Herschel, Spitzer, and MOPRA Multi-Wavelength Studies of Inner Galactic Gas Clouds
Howard A. Smith, Anthony A. Stark, Christopher L. Martin, Mireya Etxaluze Azkonaga, and the HIGGS Team
The inner few hundred parsecs of the galaxy is dominated by the Central Molecular Zone (CMZ) containing the densest concentration of gas and dust in the Galaxy, and at the very center of which lies a massive black hole. 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 Inner Galactic Gas Clouds (IGGC), but star-formation in them has been suppressed compared to other star-forming regions in the Galaxy. We have observed [CII], [NII], [OI], [OIII], and high-J CO emission lines in selected regions in IG Clumps 1 and 2; we also have complementary Herschel PACS and SPIRE photometric data, Spitzer Space Telescope IRAC and MIPS data. We also have a large, new set of molecular! line observations of the Clumps obtained with MOPRA. This poster will present the current status of our ongoing analysis of these data sets to further unravel the dynamics and physical processes underway in Clumps 1 and 2, and the implications for the inner galaxy.