Molecular Clouds in Nearby Galaxies

By Y. Fukui, A. Kawamura. 2010

166 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/256783e4b72bc3beef78aab74cb003ff8523dd01

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In Astronomy and Astrophysics

Citations in the corpus

Dusty Star Forming Galaxies at High Redshift (2014, background): “Most disk galaxies that have been studied at high enough spatial resolution to resolve (at least massive) GMCs have shown that they seem to follow similar cloud scaling relations as in the Milky Way (Bolatto et al., 2008; Fukui and Kawamura, 2010; Dobbs et al., 2013).”
A CONSTANT MOLECULAR GAS DEPLETION TIME IN NEARBY DISK GALAXIES (2011, background): “Based on detailed studies of Local Group galaxies (e.g. Blitz et al. 2007; Bolatto et al. 2008; Bigiel et al. 2010a; Fukui & Kawamura 2010), they speculated that the ap- 14 We normalize the fit at ΣH2 = 10 M⊙ pc −2 following B08. proximately linear ΣSFR-ΣH2 relation arises because star formation in…”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Studies of molecular cloud properties in other galaxies have been recently reviewed (Fukui & Kawamura 2010; Blitz et al. 2007).”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, background): “The combination of these radiative processes with stellar winds and supernova explosions drive the disruption of giant molecular clouds (GMC) in∼ 30Myr (Fukui & Kawamura 2010), the typical lifetime of a massive star that explodes as a core-collapsed supernova.”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, result): “To a similar level, our molecular dispersions agree with other GMC measurements in M31 (Rosolowsky 2007), the LMC (Fukui et al. 2008), and the SMC (Mizuno et al. 2001, see also the review by Fukui & Kawamura 2010).”
A general model for the CO–H2 conversion factor in galaxies with applications to the star formation law (2011, result): “GMCs that are not resolved (typically low-mass GMCs in large cells in the adaptive mesh) have a floor surface density of the aforementioned value imposed, consistent with observations of Local Group GMCs (e.g. Bolatto et al. 2008; Fukui & Kawamura 2010).”
LOW CO LUMINOSITIES IN DWARF GALAXIES (2012, background): “…from environment as indicated by the similarity of molecular cloud properties in our and nearby galaxies (Blitz et al. 2007; Bolatto et al. 2008; Fukui & Kawamura 2010), the universality of SFE per free-fall time in clouds of different mass and density (Krumholz & Tan 2007), and evidence in…”
The CO-to-H2 Conversion Factor (2013, background): “Very little is known currently on the distribution of GMC sizes outside the Local Group (Blitz et al. 2007; Fukui & Kawamura 2010), and although this is a potential source of uncertainty in practical terms this ratio is unlikely to be the dominant source of galaxy-to-galaxy variation in αCO.”
Molecular Clouds in the Milky Way (2015, background): “…2012, Kennicutt & Evans 2012, Krumholz 2014); interstellar turbulence (Scalo & Elmegreen 2004, Elmegreen & Scalo 2004); cold, dark clouds (Bergin & Tafalla 2007); nearby galaxies (Fukui & Kawamura 2010); magnetic fields (Crutcher 2012); and the CO-to-H2 conversion factor (Bolatto et al. 2013).”
MOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES (2013, background): “These individual elements have distinct ages and evolutionary sequences (e.g. Kawamura et al. 2009; Fukui & Kawamura 2010) so that the ratio of molecular gas to stars in a region and the emission of star formation rate tracers both evolve as a function of time (see discussion and plots in L12).”
THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, background): “In the local universe, stars form out of clouds made of molecular hydrogen (H2) (e.g., Fukui & Kawamura 2010).”
A UNIVERSAL, LOCAL STAR FORMATION LAW IN GALACTIC CLOUDS, NEARBY GALAXIES, HIGH-REDSHIFT DISKS, AND STARBURSTS (2011, unknown): “…that the properties of star-forming molecular clouds in nearby galaxies show no systematic variation with galactic properties (Bolatto et al. 2008; Fukui & Kawamura 2010) (although there is some preliminary evidence that the GMCmass function might vary from galaxy to galaxy – Rosolowsky 2005;…”
TOWARD A COMPLETE ACCOUNTING OF ENERGY AND MOMENTUM FROM STELLAR FEEDBACK IN GALAXY FORMATION SIMULATIONS (2012, methodology): “Below we discuss an alternative way of estimating τIR based on observed properties of young star clusters and molecular clumps, which can readily be implemented in simulations adopting spatial a resolution of ∆x∼ 10 − 100pc. Surface densities of observed star forming clumps Observed molecular clouds”
THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD (2011, background): “INTRODUCTION Recent surveys of CO in Local Group galaxies have achieved sufficient resolution to resolve individual molecular clouds (see reviews by Blitz et al. 2007; Fukui & Kawamura 2010).”
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS): ENVIRONMENTAL DEPENDENCE OF GIANT MOLECULAR CLOUD PROPERTIES IN M51 (2014, background): “…distributions tend to be adequately represented by simple power laws (e.g., Rosolowsky 2005 and references therein), although previous studies have noted that the cloud mass distribution steepens at high masses in the LMC (Fukui et al. 2008; Fukui & Kawamura 2010) and in M33 (Gratier et al. 2012).”
Implementing molecular hydrogen in hydrodynamic simulations of galaxy formation (2012, background): “For example, molecular clouds (MCs) are observed to be the sites of star formation both in the Milky Way (e.g. Blitz 1993) and in nearby galaxies (Fukui & Kawamura 2010).”