CO Multi-line Imaging of Nearby Galaxies (COMING). III. Dynamical effect on molecular gas density and star formation in the barred spiral galaxy NGC 4303

Yashima, Yoshiyuki, Kajikawa, Ayumi, Komatsuzaki, Ryusei, Kita, Shoichiro, Watanabe, Yoshimasa, Seta, Masumichi, Shibata, Shugo, Oi, Nagisa, Yasuda, Atsushi, Kuroda, Mayu, Yoda, Moe, Takeuchi, Tsutomu T, Noma, Yuto, Pan, Hsi-An, Matsumoto, Naoko, Morokuma-Matsui, Kana, Salak, Dragan, Sato, Yuya, Tanaka, Takahiro, Nakai, Naomasa, Nakanishi, Hiroyuki, Kaneko, Hiroyuki, Miyamoto, Yusuke, Muraoka, Kazuyuki, Kuno, Nario, Sorai, Kazuo, Yajima, Yoshiyuki

doi:10.1093/pasj/psz022

We present the results of 12CO(J = 1–0) and 13CO(J = 1–0) simultaneous mappings toward the nearby barred spiral galaxy NGC4303 as part of the CO Multi-line Imaging of Nearby Galaxies (COMING) project. Barred spiral galaxies often show lower starformation efficiency (SFE) in their bar region compared to the spiral arms. In this paper, we examine the relation between the SFEs and the volume densities of molecular gas n(H2) in the eight different regions within the galactic disk with CO data combined with archival far-ultraviolet and 24 μm data. We confirmed that SFE in the bar region is lower by 39% than that in the spiral arms. Moreover, velocity-alignment stacking analysis was performed for the spectra in the individual regions. Integrated intensity ratios of 12CO to 13CO (R12/13) ranging from 10 to 17 were the results of this stacking. Fixing a kinetic temperature ofmolecular gas, n(H2)was derived from R12/13 via non-local thermodynamic equilibrium (non-LTE) analysis. The density n(H2) in the bar is lower by 31%–37% than that in the arms and there is a rather tight positive correlation between SFEs and n(H2), with a correlation coefficient of ∼0.8. Furthermore, we found a dependence of n(H2) on the velocity dispersion of inter-molecular clouds (ΔV/sin i). Specifically, n(H2) increases as ΔV/sin i increases when ΔV/sin i < 100kms−1. On the other hand, n(H2) decreases as ΔV/sin i increases whenΔV/sin i>100kms−1. These relations indicate that the variations of SFE could be caused by the volume densities of molecular gas, and the volume densities could be governed by the dynamical influence such as cloud–cloud collisions, shear, and enhanced inner-cloud turbulence.

CO Multi-line Imaging of Nearby Galaxies (COMING). III. Dynamical effect on molecular gas density and star formation in the barred spiral galaxy NGC 4303

この論文をさがす

抄録

収録刊行物

被引用文献 (13)*注記

参考文献 (71)*注記

関連プロジェクト

キーワード

詳細情報詳細情報について

書き出し

問題の指摘