Morphology of the Galactic center from the H3+ spectrum: The Expanding Molecular Ring Takeshi Oka, Department of Astronomy and Astrophysics and Department of Chemistry, The Enrico Fermi Institute, University of Chicago, Thomas R. Geballe, Gemini Observatory Nick Indriolo, Department of Physics and Astronomy, Johns Hopkins University Miwa Goto, Universitäts-Sternwarte München, Germany June 20, 2012, Columbus meeting WH06

ζ ≥ 2 × 10-15 s-1 High ionization rate and warm and diffuse gas in the Central Molecular Zone of the Galactic center revealed from the H3+ spectroscopy ζ ≥ 2 × 10-15 s-1 T ~ 250 K, n ≤ 100 cm-3 f > 30% Oka, Geballe, Goto, Usuda, McCall 2005 ApJ, 632, 882 The Central Molecular Zone

Morphology ≡ Doppler Spectroscopy Christian Doppler 1803-1853 The Central Molecular Zone

Molecular face-on views of the GC EMR Rodríguez-Fernandez et al. 2006 Scoville, 1972 Kaifu et al. 1972 Sawada et al. 2001 Sawada et al. 2004 Bally et al. 2010 Molinari et al, 2011 Kormendy & Kennicutt, 2004, ARA&A

43 stars suitable for the H3+ spectroscopy Quintuplet Cluster E Central Cluster B2 B1 D λ C A* α κ ι δ θ γ β

We use H3+ in diffuse clouds for morphology Longitude velocity diagram B2 B1 D λ C A* α κ ι δ θ γ β

Sofue 1995, PASJ, 47, 551

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