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We have studied the properties of molecular clouds in the second quadrant ofthe Milky Way Mid-plane from l$=$104$.\!\!^{\circ}$75 tol$=$119$.\!\!^{\circ}$75 and b$=-$5$.\!\!^{\circ}$25 to b$=$5$.\!\!^{\circ}$25using the $^{12}$CO, $^{13}$CO, and C$^{18}$O $J=1-0$ emission line data fromthe Milky Way Imaging Scroll Painting project (MWISP). We have identified 857and 300 clouds in the $^{12}$CO and $^{13}$CO spectral cubes, respectively,using the DENDROGRAM + SCIMES algorithms. The distances of the molecular cloudsare estimated and the physical properties like masses, sizes, and surfacedensities of the clouds are tabulated. The molecular clouds in the Perseus armare about 30$-$50 times more massive and 4$-$6 times larger than the clouds inthe Local arm. This result, however, is likely biased by distance selectioneffects. The surface densities of the clouds are enhanced in the Perseus armwith an average value of $\sim$100 M$_{\odot}$ pc$^{-2}$. We selected the 40most extended ($>$0.35 arcdeg$^2$) molecular clouds from the $^{12}$CO catalogto build the H$_2$ column density probability distribution function (N-PDF).About 78\% of the N-PDFs of the selected molecular clouds are well fitted withlog-normal functions with only small deviations at high-densities whichcorrespond to star-forming regions with scales of $\sim$1-5 pc in the Local armand $\sim$5-10 pc in the Perseus arm. About 18\% of the selected molecularclouds have power-law N-PDFs at high-densities. In these molecular clouds, themajority of the regions fitted with the power-law correspond to molecularclumps of sizes of $\sim$1 pc or filaments of widths of $\sim$1 pc.

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

Molecular Clouds in the Second Quadrant of the Milky Way Mid-plane from  l$=$104$.\!\!^{\circ}$75 to l=119$.\!\!^{\circ}$75 and  b=$-$5$.\!\!^{\circ}$25 to b=5$.\!\!^{\circ}$25