¹²CO and ¹³CO(1-0) spectra are shown in Fig. 1 (no line components have been subtracted; see below). The emission is shown on the same velocity scale for the eight sources towards the position with strong ¹²CO line wing emission. For most sources this is at the IRAS PSC position (offset (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ )). An exception is WB89 1173 (offset (40 $^{\prime \prime }$ , 0 $^{\prime \prime }$ )). The ¹²CO line profiles are much broader than those of ¹³CO, and extend over a large range in velocity (up to 25 km $\,$ s^-1 for WB89 1187), which is typical of outflow emission. In some of the ¹³CO spectra wing emission is present as well. For three sources (WB89 1135, 1181, and 1187) the spectra also show a dip in the ¹²CO emission at the velocity of the ¹³CO peak, possibly a sign of self absorption, although for the latter source we conclude that the dip is caused by two partly overlapping velocity components (see further). A secondary maximum at +7 km $\,$ s^-1 is visible in the spectrum towards WB89 1189, and is also due to another component, which is much stronger to the SE of the IRAS position.

In the maps of WB89 1099, 1135, 1173, 1187, 1189 and 1275, we detected one or more other emission components (especially in ¹²CO), the velocity of which is often near that of the main component, hence causing confusion in identifying the outflowing gas. These components are identified at positions away from the center of the flows (where the main component of the emission tends to be narrower). Based on Gaussian fits made to the spectra at those positions, confusing components could also be subtracted from spectra taken towards the center of the outflows, where they generally almost disappear in the broad ¹²CO profile. In some cases some weak residual emission may be left in the central, broad profiles, because the velocity of the confusing emission is too close to that of the main component, and an unambiguous Gaussian fit could not always be made.

$\begin{figure}\resizebox{\hsize}{!}{\includegraphics{h1645_fig2.eps}} \end{figure}$

Figure 2: The distribution of the ¹²CO(1-0) emission of velocity components which are judged not to be associated with the outflows. The velocities of the unrelated components are indicated. Contour levels are 2 to 22 K km s^-1 in steps of 2 K km s^-1, except for WB89 1099 and 1135 where start value and contour interval are 1 K km s^-1. Observed positions are indicated as crosses, the IRAS PSC position as filled circles

The distribution of the velocity components that are unrelated to the outflows (and that were subtracted) is shown in Fig. 2. It is seen that these emission components do not have a maximum near the IRAS PSC positions, and for some sources they are only detected at the edge of the observed region. A few of those velocity components such as for WB89 1099 (4 km $\,$ s^-1), 1187 (10 km $\,$ s^-1), and 1189 (7 km $\,$ s^-1) are rather extended.

$\begin{figure}\resizebox{\hsize}{!}{\includegraphics{h1645_fig3.eps}} \end{figure}$

Figure 3: The distribution of the ¹²CO(1-0) peak $T_{\rm {A}}^*$ towards eight sources, after subtracting emission components that are unrelated to the outflow. Contour levels are 2 to 26 K in steps of 2 K. Contours at 6 and 16 K are dotted and those of 20 K and higher are white. Observed positions are indicated as crosses, the IRAS PSC position as filled circles

To investigate whether cloud temperatures have a maximum near embedded heating (IRAS) sources, we have plotted in Fig. 3 the distribution of peak temperature for the sources mapped in ¹²CO(1-0), after subtraction of unrelated (to the outflow) emission components. Towards six of the sources the maximum is within about 20 $^{\prime \prime }$ of the IRAS PSC position. Towards the two remaining sources the displacement of the peak of the temperature distribution appears to be significant (i.e. not due to noise) compared to the beamsize, and amounts up to about 59 $^{\prime \prime }$ for WB89 1173 and 52 $^{\prime \prime }$ for WB89 1275 (resp. 0.14 and 1.6 pc). The distribution of large-scale CO emission associated with our sample of sources can be seen in the low resolution maps of Murphy & May ([1991]), except for WB89 1086, 1135, and 1275, the velocities of which are outside the range discussed by these authors.

