Introduction

Erroz-Ferrer, Santiago

doi:10.1007/978-3-319-26398-4_1

Cited by 1 publication

(1 citation statement)

References 219 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…How and where stars form in galaxies are clues to understanding galaxy evolution, and require information about the distribution, dynamics, and physical properties of their molecular gas content. H II regions and massive stars are found in spiral arms (Lynds 1980;García Gómez & Athanassoula 1993;Thilker et al 2002;Oey et al 2003;Bresolin et al 2005), while only a few are found in the bar of some barred spiral galaxies (Koopmann et al 2001;James et al 2004;Hernandez et al 2005;Erroz-Ferrer et al 2015). Interacting and merging galaxies often display an abundance of star-forming regions in both their interface regions, especially compared to their spiral arms (Koopmann et al 2001;Wang et al 2004;Torres-Flores et al 2014), while little new stars form even in the spiral arms of some galaxies (van den Bergh 1976; Kennicutt & Edgar 1986;Masters et al 2010;Fraser-McKelvie et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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

Saito

Kuno

Muraoka

et al. 2019

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

Observations of the molecular gas in galaxies are vital to understanding the evolution and starforming 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 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, and 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.

show abstract