Table 1.
VLBA observations.
| Galaxy | Right ascension/declination | Fringe finder | Calibrator | RA/Dec |
|---|---|---|---|---|
| uncertainty | ||||
| J2000 | (arcsec) | |||
| Mrk 0001/NGC 0449 |  |
2007+777/3C84 | J0137+3122/J0112+3208 | 0.02/0.02 |
| J0126–0417 |  |
2007+777/3C84 | J0123–0348 | 0.04/0.04 |
| NGC 0591/Mrk 1157 |  |
2007+777/3C84 | J0137+3309 | 0.10/0.1 |
| Mrk 1029 |  |
2007+777/ DA193 | J0215+0524 | 0.18/0.18 |
| NGC 1194 |  |
2007+777/ DA193 | J0259–0019 | 0.03 /0.03 |
| J0350–0127 |  |
2007+777/DA193 | J0351–0301 | 0.15/0.15 |
| J0437+6637 |  |
2007+777/DA193 | J0449+6332/J0429+6710 | 0.12/0.12 |
| UGC 3193 |  |
2007+777/DA193 | J0453+0128 | 0.11/0.29 |
| NGC 2273 |  |
2007+777/DA193 | J0638+5933 | 0.28/0.27 |
| UGC 3789 |  |
3C84/4C39.25 | J0737+5941 | 0.08/0.08 |
| Mrk 0078 |  |
3C84/4C39.25 | J0737+6430 | 0.03/0.03 |
| Mrk 1210/Phoenix |  |
DA193/4C39.25/3C345 | J0803+0421 | 0.03/0.03 |
| Mrk 1419/NGC 2960 |  |
3C84/4C39.25 | J0930+0034 | 0.14/0.13 |
| NGC 4388 |  |
DA193/4C39.25/3C345 | J1225+1253 | 0.02/0.02 |
| NGC5765b |  |
DA193/4C39.25/3C345 | J1458+0416 | 1.25/1.25 |
| UGC 9639/Mrk 0834 |  |
4C39.25/2007+777 | J1459+4442 | 0.5/0.5 |
| NGC 6264 |  |
4C39.25/2007+777 | J1659+2629 | 0.5/0.5 |
| NGC 6323 |  |
4C39.25/2007+777 | J1707+4536 | 0.5/0.5 |
| Mrk 0001 |  |
3C84 | J0119+3210 | 0.001/0.001 |
| UGC 3193 |  |
3C84 | J0459+0229 | 0.001/0.001 |
| Mrk 1210 |  |
4C39.25/3C84 | J0803+0421 | 0.0008/0.002 |
| Mrk 1419 |  |
4C39.25/3C84 | J0930+0034 | 0.001/0.001 |
Notes. Column 1: name of galaxy. The sources in bold hold clean maser disks (see Sect. 2). Column 2: J2000 right ascension and declination. For NGC 5765b, NGC 6323, NGC 6264, and UGC 9639 the coordinates are taken from NED, and for the remaining sources the coordinates are from Kamali et al. (2017). Column 3: fringe finders. Column 4: phase calibrators. Column 5: right ascension and declination uncertainties. The second VLBA observations are presented in the lower part. The pointing coordinates for the second observations were taken from the first run of VLBA observations.
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