We present Very Large Array ( VLA ) Hi imaging of four low surface brightness ( LSB ) galaxies ( [ OBC97 ] P01-3 , [ OBC97 ] C06-1 , [ OBC97 ] C04-1 , [ OBC97 ] C04-2 ) The official ( IAU ) name of these objects are originated from O ’ Neil et al .
( 16 ) .
For convenience , however , [ OBC97 ] will be omitted hereafter . which were thought to strongly deviate from the Tully-Fisher ( TF ) relation based on Arecibo single-dish observations .
We do not detect three of the four targeted LSB galaxies in Hi down to a 4 \sigma limit of 0.08Jy km s ^ { -1 } .
We find that two of the four of these LSBs have bright galaxies at projected distances of 2.6 and 2.9 arcminutes , which have contaminated the Arecibo signal .
A further examination of the Arecibo sample shows that five out of the six galaxies that were found to deviate from TF have nearby bright galaxies ( within 3.5 arcmin and within the observed Hi velocity range ) , and we conclude that possibly all but one of the non-TF galaxies are contaminated by Hi from nearby galaxies .
The sixth galaxy was not detected by us .
A new observation by Arecibo did not confirm the earlier detection .
We present the Hi properties , kinematics , and rotation curves of three bright galaxies NGC 7631 , KUG 2318+078 , NGC 2595 which happened to be in the LSB fields and of two LSB galaxies , one of the targeted ones C04-2 and one ( UGC 12535 or P01-1 ) that was found in the field of P01-3 .
The two detected LSB galaxies fall within 2 \sigma on the TF relation .
The integrated profiles of the bright galaxies are consistent with the Arecibo results both in velocity range and amplitude , which indicates that most of the extreme deviators from the TF relation must have been affected by bright companions in this earlier Hi survey .
A more recent determination of the sidelobe structure of the Arecibo beam supports our conclusion and shows that the degree of sidelobe contamination was much larger than could have been initially predicted .
If the now unknown velocities of these non detected LSB ’ s are within our probed velocity range then the limit to their Hi mass is roughly 10 ^ { 8 } M _ { \odot } assuming H _ { 0 } = 75 km s ^ { -1 } Mpc ^ { -1 } .
Hence , we have corrected the results found in O ’ Neil et al .
( 19 ) and have reconstructed the TF relation .
These new observations then show a ) a reconstructed TF relation that has relatively large scatter at all values of rotational velocity ( possibly indicating the true range in disk galaxy properties ) and b ) the presence of at least some red , gas poor , LSB disks that indeed may be in an advanced evolutionary state as the faded remnants of their former high surface brightness actively star forming state .