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Table A.1

Overview of the different reference SFR calibrations.

SFR calibrations

Lx [erg s-1] Age range [Myr] C x Ref.

FUVcorr 0-10-100 43.35 1,2
Hαcorr 0-3-10 41.27 1,2
24 μm 0-5-100 42.69 3
70 μm 0-5-100 43.23 4
TIR 0-5-100 43.41 1,2

Composite SFR calibrations

Composite tracera ν 1σ disp [dex] Ref.

LFUV,obs+νL24bc 3.89 0.13 1
LFUV,obs+νL1.4 GHz 7.2 × 1014 0.14 1
LFUV,obs+νLTIR 0.27 0.09 1
LHα,obs+νL24b 0.020 0.12 5

Notes. In the first part, the SFR calibration coefficients are provided for several SFR indicators following the prescription log SFR = log  Lx − log  Cx. The column “Age range” specifies the lower age limit, the mean age, and the age of stars below which 90% of the emission is contributed. The last column refers to the literature work(s) reporting the calibrations. The second part gives the calibration factors for several composite SFR tracers used to correct the unobscured SFR indicators for extinction, with Cols. 2 and 3 presenting the calibration coefficients ν and average dispersion in the calibrations.

(a)

The luminosities of composite tracers are in units of erg s-1, except L1.4GHz which is in units of erg s-1 Hz-1.

(b)

The SFR calibration is valid for the emission from MIPS 24 μm or IRAS 25 μm filters, due to the excellent correspondence that exists between both bands (Kennicutt et al. 2009).

(c)

Two calibrations based on FUV and MIPS 24 μm have been reported in the literature. Zhu et al. (2008) found a calibration coefficient ν= 6.31 based on a sample of 187 star-forming non-AGN galaxies, while Hao et al. (2011) found a lower scaling factor ν= 3.89, calibrated on a sample of 144 galaxies retained from the spectrophotometric survey by Moustakas & Kennicutt (2006) (97 objects) and SINGS (47 objects, Kennicutt et al. 2003). No clear reason has been found to explain the difference in calibration coefficients derived by Zhu et al. (2008) and Hao et al. (2011).

Reference. (1) Hao et al. (2011); (2) Murphy et al. (2011); (3) Rieke et al. (2009); (4) Calzetti et al. (2010) ; (5) Kennicutt et al. (2009).

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