Table D.1
Synoptic table containing the main results for the 26 low-z broad emission-line AGNs identified or observed in the present sample of 2PBC sources.
Object | F Hβ | F [OIII] | Class | z | DL (Mpc) | E(B−V)Gal | L X |
|
|||||||
2PBC J0057.2+6401 | 5 ± 1 | 2.4 ± 0.1 | Sy1.2 | 0.291 | 1499.1 | 1.252 | 2.15 (15–150)C |
[62.3 ± 5.2] | [54.7 ± 4.3] | 0.67 (0.3–10)X | |||||
2.7 (14–195)B | |||||||
2PBC J0116.5−1235 | 0.8 ± 0.1 | 7.7 ± 0.1 | Sy1.9 | 0.144 | 682.1 | 0.020 | 0.45 (15–150)C |
[0.7 ± 0.1] | [8.1 ± 0.2] | 0.32 (0.3–10)X | |||||
0.5 (14–195)B | |||||||
2PBC J0217.0−7250 | 33 ± 1 | 14.8 ± 0.1 | Sy1.2 | 0.291 | 1499.1 | 0.035 | 1.88 (15–150)C |
[35 ± 1] | [16.1 ± 0.1] | 0.77 (0.3–10)X | |||||
2PBC J0440.6−6507 | 16 ± 1 | 13.0 ± 0.1 | Sy1.5 | 0.080 | 363.3 | 0.045 | 0.11 (15–150)C |
[18 ± 1] | [15.2 ± 0.4] | 0.05 (0.3–10)X | |||||
2PBC J0550.7−2304 | 12 ± 3 | 7.0 ± 0.7 | Sy1.5 | 0.043 | 190.2 | 0.037 | 0.05 (15–150)C |
[18 ± 6] | [8.0 ± 1.5] | 0.03 (0.3–10)X | |||||
2PBC J0653.1−1227 | 7.7 ± 0.3 | 7.80 ± 0.02 | Sy1.5 | 0.234 | 1169.1 | 0.861 | 1.31 (15–150)C |
[45 ± 6] | [48.0 ± 1.5] | 0.72 (0.3–10)X | |||||
2PBC J0709.5−3538 | 38.6 ± 2.5 | 24.6 ± 0.4 | Sy1.5 | 0.030 | 131.4 | 0.401 | 0.02 (15–150)C |
[141 ± 15] | [85 ± 1] | 0.015 (0.3–10)X | |||||
2PBC J0714.6−2521 | 6.3 ± 2.5 | 13.5 ± 0.2 | Sy1.5 | 0.042 | 185.6 | 0.512 | 0.04 (15–150)C |
[34.3 ± 3.4] | [64.1 ± 0.7] | 0.004 (0.3–10)X | |||||
0.08 (14–195)B | |||||||
2PBC J0751.6+6450 | 7.5 ± 0.5 | 73.5 ± 0.8 | Sy1.9 | 0.025 | 109.1 | 0.045 | 0.009 (15–150)C |
[8.6 ± 0.5] | [84 ± 1] | 0.002 (0.3–10)X | |||||
2PBC J0757.9+0113 | 14 ± 1 | 9.3 ± 0.7 | Sy1.5 | 0.104 | 480.0 | 0.044 | 0.3 (15–150)C |
[17 ± 1] | [11 ± 1] | 0.061 (0.3–10)X | |||||
2PBC J0812.3−4003 | 3.6 ± 0.3 | 1.6 ± 0.2 | Sy1.2 | 0.076 | 344.1 | 1.632 | 0.1 (15–150)C |
[461 ± 78] | [172 ± 8] | 0.08 (0.3–10)X | |||||
0.2 (14–195)B | |||||||
2PBC J0854.3−0826 | 0.3 ± 0.1 | 2.80 ± 0.03 | Sy1.9 | 0.189 | 920.2 | 0.032 | 0.8 (15–150)C |
[0.3 ± 0.2] | [3.0 ± 0.1] | 0.16 (0.3–10)X | |||||
1.3 (14–195)B | |||||||
2PBC J1228.1−0925 | 197 ± 37 | 104 ± 6 | Sy1.5 | 0.223 | 1107.3 | 0.036 | 1.47 (15–150)C |
