Sn 2017fgc: A fast-expanding type ia supernova exploded in massive shell galaxy ngc 474
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Author
Zeng, X.Wang, X.
Esamdin, A.
Pellegrino, C.
Burke, J.
Stahl, B.E.
Zheng, W.
Filippenko, A.V.
Andrew Howell, D.
Sand, D.J.
Valenti, S.
Mo, J.
Xi, G.
Liu, J.
Zhang, J.
Li, W.
Iskandar, A.
Zhang, M.
Lin, H.
Sai, H.
Xiang, D.
Wei, P.
Zhang, T.
Reichart, D.E.
Brink, T.G.
McCully, C.
Hiramatsu, D.
Hosseinzadeh, G.
Jeffers, B.T.
Ross, T.W.
Stegman, S.
Wang, L.
Zhang, J.
Ma, S.
Affiliation
Steward Observatory, University of ArizonaIssue Date
2021
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IOP Publishing LtdCitation
Zeng, X., Wang, X., Esamdin, A., Pellegrino, C., Burke, J., Stahl, B. E., Zheng, W., Filippenko, A. V., Andrew Howell, D., Sand, D. J., Valenti, S., Mo, J., Xi, G., Liu, J., Zhang, J., Li, W., Iskandar, A., Zhang, M., Lin, H., … Ma, S. (2021). Sn 2017fgc: A fast-expanding type ia supernova exploded in massive shell galaxy ngc 474. Astrophysical Journal.Journal
Astrophysical JournalRights
Copyright © 2021. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
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. © 2021 Institute of Physics Publishing. All rights reserved.Note
Immediate accessISSN
0004-637XVersion
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/ac0e9c