$\begin{figure}\resizebox{\hsize}{!}{\includegraphics{h1645_fig4.eps}} \end{figure}$

Figure 4: The distribution of the integrated blue (left) and red (right) ¹²CO(1-0) line wing emission towards eight sources. The lowest contour level and the contour interval are 1 K km s^-1, except for WB89 1173, 1181, and 1187 where they are 2 K km s^-1. Observed positions are indicated as crosses, the IRAS PSC position as filled circles. The arrows indicate for WB89 1173, 1181, and 1189 the direction of H₂ jets detected by Massi et al. ([1997])

To study the outflowing gas, one integrates the "cleaned'' (i.e. after subtracting the unrelated components) line profiles over some velocity interval, the outer limit $V_{\rm {max}}$ of which is taken for our sample of sources as the velocity where the emission first becomes less than 0 K, and the inner limit $V_{\rm {min}}$ of which is taken at some distance from the line center in velocity space. The precise location of the inner velocity limit is determined by the shape and width of the line profile of the underlying quiescent gas. For the inner limit we have taken the velocity of the peak of the line profile, plus (for the red wing) or minus (blue wing) the half widths at half maximum intensity of the line profile: $\Delta v_{\rm {blue}}$ or $\Delta v_{\rm {red}}$ . We took the smallest of both half widths, $\Delta v_{\rm {q}}=\min(\Delta v_{\rm {blue}}$ , $\Delta v_{\rm {red}}$ ), and to correct the wing emission for the contribution of the quiescent gas, we subtracted at each channel between $V_{\rm {min}}$ and $V_{\rm {max}}$ the contribution of a Gaussian with a width equal to 2 $\times \Delta v_{\rm {q}}$ , and a velocity equal to the velocity of the peak temperature of the line profile. The resulting distribution of the red and blue wing emission is shown in Fig. 4.

Except for WB89 1173 (blue wing), the outflow emission (i.e. ¹²CO) is centered near (i.e. within one beam of) the IRAS (0, 0) position, and moderately extended compared to the 46 $^{\prime \prime }$ 115 GHz beam. For some sources the wing emission is very small (and possibly nonexistent), such as the blue and red wing of WB89 1086, and the blue wings of WB89 1099 and WB89 1189 (although for the latter source there is clearly some weak wing emission present in Fig. 1). For the other sources with substantial wing emission one can distinguish sources where the distribution of blue and red wing emission is similar, such as WB89 1173, and sources where the emission is bipolar (e.g. WB89 1187, where the blue (red) wing has a maximum east (west) of the IRAS PSC position). Also for WB89 1135 there appears such a difference in the location of the wing emission. Towards WB89 1181 the red wing is well defined with a peak east of the PSC position, but the situation for the blue wing is less clear.

We have derived parameters of the outflows, following Snell et al. ([1984]), and assuming $T_{\rm {ex}}=20$ K, $\tau=1$ , and LTE (see Wouterloot et al. [1989]; Shepherd & Churchwell [1996]). The results are listed in Table 3. Column 1 gives the source name. Column 3 the largest velocity range of the wing emission, reached at the position listed in Col. 4. We derived the velocity range from the velocity at which the emission first reaches the 0 K level, and distinguish between the blue and red wings and the total spectrum. The blue and red wings can show their largest range at different positions and therefore the position with the largest total velocity range can also differ from that of the largest blue or red range. In Col. 5 is the median value of the line width of the subtracted line component of the quiescent gas. The standard deviation of this line width distribution at all positions in the maps is 0.5 to 1 km $\,$ s^-1, and in some sources this width increases slightly with peak $T_{\rm {A}}^*$ , probably due to contributions of the outflow which cannot be separated from the quiescent gas. Column 6 lists the offsets with strongest blue and red wing emission (largest $\int T_{\rm {A}}^*$ dv). In general the maximum outflow velocities (Col. 3 of Table 3) do not occur at positions where the total wing area (Col. 6) is largest. Probably this is due to the fact that only small part of the outflow is at the highest velocities, and due to projection effects. In Cols. 7 to 12 are the derived outflow mass, momentum and energy (for blue and red wing and the total emission), the diameter (corrected for beamsize), average outflow velocity and the dynamical timescale of the outflow. The ratio of energy and timescale is the mechanical luminosity in Col. 13.