[183 ± 56] | [113 ± 10] | 0.13 (0.3–10)X | |||||
2PBC J1251.8−5127 | 21.8 ± 1.2 | 15.0 ± 0.1 | Sy1.5 | 0.178 | 861.0 | 0.201 | 0.9 (15–150)C |
[34 ± 5] | [26 ± 5] | 0.43 (0.3–10)X | |||||
2PBC J1419.2+6804 | – | 1.7 ± 0.2 | likely Sy1.9 | 0.077 | 348.9 | 0.035 | 0.1 (15–150)C |
[1.9 ± 0.2] | 0.05 (0.2–12)N | ||||||
2PBC J1520.2−0433 | 96 ± 1 | 98 ± 1 | Sy1.5 | 0.111 | 514.7 | 0.113 | 0.2 (15–150)C |
[134 ± 1] | [135 ± 1] | 0.11 (0.3–10)X | |||||
2PBC J1548.5−3208 | – | 22.5 ± 3.4 | likely Sy1.9 | 0.048 | 213.1 | 0.109 | 0.04 (15–150)C |
[34 ± 5] | 0.04 (0.3–10)X | ||||||
2PBC J1709.7−2349 | 63 ± 13 | 18 ± 2 | Sy1.2 | 0.036 | 158.4 | 0.536 | 0.03 (15–150)C |
[392 ± 37] | [86 ± 10] | 0.02 (0.2–12)N | |||||
2PBC J1742.0−6053 | 93.4 ± 8.4 | 109 ± 10 | Sy1.5 | 0.152 | 723.6 | 0.077 | 0.6 (15–150)C |
[110 ± 10] | [132 ± 10] | 0.47 (0.3–10)X | |||||
0.7 (14–195)B | |||||||
2PBC J1809.7−6555 | – | 6.8 ± 2.5 | Sy1.5 | 0.181 | 877.0 | 0.067 | 0.7 (15–150)C |
[9 ± 3] | 0.38 (0.3–10)X | ||||||
2PBC J2030.7−7530 | 138 ± 11 | 168 ± 10 | Sy1.5 | 0.114 | 529.6 | 0.088 | 0.3 (15–150)C |
[161 ± 17] | [213 ± 10] | 0.15 (0.3–10)X | |||||
0.4 (14–195)B | |||||||
2PBC J2045.9+8321 | 3.4 ± 0.6 | 4.5 ± 0.1 | Sy1.5 | 0.283 | 1451.9 | 0.142 | 1.26 (15–150)C |
[3.8 ± 0.6] | [6.3 ± 0.2] | 0.21 (0.3–10)X | |||||
2PBC J2048.3+3812 | 1.1 ± 0.5 | 0.4 ± 0.1 | Sy1.2 | 0.106 | 489.9 | 0.890 | 0.2 (15–150)C |
[16.3 ± 0.5] | [5.0 ± 0.1] | 0.05 (0.3–10)X | |||||
0.2 (14–195)B | |||||||
2PBC J2136.3+2003 | 27.0 ± 0.2 | 2.0 ± 0.4 | Sy1 | 0.081 | 368.1 | 0.113 | 0.1 (15–150)C |
[37 ± 1] | [5 ± 2] | 0.04 (0.3–10)X | |||||
2PBC J2155.1+6205 | 1.4 ± 0.1 | 1.2 ± 0.1 | Sy1.5 | 0.058 | 259.3 | 0.754 | 0.05 (15–150)C |
[14 ± 1] | [11 ± 1] | 0.012 (0.3–10)X | |||||
2PBC J2348.9+4153 | 7.2 ± 0.3 | 2.9 ± 0.1 | Sy1.2 | 0.183 | 887.8 | 0.112 | 0.4 (15–150)C |
[9.6 ± 0.3] | [3.9 ± 0.1] | 0.02 (0.3–10)X |
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, 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. The typical error of the redshift measurement is ±0.001.
From Swift-BAT, Cusumano et al. (2010).
From Swift-BAT, Baumgartner et al. (2013).
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