\begin{table}%t1
\par
  \caption{\label{tab:results}Constraints on PBHs of mass  $M_{\star}$ for different dark matter distributions$^{{a}}$.}
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 %\centerline
 { \begin{tabular}{llcc}
\hline\hline
% after \\ : \hline or \cline{col1-col2} \cline{col3-col4} ...
DM distribution   & $f(M_{\star})$  & $\Omega_{\rm PBH}(M_{\star})$ & $\beta(M_\star)$  \\
\hline
Moore        & $ 6.04 \pm 0.05\times 10^{-9}$ & $1.38\times 10^{-9}$ & $0.98\times 10^{-27}$  \\
Moore$_{\rm c}$      & $ 1.07 \pm 0.07\times 10^{-9}$  & $0.24\times 10^{-9}$ & $0.17\times 10^{-27}$  \\
NFW           & $ 6.70 \pm 0.05\times 10^{-9}$  & $1.53\times 10^{-9}$ & $1.08\times 10^{-27}$  \\
NFW$_{\rm c}$         & $ 1.93 \pm 0.08\times 10^{-9}$  & $0.44\times 10^{-9}$ & $0.31~10^{-27}$ \\
isothermal & $11.62 \pm 0.04\times 10^{-9}$ & $2.65\times 10^{-9}$ & $1.87\times 10^{-27}$  \\
\hline
  \end{tabular}}
\par
\smallskip
$^{a}$ $f$ is the maximum fraction of dark matter in the form of PBHs, $\Omega_{\rm PBH}(M_{\star})$ is the corresponding cosmological density, and~$\beta$ is the fraction of regions undergoing collapse when the mass enclosed within the cosmological horizon was $M_{\star}$.
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\end{table}