THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS): ENVIRONMENTAL DEPENDENCE OF GIANT MOLECULAR CLOUD PROPERTIES IN M51

Colombo, D.; Hughes, Annie; Schinnerer, E.; Meidt, Sharon E.; Leroy, Adam K.; Pety, J.; Dobbs, Clare; García‐Burillo, S.; Dumas, G.; Thompson, Todd A.; Schuster, K.; Krämer, C.

doi:10.1088/0004-637x/784/1/3

Cited by 250 publications

(491 citation statements)

References 92 publications

(135 reference statements)

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“…On the contrary, our result would indicate that the GMAs are in diverse dynamical states. In fact, a lack of correlation between these two variables has also been reported in recent extragalactic observations with ≤ 50 pc resolution for a variety of galaxies (e.g., LMC, M33, M51, M101, NGC 628, and NGC 6946; Hughes et al 2013;Colombo et al 2014;Rebolledo et al 2015).…”

Section: Virial Parametersupporting

confidence: 58%

“…This dependence suggests that overall the high-M c GMAs in M100 tend to be more bound than low-M c GMAs. The dependence is also seen in the high-resolution observation of GMCs of M51 (Colombo et al 2014) and simulations (Shetty et al 2010;Fujimoto et al 2014a).…”

Section: Virial Parametermentioning

confidence: 63%

“…Extragalactic observations provide a perfect perspective for galactic-scale environments that are difficult to obtain from the edge-on Galactic observations. These observations of nearby galaxies redefine our understanding of galactic-scale environments such as galactic structures (bars, spiral arms, inter-arm regions) (Hughes et al 2013;Colombo et al 2014;Pan et al 2015a), regions of shear arising from galaxy rotation (Koda et al 2009;Meidt et al 2013;Miyamoto et al 2014), and galaxy types (dwarf, early-, and latetype galaxies) (Leroy et al 2008;Hughes et al 2013;Thilliez et al 2014) on the regulation of cloud properties. The importance of galactic-scale environments is also supported by galaxy simulations (Fujimoto et al 2014a;Renaud et al 2015).…”

Section: Introductionmentioning

confidence: 78%

“…L CO is typically higher than L CO,noex by a factor of ∼ 3 -5 for GMAs in the central region, a factor of 3 -3.5 higher in the bar and spiral arms, and ∼ 2.5 times higher in the inter-arm regions. This is because the brightness temperature gradient within the GMAs varies between the regions (Colombo et al 2014). The central region profile is the steepest, and the inter-arm profile is the most shallow.…”

Section: Comparison Of Gma Properties Between the Galactic Environmentsmentioning

confidence: 99%

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Variation in GMC Association Properties across the Bars, Spiral Arms, Inter-arms, and Circumnuclear Region of M100 (NGC 4321) Extracted from ALMA Observations

Pan

Kuno

2017

ApJ

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We study the physical properties of giant molecular cloud associations (GMAs) in M100 (NGC 4321) using the ALMA Science Verification feathered (12-m+ACA) data in 12 CO (1-0). To examine the environmental dependence of GMA properties, GMAs are classified based on their locations in the various environments as circumnuclear ring (CNR), bar, spiral, and inter-arm GMAs. The CNR GMAs are massive and compact, while the inter-arm GMAs are diffuse with low surface density. GMA mass and size are strongly correlated, as suggested by Larson (1981). However, the diverse power-law index of the relation implies that the GMA properties are not uniform among the environments. The CNR and bar GMAs show higher velocity dispersion than those in other environments. We find little evidence for a correlation between GMA velocity dispersion and size, which indicates that the GMAs are in diverse dynamical states. Indeed, the virial parameter of GMAs spans nearly two orders of magnitude. Only the spiral GMAs are in general self-gravitating. Star formation activity of the GMAs decreases in order over the CNR, spiral, bar, and the inter-arm GMAs. The diverse GMA and star formation properties in different environments lead to variations in the Kennicutt-Schmidt relation. A combination of multiple mechanisms or gas phase change is necessary to explain the observed slopes. Comparisons of GMA properties acquired with the use of the 12-m-array observations with those from the feathered data are also presented. The results show that the missing flux and extended emission cannot be neglected for the study of environmental dependence.

