Table 2: TDGs progenitors.
Run Location T a $M_{\rm tot}$ b $M_{\rm *}^{\rm old}$ c $M_{\rm *}^{\rm young}$ d
    (Myr) ($M_{\odot}$) (%) (%)
A x>0 60 $2.9 ~\mbox{$\times$ }~ 10^9$ 5% 19%
  x<0   $2.3 ~\mbox{$\times$ }~ 10^9$ 12% 13%
  x>0 430 $2.2 ~\mbox{$\times$ }~ 10^9$ 5% 44%
  x<0   $1.8 ~\mbox{$\times$ }~ 10^9$ 14% 31%
B x<0 100 $2.3 ~\mbox{$\times$ }~ 10^9$ 7% 19%
C x>0 90 $2.5 ~\mbox{$\times$ }~ 10^{9}$ e 11% 16%
  x<0   $1.8 ~\mbox{$\times$ }~ 10^9$ 11% 16%
D y>0 55 $1.1 ~\mbox{$\times$ }~ 10^9$ 3% 14%
  y<0   $2.4 ~\mbox{$\times$ }~ 10^9$ 8% 19%
a Time after the periapse.
b Total mass.
c Mass of the old stellar population from the parent's disk.
d Mass of the young stellar population born in situ. Note that this value is approximate as the measurement of the SFR is affected by the limited numerical resolution.
e In two fragments.

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