Table 1
Basic SDSS, ROSAT, and FIRST characteristics of the sample.
| ID | Name (ID) | z | Classa | Env.b | M i,PSF | F20 cm,peak | θ20 cmc | log R ∗ | log F0.1−2 keV | log M•d |
| [mag] | [mJy] | [sqarcsec] | [erg s-1 cm-2] | [M⊙] | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
|
|
||||||||||
| 1 | SDSS J153911.17+002600.7 | 0.265 | NLS1 | Int | –22.6 | 1.11 ± 0.14 | 3.9 × − − | 0.6 | –12.4 | 6.5 |
| 2 | SDSS J150521.92+014149.8 | 0.158 | NLS1 | –21.4 | 1.45 ± 0.14 | 1.8 × 0.5 | 0.6 | –12.7 | 6.7 | |
| 3 | SDSS J134206.57+050523.8 | 0.266 | NLS1 | –23.4 | 3.80 ± 0.14 | 1.6 × − − | 0.7 | –12.1 | 8.0 | |
| 4 | SDSS J150407.51-024816.5 | 0.217 | LINER | Cl | –22.9 | 36.60 ± 0.1 | 2.1 × 1.9 | 2.0 | –10.9 | 7.5f |
| 5 | SDSS J010649.39+010322.4 | 0.253 | LINER | Cl | –21.4 | 1.84 ± 0.15 | 6.5 × 4.7 | 1.5 | –11.6 | 8.6f |
| 6 | SDSS J074738.38+245637.3 | 0.130 | Sy1 | Comp | –22.2 | 2.47 ± 0.15 | 1.6 × − − | 0.5 | –12.5 | 7.4 |
| 7 | SDSS J030639.57+000343.1 | 0.107 | NLS1 | Int | –21.8 | 3.89 ± 0.15 | 0.8 × − − | 0.8 | –12.0 | 7.3 |
| 8 | SDSS J081026.07+234156.1 | 0.133 | NLS1 | –21.0 | 1.39 ± 0.14 | − − | 0.8 | –12.2 | 6.8 | |
| 9e | SDSS J162332.27+284128.7 | 0.377 | BL Lac | –22.5 | 2.79 ± 0.15 | − − | 1.4 | –12.5 | – | |
| 10 | SDSS J080322.48+433307.1 | 0.276 | Sy1 | –22.4 | 5.25 ± 0.14 | 2.3 × 1.0 | 1.4 | –12.1 | 7.9 | |
| 11e | SDSS J080644.41+484149.2 | 0.370 | Sy1 | –23.8 | 43.31 ± 0.14 | 2.7 × 1.9 | 1.9 | –11.9 | 9.4 | |
| 12 | SDSS J092710.60+532731.6 | 0.201 | passive | Cl | –21.1 | 3.58 ± 0.22 | 2.6 × − − | 1.8 | –11.8 | – |
| 13 | SDSS J134420.87+663717.6 | 0.128 | Sy1 | Int | –22.9 | 2.70 ± 0.40g | 67.2 × 53.4 | 0.2 | –11.9 | 7.6 |
Notes.
Spectral classification based on SDSS spectrum (for NLS1 see Zhou et al. 2006; Whalen et al. 2006).
Int: interacting, Cl: galaxy cluster or group, Comp: companion galaxy as judged from the SDSS images.
The FIRST catalog lists the deconvolved major and minor. Gaussian beam components. Not all deconvolved components are available.
Black-hole masses from literature: 990515 from Wu & Liu (2004). The remaining black-hole masses are from Greene & Ho (2007) unless otherwise noted.
Using M• − σ relation and [SII] line width as tracer of the bulge stellar velocity dispersion (cf., Komossa & Xu 2007).
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