Chemical differentiation in regions of high-mass star formation. CS, dust, and N2H+ in southern sources

Aims. Our goals are to compare the CS, N 2 H + , and dust distributions in a representative sample of high-mass star-forming dense cores and to determine the physical and chemical properties of these cores. Methods. We compare the results of CS(5–4) and 1.2 mm continuum mapping of twelve dense cores from the southern hemisphere presented in this work, in combination with our previous N 2 H + (1–0) and CS(2–1) data. We use numerical modeling of molecular excitation to estimate physical parameters of the cores. Results. Most of the maps have several emission peaks (clumps). The mean sizes of 17 clumps with counterparts in the continuum and CS are 0.30(0.06) pc (continuum) and 0.51(0.07) pc (CS). For the clumps with IRAS sources, we derived dust temperatures of 24-35 K, masses of 90-6900 $M_{\odot}$, molecular hydrogen column densities of $(0.7{-}12.0)\times 10^{23}$ cm -2 and luminosities of ($0.6{-}46.0)\times 10^4~L_{\odot}$. The LVG densities towards CS peaks within the 50 '' beam (0.56 pc at 2.3 kpc, the average distance of our sample source) vary from source to source in the range (3-40$)\times 10^5$ cm -3 . Masses calculated from LVG densities are higher than the CS virial masses and masses derived from continuum data, implying small-scale clumpiness of the cores. The molecular abundances towards IRAS sources in eight objects are X (CS$)=(0.3{-}2.7)\times10^{-9}$ and X (N 2 H$^+)=(0.3{-}4.4)\times10^{-10}$. The CS and continuum maps were compared with each other and with the N 2 H + (1–0) maps. For most of the objects, the CS and continuum peaks are close to the IRAS point source positions. The CS(5–4) intensities correlate with continuum fluxes per beam in all cases, but only in five cases with the N 2 H + (1–0) intensities. The study of the spatial variations of molecular integrated intensity ratios to continuum fluxes per beam reveals that I (N 2 H + )/ F 1.2 ratios drop towards the CS peaks for most of the sources, which can be due to an N 2 H + abundance decrease. For CS(5–4), the I (CS)/ F 1.2 ratios show no clear trends with distance from the CS peaks, while such ratios drop for CS(2–1) towards these peaks. Possible explanations of these results are considered. The analysis of normalized velocity differences between CS and N 2 H +  lines has not revealed indications of systematic motions towards CS peaks.