Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21923910e&link_type=abstract
American Astronomical Society, AAS Meeting #219, #239.10
Astronomy and Astrophysics
Astrophysics
Scientific paper
One of the main problems in astrophysics is the unknown nature of the Type Ia Supernova (SN Ia) progenitor system. Current models of SNe Ia involve the detonation of a Carbon-Oxygen (CO) white dwarf (WD) that has reached the Chandrasekhar Limit (1.4 Msun) via mass transfer from a companion star. Many different types of progenitor systems have been proposed that involve various possible companion stars. These can be divided into the double-degenerate (DD) model, which contains two WDs, and the single-degenerate (SD) model, which contains one CO WD and a main-sequence, sub-giant, or giant companion star. By examining remnants of known SNe Ia, we can search for any ex-companion star and thereby infer the progenitor system for a given SN Ia. It was inferred by Schaefer & Pagnotta (2011) that the progenitor of SNR 0509-67.5 was a DD system since the central region was devoid of any stars to deep limits. Using archival Hubble Space Telescope images we eliminated all but two of the various proposed models for SNR 0519-69.0, which is known to be a SN Ia based on its light-echoes (Rest et al. 2005, Hughes et al. 1995). The geometric central region was determined using both the Hα and the X-ray shell to be RA= 05:19:34.84, DEC= -69.02.06.92 (J2000). We report the stars in the geometric central region to a limiting V magnitude of 26.1. Photometric analysis of these central stars shows that none of them are red giants or subgiants. We know of only two models that are consistent with our observational limits: persistent supersoft X-ray sources and DDs. We will soon use Gemini to obtain spectra of stars in the central region of SNR 0519-69.0, and may be able to report on this at the meeting.
Edwards Zachary
Pagnotta Ashley
Schaefer Bradley E.
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