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

Abstract

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 and high-sensitivity data sets help to unravel the distributions and physical properties of the molecular clouds (MCs) in the mapped area. In the LSR velocity range from -1 to 85 km/s, the molecular material successfully traces the Local, Perseus, and Outer arms. In the TGQ, the Outer arm appears to be more prominent than that in the second Galactic quadrant (SGQ), but the Perseus arm 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 $\sim 2$ and $\sim 6$ orders of magnitude in size and mass, respectively. Tight mass-radius correlations and virial parameter-mass anticorrelations are observable. Yet, it seems that no clear correlations between velocity dispersion and effective radius can be found over the full dynamic range. The vertical distribution of the MCs renders evident pictures of the Galactic warp and flare.

arXiv comment22 pages, 13 figures, 7 tables (with machine-readable versions), published in ApJS

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