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We present 0.3" (band 6) and 1.5" (band 3) ALMA observations of the(sub)millimeter dust continuum emission for 25 radio galaxies at 1<z<5.2. Oursurvey reaches a rms flux density of ~50$\mu$Jy in band 6 and ~20$\mu$Jy inband 3. This is an order of magnitude deeper than single-dish 850 $\mu$mobservations, and reaches fluxes where synchrotron and thermal dust emissionare expected to be of the same order of magnitude. Combining our sensitive ALMAobservations with radio data from ATCA, VLA, and IR photometry from Herscheland Spitzer, we have disentangled the synchrotron and thermal dust emission. Wedetermine the star-formation rates (SFR) and AGN IR luminosities using ournewly developed spectral energy distribution fitting code MrMoose. We find thatsynchrotron emission contributes substantially at ~1 mm. Through our sensitiveflux limits and accounting for a contribution from synchrotron emission in themm, we revise downward the median SFR by a factor of 7 compared to previousestimates based solely on Herschel and Spitzer data. The hosts of theseradio-loud AGN appear predominantly below the main sequence of star-forminggalaxies, indicating that the star formation in many of the host galaxies hasbeen quenched. Future growth of the host galaxies without substantial blackhole mass growth will be needed to bring these objects on the local relationbetween the supermassive black holes and their host galaxies. Given themismatch in the timescales of any star formation that took place in the hostgalaxies and lifetime of the AGN, we hypothesize that a key role is played bystar formation in depleting the gas before the action of the powerful radiojets quickly drives out the remaining gas. This positive feedback loop ofefficient star formation rapidly consuming the gas coupled to the action of theradio jets in removing the residual gas is how massive galaxies are rapidlyquenched.

Massive galaxies on the road to quenching: ALMA observations of powerful high redshift radio galaxies