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We present a large-scale simultaneous survey of the CO isotopologues ($\rm{}^{12}{CO}$, $\rm{}^{13}{CO}$, and $\rm{C}{}^{18}{O}$) J = 1 ${-}$ 0 lineemission toward the Galactic plane region of l = 106.65$^\circ$ to109.50$^\circ$ and b = ${-}$1.85$^\circ$ to 0.95$^\circ$ using the PurpleMountain Observatory 13.7 m millimeter-wavelength telescope. Except for themolecular gas in the solar neighborhood, the emission from the molecular gas inthis region is concentrated in the velocity range of [${-}$60, ${-}$35] $\rmkm~s^{-1}$. The gas in the region can be divided into four clouds, with mass inthe range of $\sim$10$^{3}$ to 10$^{4}$\,${M_{\sun}}$. We have identified 25filaments based on the $\rm {}^{13}{CO}$ data. The median excitationtemperature, length, line mass, line width, and virial parameter of thefilaments are 10.89 K, 8.49 pc, 146.11 ${M}_{\odot}~ \rm pc^{-1}$, 1.01 $\rmkm~s^{-1}$, and 3.14, respectively. Among these filaments, eight have virialparameters of less than 2, suggesting that they are gravitationally bound andcan lead to star formation. Nineteen {H \small {II}} regions or candidates havepreviously been found in the region and we investigate the relationshipsbetween these {H \small {II}} regions/candidates and surrounding molecularclouds in detail. Using morphology similarity and radial velocity consistencybetween {H \small {II}} regions/candidates and molecular clouds as evidence forassociation, and raised temperature and velocity broadening as signatures ofinteraction, we propose that 12 {H \small {II}} regions/candidates areassociated with their surrounding molecular clouds. In the case of the {H\small {II}} region of S142, the energy of the {H \small {II}} region issufficient to maintain the turbulence in the surrounding molecular gas.

research in astronomy and astrophysics/research in astronomy and astrophysics

Molecular Clouds Associated with {H \small{II}} regions and Candidates  within l = 106.65$^\circ$ to 109.50$^\circ$ and b = ${-}$1.85$^\circ$ to  0.95$^\circ$