2020/04/13 by Wanggi Lim, Fumitaka Nakamura, Benjamin Wu +12 · 12 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Collision #Orion Nebula #Star (game theory) #Star formation #Stellar, planetary, and galactic studies #Young stellar object #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1093/pasj/psaa035
published in Publications of the Astronomical Society of Japan 73(Supplement_1), S239-S255 (Oxford University Press) · 16 pages, 11 figures, 4 tables, published in PASJ
openalex publication_date 2020/04/13 · openalex created_date 2020/04/17 · arxiv created 2020/06/25 · arxiv updated 2020/06/29 · openalex updated_date 2026/08/05
Abstract We introduce new analysis methods for studying the star cluster formation processes in Orion A, especially examining the scenario of a cloud–cloud collision. We utilize the CARMA–NRO Orion survey 13CO (1–0) data to compare molecular gas to the properties of young stellar objects from the SDSS III IN-SYNC survey. We show that the increase of v_\rm 13CO - v\rm YSO and Σ scatter of older YSOs can be signals of cloud–cloud collision. SOFIA-upGREAT 158 μm [C ii] archival data toward the northern part of Orion A are also compared to the 13CO data to test whether the position and velocity offsets between the emission from these two transitions resemble those predicted by a cloud–cloud collision model. We find that the northern part of Orion A, including regions ONC-OMC-1, OMC-2, OMC-3, and OMC-4, shows qualitative agreements with the cloud–cloud collision scenario, while in one of the southern regions, NGC 1999, there is no indication of such a process in causing the birth of new stars. On the other hand, another southern cluster, L 1641 N, shows slight tendencies of cloud–cloud collision. Overall, our results support the cloud–cloud collision process as being an important mechanism for star cluster formation in Orion A.