**Table 3:** Outflow parameters derived from ¹²CO(1-0) observations
Source	Wing	$V_{\rm {range}}$	offset	$\Delta v_{\rm {q}}$	$\int T_{\rm {A}}^*$ dv	Mass	Mom.	Energy	Diam.	$V_{\rm {out}}$	$t_{\rm {dyn}}$	$L_{\rm {mech}}$
WB89		km s^-1	$^{\prime \prime }$	km s^-1	peak ( $^{\prime \prime }$ )	$M_\odot$	$M_\odot$ km s^-1	10⁴⁴ erg	pc	km s^-1	10⁵ yr	$L_\odot$
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)
1086	blue	5.1	(40, 40)			-	-	-	-	-	-
	red	5.3	(-40, 0)			-	-	-	-	-	-
	total	9.4	(-40, 0)	1.80		-	-	-	-	-	-	-
1099	blue	10.4	(0, 0),(40, 20)		(-22, 16)	0.48	0.71	0.15	0.37	1.57	1.15
	red	7.3	(0, 0)		(46, 22)	0.59	1.26	0.45	0.22	2.46	0.44
	total	17.7	(0, 0)	1.13	(-3, 3)	1.07	1.97	0.60			0.65	0.0076
1135	blue	10.9	(0, 0)		(6, -10)	74	226	93	2.44	3.51	3.42
	red	11.6	(20, -20)		(6, 20)	78	193	68	2.65	3.10	4.22
	total	21.5	(40, 0)	2.71	(6, 2)	151	419	161			3.79	0.36
1173	blue	10.8	(60, 0)		(58, -46)	13	30	9.5	0.76	2.53	1.47
	red	10.5	(60, -20)		(38, -16)	15	28	8.2	0.75	2.18	1.70
	total	19.3	(60, -20)	2.03	(45, -15)	28	58	18			1.58	0.094
1181	blue	13.4	(0, 0)		(19, -19)	6.8	23	9.5	0.59	3.85	0.76
	red	12.5	(0, 0)		(19, -19)	7.7	26	11	0.55	3.96	0.68
	total	25.9	(0, 0)	3.16	(18, -18)	14	49	20			0.72	0.44
1187	blue	13.1	(0, 0)		(44, 19)	29	82	38	1.23	3.26	1.87
	red	15.6	(40, 40)		(-16, 0)	26	89	39	1.16	4.14	1.88
	total	25.3	(0, 0)	2.82	(20, 0)	55	171	77			1.60	0.40
1189	blue	8.3	(20, 20)		(0, 0)	1.2	2.0	0.47	0.32	2.19	0.72
	red	7.5	(-40, 20)		(19, 25)	1.2	1.8	0.36	0.31	1.69	0.90
	total	15.4	(20, 20)	1.80	(18, 25)	2.3	3.7	0.83			0.80	0.0086
1275	blue	12.3	(40, 40)		(-6, -18)	66	255	119	2.13	3.77	2.78	0.36
	red	10.5	(20, 40)			-	-	-	-	-	-
	total	21.5	(40, 40)	3.61		-	-	-	-	-	-	-

From the maps and the spectra we concluded that there is no outflow emission towards WB89 1086. This is a source showing only one line component which is slightly broader at several positions and showing only a small range in velocity with emission (see Col. 3 of Table 3). Towards WB89 1275 we derive only parameters for the blue wings because of confusion due to emission at higher velocities (39-46 km $\,$ s^-1 - see Fig. 2) which may not have been correctly subtracted.

