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ON THE PROGENITOR AND SUPERNOVA OF THE SN 2002cx-LIKE SUPERNOVA 2008ge
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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2010 (English)In: Astronomical Journal, ISSN 0004-6256, E-ISSN 1538-3881, Vol. 140, no 5, 1321-1328 p.Article in journal (Refereed) Published
Abstract [en]

We present observations of supernova (SN) 2008ge, which is spectroscopically similar to the peculiar SN 2002cx, and its pre-explosion site indicating that its progenitor was probably a white dwarf. NGC 1527, the host galaxy of SN 2008ge, is an S0 galaxy with no evidence of star formation or massive stars. Astrometrically matching late-time imaging of SN 2008ge to pre-explosion Hubble Space Telescope imaging, we constrain the luminosity of the progenitor star. Since SN 2008ge has no indication of hydrogen or helium in its spectrum, its progenitor must have lost its outer layers before exploding, meaning that it is a white dwarf, a Wolf-Rayet star, or a lower-mass star in a binary system. Observations of the host galaxy show no signs of individual massive stars, star clusters, or H (II) regions at the SN position or anywhere else, making a Wolf-Rayet progenitor unlikely. Late-time spectroscopy of SN 2008ge shows strong [Fe (II)] lines with large velocity widths compared to other members of this class at similar epochs. These previously unseen features indicate that a significant amount of the SN ejecta is Fe (presumably the result of the radioactive decay of Ni-56 generated in the SN), further supporting a thermonuclear explosion. Placing the observations of SN 2008ge in the context of observations of other objects in the same class of SNe, we suggest that the progenitor was most likely a white dwarf.

Place, publisher, year, edition, pages
2010. Vol. 140, no 5, 1321-1328 p.
Keyword [en]
astrometry, stars: evolution, supernovae: general, supernovae: individual (SN 2008ge)
National Category
Natural Sciences
Identifiers
URN: urn:nbn:se:su:diva-51685DOI: 10.1088/0004-6256/140/5/1321ISI: 000283055400016OAI: oai:DiVA.org:su-51685DiVA: diva2:385760
Note
authorCount :9Available from: 2011-01-12 Created: 2011-01-12 Last updated: 2017-12-11Bibliographically approved

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