We present deep emission-line imaging taken with the new SOAR Optical Imaging Camera of the brightest cluster galaxy ( BCG ) in the nearby ( z = 0.035 ) X-ray cluster of galaxies 2A0335+096 .
We also present our analysis of additional , multi-wavelength observations for the BCG , including long-slit optical spectroscopy , archival VLA radio data , Chandra X-ray imaging , and XMM UV-imaging .
Cluster 2A0335+096 is a bright , cool-core X-ray cluster , once known as a cooling flow .
Within the highly disturbed core revealed by Chandra X-ray observations , 2A0335+096 hosts a luminous and highly structured optical emission-line system , spanning the brightest cluster galaxy ( BCG ) and its companion .
We confirm that the redshift of the companion is within 100 km s ^ { -1 } of the BCG and has certainly interacted with the BCG , and is likely bound to it .
The comparison of optical and radio images shows curved filaments in H \alpha emission surrounding the newly resolved radio source .
The velocity structure of the emission-line bar between the BCG nucleus and the companion galaxy provides strong evidence for an interaction between the BCG and its northeast companion in the last \sim 50 million years .
The age of the radio source is similar to the interaction time , so this interaction may have provoked an episode of radio activity .
We estimate a star formation rate of \gtrsim 7 ~ { } M _ { \odot } ~ { } yr ^ { -1 } from the H \alpha and archival UV data .
This rate is similar to , but somewhat lower than , the revised X-ray cooling rate of 10 - 30 ~ { } M _ { \odot } ~ { } yr ^ { -1 } in the vicinity of the BCG , estimated from XMM spectra by Peterson et al .
( 2003 ) .
The H \alpha nebula is limited to a region of high X-ray surface brightness and cool X-ray temperatures .
However , the detailed structures of H \alpha and X-ray gas differ .
The peak of the X-ray surface brightness is not the peak of H \alpha emission , nor does it lie in the BCG .
The estimated age of the radio lobes and their interaction with the optical emission-line gas , the estimated timescale for depletion and accumulation of cold gas , and the dynamical time in the system are all similar , suggesting a common trigger mechanism .