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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 surveywith 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. Themeasurements are conducted on angular scales ${\theta}$ $\lesssim$ 1200 arcsec.On scales ${\theta}$ $\lesssim$ 200 arcsec we find that the measurements arecorrupted by residual systematic effects associated with the instrumental beamof the VLA data. Using simulations we show that we can successfully apply acorrection for these effects. Using the three lens samples (the SDSS DR10sample, the BCG sample and the SDSS-FIRST matched object sample) we measure atangential shear signal that is inconsistent with zero at the 10${\sigma}$,3.8${\sigma}$ and 9${\sigma}$ level respectively. Fitting an NFW model to thedetected signals we find that the ensemble mass profile of the BCG sampleagrees with the values in the literature. However, the mass profiles of theSDSS DR10 and the SDSS-FIRST matched object samples are found to be shallowerand steeper than results in the literature respectively. The best-fittingVirial masses for the SDSS DR10, BCG and SDSS-FIRST matched samples, derivedusing an NFW model and allowing for a varying concentration factor, areM$^{SDSS-DR10}_{200}$ = (1.2 $\pm$ 0.4) $\times$ 10$^{12}$M$_{\odot}$,M$^{BCG}_{200}$ = (1.4 $\pm$ 1.3) $\times$ 10$^{13}$M$_{\odot}$ andM$^{SDSS-FIRST}_{200}$ = 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 beboth bright in the radio and in the optical they must be embedded in very denseenvironment on scales R $\lesssim$ 1Mpc.

Galaxy-galaxy and galaxy-cluster lensing with the SDSS and FIRST surveys