| Ranged | Modified julian date | ||||||||||
| ID | Epochs | Line(s)c | (km s-1) | 54637 | 54646 | 54665 | 54671 | 54692 | 54695 | 54713 | Notes |
| W2a | 5 | Pa11-16, He I | -51.0 - -14.1 | - | -49.3 | -56.2 | -33.9 | -54.1 | - | -18.6 | Cand. binary |
| W8b | 5 | Pa11-16 | -61.6 - -40.3 | - | -61.6 | -49.9 | -40.3 | -47.4 | - | -50.7 | |
| W21 | 5 | Pa11-14 | -57.4 - -31.1 | - | -57.4 | -35.0 | -43.1 | -55.1 | - | -31.1 | |
| W23a | 5 | Pa11-16 | -62.4 - -42.9 | - | -47.9 | -55.6 | -56.6 | -42.9 | - | -62.4 | |
| W43a | 5 | Pa11-14 | -137.9 - +8.1 | - | -109.7 | -123.1 | +8.1 | -38.8 | - | -137.9 | Binary |
| W55e | 7 | Pa11-14 | -43.1 | -49.9 | -55.4 | -45.4 | -43.8 | -53.9 | -55.5 | ||
| W60e | 5 | Pa11-14 | - | -40.5 | -48.3 | -45.8 | -48.2 | - | -37.7 | ||
| W71 | 7 | Pa11-16, He I | -61.9 - -38.7 | -57.3 | -52.9 | -39.4 | -47.3 | -44.8 | -46.4 | -62.4 | |
| W78 | 5 | Pa11-15 | - | -46.7 | -46.4 | -41.3 | -39.9 | - | -49.5 | Puls. BSG | |
| W84 | 5 | Pa11-13 | - | -53.8 | -59.0 | -54.9 | -54.6 | - | -55.8 | ||
| W234e | 7 | Pa11-13 | -67.0 - -30.8 | -67.0 | -66.9 | -66.2 | -30.8 | -46.4 | -56.9 | -32.7 | Prob. binary |
| W239f | 5 | C III  8664
|
-81.6 - +14.1 | - | -26.9 | -10.7 | +14.1 | -49.7 | - | -81.6 | Wolf-Rayet |
| W243g | 5 | N I (1 & 8) | -28.8 - -20.4 | - | -22.7 | -20.4 | -27.7 | -28.3 | - | -28.8 | Puls. LBV |
| W265g | 5 | N I (1 & 8) | N/Ah | - | -47.6 | -36.8 | -36.0 | -37.9 | - | -49.8 | Puls. YHG |
| W373e | 5 | Pa11-14 | - | -50.8 | -50.9 | -45.8 | -53.8 | - | -52.9 | ||
| W3002e | 5 | Pa11-14 | - | -36.1 | -38.6 | -47.7 | -39.4 | - | -43.0 | ||
| W3003e | 5 | Pa11-14 | -54.6 - -4.4 | - | -4.4 | -43.7 | -54.6 | -22.0 | - | -10.6 | Prob. binary |
| W3004e | 5 | Pa11-14 | -62.3 - -35.5 | - | -47.9 | -62.3 | -54.3 | -35.5 | - | -46.0 | |
| W3005e | 5 | Pa11-13 | - | -43.9 | -46.9 | -52.4 | -51.6 | - | -49.9 | ||
a
Errors are not listed, but are 
4 km s-1
for the OB supergiants, 3 km s-1
for the two cool hypergiants and 
10 km s-1
for the Wolf-Rayet W239; b the
broad, weak Paschen-series absorption lines in W30a precluded
accurate RV measurement, while RV measurements for the eclipsing binary
W13 discussed in Sect. 3.1
will appear in a forthcoming paper; c the
line(s) used for RV measurement; d the
range of measured radial velocities is given for targets in which
statistically-significant variations are detected; e displays
a distorted Pa-16 line due to blending with C III8500 and a
weak Pa-15 line that yield discrepant radial velocities compared to the
other Paschen-series lines; f the
C III 8500
and C III 8664 lines seen in the
spectrum of the Wolf-Rayet W239 give discrepant RV
measurements (
25 km s-1;
see discussion in Sect. 3.2).
The value for C III 8664 is given here; g the
cool hypergiants W243 and W265 display rich
absorption-line spectra, with a large number of potential lines
suitable for RV measurement. The values given here are the average of
nine of the strongest unblended N I absorption lines from
multiplets 1 and 8 (Moore
1945). Note that in both objects species-to-species variation
in RV is seen, with clear evidence of velocity stratification in the
photosphere of W265 (see discussion in text); h
The range of observed radial velocities in W265 varies
depending on the absorption line used to make the measurement. See
Sect. 3.4.
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