\begin{table}%t2

  \caption{\label{cfisicas}Physical properties of the ionized gas for the galaxies analysed in this work.}
%\centerline
{
  \begin{tabular}{l@{\hspace{8pt}}  c@{\hspace{8pt}}c@{\hspace{8pt}}c@{\hspace{8pt}} c@{\hspace{8pt}}c@{\hspace{8pt}}c@{\hspace{8pt}} 
c@{\hspace{8pt}} c@{\hspace{8pt}} }
  \hline\hline
 Galaxy        &   \Te     & \Te\ High  & \Te\ Low  &     $n_{\rm e}$  & \CHb & $W_{\rm abs}$   &  $-W$(\Hb) \\ % &  $-W$[\ion{O}{iii}]  \\
          & \tablefootmark{(a)}    &  [K] & [K]  & [cm$^{-3}$] & & [\AA]  & [\AA] \\ % & [\AA] \\
\hline
HCG 31 AC      & D  &   $9400\pm600$   &$10~800 \pm 300$ &  $210\pm70$   & $0.09\pm0.03$ &   2.0         &   $91.1\pm2.1$ \\
HCG 31 B       & D  &  $11~500\pm700$   &$12~000 \pm 400$ &  $<$100      & $0.28\pm0.08$ &   2.0          &   $12.9\pm0.5$ \\
HCG 31 E       & D  &$  11~100 \pm 1000$ & $11~800 \pm 600$ &  $<$100      & $0.11\pm0.05$ &   2.0         &   $21.1\pm1.1$ \\
HCG 31 F1      & D  &  $12~600\pm1100$   &$12~600 \pm 700$ &  $<$100      & $0.32\pm0.06$ &   2.0         &   $218\pm13$   \\
HCG 31 F2      & D  &$  12~300 \pm 1300$ & $12~400 \pm 800$ &  $<$100      & $0.14\pm0.05$ &   2.0         &   $256\pm30$ \\
HCG 31 G       & D  &  $11~600\pm700$  & $12~000 \pm 400$ &  $<$100      & $0.09\pm0.05$ &   2.0         &   $37.0\pm1.6$ \\
%HCG 31 H       & EC 
Mkn 1087       & EC &   $7100\pm1000$   & $8000\pm1000$ &  $220\pm50$   & $0.17\pm0.02$ &   $1.7\pm0.2$ &   $22.3\pm0.9$ \\
Mkn 1087 N     & EC &  $10~900\pm1000$   &$10~600\pm1000$ &  $115\pm50$   & $0.17\pm0.02$ &   $0.2\pm0.1$ &   $25.0\pm1.7$ \\
Haro 15 C      & EC &   $9500\pm800$   & $9600 \pm 600$ &  $<$100      & $0.11\pm0.03$ &   $2.4\pm0.4$ &   $16.4\pm1.1$ \\
Haro 15 A      & D  &   $12~850\pm700$  & $12~000 \pm 500$ &  $<$100      & $0.33\pm0.03$ &   $1.3\pm0.3$ &   $75.7\pm4.2$ \\
Mkn 1199       & D  &   $5400\pm700$   & $6800\pm600$   &  $300\pm100$   & $0.30\pm0.03$ &   $1.8\pm0.4$ &   $21.4\pm1.3$ \\
Mkn 1199 NE    & EC &   $8450\pm800$   & $8900 \pm 600$ &  $<$100      & $0.16\pm0.03$ &   $0.6\pm0.3$ &   $20.2\pm2.3$ \\
Mkn 5         & D  &  $12~450\pm650$  & $11~700 \pm 450$ &  $<$100      & $0.17\pm0.02$ &   $0.8\pm0.2$ &   $75\pm5$ \\
IRAS 08208+2816& D  &  $10~100\pm700$  & $10~100 \pm 500$ &  $<$100      & $0.11\pm0.02$ &   $3.2\pm0.1$ &   $80\pm5$ \\
IRAS 08339+6517& EC &   $8700\pm1000$   & $9100\pm1000$ &     100      & $0.22\pm0.02$ &   $1.8\pm0.2$ &   $19.0\pm0.8$ \\
IRAS 08339+6517c&EC &   $9~050\pm1000$   & $9300\pm1000$ &     100      & $0.18\pm0.03$ &   $1.5\pm0.2$ &    $7.5\pm0.2$  \\
POX 4         & D  &  $14~000\pm500$  & $12~800 \pm 400$ &  $250\pm80$   & $0.08\pm0.01$ &   $2.0\pm0.1$ &   $200\pm9$ \\
POX 4 Comp     & EC &  $12~400\pm1000$  & $11~700 \pm 700$ &  $<$100      & $0.06\pm0.03$ &   $1.4\pm0.3$ &   $12\pm4$ \\
UM 420         & D  &  $13~200\pm600$  & $12~200 \pm 500$ &  $140\pm80$   & $0.09\pm0.01$ &   $2.0\pm0.1$ &   $169\pm10$ \\
