SN 2009N: linking normal and subluminous Type II-P SNe

Creators: Takáts, K.; Van Dyk, S. D.

Abstract

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 These signs are also present in the previously unpublished near-infrared spectra of SN 2008in.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 × 10^(51) erg, the ejected mass as ∼11.5 M_⊙, and the initial radius as ∼287 R_⊙.

Additional Information

© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 November 11. Received 2013 November 8; in original form 2013 October 23. First published online: December 13, 2013. KT acknowledges support by the Gemini-Conicyt project 32110024. KT, GP, JA, FB, RC, MH and FF acknowledge support from Millennium Center for Supernova Science (P10-064-F), with input from Fondo de Innovaciόn para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile. This project has been supported by the Hungarian OTKA grant NN 107637 and by the European Union together with the European Social Fund through the TÁMOP 4.2.2/B-10/1-2010-0012 grant. We acknowledge the TriGrid VL project and the INAF-Astronomical Observatory of Padua for the use of computer facilities. MLP, AP and SB acknowledge support from the PRIN-INAF 2011 Transient Universe: from ESO Large to PESSTO (P.I. S. Benetti). NER acknowledges financial support by the MICINN grant AYA2011-24704/ESP, by the ESF EUROCORES Program EuroGENESIS (MINESCO grant EUI2009-04170), and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n. 267251. FB, JA and FF acknowledge support from CONICYT through FONDECYT grants 3120227, 3110142 and 3110042, respectively. FF acknowledges partial support from Comite Mixto ESO-GOBIERNO DE CHILE. RC acknowledges support by CONICYT through Programa Nacional de Becas de Postgrado grant D-2108082, and by the Yale-Chile fellowship in astrophysics. GL is supported by the Swedish Research Council through grant No. 623-2011-7117. MS gratefully acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. This work is partially based on observations made with ESO Telescopes at the La Silla and Paranal Observatories under programme IDs 084.D-0261 and 082.A-0526, and on observations of the European supernova collaboration involved in the ESO-NTT large programme 184.D-1140 led by Stefano Benetti. This research is based in part on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council; the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; the SMARTS Consortium 1.3 m telescope and the Prompt Telescopes located at Cerro Tololo Inter-American Observatory (CTIO), Chile; the 1.5 m telescope located at Palomar Observatory, USA; the 2.2 m telescope of the Calar Alto Observatory (Sierra de Los Filabres, Spain); the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU); the 2.5 m du Pont Telescope and the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. We are grateful to the staffs at these observatories for their excellent assistance with the observations. This research has made use of the NASA/IPAC Extragalactic Database, the HyperLeda data base, NASA's Astrophysics Data System. The availability of these services is gratefully acknowledged. We thank Rupak Roy for sending us the optical spectra of SN 2008in and Morgan Fraser for the NIR spectra of SN 2009md. We also thank the referee, V. P. Utrobin, for the thorough review of the paper.

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Submitted - 1311.2525v1.pdf

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