Table 4: Values of the ongoing star formation rate SFR (in $M_\odot $/yr) derived from: the main emission lines, after correction for extinction and for the AGN contribution, and adopting the the Kennicutt's calibration; from the far-IR luminosity (Kennicutt's calibration); and from our global best-fit model. The latter has been computed combining the two youngest single stellar populations. All SFRs dignostics adopt a Salpeter IMF between 0.1 and 100 $M_\odot $.
Spectrum H$\alpha $ [OII] FIR Model
1 - - - -
2 0.22 0.59 0.25 0.21
3 1.04 4.23 2.94 4.78
South 46.60 74.67 66.02 78.40
7 2.28 6.79 2.94 2.65
8 0.29 0.85 0.25 0.19
9 - - - 0.07
10 - - - 0.07
11 0.11$^\ast$ 0.13$^\ast$ - 0.05
12 0.12$^\ast$ 0.13$^\ast$ - 0.09
North 0.48$^\ast$ 0.29$^\ast$ 1.32 0.40
15 0.14$^\ast$ 0.15$^\ast$ - 0.16
16 0.08$^\ast$ 0.15$^\ast$ - 0.08
17 0.08$^\ast$ 0.14$^\ast$ - -


$^\ast$: Values obtained assuming E(B-V)=0.4 in these regions of the galaxy.


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