CO multi-line imaging of nearby galaxies (COMING). IV. Overview of the project-Reference-Cited by-同舟云学术

CO multi-line imaging of nearby galaxies (COMING). IV. Overview of the project

Published:2019-11-19 Issue: Volume: Page:
ISSN:0004-6264
Container-title:Publications of the Astronomical Society of Japan
language:en
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Author:

Sorai Kazuo¹²³⁴⁵,Kuno Nario⁴⁵,Muraoka Kazuyuki⁶^ORCID,Miyamoto Yusuke⁷⁸,Kaneko Hiroyuki⁷^ORCID,Nakanishi Hiroyuki⁹,Nakai Naomasa⁴⁵¹⁰,Yanagitani Kazuki⁶,Tanaka Takahiro⁴,Sato Yuya⁴,Salak Dragan¹⁰,Umei Michiko²,Morokuma-Matsui Kana⁷⁸¹¹¹²^ORCID,Matsumoto Naoko¹³¹⁴,Ueno Saeko⁹,Pan Hsi-An¹⁵,Noma Yuto¹⁰,Takeuchi Tsutomu T¹⁶,Yoda Moe¹⁶,Kuroda Mayu⁶,Yasuda Atsushi⁴,Yajima Yoshiyuki²,Oi Nagisa¹⁷,Shibata Shugo²,Seta Masumichi¹⁰,Watanabe Yoshimasa⁴⁵¹⁸,Kita Shoichiro⁴,Komatsuzaki Ryusei⁴,Kajikawa Ayumi²³,Yashima Yu²³,Cooray Suchetha¹⁶^ORCID,Baji Hiroyuki⁶,Segawa Yoko²,Tashiro Takami²,Takeda Miho⁶,Kishida Nozomi²,Hatakeyama Takuya⁴,Tomiyasu Yuto⁴,Saita Chey⁹

Affiliation:

1. Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo, Hokkaido 060-0810, Japan

2. Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo, Hokkaido 060-0810, Japan

3. Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo, Hokkaido 060-0810, Japan

4. Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan

5. Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan

6. Department of Physical Science, Osaka Prefecture University, 1-1 Gakuen, Sakai, Osaka 599-8531, Japan

7. Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano 384-1305, Japan

8. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

9. Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan

10. Department of Physics, School of Science and Technology, Kwansei Gakuin University, 2-1 Gakuen, Sanda, Hyogo 669-1337, Japan

11. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan

12. Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan

13. The Research Institute for Time Studies, Yamaguchi University, Yoshida 1677-1, Yamaguchi, Yamaguchi 753-8511, Japan

14. Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

15. Institute of Astronomy and Astrophysics, Academia Sinica, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan

16. Division of Particle and Astrophysical Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan

17. Tokyo University of Science, Faculty of Science Division II, Liberal Arts, 1-3, Kagurazaka Shinjuku-ku, Tokyo 162-8601 Japan

18. College of Engineering, Nihon University, 1 Nakagawara, Tokusada, Tamuramachi, Koriyama, Fukushima 963-8642, Japan

Abstract

AbstractObservations of the molecular gas in galaxies are vital to understand the evolution and star-forming histories of galaxies. However, galaxies with molecular gas maps of their whole discs at sufficient resolution to distinguish galactic structures are severely lacking. Millimeter-wavelength studies at a high angular resolution across multiple lines and transitions are particularly needed, severely limiting our ability to infer the universal properties of molecular gas in galaxies. Hence, we conducted a legacy project with the 45 m telescope of the Nobeyama Radio Observatory, called the CO Multi-line Imaging of Nearby Galaxies (COMING), which simultaneously observed 147 galaxies with high far-infrared (FIR) flux in 12CO, 13CO, and C18O J = 1–0 lines. The total molecular gas mass was derived using the standard CO–to–H2 conversion factor and found to be positively correlated with the total stellar mass derived from the WISE 3.4 μm band data. The fraction of the total molecular gas mass to the total stellar mass in galaxies does not depend on their Hubble types nor the existence of a galactic bar, although when galaxies in individual morphological types are investigated separately, the fraction seems to decrease with the total stellar mass in early-type galaxies and vice versa in late-type galaxies. No differences in the distribution of the total molecular gas mass, stellar mass, or the total molecular gas to stellar mass ratio was observed between barred and non-barred galaxies, which is likely the result of our sample selection criteria, in that we prioritized observing FIR bright (and thus molecular gas-rich) galaxies.

Funder

National Astronomical Observatory of Japan

Jet Propulsion Laboratory

California Institute of Technology

National Aeronautics and Space Administration

University of California

Japan Society for the Promotion of Science

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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