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  5. SNe 2013K and 2013am: observed and physical properties of two slow, normal Type IIP events
 

SNe 2013K and 2013am: observed and physical properties of two slow, normal Type IIP events

Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY  
Date Issued
2018
Author(s)
TOMASELLA, Lina  
•
CAPPELLARO, Enrico  
•
Pumo, M. L.
•
Jerkstrand, A.
•
BENETTI, Stefano  
•
ELIAS DE LA ROSA, NANCY DEL CARMEN  
•
Fraser, M.
•
Inserra, C.
•
PASTORELLO, Andrea  
•
TURATTO, Massimo  
•
Anderson, J. P.
•
Galbany, L.
•
Gutiérrez, C. P.
•
Kankare, E.
•
Pignata, G.
•
Terreran, G.
•
Valenti, S.
•
Barbarino, C.
•
Bauer, F. E.
•
BOTTICELLA, MARIA TERESA  
•
Chen, T. -W.
•
Gal-Yam, A.
•
Harutyunyan, A.
•
Howell, D. A.
•
Maguire, K.
•
Morales Garoffolo, A.
•
Ochner, P.
•
Smartt, S. J.
•
Schulze, S.
•
Young, D. R.
•
ZAMPIERI, Luca  
DOI
10.1093/mnras/stx3220
Abstract
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 (∼2 × 103 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 (-15.6 mag) and SN 2013am (-16.2 mag) are fainter than standard-luminosity Type IIP SNe. The ejected nickel masses are 0.012 ± 0.010 and 0.015 ± 0.006 M☉ 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☉, pre-SN radii of ∼460 and ∼360 R☉, 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 progenitor masses from the strength of nebular emission lines, which turn out to be consistent with red supergiant progenitors of ∼15 M☉. For both SNe, a low-energy explosion of a moderate-mass red supergiant star is therefore the favoured scenario.
Volume
475
Issue
2
Start page
1937
Uri
http://hdl.handle.net/20.500.12386/27847
Url
https://academic.oup.com/mnras/article/475/2/1937/4739357
Issn Identifier
0035-8711
Ads BibCode
2018MNRAS.475.1937T
Rights
open.access
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