Kavli Affiliate: Claudio Ricci
| First 5 Authors: Enrique Lopez-Rodriguez, Enrique Lopez-Rodriguez, , ,
| Summary:
The polar mid-infrared (MIR) emission detected within 10-100s pcs in some
active galactic nuclei (AGN) has been associated with dusty winds driven away
by radiation pressure. The physical characterization of this extended polar
emission remains uncertain. Here we combine 10-21 $mu$m JWST/MIRI imaging
observations with 7-25 $mu$m JWST/MRS integral field spectroscopic
observations of 6 nearby, $barD=35.4pm4.6$ Mpc, AGN from the GATOS Survey
to quantify the nature of the extended MIR emission at ~75 pc resolution at 21
$mu$m. These AGN have similar bolometric luminosities,
$log_10(barL_bol,[erg,s^-1])=44.0pm0.3$, span a wide range of
optical outflow rates, $dotM=0.003-0.21$ M$_odot$ yr$^-1$, column
densities, $log_10(N_H^X-ray[cm^-2])=22.2-24.3$, and Eddington ratios,
$lambda_Edd=0.005-0.06$. We cross-correlate the line-only and continuum-only
images and find a poor correlation, which indicates that the extended MIR
continuum emission is spatially uncorrelated with the warm outflows associated
with narrow emission lines within 10-15 $mu$m. Line emission is resolved along
the jet axis, while dust emission is perpendicular to it. The 75-450 pc
continuum emission has a fairly constant dust temperature,
$T_d=132^+7_-7$ K, and mass, $M_d=728^+29_-27$ M$_odot$. Using
the conditions of energy balance between radiation-pressure and gravity
($lambda_Edd$ vs. N$_H$), we find that our AGN sample is in the
gravitationally bounded regime consistent with no detection of dusty winds. At
10 $mu$m, the level of extended line emission contribution is correlated with
the outflow kinetic energy and mass outflow rates. We find no correlation with
the AGN properties. These results indicate that the radio jet may be triggering
the gas outflow and line emission, while the extended dust emission is
distributed in molecular clouds and/or shocked regions.
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