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Section: Virial Parametersupporting

confidence: 58%

Section: Virial Parametermentioning

confidence: 63%

Section: Introductionmentioning

confidence: 78%

Section: Comparison Of Gma Properties Between the Galactic Environmentsmentioning

confidence: 99%

See 2 more Smart Citations

Variation in GMC Association Properties across the Bars, Spiral Arms, Inter-arms, and Circumnuclear Region of M100 (NGC 4321) Extracted from ALMA Observations

Pan

Kuno

2017

ApJ

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“…Hughes et al (2013b) and Colombo et al (2014) showed that cloud-scale CO linewidths are typically related to the arm/interarm properties, as predicted in our model. Also, Hughes et al (2013a) presented observed 12 CO(1-0) line profiles for different regions of M51 showing that the linewidths are larger at regions with higher stellar surface densities, indicating that regions of deepest potential are indeed more turbulent.…”

Section: Discussionsupporting

confidence: 84%

The onset of large-scale turbulence in the interstellar medium of spiral galaxies

Falceta‐Gonçalves¹,

Bonnell²,

Kowal³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Turbulence is ubiquitous in the interstellar medium (ISM) of the Milky Way and other spiral galaxies. The energy source for this turbulence has been much debated with many possible origins proposed. The universality of turbulence, its reported largescale driving, and that it occurs also in starless molecular clouds, challenges models invoking any stellar source. A more general process is needed to explain the observations. In this work we study the role of galactic spiral arms. This is accomplished by means of three-dimensional hydrodynamical simulations which follow the dynamical evolution of interstellar diffuse clouds (∼ 100cm −3 ) interacting with the gravitational potential field of the spiral pattern. We find that the tidal effects of the arm's potential on the cloud result in internal vorticity, fragmentation and hydrodynamical instabilities. The triggered turbulence result in large-scale driving, on sizes of the ISM inhomogeneities, i.e. as large as ∼ 100pc, and efficiencies in converting potential energy into turbulence in the range ∼ 10 to 25 % per arm crossing. This efficiency is much higher than those found in previous models. The statistics of the turbulence in our simulations are strikingly similar to the observed power spectrum and Larson scaling relations of molecular clouds and the general ISM. The dependency found from different models indicate that the ISM turbulence is mainly related to local spiral arm properties, such as its mass density and width. This correlation seems in agreement with recent high angular resolution observations of spiral galaxies, e.g. M51 and M33.

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The Lifecycle of Clusters in Galaxies

Adamo

Bastian

2017

The Birth of Star Clusters

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We review many of the basic properties of star cluster systems, and focus in particular on how they relate to their host galaxy properties and ambient environment. The cluster mass and luminosity functions are well approximated by power-laws of the form Ndm ∝ M α dm, with α ∼ −2 over most of the observable range. However, there is now clear evidence that both become steeper at high masses/luminosities, with the value of the downward turn dependent on environment. The host galaxy properties also appear to affect the cluster formation efficiency (Γ -i.e., the fraction of stars that form in bound clusters), with higher starformation rate density galaxies having higher Γ values. Within individual galaxies, there is evidence for Γ to vary by a factor of 3 − 4, likely following the molecular gas surface density, in agreement with recent predictions. Finally, we discuss cluster disruption and its effect on the observed properties of a population, focussing on the age distribution of clusters. We briefly discuss the expectations of theoretical and numerical studies, and also the observed distributions in a number of galaxies. Most observational studies now find agreement with theoretical expectations, namely nearly a constant cluster age distribution for ages up to ∼ 100 Myr (i.e. little disruption), and a drastic steepening above this value caused by a combination of cluster disruption and incompleteness. Rapid cluster disruption for clusters with ages < 100 Myr is ruled out for most galaxies.

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THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS): ENVIRONMENTAL DEPENDENCE OF GIANT MOLECULAR CLOUD PROPERTIES IN M51

Cited by 250 publications

References 92 publications

Variation in GMC Association Properties across the Bars, Spiral Arms, Inter-arms, and Circumnuclear Region of M100 (NGC 4321) Extracted from ALMA Observations

Variation in GMC Association Properties across the Bars, Spiral Arms, Inter-arms, and Circumnuclear Region of M100 (NGC 4321) Extracted from ALMA Observations

The onset of large-scale turbulence in the interstellar medium of spiral galaxies

The Lifecycle of Clusters in Galaxies

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