Discovery of an Edge-on Galaxy with X-shaped Bi-cone --- SDSS
  J171359.00+333625.5
  Using the integral field unit (IFU) data from Mapping Nearby Galaxies at
Apache Point Observatory (MaNGA) survey, we study the kinematics of gas and
stellar components in an edge-on Seyfert 2 galaxy, SDSS J171359.00+333625.5,
with X-shaped bi-conical outflows. The gas and stars therein are found to be
counter-rotating, indicating that the collision between the inner and external
gas might be an effective way to dissipate the angular momentum, which leads to
remarkable gas accretion into the galaxy center. Large [OIII]$\lambda$5007
equivalent width and AGN-like line ratio in the large bi-conical region suggest
that the gas is ionized by the central AGN. The gas velocity in the bi-cone
region shows that ionized gas is receding relative to the galaxy center, which
could be the joint effect of inflows, outflows and disk rotation. We are
probably witnessing the case where a great amount of gas in the disk is being
efficiently accreted into the central black hole, and the AGN-driven galactic
winds are blown out along the bi-cone. The kinematics of oxygen, including
rotation velocity and velocity dispersion, is different from other elements,
like hydrogen, nitrogen and sulfur. The rotation velocity estimated from oxygen
is slower than from other elements. The velocity dispersion of other elements
follows galactic gravitational potential, while the velocity dispersion of
oxygen stays roughly constant along the galactic major-axis. The further
advanced observations, e.g. of cold gas or with an IFU of higher spatial
resolution, are required to better understand this object.
