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We developed a tool that measures equivalent widths of various lines in lowresolution optical spectra, and it was applied to stellar spectra obtained aspart of SDSS-V and LAMOST programs. These lines, such as Li I which directlyindicates stellar youth, or optical H I and Ca II which in emission indicateactivity associated with stellar youth, are commonly seen in YSOs. We observeseveral notable differences in the properties of these lines between YSOs andthe field stars. Using these data, we devise a set of criteria through which itis possible to confirm the youth of stars that have been observed by the ABYSSprogram, as well as to identify likely young stars that have serendipitouslybeen observed by other programs. We examine the decrement of H lines seen inemission in CTTSs, and estimate the properties of the accretion stream that isresponsible for the production of these lines. Finally, we examine theevolution of Li I as a function of age, and characterize the scatter in itsabundance that appears to be intrinsic in young M dwarfs.

ABYSS II: Identification of young stars in optical SDSS spectra and their properties