Galactic Center Inner Galaxy Dust Clouds In The Infrared And Submillimeter

Details Galactic Center Inner Galaxy Dust Clouds In The Infrared And Submillimeter Galactic Center Inner Galaxy Dust Clouds In The Infrared And Submillimeter

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21944115t&link_type=abstract

American Astronomical Society, AAS Meeting #219, #441.15

Astronomy and Astrophysics

Astronomy

Scientific paper

The inner few hundred parsecs of the Galaxy form the Central Molecular Zone (CMZ) - the densest concentration of gas and dust in the Galaxy, including the massive black hole at its center. Farther out from the center, to about 400 parsecs, is the region called Inner Galaxy (IG) whose dynamics are dominated by the gravitational potential of the Galactic Bar. Material that slowly falls from the outer parts of the Galaxy towards the plane encounters extreme physical conditions. Dust and molecular material form dense massive clouds, the so-called CLUMPS, within which are high velocity regions called Inner Galactic Gas Clouds (IGGC). We are using Herschel HIFI and PACS [CI], [CII], [NII], [OI], [OIII], and high-J CO emission line observations in focused regions near the Galactic Center supplemented by Herschel and Spitzer photometric data and MOPRA molecular line observations to investigate the physical conditions and processes in Clump 1 and Clump 2. These clumps are of particular interest because they show very little star formation activity, contrary to their counterparts ELSEWHERE in the CMZ. This poster will present the current status of our ongoing analysis, which is focused on the gas knots IGGC 7 and 25 in Clump 1 and IGGC 16, 19, and 23 in Clump 2.

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