\begin{table}%t1
\caption{\label{HeMass}For all our models, various quantities are given here (see text for details).}
%\centerline
 {\begin{tabular}{ c c c c c c c c | c c c c c c c c}
\hline\hline
$M_{\rm ini} $ & $M_{\rm end~He} $ & $M_{\rm He} $ & $M_{\rm CO} $ & $M_{\rm rem} $ & Prog. & SN & Rem. & $M_{\rm ini}$ & $M_{\rm end~He}$ & $M_{\rm He}$ & $M_{\rm CO}$ & $M_{\rm rem}$ & Prog. & SN & Rem.\\
\hline
\multicolumn{8}{c |}{\vec{Z} {\bf = 0.004}} & \multicolumn{8}{c}{\vec{Z} {\bf = 0.020}}\\
$12$ & $11.8$ & $3.74$ & $1.78$ & $1.4$ & SG & II & NS & $12$ & $10.5$ & $3.81$ & $1.94$ & $1.4$ & SG & II & NS\\
$15$ & $14.1$ & $5.01$ & $2.84$ & $1.7$ & SG & II & NS & $15$ & $10.2$ & $5.97$ & $3.61$ & $1.7$ & SG & II & NS\\
$20$ & $18.0$ & $7.45$ & $4.79$ & $2.0$ & SG & II & NS & $20$ & $11.8$ & $9.01$ & $6.62$ & $2.0$ & SG & II & NS\\
$25$ & $20.0$ & $9.95$ & $7.06$ & $2.5$ & SG & II & NS & $25$ & $11.3$ & $11.33$ & $8.98$ & $2.5$ & WNL & II & NS\\
$30$ & $18.9$ & $14.16$ & $11.14$ & $2.9$ & SG & II & BH & $40$ & $12.7$ & $12.70$ & $11.75$ & $3.0$ &  WC & Ic & BH\\
$40$ & $22.3$ & $21.59$ & $17.16$ & $3.5$ & WNL & II & BH & $60$ & $14.6$ & $14.60$ & $13.67$ & $3.6$ & WC & Ic & BH\\
$60$ & $28.5$ & $28.50$ & $28.46$ & $4.4$ & WO & Ic & BH & $85$ & $12.3$ & $12.30$ & $11.22$ & $3.0$ & WC & Ic & BH\\
$120$ & $17.2$ & $17.20$ & $17.18$ & $3.4$ & WC & Ic & BH & $120$ & $11.3$ & $11.30$ & $10.40$ & $2.8$ & WC & Ic  & BH\\
\hline
\multicolumn{8}{c |}{\vec{Z} {\bf = 0.008}} & \multicolumn{8}{c}{\vec{Z} {\bf = 0.040}}\\
$20^1$ & $15.5$ & $-$ & $4.85$ & $2.1$ & SG & II & NS & $20$ & $9.2$ & $9.05$ & $6.84$ & $1.4$ & SG & II & NS\\
$25^1$ & $14.0$ & $-$ & $6.92$ & $2.7$ & SG & II & NS & $25$ & $9.6$ & $9.60$ & $8.19$ & $1.7$ & WC & Ib & NS\\
$30$ & $12.1$ & $12.10$ & $11.10$ & $2.9$ & WC & Ic & BH & $40$ & $11.4$ & $11.40$ & $10.48$ & $2.8$ & WC & Ic & BH\\
$40$ & $17.4$ & $17.40$ & $17.23$ & $3.5$ & WC & Ic & BH & $85$ & $7.2$ & $7.20$ & $6.07$ & $2.2$ & WC & Ic & NS\\
$60$ & $16.4$ & $16.40$ & $16.44$ & $3.3$ & WO & Ic & BH & $120$ & $7.1$ & $7.10$ & $6.10$ & $2.2$ & WC & Ic & NS\\
$120$ & $13.4$ & $13.40$ & $13.24$ & $3.0$ & WC & Ic & BH & & & & & & &\\
\hline
\multicolumn{8}{c |}{\textbf{Homogenous model at} \vec{Z} {\bf = 0.002}} & & & & & & & &\\
$60^2$ & $27.8$ & $-$ & $-$ & $4.0$ & WC & Ib &BH & & & & & & &\\
\hline
\end{tabular}}
\par
\smallskip
\par
  (1) Non-rotating models from \citet{Meynet1994a} used to estimate the minimum initial mass of stars ending their lifetime  
  in the WNL phase at that metallicity. These models were computed with artificially enhanced mass loss rates, which  
  somewhat compensates for the neglect of the effects of rotation. 
  (2) Model computed up to the end of silicon burning.   
\par
Note: All masses are given in $[{M}_\odot]$. The SN type is given for $m^{\rm min}_{\rm H}=0$, $m^{\rm min}_{\rm He}=0.6$ and supposing that a SN occurs even when a BH is formed (see text). The remnant masses used are those given by \citet{Hirschi2005a}, except for the homogenous models (see text).
\end{table}