This is the third paper in a series that reports on our investigation of the clustering properties of AGNs identified in the ROSAT All-Sky Survey ( RASS ) and Sloan Digital Sky Survey ( SDSS ) .
In this paper , we extend the redshift range to 0.07 < z < 0.50 and measure the clustering amplitudes of both X-ray and optically-selected SDSS broad-line AGNs with and without radio detections as well as for X-ray selected narrow-line RASS/SDSS AGNs .
We measure the clustering amplitude through cross-correlation functions ( CCFs ) with SDSS galaxies and derive the bias by applying a halo occupation distribution ( HOD ) model directly to the CCFs .
We find no statistically convincing difference in the clustering of X-ray and optically-selected broad-line AGNs , as well as with samples in which radio-detected AGNs are excluded .
This is in contrast to low redshift optically-selected narrow-line AGNs , where radio-loud AGNs are found in more massive halos than optical AGNs without a radio-detection .
The typical dark matter halo masses of our broad-line AGNs are log ( M _ { DMH } / [ h ^ { -1 } M _ { \odot } ] ) \sim 12.4 - 13.4 , consistent with the halo mass range of typical non-AGN galaxies at low redshifts .
We find no significant difference between the clustering of X-ray selected narrow-line AGNs and broad-line AGNs .
We confirm the weak dependence of the clustering strength on AGN X-ray luminosity at a \sim 2 \sigma level .
Finally , we summarize the current picture of AGN clustering to z \sim 1.5 based on three dimensional clustering measurements .