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Takáts, K; Pumo, M. L; Elias-Rosa, N; Pastorello, A; Pignata, G; Paillas, E; Zampieri, L; Anderson, J. P; Vinkó, J; Benetti, S; Botticella, M.-T; Bufano, F; Campillay, A; Cartier, R; Ergon, M; Folatelli, G; Foley, R. J; Förster, F; Hamuy, M; Hentunen, V.-P; Kankare, E; Leloudas, G; Morrell, N; Nissinen, M; Phillips, M. M; Smartt, S. J; Stritzinger, M; Taubenberger, S; Valenti, S; Van Dyk, S. D; Haislip, J. B; LaCluyze, A. P; Moore, J. P; Reichart, D
Monthly Notices of the Royal Astronomical Society, 2014, Volume: 438, Issue: 1Journal Article
We present ultraviolet, optical, near-infrared photometry and spectroscopy of SN 2009N in NGC 4487. This object is a Type II-P supernova with spectra resembling those of subluminous II-P supernovae, while its bolometric luminosity is similar to that of the intermediate-luminosity SN 2008in. We created synow models of the plateau phase spectra for line identification and to measure the expansion velocity. In the near-infrared spectra we find signs indicating possible weak interaction between the supernova ejecta and the pre-existing circumstellar material. These signs are also present in the previously unpublished near-infrared spectra of SN 2008in. The distance to SN 2009N is determined via the expanding photosphere method and the standard candle method as D = 21.6 ± 1.1 Mpc. The produced nickel-mass is estimated to be ∼0.020 ± 0.004 M. We infer the physical properties of the progenitor at the explosion through hydrodynamical modelling of the observables. We find the values of the total energy as ∼0.48 × 1051 erg, the ejected mass as ∼11.5 M, and the initial radius as ∼287 R.
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