All Tables

Table 1: Observed transitions.
Table 2: Number of sources detected (Y), not detected (N) or not observed (N.O.) in C¹⁷O and 1.2 mm continuum among the 111 sources detected in CS.
Table A.1: Observed sources and detection summary. RA(J2000) and Dec(J2000) represent the equatorial coordinates of the IRAS source. $v_{\rm LSR}$ is the velocity at which we centered the CS spectra during the two observing runs (see text). N.O. means that the source was not observed in that tracer. $\Delta$ is the angular separation between the IRAS position and the nearest millimeter peak detected in the SIMBA maps.
Table A.2: CS line parameters obtained from Gaussian fits $^{(\diamondsuit )}$ . Typical rms noise in the spectra is $\sim$ 0.05 K and 0.06 K for the (2-1) and (3-2) lines, respectively.
Table A.3: C¹⁷O line parameters $^{(\diamondsuit )}$ . Typical rms noise in the spectra is $\sim$ 0.05 and $\sim$ 0.06 K for the (1-0) and (2-1) lines, respectively. N.O. = not observed.
Table A.4: "Distance-independent'' parameters of the clumps. The angular diameters, $\theta$ , and integrated flux densities, $F_{\nu }$ , have been derived from the 1.2 mm continuum maps; the rotation temperatures, $T_{\rm rot}$ , the C¹⁷O column densities, $N_{\rm C^{17}O}$ , and the H₂ total column densities, $N_{\rm H_{2}}$ , have been derived from C¹⁷O line ratios (assuming a C¹⁷O mean abundance of 3.9 $\times$ 10^-8); the ${\rm H}_{2}$ volume densities, $n_{\rm H_2}$ , have been obtained from CS line ratios.
Table A.5: Distance (d), linear size (D), luminosity (L), and dust temperature ( $T_{\rm d}$ ) of all sources detected in CS. A "-'' in the columns of D and $T_{\rm d}$ indicates that we could not derive any source angular diameter.
Table A.6: Clumps masses estimated from 1.2 mm continuum ( $M_{\rm cont}$ ), assuming virial equilibrium ( $M_{\rm vir}$ ), from C¹⁷O ( $M_{\rm C^{17}O}$ ) and from CS ( $M_{\rm CS}$ ). All values are in $M_{\odot }$ units.