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One of the main achievements in modern cosmology is the so-called `unifiedmodel', which successfully describes most classes of active galactic nuclei(AGN) within a single physical scheme. However, there is a particular class ofradio-luminous AGN that presently cannot be explained within this framework --the `low-excitation' radio AGN (LERAGN). Recently, a scenario has been putforward which predicts that LERAGN, and their regular `high-excitation' radioAGN (HERAGN) counterparts represent different (red sequence vs. green valley)phases of galaxy evolution. These different evolutionary states are alsoexpected to be reflected in their host galaxy properties, in particular theircold gas content. To test this, here we present CO(1-0) observations toward asample of 11 of these systems conducted with CARMA. Combining our observationswith literature data, we derive molecular gas masses (or upper limits) for acomplete, representative, sample of 21 z<0.1 radio AGN. Our results yield thatHERAGN on average have a factor of ~7 higher gas masses than LERAGN. We alsoinfer younger stellar ages, lower stellar, halo, and central supermassive blackmasses, as well as higher black hole accretion efficiencies in HERAGN relativeto LERAGN. These findings support the idea that high- and low-excitation radioAGN form two physically distinct populations of galaxies that reflect differentstages of massive galaxy build-up.

The Molecular Gas Content of z<0.1 Radio Galaxies: Linking the AGN Accretion Mode to Host Galaxy Properties