Table 2
Synoptic table containing the main results for the 8 low-z broad emission-line AGNs (Fig. 4) identified or observed in the present sample of INTEGRAL sources.
| Object | FHα | FHβ | F [OIII] | Class | z | DL (Mpc) | E(B − V)Gal | LX |
|
|
||||||||
| IGR J03184−0014 | * | <0.05 | 0.11 ± 0.02 | Sy1.9 | 0.330 | 1867.2 | 0.063 | 6.3 (2–10; X) |
| * | [< 0.07] | [0.14 ± 0.02] | 1200 (20–40; I) | |||||
| < 880 (40–100; I) | ||||||||
| IGR J06523+5334 | – | 10.0 ± 1.0 | 3.6 ± 0.3 | Sy1.2 | 0.301 | 1678.6 | 0.062 | 5.4 (0.1–2.4; R) |
| – | [11.8 ± 1.2] | [4.2 ± 0.4] | 5.7 (2–10; X) | |||||
| 740 (20–40; I) | ||||||||
| <870 (40–100; I) | ||||||||
| IGR J13466+1921 | * | 39 ± 4 | 14.6 ± 1.0 | Sy1.2 | 0.085 | 417.1 | 0.024 | 0.73 (0.1–2.4; R) |
| * | [42 ± 4] | [15.5 ± 1.1] | 33 (17–60; I) | |||||
| 23 (14–195; B) | ||||||||
| IGR J14385+8553 | * | 11.5 ± 1.7 | 7.4 ± 0.7 | Sy1.5 | 0.081 | 396.4 | 0.191 | 6.9 (0.2–12; N) |
| * | [20 ± 3] | [12.4 ± 1.2] | < 10 (20–40; I) | |||||
| < 21 (40–100; I) | ||||||||
| IGR J16443+0131 | – | 1.2 ± 0.2 | 1.60 ± 0.16 | Sy1.5 | 0.342 | 1946.5 | 0.071 | 12 (2–10; X) |
| – | [1.8 ± 0.3] | [1.9 ± 0.2] | 340 (20–40; I) | |||||
| < 430 (40–100; I) | ||||||||
| 1RXS J175252.0 − 053210 | * | 20 ± 2 | 6.0 ± 1.0 | Sy1.2 | 0.136 | 690.2 | 0.995 | 2.7 (0.1–2.4; R) |
| * | [370 ± 40] | [100 ± 20] | 57 (20–100; I) | |||||
| IGR J19491 − 1035 | * | 220 ± 20 | 510 ± 50 | Sy1.2 | 0.0240 | 112.7 | 0.238 | 1.2 (2–10; X) |
| * | [480 ± 50] | [1000 ± 100] | 1.7 (17–60; I) | |||||
| IGR J20450+7530 | * | 11 ± 2 | < 3 | Sy1 | 0.095 | 469.3 | 0.382 | 0.84 (2–10; X) |
| * | [35 ± 8] | [< 10] | 53 (20–40; I) | |||||
| <42 (40–100; I) | ||||||||
Notes. 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, whereas X-ray luminosities are in units of 1043 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 in the redshift measurement is ± 0.001 but for the 6dFGS spectrum, for which an uncertainty of ± 0.0003 can be assumed.
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