  Aims: We searched for the molecular outflows from fifteen molecular clouds
associated with ultra-compact and compact HII (UCHII/HII) regions and discussed
possible gas heating mechanism. Methods: Mapping observations of CO $J=3-2$ and
$J=2-1$ lines were carried out with the KOSMA 3m-Telescope towards the 15 HII
regions/molecular cloud complexes. Results: Ten molecular outflows were
identified out of the fifteen HII region/molecular cloud complexes. The higher
outflow detection rate (67%) suggested that such outflows are as common in high
mass star forming regions as those in low mass star forming regions, which is
consistent with the results of other authors. The observations also showed that
the outflow might occur in the HII region. The integrated CO line intensity
ratios (${\rm R_{I_{CO(3-2)}/I_{CO(2-1)}}}$) were determined from the core
component of the spectra as well as from both the blue and red wings. Maximum
line intensity ratios from the wings and core components appeared to be related
to the mid-infrared sources imaged by Midcourse Space Experiment (MSX). The
relationship between the maximum line intensity ratios and MSX sources
indicates that the molecular gas could be heated by the emission of dust
associated with massive stars. Based on maser observations reported in the
literature, we found that ${\rm H_{2}O}$ masers were only detected in seven
regions. The ${\rm H_{2}O}$ masers in these regions are located near the MSX
sources and within the maximum line intensity ratio regions, suggesting that
${\rm H_{2}O}$ masers occur in relatively warm environments.