The outflow masses range from 1 $M_\odot$ for WB89 1099 to 150 $M_\odot$ for WB89 1135, the sources with the lowest and highest FIR luminosity in the sample which were mapped in CO (apart from WB89 1275, for which $L_{\rm {FIR}}$ is higher, but for which we could only study the blue wing emission). Also the outflow momentum and energy show extreme values towards these sources. The outflow mass in WB89 1135 is among the highest ones found anywhere (about 200 $M_\odot$ ; see e.g. Bachiller [1996]). From the masses and diameters of the outflows we obtain H₂ densities ranging from 120 cm^-3 (red wing of WB89 1135) to 1590 cm^-3 (red wing of WB89 1099). The median value is 850 cm^-3, which is typical for such sources (Lada [1985]). The dynamical timescale in Col. 12 ranges from about 0.5 10⁵ years to 4 10⁵ years, which is at the upper range of values found in such sources (see e.g. Fig. 12 in Shepherd & Churchwell [1996]). A discussion of the accuracy of outflow parameters and a comparison of different methods to derive these parameters is given by Cabrit & Bertout ([1990]). The outflow velocity in Col. 11 of Table 3 is a average value, weighted with $T_{\rm {A}}^*$ at all positions. The maximum outflow velocity in Col. 3 is larger by a factor 3.8 (median; range from 3.0 [red wing in WB89 1099] to 6.6 [blue wing in WB89 1099]). Using this velocity would result in a dynamical timescale smaller- and a mechanical luminosity larger by this factor.

3.2 CS and C¹⁸O

Towards all sources which we observed in those molecules, we detected C¹⁸O(1-0) and CS(2-1) emission. Spectra at peak positions are shown in Fig. 5. For some sources the peak positions are displaced from the positions with strongest outflow emission or from the IRAS PSC position. In most cases C¹⁸O is weaker than CS. The exception is WB89 1086 where both lines have approximately equal intensity and both are faint. We note that the CS and/or C¹⁸O linewidths for four of the sources (WB89 1086, 1099, 1173, and 1189) are smaller (1.3 km $\,$ s^-1) than for the others (2.6 km $\,$ s^-1). The same is seen in the values of $\Delta v_{\rm {q}}$ of the quiescent ¹²CO gas (Col. 5 of Table 3). This might be related to the smaller FIR luminosity of the IRAS sources ( $46-5400~L_\odot$ vs. $1630-936000~L_\odot$ ), although these luminosity ranges show some overlap.

The results from the Gaussian fits are summarized in Table 4, where we list the values for CS and C¹⁸O for the average cloud spectrum and towards the peak position. Six of the sources in Table 1 were observed in CS(2-1) by Bronfman et al. ([1996]) at the IRAS PSC position. Those not observed are WB89 1086, WB89 1173, and WB89 1187. We did not observe CS (nor C¹⁸O) towards WB89 1275. Regarding the latter source, the weak line ( $T_{\rm {mb}}=0.4$ K) detected by Bronfman et al. (compared to the peak CS temperatures in Table 4) might be caused by a clump of which the center is displaced from the PSC position, as is suggested by Fig. 3.

$\begin{figure}\resizebox{\hsize}{!}{\includegraphics{h1645_fig6.eps}} \end{figure}$

Figure 6: The distribution of $\int T_{\rm {A}}^*$ dv of CS(2-1) and C¹⁸O(1-0). The observed positions are indicated by crosses, and the IRAS PSC position by a filled circle. Lowest contour level and contour step are for CS and C¹⁸O: 0.2 and 0.15 K $\,$ km $\,$ s^-1 (WB89 1086); 0.3 and 0.2 K $\,$ km $\,$ s^-1 (WB89 1099); 0.3 and 0.2 K $\,$ km $\,$ s^-1 (WB89 1135); 0.4 and 0.3 K $\,$ km $\,$ s^-1 (WB89 1173); 2 and 0.8 K $\,$ km $\,$ s^-1 (WB89 1181); 0.4 and 0.3 K $\,$ km $\,$ s^-1 (WB89 1187); 0.3 and 0.15 K $\,$ km $\,$ s^-1 (WB89 1189); 1 K $\,$ km $\,$ s^-1 (WB89 1262). The greyscale range is 0 - 5 K $\,$ km $\,$ s^-1 (CS) or 0 - 2 K $\,$ km $\,$ s^-1 (C¹⁸O), except for WB89 1181 and 1262, where it is 0 - 19 K $\,$ km $\,$ s^-1 (CS) and 0 - 3.3 K $\,$ km $\,$ s^-1 (C¹⁸O). The arrows indicate for WB89 1173, 1181, and 1189 the direction of H₂ jets detected by Massi et al. ([1997])

