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Active galactic nucleus (AGN) feedback is postulated as a key mechanism forregulating star formation within galaxies. Studying the physical properties ofthe outflowing gas from AGN is thus crucial for understanding the co-evolutionof galaxies and supermassive black holes. Here we report 55 pc resolution ALMAneutral atomic carbon [CI] $^3P_1\text{-}^3P_0$ observations toward the central1 kpc of the nearby type-2 Seyfert galaxy NGC 1068, supplemented by 55 pcresolution CO($J=1\text{-}0$) observations. We find that [CI] emission withinthe central kpc is strongly enhanced by a factor of $>$5 compared to thetypical [CI]/CO intensity ratio of $\sim$0.2 for nearby starburst galaxies (inunits of brightness temperature). The most [CI]-enhanced gas (ratio $>$ 1)exhibits a kpc-scale elongated structure centered at the AGN that matches theknown biconical ionized gas outflow entraining molecular gas in the disk. Atruncated, decelerating bicone model explains well the kinematics of theelongated structure, indicating that the [CI] enhancement is predominantlydriven by the interaction between the ISM in the disk and the highly inclinedionized gas outflow (which is likely driven by the radio jet). Our resultsstrongly favor the "CO dissociation scenario" rather than the "in-situ Cformation" one which prefers a perfect bicone geometry. We suggest that thehigh [CI]/CO intensity ratio gas in NGC 1068 directly traces ISM in the diskthat is currently dissociated and entrained by the jet and the outflow, i.e.,the "negative" effect of the AGN feedback.

The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type-2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback