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Constraining the Properties of SNe Ia Progenitors from Light Curves

Published online by Cambridge University Press:  17 January 2013

B. Sadler ,
Peter Hoeflich ,
E. Baron ,
K. Krisciunas ,
G. Folatelli ,
M. Hamuy ,
M. Khokhlov ,
M. Phillips ,
N. Suntzeff  and
L. Wang
B. Sadler
Affiliation:
Dept. of Physics, Florida State University, USA
Peter Hoeflich
Affiliation:
Dept. of Physics, Florida State University, USA
E. Baron
Affiliation:
Dept. of Physics and Astronomy, University of Oklahoma
K. Krisciunas
Affiliation:
Dept. of Physics, Texas A & M University
G. Folatelli
Affiliation:
Dept. de Astronomia, Universidad de Chile, Santiago, Chile
M. Hamuy
Affiliation:
Dept. de Astronomia, Universidad de Chile, Santiago, Chile
M. Khokhlov
Affiliation:
Dept. Astronomy and Astrophysics, University of Chicago, USA
M. Phillips
Affiliation:
Las Campanas Observatory, La Serena, Chile
N. Suntzeff
Affiliation:
Dept. of Physics, Texas A & M University
L. Wang
Affiliation:
Dept. of Physics, Texas A & M University
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Abstract

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We present an analysis of high precision V light curves (LC) for 18 local Type Ia supernovae (SNe Ia) as obtained with the same telescope and setup at the Las Campanas Observatory (LCO). This homogeneity provides an intrinsic accuracy of a few hundredths of a magnitude with respect to individual LCs and between different objects. Based on the single degenerate (SD) scenario, we identify patterns which have been predicted by model calculations as signatures of the progenitor and accretion rate which change the explosion energy and the amount of electron capture, respectively. Using these templates as principle components and the overdetermined system of SNe pairs, we reconstruct the properties of progenitors and progenitor systems. All LCO SNe Ia follow the brightness decline relation except 2001ay. After subtraction of the two components, the remaining scatter is reduced to ≈0.01m−0.03m. SNe Ia seem to originate from progenitors with main-sequence masses MMS > 3 M⊙ with the exception of two subluminous SNe Ia with MMS < 2 M⊙. The component analysis indicates a wide range of accretion rates in the progenitor systems closing the gap to accretion induced collapses (AIC). SN1991t-like objects show differences in decline rate (dm15) but no tracers of our secondary parameters. This may point to a different origin such as the double degenerate or pulsating delayed detonation scenarios. SN2001ay does not follow the decline relation. It can be understood in the framework of C-rich white dwarfs (WDs), and this group may produce an anti-Phillips relation. We suggest that this may be a result of a common envelope phase and mixing during central He burning as in SN1987A.

Keywords

stars: white dwarfssupernovae — nuclear reactionsnucleosynthesisabundances — methods: data analysis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 309 - 313
Copyright
Copyright © International Astronomical Union 2013

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