tokens: value (see review in Zinnecker Yorke 2007 ). Increasing or decreasing the assumed excitation temperature by 5 K changes the column density by about 30%. If CS(1–0) is optically thick, as we assume for three sources in Section 4.2 below, then our calculation would be a lower limit. Given these assumptions we used the following relation (see Miettinen ( 2012 ) for a detailed discussion of the relations below): where Here 0 is the vacuum permittivity, μ el is the permanent electric dipole moment, S is the line strength, Z rot is the rotational partition function, ν is the frequency, g K is the K-level degeneracy, g I is the reduced nuclear spin degeneracy, E u is the energy of the upper-transition state, T ex is the excitation temperature and T bg is the background temperature. The dipole moment line strength ( S ) is taken from the JPL spectral line catalog (Pickett et al. 1998 ). The partition function ( Z rot ) is a linear fit to JPL data between T = 37 and 75 K. T bg was taken to be the cosmic microwave background temperature, 2.725 K. The uncertainty in the fit amplitudes and derived column densities is dominated by our flux-calibration uncertainty. Since the relationships are linear, we estimate the uncertainty in both as 20%. Figure 1. Detection of CS emission (gray) toward a candidate YSO (N92-3) on the rim of bubble N92. The Gaussian fit to the emission is shown in black. 3.2. CS Mapping The three mapped regions are shown as boxes overlaid on the GLIMPSE 8 μ m images in Figures 2 – 4 . The maps were cropped to just those regions showing emission above 3 σ . The regions containing emission were then exported to a FITS file using custom-built IDL tools and the FITS-format datacubes were analyzed using CASA. The standard moment maps (total intensity, average velocity and velocity width) are shown next to the corresponding 8 μ m emission images in Figures 2 – 4 . Figure 2. N56: (a) The region surrounding N56 mapped in CS (white outline) overlaid on a GLIMPSE 8 μ m survey image. (b) The integrated intensity map (c) the average velocity map (d) the velocity width map. Figure 3. N65: (a) The region surrounding N65 2 mapped in CS (white outline) overlaid on a GLIMPSE 8 μ m survey image (b) the integrated intensity map (c) the average velocity map (d) the velocity width map, (e) a spectrum centered on the primary peak marked in part (b), (f) a spectrum centered on the secondary peak and the shift in velocity, marked in part (c). Figure 4. N77: (a) The region surrounding N77 1 mapped in CS (white and black outline) overlaid on a GLIMPSE 8 μ m survey image (b) the integrated intensity map (c) the average velocity map (d) the velocity width map. The three maps of CS in N56, N65, and N77 (Figures 2 – 4 ) show evidence of supersonic gas motion in areas near each YSO. N56 has a weak peak in CS that corresponds to a velocity shift of ∼2 km s −1 in the gas immediately to the north. The CS emission in N65 has a clear, strong comma-like shape. The peak
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