We present new radio continuum , 21 cm HI , and 2.6 mm CO data for the peculiar radio galaxy NGC 4410A and its companion NGC 4410B , and compare with available optical and X-ray maps .
Our radio continuum maps show an asymmetric double-lobed structure , with a high surface brightness lobe extending 3 \farcm 6 ( \sim 100 kpc ) to the southeast and a 6 \farcm 2 ( \sim 180 kpc ) low surface brightness feature in the northwest .
Molecular gas is abundant in NGC 4410A , with M _ { H _ { 2 } } \sim 4 \times 10 ^ { 9 } M _ { \odot } ( using the standard Galactic conversion factor ) , but is undetected in NGC 4410B .
HI is less abundant , with M _ { HI } \sim 10 ^ { 9 } M _ { \odot } for the pair .
Our HI map shows a 3 \times 10 ^ { 8 } M _ { \odot } HI tail extending 1 \farcm 7 ( 50 kpc ) to the southeast of the pair , coincident with a faint optical tail and partially overlapping with the southeastern radio lobe .
The HI tail is anti-coincident with a 2 ^ { \prime } ( 56 kpc ) long X-ray structure aligned with a stellar bridge that connects the pair to a third galaxy .
If this X-ray emission is associated with the group , we infer 3 - 8 \times 10 ^ { 8 } M _ { \odot } of hot gas in this feature .
This may be either intracluster gas or shocked gas associated with the bridge .

Our detection of abundant interstellar gas in this pair , including an HI-rich tidal tail near the southeastern radio lobe , suggests that the observed distortions in this lobe may have been caused by the interstellar medium in this system .
The gravitational interaction of the two galaxies and the subsequent motion of the interstellar medium in the system relative to the jet may have produced sufficient ram pressure to bend and distort the radio jet .
An alternative hypothesis is that the jet was distorted by ram pressure due to an intracluster medium , although the small radial velocity of NGC 4410A relative to the group and the lack of diffuse X-ray emission in the group makes this less likely unless the group is not virialized or is in the process of merging with another group .

Using our VLA data , we also searched for HI counterparts to the other ten known members of the NGC 4410 group and CO from three other galaxies in the inner group .
In our velocity range of 6690 km s ^ { -1 } - 7850 km s ^ { -1 } , we detected six other galaxies above our HI sensitivity limits of 2 \times 10 ^ { 8 } M _ { \odot } for the inner group and 4 \times 10 ^ { 8 } M _ { \odot } for the outer group .
The total HI in the group is 1.4 \times 10 ^ { 10 } M _ { \odot } , 80 \% of which arises from four galaxies in the outer group .
Three of these galaxies ( VCC 822 , VCC 831 , and VCC 847 ) are spirals with M _ { HI } /L _ { B } ratios typical of field galaxies , while FGC 170A appears to be a gas-rich dwarf galaxy ( M _ { B } \sim - 18 ; M _ { HI } \sim 3 \times 10 ^ { 9 } M _ { \odot } ) .
In the inner group , the SBa galaxy NGC 4410D ( VCC 934 ) was detected in HI and CO ( M _ { HI } \sim 5 \times 10 ^ { 8 } M _ { \odot } and M _ { H _ { 2 } } \sim 8 \times 10 ^ { 8 } M _ { \odot } ) and has a 1 ^ { \prime } ( 28 kpc ) long HI tail that points towards the nearby disk galaxy NGC 4410F .
NGC 4410F was also detected in HI ( M _ { HI } \sim 4 \times 10 ^ { 8 } M _ { \odot } ) .
The galaxies in the inner group appear to be somewhat deficient in HI compared to their blue luminosities , suggesting phase changes driven by galaxy-galaxy or galaxy-intracluster medium encounters .