SBS 0926+606 A & D  &  $13~600\pm700$  & $12~500 \pm 500$ &  $<$100      & $0.12\pm0.03$ &   $0.7\pm0.1$ &   $125\pm6$ \\
SBS 0926+606 B & EC &  $11~500\pm1000$ &  $11~000 \pm 800$ &  $<$100      & $0.18\pm0.04$ &   $1.0\pm0.3$ &   $18\pm3$ \\
SBS 0948+532   & D  &  $13~100\pm600$  & $12~200 \pm 400$ &  $250\pm80$   & $0.35\pm0.03$ &   $0.3\pm0.1$ &   $213\pm11$ \\
SBS 1054+365   & D  &  $13~700\pm900$  & $12~600 \pm 700$ &  $<$100      & $0.02\pm0.02$ &   $0.8\pm0.1$ &   $89\pm7$ \\
SBS 1054+365 b & EC &$  11~800 \pm 1100$ & $11~300 \pm 900$ &  $300\pm200$   & $0.03\pm0.03$ &   $0.3\pm0.1$ &   $8\pm3$ \\
SBS 1211+540   & D  &  $17~100\pm600$  & $15~000 \pm 400$ &  $320\pm50$   & $0.12\pm0.01$ &   $1.3\pm0.1$ &   $135\pm10$ \\
SBS 1319+579 A & D  &  $13~400\pm500$  & $12~400 \pm 400$ &  $<$100      & $0.03\pm0.01$ & $  0.0 \pm 0.1  $ &   $285\pm14$ \\
SBS 1319+579 B & D  &  $11~900\pm800$  & $11~300 \pm 600$ &  $<$100      & $0.11\pm0.03$ &   $0.4\pm0.1$ &   $42\pm4$ \\
SBS 1319+579 C & D  &  $11~500\pm600$  & $11~050 \pm 400$ &  $<$100      & $0.02\pm0.02$ &   $0.2\pm0.1$ &   $94\pm6$ \\
SBS 1415+579 C & D  &  $16~400\pm600$  & $14~500 \pm 400$ &  $<$100      & $0.01\pm0.02$ &   $0.8\pm0.1$ &   $222\pm11$ \\
SBS 1415+579 A & D  &  $15~500\pm700$  & $13~850 \pm 500$ &  $<$100      & $0.15\pm0.03$ &   $1.0\pm0.2$ &   $130\pm8$ \\
III Zw 107 A   & D  &  $10~900\pm900$   &$10~500\pm800$   &  $200\pm60$   & $0.68\pm0.04$ &   $2.0\pm0.3$ &   $44\pm2$ \\
Tol 9         & D  &   $7600\pm1000$   & $8300 \pm 700$ &  $180\pm60$   & $0.50\pm0.05$ &   $7.5\pm0.8$ &   $33\pm2$ \\
Tol 1457-262 A & D  &  $14~000\pm700$   &$12~500\pm600$   &  $200\pm80$   & $0.57\pm0.03$ &   $1.4\pm0.2$ &   $101\pm6$ \\
Tol 1457-262 B & D  &  $15~200\pm900$    &$14~200\pm700$   &  $<$100      & $0.00\pm0.05$ &   $0.0\pm0.1$ &   $82\pm7$ \\
Tol 1457-262 C & D  &  $13~400\pm1100$   &$12~400\pm1000$ &  $200\pm100$   & $0.15\pm0.02$ &   $0.7\pm0.1$ &   $92\pm9$ \\
ESO 566-8     & D  &   $8700\pm900$   & $9100 \pm 800$ &  $300\pm100$   & $0.49\pm0.03$ &   $1.3\pm0.1$ &   $95\pm7$ \\
ESO 566-7     & EC &   $7900\pm1000$   & $8500 \pm 900$ &  $100\pm50$   & $0.23\pm0.05$ &   $2.7\pm0.2$ &   $13\pm2$ \\
NGC 5253 A     & D  &  $12~100\pm260$  & $11~170 \pm 520$ &  $580\pm110$   & $0.23\pm0.02$ &   $1.3\pm0.1$ &   $234\pm5$ \\
NGC 5253 B     & D  &  $12~030\pm260$  & $11~250 \pm 490$ &  $610\pm100$   & $0.38\pm0.03$ &   $1.7\pm0.1$ &   $254\pm5$ \\
NGC 5253 C     & D  &  $10~810\pm230$  & $10~530 \pm 470$ &  $370\pm80$   & $0.25\pm0.03$ &   $0.8\pm0.1$ &   $94\pm3$ \\
NGC 5253 D     & D  &  $11~160\pm510$   &$10~350\pm650$   &  $230\pm70$   & $0.10\pm0.02$ &   $0.6\pm0.1$ &   $39\pm2$ \\  
\hline
  \end{tabular}}
  \tablefoot{\tablefoottext{a}{In this column we indicate if \Te\ was computed using the direct method (D) or via empirical calibrations (EC).}}
  \end{table}