Table 4
Properties of core and BLR components of the Hβ emission line derived from parametric model fits.
| SDSS Name | za |  |
 |
 |
 |
 |
Flux HβBLR/Flux HβTot | Model |
|---|---|---|---|---|---|---|---|---|
| (km s−1) | (Å) | (Å) | (km s−1) | (Å) | ||||
| J0801+5210 | 3.257 ± 0.002 | 1000b | 2.4 |
4862 ± 1 | 6080 |
43.8 |
0.95 |
Gaussian |
| J0958+2827 | 3.434 ± 0.001 | 1000b | 2.1 |
4859 ± 1 | 5060 |
39.4 |
0.95 ± 0.05 | Gaussian |
| J1106+6400 | 2.221 |
1000b | 0.6 ± 0.2 | 4850 |
7920 |
92.0 ± 3.0 | 0.99 ± 0.01 | BPL |
| J1111+1336 | 3.490 |
1000b | 0.9 |
4871 |
7390 ± 110 | 71.0 |
0.99 |
BPL |
| J1157+2724 | 2.217 ± 0.001 | 1000b | 3.0 |
4849 ± 1 | 4200 |
56.0 ± 1.0 | 0.95 ± 0.03 | BPL |
| J1201+0116 | 3.248  |
1000b | 6.8  |
4855 ± 2 | 4670  |
55.0 ± 2.0 | 0.89  |
BPL |
| J1236+6554 | 3.424 ± 0.001 | 1000b | 1.2 ± 0.2 | 4848 ± 2 | 5330  |
64.0 ± 2.0 | 0.98  |
BPL |
| J1421+4633 | 3.454 ± 0.002 | 1000b | 2.2 ± 0.3 | 4838 ± 3 | 6480 ± 250 | 55.0  |
0.96  |
BPL |
| J1422+4417 | 3.648 ± 0.001 | 1000b | 3.0  |
4851 ± 2 | 4430  |
21.0 ± 1.0 | 0.89 ± 0.20 | Gaussian |
| J1521+5202 | 2.218 ± 0.001 | 1000b | 1.2 ± 0.1 | 4861 ± 1 | 7240  |
25.9 ± 0.5 | 0.96  |
Gaussian |
| J1538+0855 | 3.567  |
1000b | 2.1  |
4843 ± 2 | 5490  |
104.0  |
0.98 ± 0.02 | BPL |
| J2123–0050 | 2.282 ± 0.001 | 1000b | 1.2 ± 0.2 | 4850 ± 2 | 4900  |
41.1 ± 0.5 | 0.97  |
BPL |
| J2346–0016 | 3.511  |
1000b | 4.2 ± 0.9 | 4864  |
5820  |
66.0  |
0.94  |
BPL |
| J0745+4734c | 3.225 ± 0.001 | 470 ± 170 | – | 4862 ± 1 | 8600  |
85.5  |
0.98  |
BPL |
| J0900+4215c | 3.294 ± 0.001 | 300 ± 130 | 0.2  |
4861 ± 1 | 3210 ± 190 | 54.9  |
0.98 ± 0.02 | BPL |
| J1201+1206c | 3.512 ± 0.002 | 700 ± 200 | 10.2 ± 1.5 | 4865 ± 2 | 6160 ± 250 | 68.4  |
0.86 ± 0.07 | Gaussian |
| J1326-0005c | 3.303 ± 0.001 | 710 ± 170 | 0.4  |
4862 ± 1 | 3700 ± 160 | 96.3  |
0.93  |
BPL |
| J1549+1245c | 2.365 ± 0.001 | 270 ± 160 | 0.3  |
4871 ± 2 | 8340 ± 280 | 63.9  |
0.98  |
BPL |
Notes. Objects in boldface belong to the [OIII] sample (see Sect. 3.1 for details). (a) Redshifts are based on the core component of Hβ emission linefrom NIR spectroscopy. (b)Best-fit value corresponding to the maximum allowed value of FWHM (see Sect. 3.1). For these objects we only report the 
corresponding to the best-fit values. (c)WISSH QSOs with LUCI1 spectra analyzed in Bischetti et al. (2017). For these objects the redshifts are based on the core component of the [OIII] emission line.
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