The peculiar velocities in the Galactic outer disk--hints of the elliptical disk and the perturbation of the spiral structures

We present the peculiar in-plane velocities derived from the LAMOST red clump stars. From the variations of the in-plane velocity with the Galactocentric radius for the young and old red clump stars, we are able to identify two types of peculiar velocities: 1) both the two red clump populations show that the radial velocity is negative within $R=9.0$,kpc and becomes positive beyond (denoted as the \emph{long-wave} mode); and 2) the young red clump stars show larger mean radial velocity than the old population by about 3,km${\mathrm{s}}^{-1}$ between $R=9$ and 12,kpc (denoted as the \emph{short-wave} mode). We find that the elliptical disk induced by the rotating bar can well explain the \emph{long-wave} mode peculiar velocity. The axis ratio of the elliptical disk is around 0.8-0.95 and the disk keeps circular at $R=9.24\pm 0.2$,kpc, which should be the location of the outer Lindblad resonance radius (OLR). Adopting the circular speed of 238,km${\mathrm{s}}^{-1}$, the pattern speed of the bar is then derived as $48\pm 3$,km${\mathrm{s}}^{-1}$kpc${}^{-1}$ from the location of OLR. On the other hand, the \emph{short-wave} mode is likely the perturbation of the spiral arms as density waves.