansion velocity, and photospheric temperature of SN 2013ej, we performed hydrodynamical simulations of the explosion parameters, yielding the total explosion energy as ̃0.7× 10<SUP>51</SUP> erg, the radius of the progenitor as ̃600 R<SUB>☉</SUB>, and the ejected mass as ̃10.6 M<SUB>☉</SUB>. These results suggest that SN 2013ej likely arose from a red supergiant with a mass of 12-13 M<SUB>☉</SUB> immediately before the explosion.||Acknowledgments:||We thank all of the staff at the Li-Jiang Observatory, Yunnan Astronomical Observatory of China and Xinglong Station, National Astronomical Observatory of China for the observations and technological support. We acknowledge the use of public data from the Swift data archive. This work is also based on observations made with ESO Telescopes at the La Silla Paranal Observatory under program IDs 188.D-2003 and 191.D-0935. The work of X. Wang is supported by the Major State Basic Research Development Program (2013CB834903), the National Natural Science Foundation of China (NSFC grants 11178003 and 11325313), the Foundation of Tsinghua University (2011Z02170), and the Strategic Priority Research Program “The Emergence of Cosmological Structures” of the Chinese Academy of Sciences (grant No. XDB09000000). J.-J. Zhang is supported by the NSFC (grants 11403096), and T.-M. Zhang is supported by the NSFC (grants 11203034).||URI:||http://hdl.handle.net/20.500.12386/24254||URL:||https://ui.adsabs.harvard.edu/abs/2015ApJ...807...59H/abstract
|Appears in Collections:||1.01 Articoli in rivista|
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