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We correlate the positions of radio galaxies in the FIRST survey with the CMBlensing convergence estimated from the Atacama Cosmology Telescope over 470square degrees to determine the bias of these galaxies. We remove opticallycross-matched sources below redshift $z=0.2$ to preferentially select ActiveGalactic Nuclei (AGN). We measure the angular cross-power spectrum $C_l^{\kappag}$ at $4.4\sigma$ significance in the multipole range $100<l<3000$,corresponding to physical scales between $\approx$ 2--60 Mpc at an effectiveredshift $z_{\rm eff}= 1.5$. Modelling the AGN population with aredshift-dependent bias, the cross-spectrum is well fit by the Planck best-fit$\Lambda$CDM cosmological model. Fixing the cosmology we fit for the overallbias model normalization, finding $b(z_{\rm eff}) = 3.5 \pm 0.8$ for the fullgalaxy sample, and $b(z_{\rm eff})=4.0\pm1.1 (3.0\pm1.1)$ for sources brighter(fainter) than 2.5 mJy. This measurement characterizes the typical halo mass ofradio-loud AGN: we find $\log(M_{\rm halo} / M_\odot) = 13.6^{+0.3}_{-0.4}$.

The Atacama Cosmology Telescope: measuring radio galaxy bias through cross-correlation with lensing