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The core population and kinematics of a massive clump at early stages: an ALMA view
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The core population and kinematics of a massive clump at early stages: an ALMA view
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Paper
The core population and kinematics of a massive clump at early stages: an ALMA view
2022
Overview
High-mass star formation theories make distinct predictions on the properties of the prestellar seeds of high-mass stars. Observations of the early stages of high-mass star formation can provide crucial constraints, but they are challenging and scarce. We investigate the properties of the prestellar core population embedded in the high-mass clump AGAL014.492-00.139, and we study the kinematics at the clump and the clump-to-core scales. We have analysed an extensive dataset acquired with the ALMA interferometer. Applying a dendrogram analysis to the Band o-\\( H_2D^+\\) data, we identified 22 cores. We have fitted their average spectra in local-thermodinamic-equilibrium conditions, and we analysed their continuum emission at \\(0.8 \\, mm\\). The cores have transonic to mildly supersonic turbulence levels and appear mostly low-mass, with \\(M_core< 30 \\, M_\\). Furthermore, we have analysed Band 3 observations of the \\( N_2H^+\\) (1-0) transition, which traces the large scale gas kinematics. Using a friend-of-friend algorithm, we identify four main velocity coherent structures, all of which are associated with prestellar and protostellar cores. One of them presents a filament-like structure, and our observations could be consistent with mass accretion towards one of the protostars. In this case, we estimate a mass accretion rate of \\( M_acc 2 10^-4 \\, M_ \\, yr^-1\\). Our results support a clump-fed accretion scenario in the targeted source. The cores in prestellar stage are essentially low-mass, and they appear subvirial and gravitationally bound, unless further support is available for instance due to magnetic fields.
Publisher
Cornell University Library, arXiv.org
