The kiloparsec-scale neutral atomic carbon outflow in the nearby Type 2 Seyfert 
Galaxy NGC 1068: Evidence for negative AGN feedback

Saito, Toshiki; Takano, Shuro; Harada, Nanase; Nakajima, Taku; Schinnerer, Eva; Liu, Daizhong; Taniguchi, Akio; Izumi, Takuma; Watanabe, Yumi; Bamba, Kazuharu; Herbst, Eric; Kohno, Kotaro; Nishimura, Yuri; Stuber, Sophia; Tamura, Yoichi; Tosaki, Tomoka

doi:10.3847/2041-8213/ac59ae

Item

ITEM ACTIONSEXPORT

Add to Basket

Local TagsRelease HistoryDetailsSummary

Released

Journal Article

The kiloparsec-scale neutral atomic carbon outflow in the nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for negative AGN feedback

MPS-Authors

/persons/resource/persons268028

Liu, Daizhong
MPI for Extraterrestrial Physics, Max Planck Society;

External Resource

No external resources are shared

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

Fulltext (public)

There are no public fulltexts stored in PuRe

Supplementary Material (public)

There is no public supplementary material available

Citation

Saito, T., Takano, S., Harada, N., Nakajima, T., Schinnerer, E., Liu, D., et al. (2022). The kiloparsec-scale neutral atomic carbon outflow in the nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for negative AGN feedback. The Astrophysical Journal Letters, 927(2): L32. doi:10.3847/2041-8213/ac59ae.

Cite as: https://hdl.handle.net/21.11116/0000-000A-8EA6-B

Abstract

Active galactic nucleus (AGN) feedback is postulated as a key mechanism for regulating star formation within galaxies. Studying the physical properties of the outflowing gas from AGNs is thus crucial for understanding the coevolution of galaxies and supermassive black holes. Here we report 55 pc resolution ALMA neutral atomic carbon [C I] ³P₁−³P₀ observations toward the central 1 kpc of the nearby Type 2 Seyfert galaxy NGC 1068, supplemented by 55 pc resolution CO(J = 1−0) observations. We find that [C I] emission within the central kiloparsec is strongly enhanced by a factor of >5 compared to the typical [C I]/CO intensity ratio of ∼0.2 for nearby starburst galaxies (in units of brightness temperature). The most [C I]-enhanced gas (ratio > 1) exhibits a kiloparsec-scale elongated structure centered at the AGN that matches the known biconical ionized gas outflow entraining molecular gas in the disk. A truncated, decelerating bicone model explains well the kinematics of the elongated structure, indicating that the [C I] enhancement is predominantly driven by the interaction between the ISM in the disk and the highly inclined ionized gas outflow (which is likely driven by the radio jet). Our results strongly favor the "CO dissociation scenario" rather than the "in situ C formation" one, which prefers a perfect bicone geometry. We suggest that the high-[C I]/CO intensity ratio gas in NGC 1068 directly traces ISM in the disk that is currently dissociated and entrained by the jet and the outflow, i.e., the "negative" effect of the AGN feedback.