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We present the results of an unbiased $^{12}$CO/$^{13}$CO/C$^{18}$O ($J$ =1-0) survey in a portion of the third Galactic quadrant (TGQ): $l$ = [219.75,229.75]$^\circ$ and $b$ = [-5.25, 5.25]$^\circ$. The high-resolution andhigh-sensitivity data sets help to unravel the distributions and physicalproperties of the molecular clouds (MCs) in the mapped area. In the LSRvelocity range from -1 to 85 km/s, the molecular material successfully tracesthe Local, Perseus, and Outer arms. In the TGQ, the Outer arm appears to bemore prominent than that in the second Galactic quadrant (SGQ), but the Perseusarm is not as conspicuous as that in the SGQ. A total of 1,502 $^{12}$CO, 570$^{13}$CO, and 53 C$^{18}$O molecular structures are identified, spanning over$\sim2$ and $\sim6$ orders of magnitude in size and mass, respectively. Tightmass-radius correlations and virial parameter-mass anticorrelations areobservable. Yet, it seems that no clear correlations between velocitydispersion and effective radius can be found over the full dynamic range. Thevertical distribution of the MCs renders evident pictures of the Galactic warpand flare.

the astrophysical journal. supplement series/astrophysical journal. supplement series

Distributions and Physical Properties of Molecular Clouds in the Third  Galactic Quadrant: $l$ = [219.75, 229.75]$^\circ$ and $b$ = [-5.25,  5.25]$^\circ$