CO (J=2-1) line observations of the galactic center molecular cloud complex. II. Dynamical structure and physical conditions

A large-scale (CO)-C-12-O-16 (J = 2-1) survey of the inner few hundred parsecs of the Galaxy has been conducted using the University of Tokyo-Nobeyama Radio Observatory 60 cm survey telescope. We have taken about 700 (CO)-C-12-O-16 (J = 2-1) spectra in the region -2.degrees 5 less than or equal to l less than or equal to 2.degrees 5 and \b\ less than or equal to 1 degrees with 0.degrees 125 grid spacing, covering the entire region of the huge molecular cloud complex in the Galactic center. We refer to the CO (J = 1-0) data taken with the Columbia 1.2 m telescope and calculate the J = 2-1 to J = 1-0 intensity ratio. Velocity channel maps and longitude-velocity maps of CO (J = 2-1) line are presented, with corresponding maps of J = 2-1/J = 1-0 intensity ratio. Large-scale CO maps enable us to identify several giant molecular cloud complexes and many characteristic features of molecular gas. We identify 15 molecular cloud complexes larger than similar to 30 pc in our CO (J = 2-1) data. Their virial masses are at least 1 order of magnitude larger than the masses estimated from the CO luminosity. This discrepancy can be removed if we notice that they may not be gravitationally bound but are in pressure equilibrium with the hot gas and/or magnetic field in this region. Using the expressions of virial mass and CO mass for a cloud in the pressure equilibrium case, we get the X-factor for the Galactic center molecular clouds as X = 0.24 x 10(20) cm(-2) (K km s(-1))(-1), which is 1 order of magnitude lower than that in the Galactic disk (X = 3.0 x 10(20) cm(-2) [K km s(-1)](-1)). We estimate the total molecular mass in the Galactic center as M(H-2) congruent to 2 x 10(7) M. as a lower limit; the actual total gas mass within the central 400 pc of the Galaxy must be M(H-2) = (2-6) x 10(7) M.. We diagnose the physical conditions of the molecular gas in the Galactic center using the intensity ratio between the J = 2-1 and J = 1-0 lines. Although the CO J = 2-1/J = 1-0 line intensity ratio is high (similar to 0.74) in the midplane, molecular gas at \b\ greater than or equal to 0.degrees 25 exhibits low J = 2-1/J = 1-0 ratios (similar to 0.6). The overall J = 2-1/J = 1-0 luminosity ratio is R(2-1/(1-0)) = 0.64 +/- 0.01 if we include all the emission within \b\ less than or equal to 1 degrees, -2.degrees 5 < l < 2.degrees 5, and \V-LSR\ less than or equal to 150 km s(-1). This indicates that low-density gas less than or similar to 50 pc away from the plane dominates the total Ca luminosity of the central 400 pc of the Galaxy. The fractional distribution of the molecular gas with R(2-1/1-0)) for each cloud complex clearly demonstrates the close relationship between the gas with a very high ratio [R(2-1/1-0)) greater than or equal to 1.0] and associated UV sources.