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Massive molecular outflows associated with UCHII/HII regions
Aims: We searched for the molecular outflows from fifteen molecularclouds associated with ultra-compact and compact HII (UCHII/HII) regionsand discussed possible gas heating mechanism. Methods: Mappingobservations of CO J=3-2 and J=2-1 lines were carried out with the KOSMA3 m-Telescope towards the 15 HII regions/molecular cloud complexes. Results: Ten molecular outflows were identified out of the fifteen HIIregion/molecular cloud complexes. The higher outflow detection rate(67%) suggested that such outflows are as common in high mass starforming regions as those in low mass star forming regions, which isconsistent with the results of other authors. The observations alsoshowed that the outflow might occur in the HII region. The integrated COline intensity ratios ( RI_{CO(3-2)/I_{CO(2-1)}}) weredetermined from the core component of the spectra as well as from boththe blue and red wings. Maximum line intensity ratios from the wings andcore components appeared to be related to the mid-infrared sourcesimaged by Midcourse Space Experiment (MSX). The relationship between themaximum line intensity ratios and MSX sources indicates that themolecular gas could be heated by the emission of dust associated withmassive stars. Based on maser observations reported in the literature,we found that H2O masers were only detected in seven regions.The H2O masers in these regions are located near the MSXsources and within the maximum line intensity ratio regions, suggestingthat H2O masers occur in relatively warm environments.Appendices A and B are only available in electronic form athttp://www.aanda.org
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Observation and Astrometry data
| Constellation: | Ηνίοχος |
| Right ascension: | 04h58m16.56s |
| Declination: | +48°03'11.6" |
| Apparent magnitude: | 9.225 |
| Proper motion RA: | -4.7 |
| Proper motion Dec: | 0.7 |
| B-T magnitude: | 9.393 |
| V-T magnitude: | 9.239 |
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