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Home All issues Volume 521 (October 2010) A&A, 521 (2010) A63 Full HTML
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Table 4:

FUV, U, B, H$\alpha $, H, FIR, 15 $\mu $m, 60 $\mu $m, and 1.4 GHz luminosities for all galaxies analyzed in this work.

Galaxy 		$L_{\rm FUV}$ LU LB $L_{\rm H\alpha}$ LH $L_{\rm FIR}$ $L_{\rm 15~ \mu m}$ $L_{\rm 60~ \mu m}$ $L_{\rm 1.4~ GHz}$
  [1039 erg s-1 Å-1] [108 $L_{\odot}$] [108 $L_{\odot}$] [1040 erg s-1] [108 $L_{\odot}$] [1042 erg s-1] [1022 W Hz-1] [1023 W Hz-1] [1020 W Hz-1]

HCG 31 		49 $\pm$ 3 356 202 $\pm$ 7 52 $\pm$ 4 42.2 72 $\pm$ 6a 3.9 $\pm$ 0.7a 14.1 $\pm$ 1.1a 98 $\pm$ 14
'' AC 24.9 $\pm$ 1.5 175 92 $\pm$ 4 36.3 $\pm$ 2.3 18.0 ... ... ... 79 $\pm$ 11
'' B 11.0 $\pm$ 0.9 73.8 47.4 $\pm$ 1.8 3.1 $\pm$ 0.3 10.0 ... ... ... 7.5 $\pm$ 1.1
'' E 1.51 $\pm$ 0.12 6.3 3.13 $\pm$ 0.17 1.49 $\pm$ 0.16 0.586 ... ... ... ...
'' Fb 1.52 $\pm$ 0.15 10.9 4.0 $\pm$ 0.2 5.0 $\pm$ 0.3 0.486 ... ... ... ...
'' H 0.13 $\pm$ 0.05 ... ... 0.045 $\pm$ 0.013 ... ... ... ... ...
'' G 10.3 $\pm$ 0.6 90.4 55 $\pm$ 2 6.4 $\pm$ 0.4 13.1 ... ... ... 11.9 $\pm$ 1.8
Mkn 1087 ... 1803 1127 $\pm$ 83 70 $\pm$ 5 360 228 $\pm$ 23 15 $\pm$ 4 45 $\pm$ 5 178 $\pm$ 9
'' N ... ... 26.1 $\pm$ 0.9 2.27 $\pm$ 0.19 5.01 ... ... ... ...
Haro 15 84 $\pm$ 5 614 347 $\pm$ 13 42 $\pm$ 5 124 62 $\pm$ 6 11 $\pm$ 3 12.2 $\pm$ 1.1 160 $\pm$ 9
Mkn 1199 ... 479 291 $\pm$ 11 49 $\pm$ 7 344 116 $\pm$ 6 9.8 $\pm$ 1.1 23.8 $\pm$ 1.2 126 $\pm$ 4
'' NE ... 21.1 16.6 $\pm$ 0.6 0.90 $\pm$ 0.23 21.7 ... ... ... ...
Mkn 5 0.274 $\pm$ 0.018 4.21 2.63 $\pm$ 0.10 0.582 $\pm$ 0.014 1.89 <0.30 <0.087 0.036 $\pm$ 0.007 3.9 $\pm$ 0.8
IRAS 08208+2816 162 $\pm$ 10 879 511 $\pm$ 14 142 $\pm$ 12 373 254 $\pm$ 22 <5.5 49.7 $\pm$ 4.0 657 $\pm$ 26
IRAS 08339+6517 79 $\pm$ 4 1159 661 $\pm$ 23 120 $\pm$ 6 592 198.6 $\pm$ 1.8 18.3 $\pm$ 1.8 42.6 $\pm$ 0.3 249 $\pm$ 37
'' Comp. 1.17 $\pm$ 0.10 38 29.9 $\pm$ 1.6 2.1 $\pm$ 0.4 23.3 ... ... ... ...
POX 4 7.0 $\pm$ 0.4 104.7 51.1 $\pm$ 0.5 23.3 $\pm$ 1.9c 17.9 6.9 $\pm$ 0.5 <24 1.56 $\pm$ 0.14 10.4 $\pm$ 1.2
'' Comp. 0.667 $\pm$ 0.075 2.42 2.17 $\pm$ 0.07 0.188 $\pm$ 0.018c 1.1: ... ... ... ...
UM 420 25.4 $\pm$ 1.4 236 103 $\pm$ 4 47 $\pm$ 3 57 142: ... 27.7 74 $\pm$ 34
SBS 0926+606b 41.4 $\pm$ 3.4 52.3 26.6 $\pm$ 0.8 11.8 $\pm$ 0.7 9.49 5.8 $\pm$ 0.6 2.8 1.01 $\pm$ 0.17 10 $\pm$ 2
'' A 6.4 $\pm$ 0.4 28.1 12.8 $\pm$ 0.4 9.4 $\pm$ 0.5 3.63 ... ... ... ...
'' B 35 $\pm$ 3 24.2 13.8 $\pm$ 0.4 2.4 $\pm$ 0.2 5.86 ... ... ... ...

