Table 1
Coordinates, line-of-sight velocities, and peak flux densities of the background quasars and the strongest maser spots.
| Source | RA (J2000) | Dec (J2000) | V LSR | F Peak | rms | Cloud association |
| [hh mm ss.ssss] | [ dd ′′ ””.”””] | [km s-1] | [Jy beam-1] | [Jy beam-1] | ||
|
|
||||||
| J1808−1822 | 18 08 55.5150 | −18 22 53.383 | 0.012 | 0.001 | ||
| J1809−1520 | 18 09 10.2094 | −15 20 09.699 | 0.022 | 0.001 | ||
| J1825−1718 | 18 25 36.5323 | −17 18 49.848 | 0.096 | 0.001 | ||
| G012.68−0.18 | 18 13 54.7457 | −18 01 46.588 | 59.3 | 132.5 | 0.001 | W33 B |
| G012.81−0.19 | 18 14 13.8283 | −17 55 21.035 | 34.1/−1.4 | 1.0/0.2 | 0.018/0.007 | W33 Main |
| G012.90−0.24 | 18 14 34.4366 | −17 51 51.891 | 34.9 | 18.3 | 0.081 | W33 A |
| G012.90−0.26 | 18 14 39.5714 | −17 52 00.382 | 37.0 | 3.0 | 0.016 | W33 A |
| G012.88+0.48 | 18 11 51.4939 | −17 31 28.911 | 29.4 | 23.3 | 0.133 | |
Notes.Columns 2, 3, and 4 list the coordinates and line-of-sight velocities of the background quasars and the maser spots that were used for parallax fitting. The peak flux densities of the background quasars and the strongest maser spots and the rms of the reference channel images, obtained from epoch 2011 May 21, are listed in Cols. 5 and 6. The last column shows with which cloud the masers in the W33 complex are associated.
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