CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the   Project

Kazuo Sorai (1; 2; 3; 4; 5); Nario Kuno (4; 5); Kazuyuki Muraoka; (6); Yusuke Miyamoto (7; 8); Hiroyuki Kaneko (7); Hiroyuki Nakanishi (9),; Naomasa Nakai (4; 5; 10); Kazuki Yanagitani (6); Takahiro Tanaka (4); Yuya; Sato (4); Dragan Salak (10); Michiko Umei (2); Kana Morokuma-Matsui (7; 8; 11; and 12); Naoko Matsumoto (13; 14); Saeko Ueno (9); Hsi-An Pan (15); Yuto; Noma (10); Tsutomu T. Takeuchi (16); Moe Yoda (16); Mayu Kuroda (6); Atsushi; Yasuda (4); Yoshiyuki Yajima (2); Nagisa Oi (17); Shugo Shibata (2),; Masumichi Seta (10); Yoshimasa Watanabe (4; 5; 18); Shoichiro Kita (4),; Ryusei Komatsuzaki (4); Ayumi Kajikawa (2; 3); Yu Yashima (2; 3),; Suchetha Cooray (16); Hiroyuki Baji (6); Yoko Segawa (2); Takami Tashiro (2),; Miho Takeda (6); Nozomi Kishida (2); Takuya Hatakeyama (4); Yuto Tomiyasu (4); and Chey Saita (9) ((1) Department of Physics; Faculty of Science; Hokkaido; University; (2) Department of Cosmosciences; Graduate School of Science,; Hokkaido University; (3) Department of Physics; School of Science; Hokkaido; University; (4) Division of Physics; Faculty of Pure; Applied Sciences,; University of Tsukuba; (5) Tomonaga Center for the History of the Universe; (TCHoU); University of Tsukuba; (6) Department of Physical Science; Osaka; Prefecture University; (7) Nobeyama Radio Observatory; National Astronomical; Observatory of Japan; (8) Chile Observatory; National Astronomical; Observatory of Japan; (9) Graduate School of Science; Engineering,; Kagoshima University; (10) Department of Physics; School of Science and; Technology; Kwansei Gakuin University; (11) Institute of Space and; Astronautical Science; Japan Aerospace Exploration Agency; (12) Institute of; Astronomy; Graduate School of Science; The University of Tokyo; (13) The; Research Institute for Time Studies; Yamaguchi University; (14) Mizusawa VLBI; Observatory; National Astronomical Observatory of Japan; (15) Institute of; Astronomy; Astrophysics; Academia Sinica; (16) Division of Particle and; Astrophysical Science; Nagoya University; (17) Tokyo University of Science,; Faculty of Science Division II; (18) College of Engineering; Nihon; University)

arXiv:1910.03863·astro-ph.GA·October 10, 2019

CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project

Kazuo Sorai (1, 2, 3, 4, 5), Nario Kuno (4, 5), Kazuyuki Muraoka, (6), Yusuke Miyamoto (7, 8), Hiroyuki Kaneko (7), Hiroyuki Nakanishi (9),, Naomasa Nakai (4, 5, 10), Kazuki Yanagitani (6), Takahiro Tanaka (4), Yuya, Sato (4), Dragan Salak (10), Michiko Umei (2)

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TL;DR

This project provides a comprehensive high-resolution survey of molecular gas in 147 nearby galaxies, revealing correlations with stellar mass and analyzing the influence of galaxy morphology and bars on molecular gas distribution.

Contribution

It offers the first large-scale, multi-line molecular gas imaging survey of nearby galaxies, enabling detailed analysis of gas properties across different galaxy types.

Findings

01

Total molecular gas mass correlates with stellar mass.

02

Molecular gas fraction is independent of Hubble type and bars overall.

03

In specific types, the gas fraction varies with stellar mass.

Abstract

Observations of the molecular gas in galaxies are vital to understanding the evolution and star-forming histories of galaxies. However, galaxies with molecular gas maps of their whole discs having 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 flux in $^{12}$ CO, $^{13}$ CO, and C $^{18}$ O $J = 1 - 0$ lines. The total molecular gas mass was derived using the standard CO-to-H $_{2}$ conversion factor and found to be positively…

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