Sn 2017fgc: A fast-expanding type ia supernova exploded in massive shell galaxy ngc 474

Xiangyun Zeng, Xiaofeng Wang, Ali Esamdin, Craig Pellegrino, Jamison Burke, Benjamin E. Stahl, Wei Kang Zheng, Alexei V. Filippenko, D. Andrew Howell, D. J. Sand, Stefano Valenti, Jun Mo, Gaobo Xi, Jialian Liu, Jujia Zhang, Wenxiong Li, Abdusamatjan Iskandar, Mengfan Zhang, Han Lin, Hanna SaiDanfeng Xiang, Peng Wei, Tianmeng Zhang, D. E. Reichart, Thomas G. Brink, Curtis McCully, Daichi Hiramatsu, Griffin Hosseinzadeh, Benjamin T. Jeffers, Timothy W. Ross, Samantha Stegman, Lifan Wang, Jicheng Zhang, Shuo Ma

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11 Scopus citations


We present extensive optical photometric and spectroscopic observations of the high-velocity (HV) Type Ia supernova (SN Ia) 2017fgc, covering the phase from ~12 days before to ~389 days after maximum brightness. SN 2017fgc is similar to normal SNe Ia, with an absolute peak magnitude of MB max -19.32 ± 0.13 mag and a postpeak decline of ?m15(B) = 1.05 ± 0.07 mag. Its peak bolometric luminosity is derived as (1.32 ± 0.13) × 1043 erg s-1, corresponding to a 56Ni mass of 0.51 ± 0.03Me. The light curves of SN 2017fgc are found to exhibit excess emission in the UBV bands in the early nebular phase and pronounced secondary shoulder/maximum features in the RrIi bands. Its spectral evolution is similar to that of HV SNe Ia, with a maximum-light Si II velocity of 15,000 ± 150 km s-1 and a post-peak velocity gradient of ~120 ± 10 km s-1 day-1. The Fe II and Mg II lines blended near 4300 Å and the Fe II, Si II, and Fe III lines blended near 4800 Å are obviously stronger than those of normal SNe Ia. Inspecting a large sample reveals that the strength of the two blends in the spectra, and the secondary peak in the i/r-band light curves, are found to be positively correlated with the maximum-light Si II velocity. Such correlations indicate that HV SNe Ia may experience more complete burning in the ejecta and/or that their progenitors have higher metallicity. Examining the birthplace environment of SN 2017fgc suggests that it likely arose from a stellar environment with young and high-metallicity populations.

Original languageEnglish (US)
Article number49
JournalAstrophysical Journal
Issue number1
StatePublished - Sep 20 2021

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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  • SNIa SN2017fgc follow-up phot. & spectra

    Zeng, X. (Creator), Wang, X. (Creator), Esamdin, A. (Creator), Pellegrino, C. (Creator), Burke, J. (Creator), Stahl, B. E. (Creator), Zheng, W. (Creator), Filippenko, A. V. (Creator), Andrew, H. D. (Contributor), Sand, D. J. (Creator), Valenti, S. (Creator), Mo, J. (Creator), Xi, G. (Creator), Liu, J. (Creator), Zhang, J. (Creator), Li, W. (Creator), Iskandar, A. (Creator), Zhang, M. (Creator), Lin, H. (Creator), Sai, H. (Creator), Xiang, D. (Creator), Wei, P. (Creator), Zhang, T. (Creator), Reichart, D. E. (Creator), Brink, T. G. (Creator), McCully, C. (Creator), Hiramatsu, D. (Creator), Hosseinzadeh, G. (Creator), Jeffers, B. T. (Creator), Ross, T. W. (Creator), Stegman, S. (Creator), Wang, L. (Creator), Zhang, J. (Creator) & Ma, S. (Creator), Centre de Donnees Strasbourg (CDS), 2023


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