2007/07/28 by V. Casasola, F. Combes, D. Bettoni +1 · 1 citation
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Center (category theory) #Chemistry #Crystallography #Fragmentation (computing) #Galactic Center #Galaxies: Formation, Evolution, Phenomena #Galaxy #Geometry #HERA #Hydrogen #Hydrogen molecule #Line (geometry) #Molecular cloud #Particle physics #Physics #Spectroscopy and Laser Applications #Spiral galaxy #Stars #Telescope #astro-ph
paper · pdf · doi:10.1051/0004-6361:20077883
12 pages, 7 figures, 6 tables. Accepted for pubblication in A&A
arxiv created 2007/07/28 · openalex publication_date 2007/08/06 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the molecular gas content and the excitation and fragmentation properties in the central region of the spiral galaxy Messier 81 in both the 12CO(1–0) and 12CO(2–1) transitions. We have recently observed the two transitions of CO in the M 81 center with A, B, and HERA receivers of the IRAM 30-m telescope. We find no CO emission in the inner ~300 pc and a weak molecular gas clump structure at a distance of around 460 pc from the nucleus. Observations of the first two CO transitions allowed us to compute the line ratio, and the average ratio is 0.68 for the M 81 center. This low value, atypical both of the galactic nuclei of spiral galaxies and of interacting systems, is probably associated to diffuse gas with molecular hydrogen density that is not high enough to excite the CO molecules. After analyzing the clumping properties of the molecular gas in detail, we identify very massive giant molecular associations (GMAs) in CO(2–1) emission with masses of ~105 and diameters of ~250 pc. The deduced N(H2)/ICO ratio for the individually resolved GMAs, assumed to be virialized, is a factor of ~15 higher than the standard Galactic value, showing – as suspected – that the X ratio departs significantly from the mean for galaxies with an unusual physics of the molecular gas.