2018/11/07 by S. J. Billington, J. S. Urquhart, C. Figura +3
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxy #Maser #Physics #Protostar #Spectral line #Star (game theory) #Star formation #Stellar, planetary, and galactic studies #Young stellar object #astro-ph.GA
paper · pdf · doi:10.1093/mnras/sty3053
22 pages, 16 figures, 7 tables
arxiv created 2018/11/07 · openalex publication_date 2018/11/07 · arxiv updated 2018/11/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present the results from NH 3 mapping observations towards 34 regions identified by the Red MSX Source (RMS) survey. We have used the Australia Telescope Compact Array to map ammonia (1,1) and (2,2) inversion emission spectra at a resolution of 10 with velocity channel resolution of 0.4 km s -1 towards the positions of embedded massive star formation. Complementary data have been used from the ATLASGAL and GLIMPSE Legacy Surveys in order to improve the understanding of the regions and to estimate physical parameters for the environments. The fields have typical masses of 1000 M , radii of 0.15 pc and distances of 3.5 kpc. Luminosities range between 10 3 to 10 6 L and kinetic temperatures between 10 and 40 K. We classify each field into one of two subsets in order to construct an evolutionary system for massive star formation in these regions based on the morphology and relative positions of the NH 3 emission, RMS sources and ATLASGAL thermal dust emission. Differences in morphology between NH 3 emission and ATLASGAL clumps are shown to correspond to evolutionary stages of ongoing massive star formation in these regions. The study has been further refined by including the positions of known methanol and water masers in the regions to gain insight into possible protostellar regions and triggered star formation.