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Correlations between the mass of a supermassive black hole and the propertiesof its host galaxy (e.g., total stellar mass (M*), luminosity (Lhost)) suggestan evolutionary connection. A powerful test of a co-evolution scenario is tomeasure the relations MBH-Lhost and MBH-M* at high redshift and compare withlocal estimates. For this purpose, we acquired HST imaging with WFC3 of 32X-ray-selected broad-line AGN at 1.2<z<1.7 in deep survey fields. By applyingstate-of-the-art tools to decompose the HST images including available ACSdata, we measured the host galaxy luminosity and stellar mass along with otherproperties through the 2D model fitting. The black hole mass was determinedusing the broad Halpha line, detected in the near-infrared with Subaru/FMOS,which potentially minimizes systematic effects using other indicators. We findthat the observed ratio of MBH to total M* is 2.7 times larger at z~1.5 than inthe local universe, while the scatter is equivalent between the two epochs. Anon-evolving mass ratio is consistent with the data at the 2-3 sigma confidencelevel when accounting for selection effects and their uncertainties. Therelationship between MBH-Lhost paints a similar picture. Therefore, our resultscannot distinguish whether SMBHs and their total M* and Lhost proceed inlockstep or whether the growth of the former somewhat overshoots the latter,given the uncertainties. Based on a statistical estimate of the bulge-to-totalmass fraction, the ratio MBH/M* is offset from the local value by a factor of~7 which is significant even accounting for selection effects. Taken together,these observations are consistent with a scenario in which stellar mass issubsequently transferred from an angular momentum supported component of thegalaxy to the pressure supported one through secular processes or minor mergersat a faster rate than mass accretion onto the SMBH.

The mass relations between supermassive black holes and their host galaxies at 1