\begin{table}%t3 \caption{\label{mecanismo}Ionization in the extra-nuclear ionized regions of LIRGs.} \par %%\centering \par { \begin{tabular}{cllp{8.8cm}} \hline \hline \noalign{\smallskip} Galaxy & Mechanism\tablefootmark{a} & $r$\tablefootmark{b} & Comment \\ (IRAS number) & & & \\ \hline \multicolumn{4}{c}{Class 0}\\ F06295$-$1735 & Young stars & 0.22 & \\ F06592$-$6313 & \ldots & 0.42 & No \oi\ nor \sii\ data. $r$ based on \nha.\\ F07027$-$6011~N\tablefootmark{c} & Young stars and shocks (100$-$200~km~s$^{-1}$) & 0.44 & Part of the shocks may be associated to the nucleus according \oha \ map.\\ F07027$-$6011~S & Young stars & 0.21 & $r$ based on \sha. $r$ based on \oha\ not reliable.\\ F07160$-$6215 & Shocks (100$-$300~km~s$^{-1}$) & 0.31 & $r$ based on \sha. No \oi\ data.\\ F10015$-$0614 & Young stars & 0.15 & \\ F10409$-$4556 & \ldots & 0.37 & $r$ based on \nha. No \oi\ nor \sii\ data.\\ F10567$-$4310 & Young stars & 0.23 & $r$ based on \sha. No \oi\ data.\\ F11254$-$4120 & Young stars & 0.71 & $r$ based on \nha. $r$ based on \sha\ not reliable. No \oi\ data. Possible shocks associated to the bar according to the \sha \ map. \\ F11506$-$3851 & Young stars & 0.19 & Some small areas better explained with low velocity shocks.\\ F12115$-$4656 & Young stars & --0.24 & \\ F13229$-$2934\tablefootmark{d} & Shocks (100$-$300~km~s$^{-1}$) & 0.47 & Some areas explained by stars, mostly associated with the arms. Part of the high excitation may be associated to the nucleus according to the \oha \ map. \\ F22132$-$3705 & Young stars & 0.10 & Small areas better explained with low velocity ($<$100~km~s$^{-1}$) shocks.\\ \hline \multicolumn{4}{c}{Class 1}\\ F01159$-$4443 & Low velocity ($<$100~km~s$^{-1}$) shocks & 0.23 & Some regions explained by stars.\\ ESO 297-G011 & Young stars & --0.12 & Some small areas explained by shocks. $r$ based on \sha. $r$ based on \oha\ not reliable.\\ ESO 297-G012 & Young stars and shocks & --0.56 & $r$ based on \nha. $r$ based on \oha\ or \sha\ not reliable.\\ F06076$-$2139 & \ldots & 0.75 & $r$ based on \nha \ data. No \oi\ nor \sii\ data.\\ F06259$-$4708 P1 & Young stars & 0.74 & Low velocity (100--150~km~s$^{-1}$) shocks also present.\\ F06259$-$4708 P2 & Shocks (100--150~km~s$^{-1}$) and young stars & 0.31 & \\ 08424$-$3130 & Stars and shocks (${\sim}100$~km~s$^{-1}$) & 0.61 & $r$ based on \sha. $r$ based on \oha\ not reliable. Northern galaxy mainly shocks; southern one mainly stars. \\ F08520$-$6850 & Stars and shocks (${\sim}100$~km~s$^{-1}$) & 0.40 & \\ IC 563 & Young stars & 0.22 & Low velocity (100--150~km~s$^{-1}$) shocks could be also present.\\ IC 564 N & Young stars & 0.44 & Low velocity (100--150~km~s$^{-1}$) shocks also present. $r$ based on \nha. No \oi\ data. $r$ based on \sha\ not reliable.\\ IC 564 S & Young stars & 0.34 & $r$ based on \nha. No \oi\ data. $r$ based on \sha\ not reliable.\\ 12042$-$3140 & Young stars and shocks (100--150~km~s$^{-1}$) & 0.81 & Northern galaxy mainly stars, Southern one shocks. \\ 12596$-$1529 & Young stars and low velocity shocks & 0.47 & $r$ based on \sha\ data. No \oi\ data. $r$ based on \sha\ not reliable.\\ F14544$-$4255 E & Young stars & 0.67 & $r$ based on \sha. No \oi\ data.\\ F14544$-$4255 W\tablefootmark{d} & High velocity (100--300~km~s$^{-1}$) shocks & 0.67 & Shocks may be associated to the nucleus according to the \oha\ map.\\ 18093$-$5744 N & Young stars & 0.09 & Low velocity shocks also possible.\\ 18093$-$5744 C & Stars older than 3~Myr and/or with $Z $ $-1.2$. Part of the shocks may be associated to the nucleus \\ 17138$-$1017 & Young stars and low velocity shocks & --0.23 & No \oi data; $r$ according to \sha \ data \\ 21453$-$3511\tablefootmark{d} & High velocity (100--300~km~s$^{-1}$) shocks and/or AGN. & 0.76 & Young stars (spiral arms). Shocks may be associated to the nucleus according \oha\ map.\\ \hline \end{tabular}} \tablefoot {\tablefoottext{a}{At least otherwise indicated, based on the comparison of the data with several ionization models in the \oha~$-$ \nha~diagnostic diagram. For the present analysis solar metallicity has been considered as baseline. If~higher metallicity (e.g.~$Z=2~Z_\odot$) is considered, a higher presence of shocks with respect to stars would have been obtained (see Fig.~\ref{figo1havsn2gha}).} \\ \tablefoottext{b}{Pearson coefficient inferred from the \oha~$-$~$\sigma$~relation (see~text). For~objects where \oi\ was not detected or the $r$~coefficient did not reach a confidence level of~90\%, $r$~was obtained from the \sha \ or \nha, as~indicated.}\\ \tablefoottext{c}{Classified as Seyfert \citep{kew01a}.}\\ \tablefoottext{d}{Classified as Seyfert \citep{cor03}.}} \vspace*{3mm} \end{table}