OISTER optical and near-infrared observations of the super-Chandrasekhar supernova candidate SN 2012dn: Dust emission from the circumstellar shell

Masayuki Yamanaka, Keiichi Maeda, Masaomi Tanaka, Nozomu Tominaga, Koji S. Kawabata, Katsutoshi Takaki, Miho Kawabata, Tatsuya Nakaoka, Issei Ueno, Hiroshi Akitaya, Takahiro Nagayama, Jun Takahashi, Satoshi Honda, Toshihiro Omodaka, Ryo Miyanoshita, Takashi Nagao, Makoto Watanabe, Mizuki Isogai, Akira Arai, Ryosuke ItohTakahiro Ui, Makoto Uemura, Michitoshi Yoshida, Hidekazu Hanayama, Daisuke Kuroda, Nobuharu Ukita, Kenshi Yanagisawa, Hideyuki Izumiura, Yoshihiko Saito, Kazunari Masumoto, Rikako Ono, Ryo Noguchi, Katsura Matsumoto, Daisaku Nogami, Tomoki Morokuma, Yumiko Oasa, Kazuhiro Sekiguchi

Research output: Contribution to journalArticle

12 Citations (Scopus)

Abstract

We present extensively dense observations of the super-Chandrasekhar supernova (SC SN) candidate SN 2012dn from -11 to +140 d after the date of its B-band maximum in the optical and near-infrared (NIR) wavelengths conducted through the OISTER ToO (Optical and Infrared Synergetic Telescopes for Education and Research Target of Opportunity) program. The NIR light curves and color evolutions up to 35 days after the B-band maximum provided an excellent match with those of another SC SN 2009dc, providing further support to the nature of SN 2012dn as an SC SN. We found that SN 2012dn exhibited strong excesses in the NIR wavelengths from 30 d after the B-band maximum. The H- and Ks-band light curves exhibited much later maximum dates at 40 and 70 d after the B-band maximum, respectively, compared with those of normal SNe Ia. The H- and Ks-band light curves subtracted by those of SN 2009dc displayed plateaued evolutions, indicating an NIR echo from the surrounding dust. The distance to the inner boundary of the dust shell is limited to 4.8-6.4 × 10-2 pc. No emission lines were found in its early phase spectra, suggesting that the ejecta-circumstellar material interaction could not occur. On the other hand, we found no signature that strongly supports the scenario of dust formation. The mass-loss rate of the pre-explosion system is estimated to be 10-6-10-5 M yr-1, assuming that the wind velocity of the system is 10-100 km s-1, which suggests that the progenitor of SN 2012dn could be a recurrent nova system. We conclude that the progenitor of this SC SN could be explained by the single-degenerate scenario.

Original languageEnglish
Article number68
JournalPublications of the Astronomical Society of Japan
Volume68
Issue number5
DOIs
Publication statusPublished - 2016 Oct 1
Externally publishedYes

Keywords

  • supernovae: general
  • supernovae: individual (SN 2012dn, SN 2009dc)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Yamanaka, M., Maeda, K., Tanaka, M., Tominaga, N., Kawabata, K. S., Takaki, K., Kawabata, M., Nakaoka, T., Ueno, I., Akitaya, H., Nagayama, T., Takahashi, J., Honda, S., Omodaka, T., Miyanoshita, R., Nagao, T., Watanabe, M., Isogai, M., Arai, A., ... Sekiguchi, K. (2016). OISTER optical and near-infrared observations of the super-Chandrasekhar supernova candidate SN 2012dn: Dust emission from the circumstellar shell. Publications of the Astronomical Society of Japan, 68(5), [68]. https://doi.org/10.1093/pasj/psw047