Table 4
Position angle and inclination of the host galaxies, the spectral indices, and the disk maser properties.
| Spectral indices | Galaxy scale | This work | Maser disk | ||||||||||
| Galaxy |
|
|
|
|
PA | Inclination | PA | PA | Inclination | R in | R out | M SMBH | Ref. |
| (°) | (°) | (°) | (°) | (°) | (pc) | (pc) | (107M⊙) | ||||||
|
|
|||||||||||||
| ESO558-G009 | 0.88 ± 0.02 | ... | 1.11 ± 0.94 | 0.76 ± 0.22 | 8.0 | 81.2 | 155 ± 33 | 256 | 98 | 0.20 | 0.47 | 1.7 | 1 |
| IC 0485 | ... | ... | ... | ... | 153.9 | 90.0 | ... | ... | ... | ... | ... | ... | ... |
| IC 2560 | 0.88 ± 0.02 | ... | 1.31 ± 0.88 | 0.88 ± 0.21 | 45.7 | 65.6 | 25 ± 11 | ... | ... | ... | ... | ... | ... |
| J0126-0417 | ... | ... | –2.06 ± 2.58 | 0.87 ± 2.34 | 100.0 | ... | 146 ± 86 | ... | ... | ... | ... | ... | ... |
| J0350-0127 | ... | ... | ... | –2.63 ± 4.32 | 155.0 | ... | 134.6 ± 8.1 | ... | ... | ... | ... | ... | ... |
| J0437+2456 | ... | ... | ... | ... | ... | ... | ... | 20 | 81 | 0.04 | 0.13 | 0.29 | 1 |
| J0437+6637 | 1.12 ± 0.08 | ... | ... | –0.52 ± 1.58 | 117.0 | 53.0 | ... | ... | ... | ... | ... | ... | ... |
| J0836+3327 | ... | ... | ... | ... | 51.6 | 57.7 | ... | ... | ... | ... | ... | ... | ... |
| J1658+3923 | ... | 0.95 ± 0.07 | ... | 2.36 ± 2.77 | 104.3 | 90.0 | 81.4 ± 4.7 | ... | ... | ... | ... | ... | ... |
| Mrk 0001 | 0.93 ± 0.01 | ... | 1.06 ± 0.30 | 0.93 ± 0.06 | 77.5 | 60.8 | 119.6 ± 2.1 | ... | ... | 0.70 | 1.10 | 1.0 | 2 |
| Mrk 0078 | 0.96 ± 0.02 | ... | 0.82 ± 0.58 | 1.01 ± 0.17 | 87.0 | 49.5 | 81 ± 10 | ... | ... | ... | ... | ... | ... |
| Mrk 1029 | 0.73 ± 0.04 | 0.61 ± 0.04 | ... | 0.72 ± 2.37 | 73.5 | 45.9 | 59 ± 11 | 218 | 79 | 0.23 | 0.45 | 0.19 | 1 |
| Mrk 1210 | 0.79 ± 0.01 | ... | 0.03 ± 0.08 | –0.12 ± 0.93 | 160.0 | 15.6 | 179 ± 83 | ... | ... | 0.62 | 1.06 | 14.6 | 2 |
| Mrk 1419 | 0.96 ± 0.06 | 0.84 ± 0.05 | 3.0 ± 2.72 | –0.67 ± 1.92 | 40.2 | 41.5 | 117 ± 84 | 229 | 89 | 0.13 | 0.37 | 1.16 | 3 |
| NGC 0591 | 0.98 ± 0.02 | ... | 2.47 ± 1.49 | 1.31 ± 1.60 | 0.2 | 40.3 | 153.3 ± 2.8 | ... | ... | ... | ... | ... | ... |
| NGC 1194 | ... | 0.10 ± 0.03 | –0.20 ± 0.63 | –0.25 ± 0.27 | 139.3 | 71.1 | 75 ± 82 | 157 | 85 | 0.54 | 1.33 | 6.5 | 3 |
| NGC 2273 | 1.00 ± 0.04 | ... | 0.55 ± 1.13 | 1.86 ± 1.15 | 63.3 | 57.4 | 82.8 ± 2.8 | 153 | 84 | 0.028 | 0.084 | 0.75 | 3 |
| NGC 2979 | 1.19 ± 0.04 | ... | 0.91 ± 1.94 | 0.65 ± 0.92 | 21.0 | 57.5 | 138 ± 51 | ... | ... | ... | ... | ... | ... |
| NGC 3393 | 0.87 ± 0.03 | ... | 1.02 ± 0.26 | 2.10 ± 3.18 | 12.8 | 30.9 | 165 ± 50 | ... | ... | ... | ... | ... | ... |
| NGC 4388 | 0.84 ± 0.02 | 0.52 ± 0.02 | –0.10 ± 0.22 | 3.36 ± 3.58 | 91.1 | 90.0 | 24 ± 54 | 107 | ... | 0.24 | 0.29 | 0.84 | 3 |
| NGC 5495 | 1.44 ± 0.06 | ... | ... | 0.43 ± 1.38 | 44.5 | 34.7 | 167 ± 24 | 176 | 95 | 0.10 | 0.30 | 1.1 | 1 |
| NGC 5728 | 1.09 ± 0.02 | ... | –1.26 ± 0.37 | –1.53 ± 0.17 | 14.5 | 59.1 | ... | ... | ... | 0.27 | 0.55 | 2.3 | 2 |
| UGC 3193 | 0.47 ± 0.02 | ... | 2.08 ± 1.12 | 0.96 ± 1.92 | 177.4 | 76.1 | 167.2 ± 4 | ... | ... | 0.16 | 2.12 | 0.8 | 2 |
| UGC 3789 | 1.40 ± 0.04 | 1.34 ± 0.03 | 1.89 ± 4.26 | 2.83 ± 1.76 | 166.0 | 43.2 | 117 ± 22 | 41 | >88 | 0.084 | 0.30 | 1.04 | 3 |
Notes. Column 1: source name. Column 2: spectral indices between NVSS 1.4 GHz and 33 GHz, with uncertainties. Column 3: spectral indices between FIRST 1.4 GHz and 33 GHz, with uncertainties. Columns 4 and 5: spectral indices between 30 GHz and 36 GHz from our 8 GHz bandwidth observations, first by splitting the data and second by setting the Taylor coefficients as two in CASA (see Sect. 5.2). Columns 6 and 7: large scale position angle and inclination (from HyperLeda database). Column 8: position angle of the 33 GHz continuum component with formal errors, obtained from Gaussian fits to a region containing all the significant emission. Columns 9 and 10: maser disk position angle and inclination. Columns 11 and 12: maser disk inner and outer radii in pc. Column 13: black hole mass. Column 14: references for disk maser radii and MSMBH: (1) Gao et al. (2017); (2) Braatz et al. (2015); (3) Kuo et al. (2011).
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