title: Exploring the central molecular zone of the Galaxy using spectroscopy of H3+ and CO.
abstract: The central 400 parsecs of the Milky Way, a region known as the central molecular zone (CMZ), contains interstellar gas in a wide range of physical environments, from ultra-hot, rarified and highly ionized to warm, dense and molecular. The combination of infrared spectroscopy of H(3)(+) and CO is a powerful way to determine the basic properties of molecular interstellar gas, because the abundance ratio of H(3)(+) to CO in 'dense' clouds is quite different from that in 'diffuse' clouds. Moreover, the energy-level structure and the radiative properties of H(3)(+) combined with the unusually warm temperatures of molecular gas in the CMZ make H(3)(+) a unique probe of the physical conditions there. This paper describes how, using infrared absorption spectroscopy of H(3)(+) and CO, it has been discovered that a large fraction of the volume of the CMZ is filled with warm, diffuse and partially molecular gas moving at speeds of up to approximately 200 km s(-1) and that the mean cosmic ray ionization rate in the CMZ exceeds by roughly an order of magnitude values found in diffuse molecular clouds elsewhere in the Galaxy.
authors.affiliation: Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720, USA. tgeballe@gemini.edu
authors.forename: T R
authors.initials: TR
authors.lastname: Geballe