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Table 3

Overview of different BPS models.

Model Description Reference

Star formation history BP Star formation rate and space density depends on time and location 1
in the Galaxy. SFR peaks at early times, declines afterwards
cSFR Constant space density and SFR for 10 Gyr

Initial period distribution Abt Log-uniform 2
Lognormal Lognormal distribution with a mean of 5.03 d 3

Common-envelope phase γα γ = 1.75, αλ = 2; Preferred for unresolved DWDs 4, 5, 6
αα αλ = 2 4, 6
αα2 αλ = 0.25; Preferred for unresolved WDMS 7, 8, 9

Notes. There are two models for the SFH, two for the period distribution, and three for the CE-phase, giving 12 models in total. 1Boissier & Prantzos (1999); 2Abt (1983); 3Raghavan et al. (2010); 4Nelemans et al. (2000); 5Nelemans et al. (2001b); 6Toonen et al. (2012); 7Zorotovic et al. (2010); 8Toonen & Nelemans (2013); 9Camacho et al. (2014).

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