$\begin{figure}\resizebox{12cm}{!}{\includegraphics{h1645_fig7.eps}} % \end{figure}$

Figure 7: The distribution of peak $T_{\rm {A}}^*$ dv of CS(2-1) and C¹⁸O(1-0) for some of the sources. The observed positions are indicated by crosses, and the IRAS PSC position by a filled circle. Lowest contour level and contour step are both for CS and C¹⁸O 0.2 K. The arrows indicate for WB89 1173 and 1189 the direction of H₂ jets detected by Massi et al. ([1997])

The CS(2-1) and C¹⁸O(1-0) spectra do not show other velocity components. However, outflow emission is visible in some of the CS(2-1) spectra, e.g. WB89 1099 (see also Nielsen et al. [1998]), 1135 and 1181. Also towards WB89 1262, not observed in CO, CS shows line wings. However the signal-to-noise ratio is not good enough at all positions to distinguish between the distributions of outflow and quiescent gas in those four objects. We made Gaussian fits to the CS(2-1) and C¹⁸O(1-0) spectra, and the resulting $\int T_{\rm {A}}^*$ dv distributions are shown Fig. 6. Those of the peak $T_{\rm {A}}^*$ are essentially identical in most cases. Sources where the distribution of peak $T_{\rm {A}}^*$ is different are shown in Fig. 7. In most sources the two molecules show a maximum at or close to the PSC position. An exception is the CS emission from WB89 1086, which is rather weak towards (0, 0) and shows somewhat stronger emission northeast of the PSC position. WB89 1173 shows a maximum of $\int T_{\rm {A}}^*$ dv of CS at (0, 0), but the maximum of the distribution of $T_{\rm {A}}^*$ is displaced to the offset (37 $^{\prime \prime }$ , -35 $^{\prime \prime }$ ). In C¹⁸O this source shows a number of peaks displaced from the PSC position. The maximum in WB89 1181 is slightly to the west of the PSC position, the CS emission peaks closer to (0, 0) than the C¹⁸O, which is at (-41 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) (peak $T_{\rm {A}}^*$ ) or (-60 $^{\prime \prime }$ , -24 $^{\prime \prime }$ ) ( $\int T_{\rm {A}}^*$ dv). The CS distribution near WB89 1187 shows a chain of three clumps, the most eastern one of which coincides with the IRAS PSC position; The strongest $T_{\rm {A}}^*$ is towards the eastern one at (65 $^{\prime \prime }$ , -6 $^{\prime \prime }$ ). Offsets mentioned above can differ from those in Table 4 because they were derived from the contour maps rather than from the individual spectra.

Towards four of the sources, Massi et al. ([1997]) searched for and detected NIR H₂emission: WB89 1173, 1181, 1187, and 1189. We have indicated for three of those sources (using updated information from Massi [1999]) their direction as 1 $^\prime$ arrows in Figs. 4, 6, and 7. The origin (for WB89 1173) or the centers of the arrows coincide with the embedded (NIR) objects proposed by Massi et al. ([1997]) to be the jets' origin. It seems that in all cases the direction is approximately parallel to the short axis of the CS or C¹⁸O clumps. In none of the three cases the direction is that of one of the outflows found in CO (see Fig. 4). These H₂ features are extremely small (some arcseconds) for WB89 1173 and 1189, and for the latter source this emission is outside the CS and C¹⁸O clumps (see Fig. 6). On the other hand, in WB89 1181 nine individual H₂ features can be distinguished, up to 30 $^{\prime \prime }$ northwest and southeast from an embedded star, which is close to the IRAS PSC position and lies inside the dense clumps. The H₂ emission towards WB89 1187 is very weak.

We can compare the locations of CS and C¹⁸O clumps in Fig. 6 with the distribution of ¹²CO(1-0) line wings in Fig. 4. Although in both figures the structures seen are not much larger than the angular resolution of the observations, there are a few sources where the cloud cores are clearly separated from the outflows (projected on the sky). Examples are the red wing of WB89 1099, both wings of WB89 1181, and the red wing of WB89 1187, where the outflow gas thus moves away from the dense cores. The situation is less clear towards the other sources, possibly due to projection effects.

