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tokens: on the age and wind velocity of the driving W-R star and also on the initial density of the surrounding molecular cloud. Figure 6 (b) shows the 13 CO spectrum of the G27 region. The molecular cloud hosting this particular region is located at a velocity range of 88–95 km s −1 (see Dewangan et al. 2016 ). The spectrum is constructed by combining all 13 CO emission within a 45′′ diameter (i.e., the beam size of the GRS data) centered on the W-R star. Two emission peaks are clearly visible in the spectrum. We estimated the kinematic distance corresponding to the velocity of the trough ( v LSR ∼ 92.0 km s −1 ; see Figure 6 (b)) using the “Kinematic Distance Calculation Tool” 10 10 http://www.treywenger.com/kd/index.php of Wenger et al. ( 2018 ), which evaluates a Monte Carlo kinematic distance adopting the solar Galactocentric distance of 8.31 ± 0.16 kpc (Reid et al. 2014 ). The calculation yields a near kinematic distance ( d near ) of 5.2 ± 0.6 kpc. The spectrophotometric distance of the W-R star associated with the reference region is 5.2 ± 0.5 kpc (Dewangan et al. 2016 , see also Table 1 ). A well-matched distance of a W-R star with the velocity of the trough in the 13 CO spectrum implies a physical association of the W-R star with this particular molecular cloud, and more precisely, with the trough at a v LSR of 92.0 km s −1 . The 13 CO spectrum (Figure 6 (b)) also exhibits two emission peaks corresponding to blueshifted (90.2 km s −1 ) and redshifted (93.2 km s −1 ) parts of the cloud, possibly dispersed by the energetics of the W-R star. Evidence of the influence of the W-R star was already found for this region by Dewangan et al. ( 2016 ). Hence, any region with a double-peaked 13 CO spectrum toward the position of a W-R star exhibiting a trough might be explored for any impact of W-R stars on their parent molecular clouds. The 13 CO spectra for our selected regions are constructed by integrating all emission within a 45′′ diameter, centered on the positions of the W-R stars (Figure 7 ) for velocity ranges where dust clumps are generally identified (see Section 2 ). All spectra show similar double-peaked spectral signatures as seen in the spectrum toward the reference region (see Figure 6 (b)) except for the G34 region. The spectrum for the G34 region constructed for a 45′′ diameter shows three peaks (see Figure 7 (c)). However, the highest velocity peak (at v LSR of ∼61 km s −1 ) dissolves when the spectrum is produced for a 240′′ diameter. This implies a small component of molecular gas along the sight line to the W-R star, which is peaking at a v LSR of 61 km s −1 . The emission peaks, troughs, and corresponding velocities are marked and labeled in Figure 7 . Figure 7. 13 CO spectra of our five selected regions (a) G15, (b) G24, (c) G34, (d) G35, and (e) G51. The spectra were constructed following the same procedure as that applied to the reference region, G27 (see the caption of Figure 6 ). Velocities corresponding to the blue- and