SBS 0948+532

 ... 121.3 36.7 $\pm$ 1.0 78 $\pm$ 3 15.8 ... ... ... <38
SBS 1054+365 0.090 $\pm$ 0.006 0.982 0.655 $\pm$ 0.018 0.450 $\pm$ 0.017 0.413 0.23 $\pm$ 0.03 <0.042 0.041 $\pm$ 0.005 0.098 $\pm$ 0.011
SBS 1211+540 0.076 $\pm$ 0.005 0.608 0.316 $\pm$ 0.008 0.141 $\pm$ 0.005 0.127 ... ... ... <0.50
SBS 1319+579 0.86 $\pm$ 0.05 63.1 40.2 $\pm$ 1.4 2.38 $\pm$ 0.15 28.6 5.3: ... 0.85 <2.9
SBS 1415+437 0.409 $\pm$ 0.023 1.69 1.00 $\pm$ 0.03 0.50 $\pm$ 0.02 0.581 ... ... ... <0.052
III Zw 107 ... 286 177 $\pm$ 5 40.1 $\pm$ 1.8 77.3 50 $\pm$ 8 <7.3 10.4 $\pm$ 1.5 62 $\pm$ 4
Tol 9 9.5 $\pm$ 0.7 118 79 $\pm$ 2 22.9 $\pm$ 1.6 55.5 35.4 $\pm$ 1.6 2.5 $\pm$ 0.7 6.1 $\pm$ 0.5 87.3 $\pm$ 1.6
Tol 1457-262b 38.6 $\pm$ 2.6 319 182 $\pm$ 5 63 $\pm$ 3 109 82 $\pm$ 6 <6.5 17.2 $\pm$ 1.1 216 $\pm$ 10
'' Obj 1 29.2 $\pm$ 1.6 223 121 $\pm$ 3 46.2 $\pm$ 2.7 58.6 ... ... ... ...
'' Obj 2 9.2 $\pm$ 1.1 97.3 60.3 $\pm$ 1.7 17.2 $\pm$ 0.8 45.3 ... ... ... ...
'' #15 1.10 $\pm$ 0.21 8.39 6.08 $\pm$ 0.23 0.47 $\pm$ 0.04 5.5: ... ... ... ...
Arp 252b 47.4 $\pm$ 3.3 711 435 $\pm$ 13 90 $\pm$ 6 423 361 $\pm$ 19 38 $\pm$ 5 79 $\pm$ 4 1968 $\pm$ 60
'' ESO 566-8 38.5 $\pm$ 2.7 597 350 $\pm$ 10 84 $\pm$ 6 313 ... ... ... ...
'' ESO 566-7 8.9 $\pm$ 0.6 114 85 $\pm$ 3 6.3 $\pm$ 0.4 110 ... ... ... ...
NGC 5253 2.35 $\pm$ 0.15 36.6 22.9 $\pm$ 0.2 4.4 $\pm$ 0.2 14.2 2.583 $\pm$ 0.009 0.479 $\pm$ 0.004 0.571 $\pm$ 0.001 1.47 $\pm$ 0.06

Notes. (a) As IRAS data do not allow to be distinguished regions within the HCG 31 group, this value considers the flux of all galaxy members.
(b) We are considering the flux of two galaxies: members F1 and F2 for HCG 31 F; galaxies A and B for SBS 0926+606; obj 1 and obj 2 for Tol 1457-262; and ESO 566-8 (A) and ESO 566-7 (B) for Arp 252.
(c) As we pointed out in Paper I, the H$\alpha $ flux for POX 4 provided by Méndez & Esteban (1999) seems to be overestimated, so we consider here the value provided by Gil de Paz et al. (2003), which is 0.61 times smaller. We also scale our H$\alpha $ flux of POX 4 Comp using this factor.


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