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Home All issues Volume 508 / No 2 (December III 2009) A&A, 508 2 (2009) 645-664 Full HTML
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Table 10:

Luminosities, size and SFR of our galaxies.
  NGC 1705 a Haro 11 a Mrk 1089
$L_{\rm TIR}$= $L_{[3~\mu {\rm m},1100~\mu {\rm m}]}$ ($L_\odot$) (1) 5.8 $\times$ 107 1.7 $\times$ 1011 3.9 $\times$ 1010
  (2) 4.9 $\times$ 107 1.4 $\times$ 1011 3.8 $\times$ 1010
  (3) 5.9 $\times$ 107 1.6 $\times$ 1011 4.3 $\times$ 1010
$L_{[3~\mu{\rm m},50~\mu{\rm m}]}$($L_\odot$)   1.9 $\times$ 107 1.2 $\times$ 1011 1.4 $\times$ 1010
$L_{[50~\mu{\rm m},100~\mu{\rm m}]}$($L_\odot$)   2.2 $\times$ 107 4.1 $\times$ 1010 1.3 $\times$ 1010
$L_{[100~\mu{\rm m},1100~\mu{\rm m}]}$($L_\odot$)   1.6 $\times$ 107 9.6 $\times$ 109 1.1 $\times$ 1010
$L_{\rm FIR}$= $L_{[8~\mu{\rm m},1100~\mu{\rm m}]}$ ($L_\odot$)   5.1 $\times$ 107 1.6 $\times$ 1011 3.7 $\times$ 1010
$L_{\rm H\alpha}$(erg s-1) c   6.34 $\times$ 1038 3.2 $\times$ 1042 4.57 $\times$ 1041
Size   0.5' $\times$ 0.5' 0.25' $\times$ 0.25' 0.31' $\times$ 0.12'
SFR ($M_\odot $ yr-1 kpc-2) d (4) 1.6 $\times$ 10-3 5.1 $\times$ 10-2 5 $\times$ 10-2
  (5) 9.4 $\times$ 10-4 - 5.8 $\times$ 10-2
  (6) 5.2 $\times$ 10-4 2.4 $\times$ 10-2 1.4 $\times$ 10-2
  (7) 5.7 $\times$ 10-4 3 $\times$ 10-2 1.8 $\times$ 10-2

a The models used for NGC 1705 and Haro 11 include an independent, very cold dust component at 10 K with an emissivity $\beta $ = 1.
b Total infrared luminosities ( $L_{\rm TIR}$) are estimated: 1) by integrating our SED models with a submm constraint from 3 to 1100 $\mu $m; 2) from the Dale & Helou (2002) formula; 3) from the Draine & Li (2007) formula.
c H$\alpha $ luminosities ( $L_{\rm H\alpha}$) are given in Cannon et al. (2006) for NGC 1705, Bergvall et al. (2000) for Haro 11 and c) Iglesias-Paramo & Vilchez (1997) for Mrk 1089.
d Star formation rates (SFR) are estimated: 4) using the relation of Kennicutt (1998) based on $L_{\rm FIR}$; 5) using the relation of Zhu et al. (2008) based on $\nu$ $L_{\nu}$[24 $\mu $m]. (this last relation is only valid for galaxies with a $L_{\rm TIR}$ < 10 $^{11}~L_{\odot}$and can not be used for Haro 11); 6) using the relation of Calzetti (2007) based on the 24 $\mu $m luminosity (L24) alone; 7) using the relation of Calzetti (2007) based on L24 and  $L_{\rm H\alpha}$.


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