A hidden population of active galactic nuclei can explain the overabundance of luminous $z>10$ objects observed by JWST

TL;DR

This paper proposes that a hidden population of active galactic nuclei (AGNs) can explain the observed excess of luminous galaxies at redshifts greater than 10 in JWST data, by boosting galaxy luminosities without altering morphologies.

Contribution

It introduces a semi-empirical model linking dark matter halos, galaxies, and SMBHs, demonstrating that low-luminosity AGNs can account for the overabundance of luminous high-$z$ objects.

Findings

AGN emission can explain the luminosity excess at $z>10$

Hidden low-luminosity AGNs are consistent with observed morphologies

Overmassive black holes relative to host galaxies are required

Abstract

The first wave of observations with JWST has revealed a striking overabundance of luminous galaxies at early times ($z>10$) compared to models of galaxies calibrated to pre-JWST data. Early observations have also uncovered a large population of supermassive black holes (SMBHs) at $z>6$. Because many of the high-$z$ objects appear extended, the contribution of active galactic nuclei (AGNs) to the total luminosity has been assumed to be negligible. In this work, we use a semi-empirical model for assigning AGNs to galaxies to show that active galaxies can boost the stellar luminosity function (LF) enough to solve the overabundance problem while simultaneously remaining consistent with the observed morphologies of high-$z$ sources. We construct a model for the composite AGN+galaxy LF by connecting dark matter halo masses to galaxy and SMBH masses and luminosities, accounting for dispersion in the mapping between host galaxy and SMBH mass and luminosity. By calibrating the model parameters -- which characterize the $M_\bullet-M_\star$ relation -- to a compilation of $z>10$ JWST UVLF data, we show that AGN emission can account for the excess luminosity under a variety of scenarios, including one where 10\% of galaxies host BHs of comparable luminosities to their stellar components. Using a sample of simulated objects and real observations, we demonstrate that such low-luminosity AGNs can be `hidden' in their host galaxies and be missed in common morphological analyses. We find that for this explanation to be viable, our model requires a population of BHs that are overmassive ($M_\bullet/M_\star\sim10^{-2}$) with respect to their host galaxies compared to the local relation and are more consistent with the observed relation at $z=4-8$. We explore the implications of this model for BH seed properties and comment on observational diagnostics necessary to further investigate this explanation.