2010/01/26 by E. Muller, J. Ott, A. Hughes +9 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Brightness #Component (thermodynamics) #Envelope (radar) #Galaxies: Formation, Evolution, Phenomena #Molecular cloud #Population #Range (aeronautics) #Small Magellanic Cloud #Surface brightness #astro-ph.GA
paper · pdf · doi:10.1088/0004-637x/712/2/1248
12 pages, 8 Figures. Accepted for publication in ApJ, March 2010
arxiv created 2010/01/26 · openalex publication_date 2010/03/12 · arxiv updated 2015/05/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present here the first results from a high-resolution survey of the 12 CO( J = 1–0) emission across the northern part of the poorly enriched Small Magellanic Cloud (SMC), made with the ATNF Mopra telescope. Three molecular complexes detected in the lower resolution NANTEN survey are mapped with a beam FWHM of ∼42'', to sensitivities of approximately 210 mK per 0.9 km s −1 channel, resolving each complex into 4–7 small clouds of masses in the range of M vir ∼ 10 3 –10 4 M ☉ and with radii no larger than 16 pc. The northern SMC CO clouds follow similar empirical relationships to the southern SMC population, yet they appear relatively under-luminous for their size, suggesting that the star-forming environment in the SMC is not homogeneous. Our data also suggests that the CO cloud population has little or no extended CO envelope on scales ≳30 pc, further evidence that the weak CO component in the north SMC is being disassociated by penetrating UV radiation. The new high-resolution data provide evidence for a variable correlation of the CO integrated brightness with integrated H i and 160 μm emission; in particular CO is often, but not always, found coincident with peaks of 160 μm emission, verifying the need for matching-resolution 160 μm and H i data for a complete assessment of the SMC H 2 mass.