Stritzinger, Maximilian and Mazzali, P. and Phillips, Mark M. and Immler, Stefan and Soderberg, Alicia and Sollerman, Jesper and Boldt, Luis and Braithwaite, Jonathan and Brown, Peter and Burns, Christopher R. and Contreras, Carlos and Covarrubias, Ricardo and Folatelli, Gastón and Freedman, Wendy L. and González, Sergio and Hamuy, Mario and Krzeminski, Wojtek and Madore, Barry F. and Milne, Peter and Morrell, Nidia and Persson, S. E. and Roth, Miguel and Smith, Mathew and Suntzeff, Nicholas B. (2009) The He-rich core-collapse supernova 2007Y: observations from x-ray to radio wavelengths. Astrophysical Journal, 696 (1). pp. 713-728. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20090918-110314549
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A detailed study spanning approximately a year has been conducted on the Type Ib supernova (SN) 2007Y. Imaging was obtained from X-ray to radio wavelengths, and a comprehensive set of multi-band (w2m2w1u'g'r'i'UBVYJHK_s ) light curves and optical spectroscopy is presented. A virtually complete bolometric light curve is derived, from which we infer a ^(56)Ni mass of 0.06 M_☉sun. The early spectrum strongly resembles SN 2005bf and exhibits high-velocity features of Ca II and Hα; during late epochs the spectrum shows evidence of an ejecta-wind interaction. Nebular emission lines have similar widths and exhibit profiles that indicate a lack of major asymmetry in the ejecta. Late phase spectra are modeled with a non-LTE code, from which we find ^(56)Ni, O, and total-ejecta masses (excluding He) to be 0.06, 0.2, and 0.42 M_☉ sun, respectively, below 4500 km s^–1. The ^(56)Ni mass confirms results obtained from the bolometric light curve. The oxygen abundance suggests that the progenitor was most likely a ≈3.3 M_☉ sun He core star that evolved from a zero-age-main-sequence mass of 10-13 M_☉ sun. The explosion energy is determined to be ≈1050 erg, and the mass-loss rate of the progenitor is constrained from X-ray and radio observations to be less than or similar to 10–6 M_☉ sun yr^–1. SN 2007Y is among the least energetic normal Type Ib SNe ever studied.
|Additional Information:||© 2009 The American Astronomical Society (AAS) Received 2009 January 18, accepted for publication 2009 February 12. This material is based upon work supported by the National Science Foundation (NSF) under grant AST–0306969. The Dark Cosmology Centre is funded by the Danish NSF. M.S. acknowledges support from the MPA’s visitor programme. J.S. is a Royal Swedish Academy of Sciences Research Fellow supported by a grant from the Knut and Alice Wallenberg Foundation. M.H. ackowledges support from Iniciativa Cientifica Milenio through grant P06-045-F and CONICYT through Centro de Astrofisica FONDAP (grant 15010003), Programa Financiamiento Basal (grant PFB 06), and Fondecyt (grant 1060808). We have 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. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.|
|Subject Keywords:||galaxies: individual: NGC 1187; supernovae: general; supernovae: individual; SN 2007Y|
|Official Citation:||The He-Rich Core-Collapse Supernova 2007Y: Observations from X-Ray to Radio Wavelengths Maximilian Stritzinger, Paolo Mazzali, Mark M. Phillips, Stefan Immler, Alicia Soderberg, Jesper Sollerman, Luis Boldt, Jonathan Braithwaite, Peter Brown, Christopher R. Burns, Carlos Contreras, Ricardo Covarrubias, Gastón Folatelli, Wendy L. Freedman, Sergio González, Mario Hamuy, Wojtek Krzeminski, Barry F. Madore, Peter Milne, Nidia Morrell, S. E. Persson, Miguel Roth, Mathew Smith, and Nicholas B. Suntzeff 2009 ApJ 696 713-728 doi: 10.1088/0004-637X/696/1/713|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Joy Painter|
|Deposited On:||21 Sep 2009 22:10|
|Last Modified:||26 Dec 2012 11:24|
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