\begin{table}%t4
  \caption{Kolmogorov-Smirnov tests of the consistency of different CCSN distributions
with two exponential disk models.
\label{SNvsdisks}}
%\centerline
 {
  \begin{tabular}{lcccc} \hline
    \hline\\[-3.2mm]
\multicolumn{1}{c}{Sample}&$\tilde{P}_{\rm KS}^{\rm Freeman}$ &$\hat{P}_{\rm KS}^{\rm Freeman}$& $\tilde{P}_{\rm KS}^{\rm hosts}$&$\hat{P}_{\rm KS}^{\rm hosts}$\\
\multicolumn{1}{c}{(1)}&(2)&(3)&(4)&(5)\\
\hline
Full sample&\textbf{0.002}&\textbf{0.010}&0.895&\textbf{0.010}\\
\hline
    Sa-Sbc&\textbf{0.040}&\textbf{0.028}&0.749&\textbf{0.012}\\
    Sc-Sd&\textbf{0.044}&0.602&0.328&0.166\\
    Sa-Sbc (SNe~Ib/c)&\textbf{0.000}&\textbf{0.016}&\textbf{0.003}&0.091\\
    Sc-Sd ~\ (SNe~Ib/c)&0.111&0.944&0.335&0.973\\
    Sa-Sbc (SNe~II)&0.434&\textbf{0.021}&0.229&\textbf{0.001}\\
    Sc-Sd ~\ (SNe~II)&0.219&0.252&0.693&0.106\\
    Sa-Sd ~\ (without bars)&\textbf{0.006}&0.194&0.302&0.208\\
    Sa-Sd ~\ (with bars)&0.157&\textbf{0.036}&0.814&\textbf{0.013}\\
    Sa-Sbc (without bars)&\textbf{0.037}&0.162&0.703&0.387\\
    Sa-Sbc (with bars)&0.298&0.296&0.390&\textbf{0.006}\\
    Sc-Sd ~\ (without bars)&\textbf{0.036}&0.965&0.428&0.566\\
    Sc-Sd ~\ (with bars)&0.873&0.265&0.686&0.259\\
    $-23 < M_{\rm disk} \leq -20.5$&\textbf{0.003}&0.733&\textbf{0.039}&0.947\\
    $-20.5 < M_{\rm disk} < -18$&0.359&\textbf{0.007}&0.055&\textbf{0.000}\\
    $19.65 < \mu_0^{\rm disk} \leq 20.60$&0.064&0.396&0.940&0.055\\
    $20.60 < \mu_0^{\rm disk} < 21.85$&\textbf{0.023}&\textbf{0.049}&0.676&0.125\\
    $0^\circ \leq i \leq 30^\circ$&\textbf{0.032}&0.889&0.059&0.532\\
    $30^\circ < i \leq 50^\circ$&\textbf{0.029}&\textbf{0.005}&0.797&\textbf{0.003}\\
\hline
    SNe~Ib&\textbf{0.019}&0.302&0.160&0.840\\
    SNe~Ic&\textbf{0.002}&0.109&\textbf{0.042}&0.523\\
    SNe~Ib/c&\textbf{0.000}&0.105&\textbf{0.014}&0.621\\
    SNe~II&0.102&\textbf{0.006}&0.496&\textbf{0.001}\\
    \hline
  \end{tabular}}
\par
\medskip
Notes: Column~1: sample;
Col.~2: KS test probabilities that
CCSN subsamples have  isophotal radius -- normalized distributions consistent
with the Freeman disk;
Col.~3: same as Col.~2, but with scale-length normalization;
Col.~4: same as Col.~2, but for the host stellar disk;
Col.~5: same as Col.~4, but with scale-length normalization.
CCSN distributions
inconsistent with these exponential models are highlighted in bold.
\end{table}