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A Luminous Peculiar Type Ia Supernova SN 2011hr: More Like SN 1991T or SN 2007if?

Journal
Date Issued
2016
Author(s)
Zhang, Ju-Jia
•
Wang, Xiao-Feng
•
Sasdelli, Michele
•
Zhang, Tian-Meng
•
Liu, Zheng-Wei
•
Mazzali, Paolo A.
•
Meng, Xiang-Cun
•
Maeda, Keiichi
•
Chen, Jun-Cheng
•
Huang, Fang
•
Zhao, Xu-Lin
•
Zhang, Kai-Cheng
•
Zhai, Qian
•
•
Wang, Bo
•
Chang, Liang
•
Yi, Wei-Min
•
Wang, Chuan-Jun
•
Wang, Xue-Li
•
Xin, Yu-Xin
•
Wang, Jian-Guo
•
Lun, Bao-Li
•
Zheng, Xiang-Ming
•
Zhang, Xi-Liang
•
Fan, Yu-Feng
•
Bai, Jin-Ming
DOI
Abstract
Photometric and spectroscopic observations of a slowly declining, luminous Type Ia supernova (SN Ia) SN 2011hr in the starburst galaxy NGC 2691 are presented. SN 2011hr is found to peak at {M}B=-19.84+/- 0.40 {mag}, with a postmaximum decline rate ∆m15(B) = 0.92 ± 0.03 mag. From the maximum-light bolometric luminosity, L=(2.30+/- 0.90)× {10}43 {erg} {{{s}}}-1, we estimate the mass of synthesized 56Ni in SN 2011hr to be M{(}56{Ni})=1.11+/- 0.43 {M}☉ . SN 2011hr appears more luminous than SN 1991T at around maximum light, and the absorption features from its intermediate-mass elements (IMEs) are noticeably weaker than those of the latter at similar phases. Spectral modeling suggests that SN 2011hr has IMEs of ∼0.07 {M}☉ in the outer ejecta, which is much lower than the typical value of normal SNe Ia (I.e., 0.3-0.4 {M}☉ ) and is also lower than the value of SN 1991T (I.e., ∼0.18 {M}☉ ). These results indicate that SN 2011hr may arise from a Chandrasekhar-mass white dwarf progenitor that experienced a more efficient burning process in the explosion. Nevertheless, it is still possible that SN 2011hr may serve as a transitional object connecting the SN 1991T-like SNe Ia with a superluminous subclass like SN 2007if given that the latter also shows very weak IMEs at all phases.
Volume
817
Issue
2
Start page
114
Uri
Url
Issn Identifier
0004-637X
Ads BibCode
2016ApJ...817..114Z
Rights
open.access
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