2021/11/30 by A. Y. Yang, J. S. Urquhart, F. Wyrowski +28 · 29 citations
Chemistry · Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #Biology #Context (archaeology) #Geometry #Line (geometry) #Molecular Spectroscopy and Structure #Outflow #Physics #Spectral line #Star (game theory) #Star formation #Stars #astro-ph.GA
paper · pdf · open access · doi:10.1051/0004-6361/202142039
published in Astronomy and Astrophysics 658, A160 (EDP Sciences) · 13 pages, 10 figures, accepted by Astronomy & Astrophysics (A&A)
openalex publication_date 2021/11/30 · arxiv created 2021/12/01 · arxiv updated 2022/03/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Context. The formation processes of massive stars are still unclear but a picture is emerging involving accretion disks and molecular outflows in what appears to be a scaled-up version of low-mass star formation. A census of outflow activity towards massive star-forming clumps in various evolutionary stages has the potential to shed light on massive star formation (MSF). Aims. We conducted an outflow survey towards ATLASGAL clumps using SEDIGISM data and aimed to obtain a large sample of clumps exhibiting outflows in different evolutionary stages. Methods. We identify the high-velocity wings of the 13CO lines toward ATLASGAL clumps by (1) extracting the simultaneously observed 13CO and C18O spectra from SEDIGISM, and (2) subtracting Gaussian fits to the scaled C18O from the 13CO, line after considering opacity broadening. Results. We have detected high-velocity gas towards 1192 clumps out of a total sample of 2052, giving an overall detection rate of 58%. Outflow activity has been detected in the earliest quiescent clumps (i.e., 70μm weak), to the most evolved HII region stages i.e., 8μm bright with MSF tracers. The detection rate increases as a function of evolution (quiescent=51%, protostellar=47%, YSO=57%, UCHII regions=76%). Conclusion. Our sample is the largest outflow sample identified so far. The high-detection rate from this large sample is consistent with previous results and supports that outflows are a ubiquitous feature of MSF. The lower detection rate in early evolutionary stages may be due to that outflows in the early stages are weak and difficult to detect. We obtain a statistically significant sample of outflow clumps for every evolutionary stage, especially for outflow clumps in the 70μm dark stage. This suggests that the absence of 70μm emission is not a robust indicator of starless/pre-stellar cores.