Table 3
Synoptic table containing the main results for the seven high-redshift QSOs (z > 0.5; Figs. 5 and 6) identified in the present sample of INTEGRAL sources.
| Object | F [OII] | F MgII | F CIII] | F CIV | z | DL (Mpc) | E(B − V)Gal | L X |
|
|
||||||||
| IGR J02115−4407 | – | 9.5 ± 1.0 | 6.6 ± 0.6 | – | 1.212 | 9025.9 | 0.017 | 150 (20–40; I) |
| – | [10.0 ± 1.0] | [12.4 ± 01.2] | – | <220 (40–100; I) | ||||
| IGR J03564+6242 | – | 5.7 ± 0.5 | 1.4 ± 0.4 | – | 1.109 | 8086.6 | 0.910 | 2.0 (2–10; X) |
| – | [54 ± 5] | [6 ± 2] | – | 190 (20–100; I) | ||||
| IGR J09034+5329 | – | 2.9 ± 0.3 | 2.9 ± 0.3 | – | 1.253 | 9405.2 | 0.015 | 180 (20–40; I) |
| – | [3.0 ± 0.3] | [3.0 ± 0.3] | – | <270 (40–100; I) | ||||
| IGR J16388+3557 | – | – | 4.5 ± 0.5 | 1.9 ± 0.3 | 2.020 | 16 936.9 | 0.021 | 750 (20–100; I) |
| – | – | [5.0 ± 0.5] | [2.0 ± 0.3] | |||||
| IGR J21319+3619 | – | 2.4 ± 0.2 | 1.40 ± 0.15 | 2.3 ± 0.2 | 1.488 | 11 631.4 | 0.212 | <50 (20–40; I) |
| – | [3.2 ± 0.3] | [2.8 ± 0.3] | [5.7 ± 0.6] | <90 (40–100; I) | ||||
| IGR J23558−1047 | – | 4.9 ± 0.5 | – | – | 1.108 | 8077.6 | 0.034 | 0.66 (2–10; X) |
| – | [5.0 ± 0.5] | – | – | 480 (20–100; I) | ||||
|
|
||||||||
| IGR J19295−0919 | 0.65 ± 0.03 | – | – | – | 0.741 | 4918.3 | 0.292 | 50 (20–100; I) |
| [1.32 ± 0.07] | – | – | – | |||||
Notes.The upper part deals with the Type 1 QSOs of the sample, while the lower part with the single Type 2 QSO identified in this paper. Emission-line fluxes are reported both as observed and (between square brackets) corrected for the intervening Galactic absorption E(B − V)Gal along the object line of sight (from Schlegel et al. 1998). Line fluxes are in units of 10-15 erg cm-2 s-1, X-ray luminosities are in units of 1045 erg s-1, and the reference band (between round brackets) is expressed in keV. In the last column, the upper case letter indicates the satellite and/or the instrument with which the corresponding X-ray flux measurement was obtained (see text). The typical error of the redshift measurement is ±0.001 except for the spectrum of IGR J16388+3557, for which an uncertainty of ±0.005 is assumed.
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