We perform a galaxy-galaxy lensing study by correlating the shapes of \sim 2.7 \times 10 ^ { 5 } galaxies selected from the VLA FIRST radio survey with the positions of \sim 38.5 million SDSS galaxies , \sim 132000 BCGs and \sim 78000 SDSS galaxies that are also detected in the VLA FIRST survey .
The measurements are conducted on angular scales \theta \lesssim 1200 arcsec .
On scales \theta \lesssim 200 arcsec we find that the measurements are corrupted by residual systematic effects associated with the instrumental beam of the VLA data .
Using simulations we show that we can successfully apply a correction for these effects .
Using the three lens samples ( the SDSS DR10 sample , the BCG sample and the SDSS-FIRST matched object sample ) we measure a tangential shear signal that is inconsistent with zero at the 10 \sigma , 3.8 \sigma and 9 \sigma level respectively .
Fitting an NFW model to the detected signals we find that the ensemble mass profile of the BCG sample agrees with the values in the literature .
However , the mass profiles of the SDSS DR10 and the SDSS-FIRST matched object samples are found to be shallower and steeper than results in the literature respectively .
The best-fitting Virial masses for the SDSS DR10 , BCG and SDSS-FIRST matched samples , derived using an NFW model and allowing for a varying concentration factor , are { M } _ { 200 } ^ { SDSS - DR 10 } = ( 1.2 \pm 0.4 ) \times 10 ^ { 12 } { M } _ { \odot } , { M } _ { 200 } ^ { BCG } = ( 1.4 \pm 1.3 ) \times 10 ^ { 13 } { M } _ { \odot } and { M } _ { 200 } ^ { SDSS - FIRST } = 8.0 \pm 4.2 \times 10 ^ { 13 } { M } _ { \odot } respectively .
These results are in good agreement ( within \sim 2 \sigma ) with values in the literature .
Our findings suggest that for galaxies to be both bright in the radio and in the optical they must be embedded in very dense environment on scales R \lesssim 1 Mpc .