The Fabry–Perot scanning interferometer mounted on the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences is used to study the distribution and kinematics of ionized gas in the peculiar galaxy Arp 212 ( NGC 7625 , III Zw 102 ) .
Two kinematically distinct subsystems—the inner disk and outer emission filaments—are found within the optical radius of the galaxy .
The first subsystem , at galactocentric distances r < 3.5 kpc , rotates in the plane of the stellar disk .
The inner part of the ionized-gas disk ( r < 1.5 –2 kpc ) exactly coincides with the previously known disk consisting of molecular gas .
The second subsystem of ionized gas is located at galactocentric distances 2–6 kpc .
This subsystem rotates in a plane tilted by a significant angle to the stellar disk .
The angle of orbital inclination in the outer disk increases with galactocentric distance and reaches 50 \hbox { $ { } ^ { \circ } $ } at r \approx 6 kpc .
The ionized fraction of the gaseous disk does not show up beyond this galactocentric distance , but we believe that the HI disk continues to warp and approaches the plane that is polar with respect to the inner disk of the galaxy .
Hence Arp 212 can be classified as a galaxy with a polar ring ( or a polar disk ) .
The observed kinematics of the ionized and neutral gas can be explained assuming that the distribution of gravitational potential in the galaxy is not spherically symmetric .
Most probably , the polar ring have formed via accretion of gas from the dwarf satellite galaxy UGC 12549 .