From our data we derived the clump parameters listed in Table 5. The radii in Cols. 2 (CS) and 4 (C¹⁸O) were obtained from the area in the grid where these molecules were detected: $r = \sqrt{\rm Area/\pi}$ . This radius was corrected for the beam size. There was not always enough time to observe a large enough area of sky, hence for some clumps the values are lower limits. This applies mostly to CS in WB89 1173 and to C¹⁸O in WB89 1187 (but it is possible that near the other sources there are also more clumps which we did not trace). We applied another method to derive the clump radii in Cols. 3 and 5. Here we used their area at the half-intensity level. These values are smaller of course than those in Cols. 2 and 4. Because clouds are not spherical in most cases, all numbers should be considered as equivalent cloud radii. The virial mass in Cols. 6 and 7 was derived assuming a density distribution proportional to r^-2 ( $M_{\rm {vir}} = 126r\Delta v^2$ ; see e.g. MacLaren et al. [1988]), and here we used the radii in Cols. 2 and 4. The values derived from C¹⁸O can be compared with the LTE masses in Col. 8, which were derived assuming C¹⁸O is optically thin (using N(H $_2)=3.0\ 10^{16}~T_{\rm {ex}}~\int T_{\rm {A}}^*$ (C¹⁸O)/0.7 dv; Wilson et al. [1986]). We used a ratio ¹²CO/C¹⁸O of 560 (Wilson & Rood [1994]), an excitation temperature $T_{\rm {ex}}$ of 20 K, a ¹²CO/H₂ abundance of 10^-4, and multiplied by a factor 1.36 to take He into account (0.7 is the SEST main beam efficiency). For most clouds the $M_{\rm {vir}}$ is the larger mass. The differences are not larger than typically found for such objects, however. If one uses the conversion factor from N(C¹⁸O) to N(H₂) found by Frerking et al. ([1982]), instead of the above mentioned abundance ratios, the masses would become about a factor 2 larger. From the masses in Col. 8 and the cloud radii in Col. 4 we obtain the average density in Col. 9. If we had used the radii in Col. 5 instead, the density range would have been 5300 to 60400 cm^-3 instead of 820 to 16900 cm^-3.

We find velocity gradients in CS and C¹⁸O towards five of the mapped clouds. Position-velocity plots from Gaussian fits along the direction showing the gradient are shown in Fig. 8. Least squares fits to these data gave the velocity gradient in Col. 10 of Table 5. It appears that the gradient in the CS cloud near WB89 1187 is due to three clumps with a constant velocity each. For comparison with the assumed C¹⁸O excitation temperature (20 K) we list in Col. 11 the excitation temperature derived from the maximum ¹²CO(1-0) $T_{\rm {A}}^*$ in the cloud at the offset position in Col. 12. The value in the cloud center for C¹⁸O will be higher or lower, depending on whether there are heating sources or not. NH₃ observations of similar clouds showed that the kinetic temperature also depends on the luminosity of the embedded source (see e.g. Wouterloot et al. [1988]).

