Table 3
The sub-mm z ~ 2 QSO sample: luminosities, black hole masses, and Eddington rates.
| Name | log Lbol | log LFIR | log MBH (Hα) | log MBH (L5100) | log L/LEdd |
| (erg s-1) | (L⊙) | (M⊙) | (M⊙) | ||
| (1) | (2) | (3) | (4) | (5) | (6) |
|
|
|||||
| LBQS B0018-0220 | 47.30 ± 0.04 | 13.17 ± 0.76 | 8.62 ± 0.14 | 9.07 ± 0.10 | 0.06 ± 0.06 |
| HS B0035+4405 | 47.58 ± 0.04 | 12.90 ± 0.84 | 9.17 ± 0.14 | 9.29 ± 0.09 | 0.08 ± 0.10 |
| [ HB89 ] 0933+733 | 47.57 ± 0.04 | 12.93 ± 0.80 | 9.29 ± 0.14 | 9.45 ± 0.09 | −0.10 ± 0.09 |
| HS B1049+4033 | 47.39 ± 0.04 | 12.88 ± 0.79 | 9.06 ± 0.14 | 9.33 ± 0.09 | −0.14 ± 0.07 |
| HS B1103+6416 | 47.59 ± 0.04 | 12.96 ± 0.83 | 9.52 ± 0.14 | 9.73 ± 0.08 | −0.36 ± 0.08 |
| HS B1141+4201 | 47.44 ± 0.04 | 12.88 ± 0.84 | 9.23 ± 0.14 | 9.48 ± 0.09 | −0.23 ± 0.08 |
| SBS B1408+567 | 47.16 ± 0.04 | 13.37 ± 0.65 | 8.79 ± 0.14 | 9.06 ± 0.09 | −0.06 ± 0.08 |
| SBS B1542+541 | 47.40 ± 0.04 | 12.94 ± 0.84 | 9.87 ± 0.14 | 10.00 ± 0.08 | −0.79 ± 0.09 |
| HS B1611+4719 | 47.16 ± 0.04 | 13.02 ± 0.74 | 8.87 ± 0.14 | 9.12 ± 0.09 | −0.12 ± 0.08 |
| J164914.9+530316 | 47.32 ± 0.04 | 13.03 ± 0.76 | 8.88 ± 0.14 | 9.13 ± 0.09 | 0.02 ± 0.08 |
Notes. Columns are: (1) QSO name; (2) Log of the bolometric luminosity and its 1σ error; (3) Log of the FIR luminosity (calculated from the sub-mm flux following McMahon et al. (1999) with β = 1.5 and Td = 40 K) and its 1σ error (which reflects only on the error of the submm flux). (4) Log of the black hole mass as estimated from LHα and FWHMHα, and its 1σ error (see text); (5) Log of the black hole mass as estimated from L5100 and FWHMHα, and its 1σ error (see text); (6) Log of the accretion rate as a fraction of the Eddington accretion Rate.The flux to luminosity conversion was made using a luminosity distance derived within the standard cosmology with parameters listed in Sect. 1. The errors listed in this table reflect measurement errors and some of the declared errors in the scaling relationships used. More realistically, the scaling relations used to estimate black hole masses are expected to have errors of a factor of a few.
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