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We present the result of an unbiased CO survey in Galactic range of34.75$^{\circ}\leq$l$\leq$ 45.25$^{\circ}$ and -5.25$^{\circ}\leq$b$\leq$5.25$^{\circ}$, and velocity range beyond the Outer arm. A total of 168molecular clouds (MCs) are identified within the Extreme Outer Galaxy~(EOG)region, and 31 of these MCs are associated with 13CO emission. However, none ofthem show significant C18O emission under current detection limit. The typicalsize and mass of these MCs are 5~pc and 3$\times$10$^{3}M_{\sun}$, implying thelack of large and massive MCs in the EOG region. Similar to MCs in the outerGalaxy, the velocity dispersions of EOG clouds are also correlated with theirsizes, however, are well displaced below the scaling relationship defined bythe inner Galaxy MCs. These MCs with a median Galactocentric radius of 12.6kpc, show very different distributions from those of the MCs in the Outer armpublished in our previous paper, while roughly follow the OuterScutum-Centaurus arm defined by Dame & Thaddeus 2011. This result may provide arobust evidence for the existence of the Outer Scutum-Centaurus arm. The lowerlimit of the total mass of this segment is about 2.7$\times$10$^5$ $M_{\sun}$,which is about one magnitude lower than that of the Outer arm. The meanthickness of gaseous disk is about 1.45$^{\circ}$ or 450~pc, and the scaleheight is about 1.27$^{\circ}$ or 400~pc above the $b=0^{\circ}$ plane. Thewarp traced by CO emission is very obvious in the EOG region and its amplitudeis consistent with the predictions by other warp models using differenttracers, such as dust, HI and stellar components of our Galaxy.

Molecular clouds in the extreme outer Galaxy between $l=34.75^{\circ}$ to $45.25^{\circ}$