Table 5
MAGPHYS 1σ confidence interval for the SFR, stellar mass, bolometric dust luminosity, and sSFR derived from fitting the optical/NIR SEDs of the spectroscopic targets with the best secure redshift identification.
| ID | SFR | L dust | M ⋆ | sSFR | |
| [ M⊙ yr-1 ] | [ L⊙ ] | [ M⊙ ] | [ yr-1 ] | ||
|
|
|||||
| A1 | 23.3 − 571 | (0.34 − 6.02) × 1012 | (0.83 − 1.29) × 1011 | (0.19 − 6.68) × 10-9 | |
| A2 | 15.5 − 50 | (2.0 − 7.1) × 1011 | (1.26 − 1.74) × 1011 | (1.1 − 3.3) × 10-10 | |
| B2a | 1.2 − 2.8 | (1.0 − 4.0) × 1010 | (1.8 − 2.3) × 1010 | (0.7 − 1.5) × 10-10 | |
|
|
|||||
| A3 | 2.4 − 12.9 | (0.7 − 3.1) × 1011 | (6.8 − 7.91) × 1010 | (0.3 − 1.7) × 10-10 | |
| A4a | 45.4 − 115.3 | (0.56 − 1.48) × 1012 | (1.10 − 1.35) × 1011 | (0.37 − 1.06) × 10-9 | |
| D1 | 18.7 − 98.2 | (0.28 − 1.35) × 1012 | (0.98 − 1.41) × 1011 | (1.5 − 8.4) × 10-10 | |
Notes. These quantities have been obtained using the Chabrier (2003) initial mass function (IMF). To rescale them to a Salpeter (1955) IMF, an average factor of 1.4 should be applied to the SFRs and stellar masses.
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