Astrophys. J., 720, 392-408 (2010/September-1)
Ammonia and CO observations toward low-luminosity 6.7 GHz methanol masers.
WU Y.W., XU Y., PANDIAN J.D., YANG J., HENKEL C., MENTEN K.M. and ZHANG S.B.
Abstract (from CDS):
To investigate whether distinctions exist between low- and high-luminosity Class II 6.7 GHz methanol masers, we have undertaken multi-line mapping observations of various molecular lines, including the NH3(1,1), (2,2), (3,3), (4,4), and 12CO (1-0) transitions, toward a sample of nine low-luminosity 6.7 GHz masers and 12CO (1-0) observations toward a sample of eight high-luminosity 6.7 GHz masers, for which we already had NH3 spectral line data. Emission in the NH3(1,1), (2,2), and (3,3) transitions was detected in eight out of nine low-luminosity maser sources, in which 14 cores were identified. We derive densities, column densities, temperatures, core sizes, and masses of both low- and high-luminosity maser regions. A comparative analysis of the physical quantities reveals marked distinctions between the low-luminosity and high-luminosity groups: in general, cores associated with high-luminosity 6.7 GHz masers are larger and more massive than those traced by low-luminosity 6.7 GHz masers; regions traced by the high-luminosity masers have larger column densities but lower densities than those of the low-luminosity maser regions. Further, strong correlations between 6.7 GHz maser luminosity and NH3(1,1) and (2,2) line widths are found, indicating that internal motions in high-luminosity maser regions are more energetic than those in low-luminosity maser regions. A 12CO (1-0) outflow analysis also shows distinctions in that outflows associated with high-luminosity masers have wider line wings and larger sizes than those associated with low-luminosity masers.
ISM: jets and outflows - ISM: molecules - masers - stars: formation
Tables 5-6: [WXP2010] GLLL.ll+BB.bb N N=14.
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