Astrophys. J., 677, 353-372 (2008/April-2)
Infall and outflow of molecular gas in Sgr B2.
QIN S.-L., ZHAO J.-H., MORAN J.M., MARRONE D.P., PATEL N.A., WANG J.-J., LIU S.-Y. and KUAN Y.-J.
Abstract (from CDS):
Observations of two H2 CO (303-202and 321-220) lines and continuum emission at 1.3 mm toward Sgr B2(N) and Sgr B2(M) have been carried out with the SMA. The mosaic maps of Sgr B2(N) and Sgr B2(M) in both continuum and lines show a complex distribution of dust and molecular gas in both clumps and filaments surrounding the compact star formation cores. We have observed a decelerating outflow originated from the Sgr B2(M) core, showing that both the redshifted and blueshifted outflow components have a common terminal velocity. This terminal velocity is 58±2 km/s. It provides an excellent method for determination of the systematic velocity of the molecular cloud. The SMA observations have also shown that a large fraction of absorption against the two continuum cores is redshifted with respect to the systematic velocities of Sgr B2(N) and Sgr B2(M), respectively, suggesting that the majority of the dense molecular gas is flowing into the two major cores where massive stars have been formed. We have solved the radiative transfer in a multilevel system with LVG approximation. The observed H2 CO line intensities and their ratios can be adequately fitted with this model for the most of the gas components. However, the line intensities between the higher energy level transition H2CO(321-220) and the lower energy level transition H2CO(303-202) is reversed in the redshifted outflow region of Sgr B2(M), suggesting the presence of inversion in population between the ground levels in the two K ladders (K–1=0 and 2). The possibility of weak maser processes for the H2 CO emission in Sgr B2(M) is discussed.
Galaxy: Center - ISM: individual (Sgr B2) - ISM: Kinematics and Dynamics - ISM: Molecules - Radio Lines: ISM - Stars: Formation
Tables 1, 2, Figs: [QZM2008] AW (Nos NE, NW, ME, MW), [QZM2008] MN (Nos M1-M5).
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