Populations of evolved massive binary stars in the Small Magellanic Cloud - II. Predictions from rapid binary evolution

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Table 1.

SN properties for the fiducial scenario.

SN type	distribution	char. velocity
ECSN	flat	w ∈ [0, 50] km/s

CCSN H-rich	Maxwellian	$w_{rms} = \sqrt{3} \cdot 265 km / s$ $w_{\mathrm{rms}} = \sqrt{3} \cdot 265\,\mathrm{km/s}$
CCSN HeS*	Maxwellian	$w_{rms} = \sqrt{3} \cdot 120 km / s$ $w_{\mathrm{rms}} = \sqrt{3} \cdot 120\,\mathrm{km/s}$
CCSN BB/BC*	Maxwellian	$w_{rms} = \sqrt{3} \cdot 60 km / s$ $w_{\mathrm{rms}} = \sqrt{3} \cdot 60\,\mathrm{km/s}$

BH formation	flat	w = 0

Notes. For CCSNe we distinguish between hydrogen-rich models, HeS, and models exploding at the end of Case BB/BC mass transfer. *Stripped models have a 20% probability of receiving a higher kick ( $w_{rms} = \sqrt{3} \cdot 200 km / s$ $w_{\mathrm{rms}} = \sqrt{3} \cdot 200\,\mathrm{km/s}$ ).

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