Kavli Affiliate: Claudio Ricci
| Summary:
A tight correlation between nuclear millimeter (mm) and X-ray emission has recently been found in nearby ($z < 0.01$) and low-Eddington ratio ($rm λ_Edd < 0.1$) radio-quiet (RQ) Active Galactic Nuclei (AGN), suggesting a common origin in the hot X-ray corona. We test this relation in nine more distant RQ AGN ($z sim 0.06-0.16$) with higher bolometric luminosities ($log(L_rm bol/mathrmerg,s^-1)=45.3-46.3$), Eddington ratios ($rm λ_Edd = 0.19-0.85$), and X-ray bolometric corrections ($κ_2-10=29-194$), selected from the Burst Alert Telescope (BAT) survey. We obtained quasi-simultaneous observations with Swift at 2-10 keV and the Atacama Large Millimeter/submillimeter Array (ALMA) at 100 GHz and with high angular resolution ($<0.14$"). We find that these high-luminosity AGN lie above the mm/X-ray correlation defined by lower-luminosity sources. A joint fit to both samples yields a second-degree polynomial with an intrinsic scatter of 0.32 dex. Furthermore, the mm emission correlates linearly with both the UV disk luminosity and $L_rm bol$, with intrinsic scatters of 0.45 and 0.35 dex, respectively. We propose that the deviation from the linear mm/X-ray relation arises from a two-component coronal electron population: thermal electrons that produce X-rays, but become less efficient at higher luminosities, and non-thermal electrons that produce mm emission and remain tied to $L_rm bol$. Additional mm emission from outflow-driven shocks may also contribute, though SED modeling and spectral index studies favor a coronal origin.
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