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The hot ($>10^6$ K) phase of the circumgalactic medium (CGM) contains a largefraction of baryons in galaxies. It also retains signatures of the processesthat shaped the galaxies, such as feedback from active galactic nuclei (AGNs)and supernovae, and offers a uniquely powerful way to constrain theoreticalmodels of feedback. It is, however, notoriously difficult to detect. Bystacking 2643 optically selected galaxies in the eROSITA Final Equatorial DepthSurvey (eFEDS), we present spatially resolved properties of the extended CGM inboth star-forming and quiescent galaxies spanning an order of magnitude instellar mass. We mask out resolved point sources and galaxy groups/clusters andmodel the contribution from X-ray binaries and the hot ISM, producing accurateradial profiles. We compare the profiles to mock X-ray observations of galaxystacks in the IllustrisTNG100 (TNG) and EAGLE cosmological simulations. Wedetect extended emission from both the high-mass($10.7<\log(M_*/M_\odot)<11.2$) and low-mass ($10.2<\log(M_*/M_\odot)<10.7$)galaxy stacks. Galaxies have somewhat more luminous CGM between $10-100$~kpc ifthey are more massive or star-forming. However, the luminosity increases slowerwith stellar mass than predicted in simulations. Simulated quenched galaxiesare far dimmer than observed, suggesting that they rely too heavily on CGMejection for quenching. Star-forming galaxies are observed to have flatter andmore extended profiles than in simulations, suggesting under-efficient stellarfeedback models. Our results highlight the need to modify future prescriptionsof galaxy feedback models.

Testing galaxy feedback models with the first resolved profiles of the circumgalactic medium