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We estimate the amount of negative feedback energy injected into the ISM ofthe host galaxy of 3C273, a prototypical radio loud quasar. We obtained 93, 233and 343 GHz continuum images with the Atacama Large Millimeter/Sub-millimeterArray (ALMA). After self calibration and point source subtraction, we reach animage dynamic range of $\sim 85000$ at 93\ GHz, $\sim 39000$ at 233\ GHz and$\sim 2500$ at 343\ GHz. These are currently the highest image dynamic rangeobtained using ALMA. We detect spatially extended millimeter emissionassociated with the host galaxy, cospatial with the Extended Emission LineRegion (EELR) observed in the optical. The millimeter spectral energydistribution and comparison with centimeter data show that the extendedemission cannot be explained by dust thermal emission, synchrotron or thermalbremsstrahlung arising from massive star formation. We interpret the extendedmillimeter emission as thermal bremsstrahlung from gas directly ionized by thecentral source. The extended flux indicates that at least $\sim 7\%$ of thebolometric flux of the nuclear source was used to ionize atomic hydrogen in thehost galaxy. The ionized gas is estimated to be as massive as $10^{10}$ to$10^{11}\ \mathrm{M_\odot}$, but the molecular gas fraction with respect to thestellar mass is consistent with other ellipticals, suggesting that directionization ISM by the QSO may not be sufficient to suppress star formation, orwe are witnessing a short timescale before negative feedback becomesobservable. The discovery of a radio counterpart to EELRs provides a newpathway to studying the QSO-host ISM interaction.

Detection of extended millimeter emission in the host galaxy of 3C273 and its implications for QSO feedback via high dynamic range ALMA imaging