MALT90 molecular content on high-mass IR-dark clumps

Abstract

Context. High mass stars form in groups or clusters in dense molecular clumps with sizes of 1 pc and masses of 200 M⊙. Infrared-dark clumps and the individual cores within them with sizes < 0.1 pc and masses < 100 M⊙ are important laboratories for high-mass star formation in order to study the initial conditions. Aims. We investigate the physical and chemical properties of high-mass clumps in order to better understand the early evolutionary stages and find targets that show star formation signs such as infall motions or outflows. Methods. We selected the high-mass clumps from ATLASGAL survey that were identified as dark at 8/24 μm wavelengths. We used MALT90 Survey data which provides a molecular line set (HCO+, HNC, HCN, N2H+, H13CO+, HN13C, SiO) to investigate the physical and chemical conditions in early stages of star formation. Results. Eleven sources have significant SiO detection (over 3σ) which usually indicates outflow activity. Thirteen sources are found with blue profiles in both or either HCO+ and/or HNC lines and clump mass infall rates are estimated to be in the range of 0.2 × 10−3 M⊙ yr−1 − 1.8 × 10−2 M⊙ yr−1. The excitation temperature is obtained as < 24 K for all sources. The column densities for optically thin lines of H13CO+ and HN13C are in the range of 0.4–8.8 (×1012) cm−2, and 0.9–11.9 (×1012) cm−2, respectively, while it is in the range of 0.1–7.5 (×1014) cm−2 for HCO+ and HNC lines. The column densities for N2H+ were ranging between 4.4–275.7 (×1012) cm−2 as expected from cold dense regions. Large line widths of N2H+ might indicate turbulence and large line widths of HCO+, HNC, and SiO indicate outflow activities. Mean optical depths are 20.32, and 23.19 for optically thick HCO+ and HCN lines, and 0.39 and 0.45 for their optically thin isotopologues H13CO+ and HN13C, respectively. Conclusions. This study reveals the physical and chemical properties of 30 high-mass IR-dark clumps and the interesting targets among them based on their emission line morphology and kinematics.