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|Title:||On the triple peaks of SNHunt248 in NGC 5806||Authors:||Kankare, E.
Smartt, S. J.
Chambers, K. C.
ELIAS DE LA ROSA, NANCY DEL CARMEN
Smith, K. W.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||581||First Page:||L4||Abstract:||We present our findings on a supernova (SN) impostor, SNHunt248, based on optical and near-IR data spanning ~15 yr before discovery, to ~1 yr post-discovery. The light curve displays three distinct peaks, the brightest of which is at M<SUB>R</SUB> ~ -15.0 mag. The post-discovery evolution is consistent with the ejecta from the outburst interacting with two distinct regions of circumstellar material. The 0.5-2.2 μm spectral energy distribution at -740 d is well-matched by a single 6700 K blackbody with log (L/L<SUB>☉</SUB>) ~ 6.1. This temperature and luminosity support previous suggestions of a yellow hypergiant progenitor; however, we find it to be brighter than the brightest and most massive Galactic late-F to early-G spectral type hypergiants. Overall the historical light curve displays variability of up to ~ ± 1 mag. At current epochs (~1 yr post-outburst), the absolute magnitude (M<SUB>R</SUB> ~ - 9 mag) is just below the faintest observed historical absolute magnitude ~10 yr before discovery. Tables 1-4 are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201526631/olm">http://www.aanda.org</A>||Acknowledgments:||We thank the anonymous referee for useful comments and Justyn Maund for helpful discussions. We are grateful to Kathleen Eckert and co-authors for providing early access to DECam data for NGC 5806 (NOAO 2014A-0256). We thank Stefano Benetti and Leonardo Tartaglia for their help with some of the observations. R.K. and S.J.S. acknowledge support from STFC (ST/L000709/1). S.J.S. acknowledges funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. (291222). This work was partly supported by the European Union FP7 programme through ERC grant number 320360. A.P. and L.T. are partially supported by the PRIN-INAF 2012 with the project “Transient Universe: from ESO Large to PESSTO”. N.E.R. acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 “Astronomy Fellowships in Italy” (AstroFIt). Support for H.K. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, M.A.S. H.K. acknowledges support by CONICYT through FONDECYT grant 3140563. This work is based on observations made at the following facilities: CFHT, CRTS, CTIO, ESO (programme IDs 091.D-0516, 093.D-0798, 095.D-0793, 177.A-3016, and 184.D-1151), FTN, Gemini, GTC, INAF, ING, KPNO, LT, NOT, PS1, SDSS, and TNG. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). Operation of the Pan-STARRS1 telescope is supported by the National Aeronautics and Space Administration under Grant No. NNX12AR65G and Grant No. NNX14AM74G issued through the NEO Observation Program.||URI:||http://hdl.handle.net/20.500.12386/24153||URL:||https://www.aanda.org/articles/aa/abs/2015/09/aa26631-15/aa26631-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201526631||Bibcode ADS:||2015A&A...581L...4K||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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