Table 5.
Results of the SED modeling.
| Galaxy ID | log(M⋆/M⊙) | LFIR | SFRSED | SFR24 μm | sSFR | sSFRMS |
|---|---|---|---|---|---|---|
| (L⊙) | (M⊙/yr) | (M⊙/yr) | (Gyr−1) | (Gyr−1) | ||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
| DES-RG 399 | 10.96 | <3.9e+11 | <68 |  |
 |
0.11 |
| DES-RG 708 | 11.45 | <1.51e+12 | <263 |  |
 |
0.13 |
| COSMOS-FRI 16 | 11.09 | <2.7e+11 | <48 |  |
 |
0.40 |
| COSMOS-FRI 31 | 10.94 | <4.1e+11 | <72 | <42 | <0.48 | 0.38 |
| COSMOS-FRI 70 | 11.36 | <1.2e+13 | <2050 |  |
 |
1.30 |
Notes. (1) Galaxy name; (2) stellar mass; (3) FIR (8–1000) μm luminosity; (4) SFR estimated integrating the best fit SED model between (8–1000) μm in the rest frame; (5) SFR estimated from the available ∼24 μm (WISE W4 or Spitzer MIPS) flux and the Calzetti et al. (2007) relation, for COSMOS-FRI 31 the 2σ upper limit is reported; (6) specific SFR derived as sSFR = SFR24 μm/M⋆, where the uncertainties are obtained by propagating those of of SFR24 μm and those ∼0.3 dex of M⋆; (7) specific SFR from Speagle et al. (2014) for main sequence (MS) field galaxies of redshift and stellar mass equal to those of our targets.
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