Arizona Radio Observatory (ARO) Facilities Located at Mt. Graham, AZ (Elevation 3200m) 15 mm rms surface accuracy Two large receiver rooms located at each side of the Nasmyth foci provides space for several receiver systems. SMT 10-Meter Kitt Peak 12-Meter Continuous 65 to 300 GHz Dual channel single sideband SIS receivers Remote observing from virtually any computer Fast On-The-Fly mapping 24-7 operations Current Systems 210-275 GHz SIS 320-375 Dual channel SIS 430-490 GHz SIS 19-element bolometer array (345 GHz) HEB at 660 and 810 GHz 130-300 Dual channel single sideband (Fall 2002)

v=1 J=3-2 SiO Masers in VY CMa 129GHz VLBI Image using all phase and amp information. Masers must be near star. Masing may occur in stellar disk oriented at right angles to observed reflection nebula. Maser structure possibly related to episodic mass loss. 30 AU

Orion Outflow in J=6-5 13CO at 661 GHz with the SMT 10 m Da (arcsec) Dd (arcsec) Intensity (K km s-1) First map of Orion-KL for this transition of 13CO The receiver used was a 660 GHz HEB on loan from SAO (R. Blundell) Reveals the location and morphology of the hot gas in the Orion KL outflow region T. Wilson, M. Dumke, and D. Muders (MPIfR)

Strong Velocity Gradients in Shredded Gas CO emission along the Galactic equator is primarily localized in a number of sharp streaks, broad in velocity but only a few tenths of a parsec across—about half the width of a single giant molecular cloud core (GMC). Internal kinematics show wide lines occurring more than 75 pc perpendicular (not along) to the galactic plane. Maps of the J=1→0 lines of CO (left), 13CO (middle), and the J=2→1 line of CS (right), showing broad, yet spatially distinct features more than 30′ across the galactic plane. Galactic structure is another area of study for the KP12m. Maps of CO, 13CO, and CS (J=2?1) emission, made by H. Liszt (NRAO), have provided three views of an enigmatic aspect of the molecular gas distribution in the center of the Milky Way (see Figure 9). As shown in this figure, along the galactic equator CO emission is primarily localized in a number of sharp "streaks", broad in velocity but only a few tenths of a parsec across-about the width of a single giant molecular core (GMC). These maps also resolve the internal kinematics of these molecules and show that 150-200 km/s wide lines occur more than 30' (or 75pc) perpendicular (not along) the galactic plane. A Hydrodynamic model of gas flow in a strongly-barred gravitational potential suggests that such broad lines should occur whenever GMC's traverse the standing shocks which cause prominent dust lanes. The small volume-filling factor of molecular gas then accounts for the finite number of broad-lined features. A Hydrodynamic model of gas flow in a barred gravitational potential suggests that such broad lines should be present whenever GMCs traverse the standing shocks which cause prominent dust lanes. Courtesy of H. Liszt (NRAO)