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We present results from a survey of 70 radio galaxies (RGs) at redshifts1<z<5.2 using the PACS and SPIRE on-board Herschel. Combined with existingmid-IR photometry from Spitzer and observations obtained with LABOCA, the SEDsof galaxies in our sample are continuously covered across 3.6-870um. The totalinfrared luminosities of these RGs are such that they almost all are eitherultra-or hyper-luminous infrared galaxies. We fit the infrared SEDs with a setof empirical templates which represent dust heated (1) by a variety of SB and(2) by a AGN. We find that the SEDs of RGs require the dust to be heated byboth AGN and SB, but the luminosities of these two components are not stronglycorrelated. Assuming empirical relations and simple physical assumptions, wecalculate the SFR, the black hole mass accretion rate (MdotBH), and the blackhole mass (MBH) for each RG. We find that the host galaxies and their BHs aregrowing extremely rapidly, having SFR~100-5000 Msun/yr and MdotBH~1-100Msun/yr. The mean sSFR of RGs at z>2.5 are higher than the sSFR of typicalstar-forming galaxies over the same redshift range but are similar or perhapslower than the galaxy population for RGs at z<2.5. By comparing the sSFR andthe specific black hole mass accretion rate, we conclude that BHs in radio loudAGN are already, or soon will be, overly massive compared to their hostgalaxies in terms of expectations from the local MBH-MGal relation. In order to``catch up'' with the BH, the galaxies require about an order-of magnitude moretime to grow in mass, at the observed SFRs, compared to the time the BH isactively accreting. However, during the current cycle of activity, we arguethat this catching-up is likely to be difficult due to the short gas depletiontimes. Finally, we speculate on how the host galaxies might grow sufficientlyin stellar mass to ultimately fall onto the local MBH-MGal relation.

Rapidly growing black holes and host galaxies in the distant Universe from the Herschel Radio Galaxy Evolution Project