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Using of a new N-body simulation, as well as Gaia DR2/EDR3 data complementedby data from the Galah, APOGEE, LAMOST surveys, we explore the possible linkbetween the MW spiral arms, RVphi-ridges and moving groups in local UV space.We show that the tightly wound main spiral arms in the N-body model can besuccessfully identified using overdensities in angular momentum (AM) or guidingspace, as well as in the distribution of dynamically cold stars close to theirguiding centers. Stars in the AM overdensities that travel over many kpc inradius trace extended density ridges in RVphi space and overdensities in the UVplane of a SNd-like region, similar to those observed in the Gaia data.Similarly, the AM space of the MW contains several overdensities whichcorrelate with a wave-like radial velocity pattern; this pattern is alsoreproduced by stars well beyond the SNd. We find that the fraction of Gaiastars located near their guiding centers shows three large-scale structuresthat approximately coincide with the MW spiral arms traced by distributions ofmaser sources in the Sagittarius, Local, and Perseus arms. Similar to themodel, the stars in the AM overdensities follow the main RVphi ridges. Whenthese ridges cross the SNd, they can be matched with the main UV features. Thuswe suggest that the Hat is the inner tail of the Perseus arm, one of theHercules components is the Sagittarius arm and the Arcturus stream is likely tobe the outermost tail of the Scutum-Centaurus arm. Based on previous work, thebar corotation is suggested to coincide with the Hercules stream, and the OLRwith the Sirius stream. The latter is supported by a sharp decrease of the meanmetallicity beyond the Sirius stream, which is an expected behaviour of theOLR. In various phase-space coordinates the AM overdensities stars havesystematically higher mean metallicity...(Abridged)

Chemo-kinematics of the Milky Way spiral arms and bar resonances: connection to ridges and moving groups in the Solar vicinity