Table A.1.
Properties of the WISSH quasars and the additional sources from the C17 sample.
| Name | z (a) | vCIV (b) | L2500 Å (c) | νL6μm (c) | Lbol | λEdd (d) |
|---|---|---|---|---|---|---|
| (SDSS) | (km s−1) | log(erg s−1 Hz−1) | log(erg s−1) | log(erg s−1) | ||
| WISSH sample | ||||||
| J0801+5210 | 3.257 |
 |
32.3 | 47.2 | 47.8 (c) | 0.7 |
| J0900+4215 (e) | 3.294 |
 |
32.4 | 47.3 | 48.0 (c) | 3.1 |
| J0958+2827 | 3.434 |
 |
32.1 | 46.9 | 47.6 (c) | 0.8 |
| J1106+6400 | 2.221 |
 |
32.3 | 47.1 | 47.8 (c) | 0.5 |
| J1111+1336 | 3.490 |
 |
32.2 | 47.1 | 47.7 (c) | 0.5 |
| J1201+0116 | 3.248 |
 |
32.1 | 47.1 | 47.6 (c) | 1.0 |
| J1236+6554 | 3.424 |
 |
32.2 | 47.0 | 47.7 (c) | 0.8 |
| J1326-0005 | 3.303 |
 |
32.2 | 47.1 | 47.8 (c) | 2.1 |
| J1421+4633 | 3.454 |
 |
32.2 | 47.0 | 47.7 (c) | 0.6 |
| J1441+0454 (e) | 2.075 |
 (f) |
31.9 | 46.8 | 47.3 (c) | 0.7 (f) |
| J1521+5202 | 2.218 |
 |
32.4 | 47.2 | 47.9 (c) | 0.7 |
| J1549+1245 (e) | 2.365 |
 |
32.3 | 47.1 | 47.8 (c) | 0.4 |
| J2123-0050 | 2.282 |
 |
32.2 | 47.0 | 47.7 (c) | 1.1 |
| C17 sample | ||||||
| J0304-0008 | 3.296 | −583 ± 16 | – | – | 47.4 (g) | 1.6 |
| J0929+2825 | 3.407 | −2080 ± 264 | – | – | 47.6 (g) | 0.4 |
| J0942+0422 | 3.284 | −860 ± 117 | – | – | 47.8 (g) | 1.5 |
| J1426+6025 | 3.197 | −3503 ± 45 | – | – | 48.0 (g) | 0.5 |
| J1621-0042 | 3.729 | −713 ± 124 | – | – | 47.9 (g) | 1.0 |
Notes.
For the WISSH quasars, the redshifts were derived from the narrow component of the Hβ emission line (see Bischetti et al. 2017; Vietri et al. 2018);
Peak of the CIV emission line in units of km s−1 relative to the Hβ emission line as reported by Vietri et al. (2018) and C17 for the WISSH and C17 samples, respectively. It is important to notice that Vietri et al. (2018) and C17 adopt slightly different definitions of vCIV. Vietri et al. (2018) estimated vCIV to be relative to the wavelength of the peak of the modelled CIV line, while C17 used the wavelength that bisects the cumulative flux distribution of the modelled line as a reference;
Extinction-corrected derived from spectral energy distribution modelling (Duras et al. 2017; Duras et al. in prep.);
From Vietri et al. (2018) and C17;
From 5100 Å assuming a bolometric correction from Runnoe et al. (2012).
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