Panel a) distribution of rotation velocity versus mass of the companion stars at the moment of the explosion as obtained by Han (2008). The number of systems decreases from the inner to outer regions. The blue area contains 50.0% of all stars, blue plus green 68.3%, and so on. Panel b) as panel a), but now the distribution is shown after the impact. The distribution is shifted to lower rotational velocity and slightly lower masses. The unbound mass stripped by the SN impact is calculated by using Eq. (2) of Liu et al. (2012), and the post-impact rotational velocity of the companion star is computed employing the linear relation shown in Fig. 13 (see text). The location of Tycho G according to Kerzendorf et al. (2009, 2012) is shown with the error in black assuming a solar mass star with 5% error (Ruiz-Lapuente et al. 2004) and an inclination angle of i = 60°. The black square gives the location of Tycho G for an assumed inclination angle of i = 30°. The red vertical dashed line corresponds to the lowest rotational velocity covered by our hydrodynamical simulations (i.e., MS_081 model in Table 1).
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