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Table 2:

Physical properties of the ionized gas for the galaxies analysed in this work.
Galaxy $T_{\rm e}$ $T_{\rm e}$High $T_{\rm e}$Low $n_{\rm e}$ c(H$\beta $) $W_{\rm abs}$ -W(H$\beta $)
  (a) [K] [K] [cm-3]   [Å] [Å]
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 $0.28 \pm 0.08$ 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 $37.0\pm1.6$
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 \pm 0.1 $ $82\pm7$
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 $11~160\pm510$ $10~350\pm650$ $230\pm70$ $0.10\pm0.02$ $0.6\pm0.1$ $39\pm2$

Notes. (a) In this column we indicate if $T_{\rm e}$ was computed using the direct method (D) or via empirical calibrations (EC).


Source LaTeX | All tables | In the text

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