**Table 4:** CS and C¹⁸O results. The first line for each source gives the parameters of the averaged cloud spectrum, the second line those at the peak $T_{\rm {A}}^*$ position
Source		CS				C¹⁸O
WB89		$T_{\rm {A}}^*$	offset	$V_{\rm {lsr}}$	$\Delta v$	$T_{\rm {A}}^*$	offset	$V_{\rm {lsr}}$	$\Delta v$
		K	$^{\prime \prime }$	km $\,$ s^-1	km $\,$ s^-1	K	$^{\prime \prime }$	km $\,$ s^-1	km $\,$ s^-1
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
1086	aver.	0.12 (0.02)		63.84 (0.08)	1.12 (0.16)	0.16 (0.02)		63.63 (0.07)	1.63 (0.17)
	peak	0.57 (0.08)	(-40, -80)	63.89 (0.07)	0.60 (0.13)	0.44 (0.02)	(0, 0)	63.88 (0.03)	1.03 (0.06)
1099	aver.	0.52 (0.03)		5.85 (0.02)	1.12 (0.06)	0.45 (0.03)		5.81 (0.02)	0.94 (0.05)
	peak	2.33 (0.18)	(0, 0)	6.06 (0.01)	1.34 (0.03)	1.05 (0.05)	(0, 0)	6.04 (0.01)	0.93 (0.03)
1135	aver.	0.36 (0.03)		54.66 (0.05)	2.07 (0.12)	0.26 (0.03)		54.53 (0.05)	1.77 (0.14)
	peak	1.05 (0.07)	(0, 0)	54.83 (0.03)	2.88 (0.09)	0.45 (0.06)	(0, 0)	55.13 (0.05)	3.34 (0.13)
1173	aver.	0.59 (0.02)		7.37 (0.02)	1.24 (0.05)	0.57 (0.04)		7.36 (0.01)	1.31 (0.03)
	peak	1.53 (0.16)	(40, -40)	7.20 (0.04)	1.17 (0.09)	1.45 (0.13)	(-40, 0)	7.25 (0.02)	0.99 (0.08)
1181	aver.	1.15 (0.05)		4.01 (0.02)	3.47 (0.04)	0.36 (0.02)		4.20 (0.02)	2.95 (0.05)
	peak	4.15 (0.20)	(0, 0)	4.08 (0.01)	4.03 (0.03)	1.00 (0.11)	(-40, 0)	3.45 (0.05)	3.08 (0.12)
1187	aver.	0.53 (0.03)		12.19 (0.02)	2.79 (0.04)	0.31 (0.03)		12.06 (0.04)	2.55 (0.10)
	peak	1.25 (0.20)	(40, 0)	12.97 (0.08)	2.20 (0.13)	0.72 (0.12)	(40, 0)	12.58 (0.07)	1.83 (0.18)
1189	aver.	0.36 (0.03)		2.47 (0.03)	1.37 (0.08)	0.41 (0.02)		2.44 (0.02)	1.26 (0.05)
	peak	1.61 (0.20)	(40, 0)	2.31 (0.04)	1.56 (0.09)	1.06 (0.11)	(40, 0)	2.35 (0.03)	1.02 (0.07)
1262	aver.	0.77 (0.04)		9.50 (0.02)	2.57 (0.05)	not observed
	peak	3.75 (0.26)	(0, 0)	9.38 (0.03)	3.15 (0.08)

**Table 5:** Properties of clumps mapped in CS and C¹⁸O
Source	r				$M_{\rm {vir}}$		$M_{\rm {LTE}}$	n	dv/dr	$T_{\rm {ex}}$	offset
WB89	pc				$M_\odot$		$M_\odot$	cm^-3	km s^-1 pc^-1	K	$^{\prime \prime }$
	CS		C¹⁸O		CS	C¹⁸O	C¹⁸O			¹²CO
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)
1086	1.4	<0.9¹	1.2	0.70	260	480	500	1000		23.0	(-24, -6)
1099	0.29	0.10	0.24	0.16	47	29	25	6500	+1.51 (0.23)	15.5	(-15, 16)
1135	1.5	0.69	2.1	1.1	920	830	2120	820	-0.40 (0.08)	16.1	(-2, -11)
1173	>0.76	>0.39²	1.1	0.72	>150	240	6300	16900		41.1	(-42, 46)
1181	0.50	0.17	0.56	0.30	770	625	260	5300	-2.01 (0.39)	29.3	(6, 19)
1187	1.8	1.1	>0.81	>0.68	1770	>700	>470	3200	+0.42 (0.04)	23.2	(17, 3)
1189	0.19	0.09	0.17	0.11	47	36	17	12400	+1.91 (0.20)	29.0	(13, 19)
1262	1.6	0.47			1350
1275										28.4	(47, 24)
¹ Two unresolved clumps.
² The main clump; there are also two unresolved (<0.18 pc) clumps.

3 Results

3.1 ¹²CO and ¹³CO

3.2 CS and C¹⁸O

3 Results

3.1 12CO and 13CO

3.2 CS and C18O

3.1 ¹²CO and ¹³CO

3.2 CS and C¹⁸O