Signatures of inflow motion in cores of massive star formation: Potential collapse candidates

TL;DR

This study uses molecular line observations to identify inflow signatures in high-mass star-forming cores, revealing ongoing accretion even in later evolutionary stages, and highlighting differences from low-mass star formation processes.

Contribution

It provides the first systematic evidence of inflow motions in high-mass star-forming regions and compares these signatures across different evolutionary stages.

Findings

29% of sources show blue profiles indicating inflow.

Higher inflow signature prevalence in UC HII regions (58%) than precursors (17%).

Differences in inflow signatures suggest fundamental distinctions from low-mass star formation.

Abstract

Using the IRAM 30 m telescope, a mapping survey in optically thick and thin lines was performed towards 46 high mass star-forming regions. The sample includes UC H{\sc ii} precursors and UC H{\sc ii} regions. Seventeen sources are found to show "blue profiles", the expected signature of collapsing cores. The excess of sources with blue over red profiles ([$N_{\rm blue}$ -- $N_{\rm red}$]/$N_{\rm total}$) is 29% in the HCO$^+$ $J$=1--0 line, with a probability of 0.6% that this is caused by random fluctuations. UC H{\sc ii} regions show a higher excess (58%) than UC H{\sc ii} precursors (17%), indicating that material is still accreted after the onset of the UC H{\sc ii} phase. Similar differences in the excess of blue profiles as a function of evolutionary state are not observed in low mass star-forming regions. Thus, if confirmed for high mass star-forming sites, this would point at a fundamental difference between low- and high-mass star formation. Possible explanations are inadequate thermalization, stronger influence of outflows in massive early cores, larger gas reserves around massive stellar objects or different trigger mechanisms between low- and high- mass star formation.