# The AGN-Star Formation Connection: Future Prospects with JWST

## TL;DR

This paper discusses how JWST's MIRI instrument will improve the detection and understanding of dust-obscured AGN and their host galaxies at cosmic noon, enhancing our knowledge of galaxy evolution.

## Contribution

It introduces new infrared color diagnostics for JWST/MIRI to identify dust-obscured AGN and composite galaxies at z~1-2, surpassing previous Spitzer/IRAC capabilities.

## Key findings

- MIRI will detect over 4 times more AGN hosts than Spitzer/IRAC.
- Star formation rates need correction for AGN contribution to avoid overestimation.
- MIRI color technique can identify low Eddington ratio AGN and higher sSFR hosts.

## Abstract

The bulk of the stellar growth over cosmic time is dominated by IR luminous galaxies at cosmic noon (z=1-2), many of which harbor a hidden active galactic nucleus (AGN). We use state of the art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGN from dusty star forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 micron counts of SFGs, AGN/star forming "Composites", and AGN. AGN and Composites dominate the counts above 0.8 mJy at 24 micron, and Composites form at least 25% of an IR sample even to faint detection limits. We develop methods to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGN and Composite galaxies from z~1-2. With the sensitivity and spacing of MIRI filters, we will detect >4 times as many AGN hosts than with Spitzer/IRAC criteria. Any star formation rates based on the 7.7 micron PAH feature (likely to be applied to MIRI photometry) must be corrected for the contribution of the AGN, or the SFR will be overestimated by ~35% for cases where the AGN provides half the IR luminosity and ~50% when the AGN accounts for 90% of the luminosity. Finally, we demonstrate that our MIRI color technique can select AGN with an Eddington ratio of $\lambda_{\rm Edd}\sim0.01$ and will identify AGN hosts with a higher sSFR than X-ray techniques alone. JWST/MIRI will enable critical steps forward in identifying and understanding dust-obscured AGN and the link to their host galaxies.