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Paper text:
mrk334 is a sy1.8 galaxy , located at the distance of 88 mpc ( the scale is 430 pc/@xmath0 ) .
this galaxy demonstrates merging features as tidal tail and bright region ` a ' on the west from the nucleus .
according @xcite , the region " a can be a second nucleus or a remainder of a satellite galaxy , which was devoured by mrk334 . on the mpfs maps in different emission lines ,
three bright regions can be distinguish : nucleus , regions ` a ' and ` b ' ( fig .  [ smir : fig1 ] ) .
spectra from these regions differ from each other and the gas ionization state vary from one region to another dramatically : on the diagnostic diagrams , the points belonging to the knot ` b ' lie in the region of ionization by a nonthermal radiation .
all points that correspond to the knot ` a ' fall into the photoionization region .
surprising , that the nucleus is located in the hii / liner boundary i.e. , the gas can also be partially ionized here by both shocks and radiation from young hot stars , but not by non - thermal source ! also , on the [ sii ] ratio map the region with the lowest density is the knot ` b ' , whereas the density in the knot ` a ' is much higher .
velocity fields corresponding to the most emission lines show almost circular rotation of ionized gas .
only [ oiii]@xmath1 velocity field is an exception and reveals outflow from the nucleus .
it becomes apparent in the excess of blue - shifted velocities in the center of the galaxy . on the large - scale h@xmath2 residual velocity field ( observational velocities minus model of pure circular rotation ) strong non - circular velocity perturbations in the knot ` b '
are seen ( fig .
[ smir : fig1 ] , right ) .
the amplitude of the velocity deviations reaches 50kms@xmath3 .
on the deep images obtained on the 6 m telescope we find new numerous faint elongated structures ( tidal debris ) at different spatial scales .
it confirms the merging with a satellite .
this event strongly affects the disc structure and kinematics in mrk334 .
knot ` a ' can be a region of violent star formation , ionizing diagrams confirm this conclusion .
what is the knot ` b ' located at the distances of 1 - 3 kpc from the nucleus ? if an jet from the active nucleus is placed here , then we must detect a non - thermal radio emission .
however , radio maps @xcite disprove this hypothesis .
we suggest that knot ` b ' is a region where a satellite debris passing through the disk of the main galaxy .
this merging event can trigger the fueling of agn in mrk 334 .
we have studied the kinematics of the ionized gas and stellar component in mrk334 using methods of panoramic ( 3d ) spectroscopy . 
 the observations were performed at the prime focus of the sao ras 6-m telescope with the integral - field spectrograph mpfs @xcite and with a scanning fabry - perot interferometer ( fpi ) , installed on the multimode device scorpio @xcite . based on these data , 
 the monochromatic maps and velocity fields in different emission lines of the ionized gas were constructed . 
 the diagnostic diagrams have been made based on the emission lines ratios .