Theoretical uncertainties of the Type Ia supernova rate

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Table 3

Fraction η of the binary systems with a primary mass between 3 M_⊙ and 8 M_⊙ that result in a SN Ia and the expected SN Ia rate versus the CC SN rate of different models with varying IMFs compared with the observations.

Model	IMF	η (%)	N_SNeIa/N_CCSNe ^a

Standard	Kroupa et al. (1993)	2.4	0.07−0.14
O₁	Scalo (1998)	2.4	0.05−0.09
O₂	Kroupa (2001)	2.3	0.04−0.09
O₃	Chabrier (2003)	2.5	0.05−0.09
O₄	Bell et al. (2003)	2.3	0.04 - 0.09

Observed	−	15 (2−40)^b	0.28 ± 0.07 ^c

Notes.

^(a)

The upper and lower limit are determined by assuming that only the primary or both stars explode as a CC SNe in a binary system with a primary mass between 8 M_⊙ and 25 M_⊙.

^(b)

Maoz (2008).

^(c)

Cappellaro et al. (1999).

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