A1 Refereed original research article in a scientific journal
SNe 2013K and 2013am: observed and physical properties of two slow, normal Type IIP events
Authors: Tomasella L, Cappellaro E, Pumo ML, Jerkstrand A, Benetti S, Elias-Rosa N, Fraser M, Inserra C, Pastorello A, Turatto M, Anderson JP, Galbany L, Gutierrez CP, Kankare E, Pignata G, Terreran G, Valenti S, Barbarino C, Bauer FE, Botticella MT, Chen TW, Gal-Yam A, Harutyunyan A, Howell DA, Maguire K, Garoffolo AM, Ochner P, Smartt SJ, Schulze S, Young DR, Zampieri L, Zampieri L
Publisher: OXFORD UNIV PRESS
Publication year: 2018
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Journal acronym: MON NOT R ASTRON SOC
Volume: 475
Issue: 2
First page : 1937
Last page: 1959
Number of pages: 23
ISSN: 0035-8711
DOI: https://doi.org/10.1093/mnras/stx3220
We present 1 yr of optical and near-infrared photometry and spectroscopy of the Type IIP SNe 2013K and 2013am. Both objects are affected by significant extinction, due to their location in dusty regions of their respective host galaxies, ESO 009-10 and NGC 3623 (M65). From the photospheric to nebular phases, these objects display spectra congruent with those of underluminous Type IIP SNe (i.e. the archetypal SNe 1997D or 2005cs), showing low photospheric velocities (similar to 2 x 10(3) km s(-1) at 50 d) together with features arising from Ba II that are particularly prominent in faint SNe IIP. The peak V-band magnitudes of SN 2013K (-15.6mag) and SN 2013am (-16.2mag) are fainter than standard-luminosity Type IIP SNe. The ejected nickel masses are 0.012 +/- 0.010 and 0.015 +/- 0.006 M-circle dot for SN 2013K and SN 2013am, respectively. The physical properties of the progenitors at the time of explosion are derived through hydrodynamical modelling. Fitting the bolometric curves, the expansion velocity and the temperature evolution, we infer total ejected masses of 12 and 11.5 M-circle dot, preSN radii of similar to 460 and similar to 360 R-circle dot, and explosion energies of 0.34 foe and 0.40 foe for SN 2013K and SN 2013am. Late time spectra are used to estimate the progenitormasses from the strength of nebular emission lines, which turn out to be consistent with red supergiant progenitors of similar to 15 M-circle dot. For both SNe, a low-energy explosion of a moderate-mass red supergiant star is therefore the favoured scenario.
