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|Title:||The nature of supernovae 2010O and 2010P in Arp 299 - I. Near-infrared and optical evolution||Authors:||Kankare, E.
ELIAS DE LA ROSA, NANCY DEL CARMEN
Hentunen, V. -P.
Pérez-Torres, M. -A.
|Issue Date:||2014||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||440||Issue:||2||First Page:||1052||Abstract:||We present near-infrared and optical photometry, plus optical spectroscopy of two stripped-envelope supernovae (SNe) 2010O and 2010P that exploded in two different components of an interacting luminous infrared galaxy Arp 299 within only a few days of one another. SN 2010O is found to be photometrically and spectroscopically similar to many normal Type Ib SNe and our multiwavelength observations of SN 2010P suggest it to be a Type IIb SN. No signs of clear hydrogen features or interaction with the circumstellar medium are evident in the optical spectrum of SN 2010P. We derive estimates for the host galaxy line-of-sight extinctions for both SNe, based on both light curve and spectroscopic comparison finding consistent results. These methods are also found to provide much more robust estimates of the SN host galaxy reddening than the commonly used empirical relations between extinction and equivalent width of Na I D absorption features. The SN observations also suggest that different extinction laws are present in different components of Arp 299. For completeness, we study high-resolution pre-explosion images of Arp 299 and find both SNe to be close to, but not coincident with, extended sources that are likely massive clusters. A very simple model applied to the bolometric light curve of SN 2010O implies a rough estimate for the explosion parameters of E<SUB>k</SUB> ≈ 3 × 10<SUP>51</SUP> erg, M<SUB>ej</SUB> ≈ 2.9 M<SUB>☉</SUB> and M<SUB>Ni</SUB> ≈ 0.16 M<SUB>☉</SUB>.||Description:||We thank the anonymous referee for very useful comments. We thank Mattias Ergon for providing the spectrum of SN 2011dh for our comparison. EK acknowledges financial support from the Jenny and Antti Wihuri Foundation. SM and CR-C acknowledge support from the Academy of Finland (Project 8120503). AP is partially supported by the PRIN-INAF 2011 with the project ‘Transient Universe: From ESO Large to PESSTO’. NE-R acknowledges financial support by the MICINN grant AYA2011-24704/ESP, by the ESF EUROCORES Program EuroGENESIS (MINECO grants EUI2009-04170) and by the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no 267251. CR-C acknowledges financial support from the ALMA-CONICYT FUND Project 31100004. AA, RH-I and M-AP-T acknowledge support from the Spanish MINECO Projects AYA2009-13036-CO2-01 and AYA2012-38491-C02-02, cofunded with FEDER funds. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper is based on observations made with 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 Liverpool Telescope is 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. This paper makes use of data obtained from the Isaac Newton Group Archive which is maintained as part of the CASU Astronomical Data Centre at the Institute of Astronomy, Cambridge. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We have made use of the Weizmann interactive supernova data repository (www.weizmann.ac.il/astrophysics/wiserep).||URI:||http://hdl.handle.net/20.500.12386/12144||ISSN:||0035-8711||DOI:||10.1093/mnras/stt2289||Bibcode ADS:||2014MNRAS.440.1052K|
|Appears in Collections:||1.01 Articoli in rivista|
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