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Pastorello, A; Wang, X.-F; Ciabattari, F; Bersier, D; Mazzali, P. A; Gao, X; Xu, Z; Zhang, J.-J; Tokuoka, S; Benetti, S; Cappellaro, E; Elias-Rosa, N; Harutyunyan, A; Huang, F; Miluzio, M; Mo, J; Ochner, P; Tartaglia, L; Terreran, G; Tomasella, L; Turatto, M
Monthly Notices of the Royal Astronomical Society, 02/2016, Volume: 456, Issue: 1Journal Article
We present spectroscopic and photometric data of the Type Ibn supernova (SN) 2014av, discovered by the Xingming Observatory Sky Survey. Stringent pre-discovery detection limits indicate that the object was detected for the first time about 4 d after the explosion. A prompt follow-up campaign arranged by amateur astronomers allowed us to monitor the rising phase (lasting 10.6 d) and to accurately estimate the epoch of the maximum light, on 2014 April 23 (JD = 245 6771.1 ± 1.2). The absolute magnitude of the SN at the maximum light is M R = −19.76 ± 0.16. The post-peak light curve shows an initial fast decline lasting about three weeks, and is followed by a slower decline in all bands until the end of the monitoring campaign. The spectra are initially characterized by a hot continuum. Later on, the temperature declines and a number of lines become prominent mostly in emission. In particular, later spectra are dominated by strong and narrow emission features of He i typical of Type Ibn supernovae (SNe), although there is a clear signature of lines from heavier elements (in particular O i, Mg ii and Ca ii). A forest of relatively narrow Fe ii lines is also detected showing P-Cygni profiles, with the absorption component blueshifted by about 1200 km s−1. Another spectral feature often observed in interacting SNe, a strong blue pseudo-continuum, is seen in our latest spectra of SN 2014av. We discuss in this paper the physical parameters of SN 2014av in the context of the Type Ibn SN variety.
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