We attempt to visually classify the morphologies of 18190 molecular clouds, which are identified in the ^12^CO(1-0) spectral line data over ~450deg^2^ of the second Galactic quadrant from the Milky Way Imaging Scroll Painting project. Using the velocity-integrated intensity maps of the ^12^CO(1-0) emission, molecular clouds are first divided into unresolved and resolved ones. The resolved clouds are further classified as nonfilaments or filaments. Among the 18190 molecular clouds, ~25% are unresolved, ~64% are nonfilaments, and ~11% are filaments. In the terms of the integrated flux of ^12^CO(1-0) spectra of all 18190 molecular clouds, ~90% are from filaments, ~9% are from nonfilaments, and the remaining ~1% are from unresolved sources. Although nonfilaments are dominant in the number of the discrete molecular clouds, filaments are the main contributor of ^12^CO emission flux. We also present the number distributions of the physical parameters of the molecular clouds in our catalog, including their angular sizes, velocity spans, peak intensities of ^12^CO(1-0) emission, and ^12^CO(1-0) total fluxes. We find that there is a systematic difference between the angular sizes of the nonfilaments and filaments, with the filaments tending to have larger angular scales. The H2 column densities of them are not significantly different. We also discuss the observational effects, such as those induced by the finite spatial resolution, beam dilution, and line-of-sight projection, on the morphological classification of molecular clouds in our sample.

Cone search capability for table J/ApJS/257/51/table1 (A catalog of molecular clouds)