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Table 3

Prescriptions to estimate the SFR from the relation log SFR [M yr-1] = β + α × log Lline [ L] depending on galaxy type, i.e., metal-poor dwarf galaxies, Hii/starburst galaxies, composite, or AGN sources, ULIRGs, and high-redshift galaxies.

SFR calibrator Number of galaxies Slope Intercept 1σ dispersion [dex]

SFR calibration: entire literature sample

[CII] 530 1.01 ± 0.02 –6.99 ± 0.14 0.42 (2.6)
[OI] 63 150 1.00 ± 0.03 –6.79 ± 0.22 0.42 (2.6)
[OIII] 88 a 83 1.12 ± 0.06 –7.48 ± 0.42 0.66 (4.6)

SFR calibration: metal-poor dwarf galaxies
[CII] 42 0.80 ± 0.05 –5.73 ± 0.32 0.37 (2.3)
[OI] 63 31 0.91 ± 0.05 –6.23 ± 0.30 0.27 (1.9)
[OIII] 88 a 28 0.92 ± 0.05 –6.71 ± 0.33 0.30 (2.0)

SFR calibration: HII/starburst galaxies
[CII] 184 1.00 ± 0.04 –7.06 ± 0.33 0.27 (1.9)
[OI] 63 41 0.89 ± 0.06 –6.05 ± 0.44 0.20 (1.6)
[OIII] 88a 9 0.69 ± 0.09 –3.89 ± 0.63 0.23 (1.7)
SFR calibration: composite/AGN sources
[CII] 212 0.90 ± 0.04 –6.09 ± 0.29 0.37 (2.3)
[OI] 63 37 0.76 ± 0.09 –5.08 ± 0.73 0.35 (2.2)
[OIII] 88a 20 0.87 ± 0.14 –5.46 ± 0.98 0.35 (2.2)
SFR calibration: ULIRGs
[CII] 65 1.0b –6.28 ± 0.04 0.31 (2.0)
[OI] 63 35 1.0b –6.23 ± 0.06 0.33 (2.1)
[OIII] 88 23 1.0b –5.80 ± 0.09 0.40 (2.5)
SFR calibration: high-redshift (z> 0.5)
[CII] 27 1.18 ± 0.19 –8.52 ± 1.92 0.40 (2.5)
[OI] 63 6 1.0b –7.03 ± 0.29 0.64 (4.4)
[OIII] 88 3 1.0b –6.89 ± 0.30 0.42 (2.6)

Notes. The first and second columns indicate the FIR fine-structure line(s) and number of galaxies used in the SFR calibration, with the slope(s) α, intercept β, and dispersion of the best-fit line for the different samples presented in Cols. 3, 4, and 5. Between parentheses, we note the uncertainty factor on the derived SFR estimates corresponding to the dispersion in the relation.

(a)

We only rely on Herschel observations for the SFR calibrations for [Oiii]88 because of the significant difference found between the calibration of the Herschel and ISO instruments (see Sect. A.4).

(b)

The number of galaxies and/or FIR line luminosity range was insufficient to constrain the slope and intercept of the best-fit line. Therefore, the fitting procedure was performed for a fixed slope of 1.

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