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Table 4.

Parameters derived for the sample of unobscured QSOs in this work.

Target log(Lbol) log(LIR) log(M*) SFRIR Mgas tdep fgas fAGN H2,out
[erg s−1] [L] [M] [M yr−1] [M(×109)] [Myr] [M yr−1]
J1524+4409 43.3 11.8 10.0 94 30 ± 1 290 0.73 0.07 < 660
B1608+656 ( * ) 42.8 11.2 11 25 < 2 < 70 < 0.02 0.86
J1330+1810 43.4 11.7 9.5 80 11 ± 0.2 130 0.79 0.39 < 130
J1455+1447 44.5 11.7 9.5 70 7 ± 1.5 100 0.70 0.49 < 275
J1633+3134 ( * ) 46.1 12 8.7 160 9 ± 5 60 0.91 0.67 < 170
J0924+0219 44.0 11.6 10 61 21 ± 2 900 0.84 0.33 < 210
J1650+4251 45.9 11.9 10 110 15 ± 8 130 0.52 0.43 < 317
B1152+200 ( * ) 45.9 11.2 9.9 26 < 2 < 70 < 0.20 0.83
B1600+434 ( * ) 44.7 11.4 10.4 34 < 2 < 60 < 0.06 0.07
J0806+2006 43.0 11.8 10.2 88 4 ± 2 50 0.20 0.30 < 450

Notes. Columns give the following information: bolometric luminosity, IR luminosity integrated between 8–1000 μm and corrected for AGN contamination, stellar mass, IR–derived SFR, gas mass, depletion time, gas fraction, fraction of the AGN contribution to the total IR luminosity, and 3σ upper limits on mass outflow rates. The values were corrected for magnification as listed in Table 1. ( * )Sources are classified as radio–loud QSOs (Stacey et al. 2018).

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