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Table 5

SFR parameters for the different regions.

Band Fluxa Luminositya SFRb τdep c ΣSFR b
[mJy]d [1038 erg s-1] [10-4M⊙ yr-1] [1010 yr] [10-4M⊙ yr-1 kpc-2]
[10-15 erg cm-2 s-1] d
Total emission
FUV 0.039 ± 0.004 265.4 39.1 0.42 7.56
Hα 4.24 ± 0.42 1.46 7.8 2.1 1.52
8 μm 1.25 ± 0.18 161.33 19.4 0.8 3.74
8 μm+Hα − − 17.8 0.9 3.44
24 μm 1.00 ± 0.30 43.19 15.2 1.1 2.95
24 μm+FUV − − 19.4 0.8 3.77
24 μm+Hα − − 12.5 1.3 2.43
NE cloud
FUV 0.030 ± 0.003 205.2 30.2 0.54 10.47
Hα 3.76 ± 0.38 1.22 6.6 1.6 2.27
8 μm 0.92 ± 0.12 118.67 14.2 0.7 4.94
8 μm+Hα − − 13.9 0.7 4.82
24 μm 0.87 ± 0.18 37.33 13.3 0.8 4.54
24 μm+FUV − − 15.7 1.0 5.33
SW cloud
FUV 0.008 ± 0.001 51.7 7.6 2.2 4.43
Hα 0.60 ± 0.06 0.19 1.0 5.9 0.60
8 μm 0.26 ± 0.05 33.26 4.0 1.5 2.32
8 μm+Hα − − 3.1 2.0 1.79

Notes.

(a)

The fluxes and luminosities are corrected for Galactic foreground emission as explained in Sect. 3.5.

(b)

The SFRs derived from the UV flux takes into account both the Galactic foreground extinction and an internal extinction derived from the stellar population fit (see Table 3 and Sect. 3.6).

(c)

Molecular gas depletion timescale, calculated as the ratio between the SFR from column 4 and the molecular gas mass from Table 1.

(d)

The unit for most fluxes entries is mJy, expect for Hα which is given in 10-15 erg cm-2 s-1.

(e)

We did not detect any significant emission at 24 μm in the SW region.

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