\begin{table}%t3
\caption{\label{hMLall}Maximum likelihood fits of an exponential surface density profile to the
radial distribution of CCSNe.}
%\centerline
 {
\par
\hskip-1mm\begin{tabular}{lrcccc} \hline
    \hline\\[-3.2mm]
\multicolumn{1}{c}{Sample}&$N_{\rm SN}$&$\tilde{h}_{\rm SN}$&$\hat{h}_{\rm SN}$&$\tilde{P}_{\rm KS}$&$\hat{P}_{\rm KS}$\\
\multicolumn{1}{c}{(1)}&(2)&(3)&(4)&(5)&(6)\\
\hline
    Full sample&224&$0.29\pm0.01$&$1.25\pm0.06$&0.194&0.646\\
\hline
    Sa-Sbc&127&$0.31\pm0.02$&$1.35\pm0.09$&0.235&0.412\\
    Sc-Sd&97&$0.28\pm0.02$&$1.13\pm0.07$&0.890&0.872\\
    Sa-Sbc (SNe~Ib/c)&25&$0.23\pm0.04$&$0.93\pm0.19$&0.098&0.213\\
    Sc-Sd ~\ (SNe~Ib/c)&30&$0.24\pm0.03$&$1.03\pm0.13$&1.000&0.986\\
    Sa-Sbc (SNe~II)&102&$0.32\pm0.02$&$1.46\pm0.10$&0.441&0.965\\
    Sc-Sd ~\ (SNe~II)&67&$0.29\pm0.02$&$1.17\pm0.09$&0.783&0.793\\
    Sa-Sd ~\ (without bars)&133&$0.29\pm0.02$&$1.18\pm0.08$&0.273&0.707\\
    Sa-Sd ~\ (with bars)&91&$0.30\pm0.02$&$1.37\pm0.10$&0.453&0.931\\
    Sa-Sbc (without bars)&58&$0.32\pm0.03$&$1.26\pm0.14$&\textbf{0.043}&0.523\\
    Sa-Sbc (with bars)&69&$0.29\pm0.02$&$1.43\pm0.13$&0.899&0.973\\
    Sc-Sd ~\ (without bars)&75&$0.26\pm0.02$&$1.11\pm0.09$&0.977&0.997\\
    Sc-Sd ~\ (with bars)&22&$0.32\pm0.04$&$1.19\pm0.14$&0.884&0.829\\
    $-23 < M_{\rm disk} \leq -20.5$&123&$0.27\pm0.02$&$1.06\pm0.07$&0.586&0.933\\
    $-20.5 < M_{\rm disk} < -18$&101&$0.32\pm0.02$&$1.49\pm0.10$&0.308&0.603\\
    $19.65 < \mu_0^{\rm disk} \leq 20.60$&102&$0.28\pm0.02$&$1.35\pm0.10$&0.895&0.840\\
    $20.60 < \mu_0^{\rm disk} < 21.85$&122&$0.30\pm0.02$&$1.18\pm0.08$&0.203&0.803\\
    $0^\circ \leq i \leq 30^\circ$&68&$0.26\pm0.02$&$1.11\pm0.10$&0.912&0.453\\
    $30^\circ < i \leq 50^\circ$&156&$0.31\pm0.02$&$1.32\pm0.08$&0.153&0.719\\
\hline
    SNe~Ib&20&$0.23\pm0.03$&$0.90\pm0.11$&0.765&0.993\\
    SNe~Ic&27&$0.22\pm0.03$&$0.97\pm0.18$&0.671&0.644\\
    SNe~Ib/c&55&$0.24\pm0.02$&$0.99\pm0.11$&0.476&0.707\\
    SNe~II&169&$0.31\pm0.02$&$1.34\pm0.07$&0.328&0.746\\
\hline
\multicolumn{2}{l}{stars (in Freeman disk)}&$0.32\pm0.03$&$1.23\pm0.17$&&\\
\multicolumn{2}{l}{stars (in SN host disks)}&$0.26\pm0.02$&\multicolumn{1}{l}{1.00}&&\\
\multicolumn{2}{l}{\ion{H}{ii} regions (Freeman disk)}&$0.26\pm0.13$&$1.00\pm0.50$&&\\
\multicolumn{2}{l}{\ion{H}{ii} regions (SN host disk)}&$0.21\pm0.11$&$0.80\pm0.40$&&\\
    \hline
  \end{tabular}}
\par
\medskip
Notes: Column~1 gives the CCSN sample, Col.~2 number of CCSNe in the sample,
Col.~3 the maximum likelihood value of $\tilde h_{\rm SN} = h_{\rm SN}/R_{25}$,
Col.~4 the maximum likelihood value of $\hat{h}_{\rm SN} = h_{\rm SN}/h$, and
Cols.~5 and~6 give the KS test probabilities that
the surface density distribution of CCSNe is consistent with an exponential
law with the isophotal radius (Col.~5) and scale length (Col.~6)
normalizations.
The four last lines are not for the SNe, but for the stars (first two
of these lines) and \ion{H}{ii} regions (last two lines),
with the
centrally extrapolated surface brightness taken from the Freeman disk  (first and third of these lines)
and the hosts (second and fourth of these lines).
The value of unity in Col.~4 in the second of these lines is a direct consequence of
$h_{\rm SN} = h$ and thus has no uncertainty associated with it.
The values of Col.~4 in the first of these lines is scaled relative to that
of the the second of these lines, according to the mean
value of $\langle h /R_{25} \rangle$ (Sect.~\ref{norm}).
Similarly the last two lines of Col.~4 are scaled to the corresponding values in Col.~3.
The statistically significant deviation from an exponential law is highlighted
in bold.
\end{table}