Chemo-kinematics of the Milky Way spiral arms and bar resonances:
  connection to ridges and moving groups in the Solar vicinity
  Using of a new N-body simulation, as well as Gaia DR2/EDR3 data complemented
by data from the Galah, APOGEE, LAMOST surveys, we explore the possible link
between 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 be
successfully identified using overdensities in angular momentum (AM) or guiding
space, as well as in the distribution of dynamically cold stars close to their
guiding centers. Stars in the AM overdensities that travel over many kpc in
radius trace extended density ridges in RVphi space and overdensities in the UV
plane of a SNd-like region, similar to those observed in the Gaia data.
Similarly, the AM space of the MW contains several overdensities which
correlate with a wave-like radial velocity pattern; this pattern is also
reproduced by stars well beyond the SNd. We find that the fraction of Gaia
stars located near their guiding centers shows three large-scale structures
that approximately coincide with the MW spiral arms traced by distributions of
maser sources in the Sagittarius, Local, and Perseus arms. Similar to the
model, the stars in the AM overdensities follow the main RVphi ridges. When
these ridges cross the SNd, they can be matched with the main UV features. Thus
we suggest that the Hat is the inner tail of the Perseus arm, one of the
Hercules components is the Sagittarius arm and the Arcturus stream is likely to
be the outermost tail of the Scutum-Centaurus arm. Based on previous work, the
bar corotation is suggested to coincide with the Hercules stream, and the OLR
with the Sirius stream. The latter is supported by a sharp decrease of the mean
metallicity beyond the Sirius stream, which is an expected behaviour of the
OLR. In various phase-space coordinates the AM overdensities stars have
systematically higher mean metallicity...(Abridged)
