We present \sim 3 ^ { { } ^ { \prime \prime } } resolution maps of CO , its isotopologues , and HCN from in the center of Maffei 2 .
The J=1–0 rotational lines of ^ { 12 } CO , ^ { 13 } CO , C ^ { 18 } O and HCN , and the J=2–1 lines of ^ { 13 } CO and C ^ { 18 } O were observed with the OVRO and BIMA arrays .
The lower opacity CO isotopologues give more reliable constraints on H _ { 2 } column densities and physical conditions than optically thick ^ { 12 } CO .
The J=2–1/1–0 line ratios of the isotopologues constrain the bulk of the molecular gas to originate in low excitation , subthermal gas .
From LVG modeling , we infer that the central GMCs have n _ { H _ { 2 } } \sim 10 ^ { 2.75 } ~ { } cm ^ { -3 } and T _ { k } ~ { } \sim 30 K. Continuum emission at 3.4 mm , 2.7 mm and 1.4 mm was mapped to determine the distribution and amount of H ii regions and dust .
Column densities derived from C ^ { 18 } O and 1.4 mm dust continuum fluxes indicate the standard Galactic conversion factor overestimates the amount of molecular gas in the center of Maffei 2 by factors of \sim 2-4 .
Gas morphology and the clear “ parallelogram ” in the Position-Velocity diagram shows that molecular gas orbits within the potential of a nuclear ( \sim 220 pc ) bar .
The nuclear bar is distinct from the bar that governs the large scale morphology of Maffei 2 .
Giant molecular clouds in the nucleus are nonspherical and have large linewidths , due to tidal effects .
Dense gas and star formation are concentrated at the sites of the x _ { 1 } - x _ { 2 } orbit intersections of the nuclear bar , suggesting that the starburst is dynamically triggered .