ALMA [C i] observations toward the central region of Seyfert galaxy NGC 613

PASJ: Publications of the Astronomical Society of Japan

Seta, Masumichi¹  Salak, Dragan²  Nakai, Naomasa²  Miyamoto, Yusuke³  Watanabe, Yoshimasa⁴  Ishii, Shun⁴ 

[1] Department of Physics, School of Science and Technology, Kwansei Gakuin University, 2-1 Gakuen, Sanda, Hyogo 669-1337, Japan;Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, Tsukuba, Ibaraki 305-8571, Japan;Nobeyama Radio Observatory, NAOJ, Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan;Tomonaga Center for the History of the Universe, University of Tsukuba, Tsukuba, Ibaraki 305-8571, Japan

关键词: galaxies: active;    galaxies: individual;    galaxies: ISM;    radio lines: ISM;    ISM: jets and outflows;   

DOI  :  10.1093/pasj/psy016

学科分类：天文学(综合)

来源: Oxford University Press

【 摘 要 】

We report ALMA observations of [C i](3P1 − 3P0), 13CO, and C18O(J = 1–0) toward the central region of a nearby Seyfert galaxy NGC 613. The very high resolutions of 0|${^{\prime\prime}_{.}}$|26 × 0|${^{\prime\prime}_{.}}$|23 (=22 × 20 pc) for [C i] and 0|${^{\prime\prime}_{.}}$|42 × 0|${^{\prime\prime}_{.}}$|35 (=36 × 30 pc) for 13CO, and C18O resolve the circumnuclear disk (CND) and star-forming ring. The distribution of [C i] in the ring resembles that of the CO emission, although [C i] is prominent in the CND. This can be caused by the low intensities of the CO isotopes due to the low optical depths under the high temperature in the CND. We found that the intensity ratios of [C i] to 12CO(3–2) (⁠|$R_{\rm C\,{\small I}/CO}$|⁠) and to 13CO(1–0) (⁠|$R_{\rm C\,{\small I}/^{13}CO}$|⁠) are high at several positions around the edge of the ring. The spectral profiles of CO lines mostly correspond each other in the spots of the ring and high |$R_{\rm C\,{\small I}/CO}$|⁠, but those of [C i] at spots of high |$R_{\rm C\,{\small I}/CO}$| are different from those of CO. These results indicate that [C i] at the high |$R_{\rm C\,{\small I}/CO}$| traces different gas from that traced by the CO lines. The [C i] kinematics along the minor axis of NGC 613 could be interpreted as a bubbly molecular outflow. The outflow rate of molecular gas is higher than star formation rate in the CND. The flow could be mainly boosted by the active galactic nucleus through its radio jets.

【 授权许可】

CC BY