Table 2
MIRO/SINFONI sample: main properties.
| MIRO | N H | log (L2 − 10) | log (L5.8) | log (Lbol) | S radio | q 24 | M ∗ | SFR | log (RSB)b | E(B − V)host | E(B − V)AGN | |||
| 1023 cm-2 | erg s-1 | erg s-1 | erg s-1 | μJy | 1011M⊙ | M⊙/yr | ||||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | |||
|
|
||||||||||||||
| 18 744 | 2.4 |
43.82 | 44.85 | 45.11 | 424 ± 28 | 2.3 | 2.0 | 99 | 0.2 | 0.5 | 2.7 | |||
| 10 561 | 2.9 |
43.96 | 45.35 | 45.97 | 72 ± 15 | 0.4 | 1.5 | 196 | 0.3 | 0.7 | 4.0 | |||
| 28 704 | – | – | 45.32 | 47.63 | 154 ± 25 | 2.0 | 0.6 | 11(<25)a | –0.8(<–0.5)a | 0.5 | 4.1 | |||
| 20 581 | 6.8 |
45.00 | 45.89 | 46.61 | 5430 ± 60 | –0.6 | 1.9 | 48(<132)a | –0.6(<–0.2)a | 0.6 | 2.0 | |||
Notes. (1) Target name; (2) column density; (3) intrinsic X-ray luminosity; (4) rest-frame 5.8 μm luminosity; (5) bolometric luminosity; (6) rest-frame 1.4 GHz flux; (7) q24obs = log (f24 μm/f1.4 GHz) (Bonzini et al. 2013); (8) stellar mass; (9) star formation rate; (10) starburstiness, defined as the ratio between the specific star formation rate (sSFR = SFR/M∗) and that expected for main-sequence galaxies at given computed stellar mass and spectroscopic redshift (sSFRMS,z), according to the relation of Whitaker et al. (2012); (11) galaxy reddening; (12) AGN reddening.
Values in the parenthesis refer to measurements constrained using upper limits in the FIR SED (see Fig. 5).
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