Exploring the Central Molecular Zone of the Galaxy with H3+ and CO

Details Exploring the Central Molecular Zone of the Galaxy with H3+ and CO Exploring the Central Molecular Zone of the Galaxy with H3+ and CO

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280e..69g&link_type=abstract

The Molecular Universe, Proceedings of the 280th Symposium of the International Astronomical Union held in Toledo, Spain, May 30

Astronomy and Astrophysics

Astronomy

Scientific paper

We report on our ongoing study of the warm (200-300K) and diffuse (N˜100 cm-3) gaseous component of the Central Molecular Zone (CMZ) of the Galactic center (GC), detected earlier via infrared spectroscopy of H3+ toward bright sources in the central parsec and 30 pc to the east. Using newly discovered bright infrared point sources along widely spaced lines of sight to the CMZ, and comparing high resolution H3+ and CO spectroscopy we find that this gaseous component is highly extended in galactic longitude and probably fills a considerable fraction of the volume of the CMZ. Some of the new sightlines provide first every 2--5 μm looks into the well-known molecular cloud complexes Sgr B and Sgr E. We discuss the physical and chemical nature of the warm diffuse component in the various sightlines and in the CMZ as a whole as well as constraints on the cosmic ray ionization rate of H2 in the CMZ.

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