CO in the Disk of the Barred Spiral Galaxy M83: CO (1–0), CO (2–1), and Neutral Gas

Crosthwaite, Lucian P.; Turner, Jean L.; Buchholz, Leah M.; Ho, P. T. P.; Martin, Robert N.

doi:10.1086/339479

Cited by 68 publications

(26 citation statements)

References 69 publications

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“…The observed differences between the inner and outer fields is in agreement with the mass and environmentally dependent disruption model of Lamers et al (2005b), as the gas surface density in the inner region is higher by a factor of 3-4 than the outer region (Crosthwaite et al 2002). The observed differences also agree, at least in a qualitative sense, with the mass-independent cluster disruption model by Elmegreen & Hunter (2010) as well as the mass-dependent model presented by Gieles et al (2006), as the ambient GMC density is expected in both models to strongly affect the disruption process.…”

Section: Discussion a N D C O N C L U S I O N Ssupporting

confidence: 89%

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Evidence for environmentally dependent cluster disruption in M83

Bastian

Adamo

Gieles

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

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Using multiwavelength imaging from the Wide Field Camera 3 on the Hubble Space Telescope we study the stellar cluster populations of two adjacent fields in the nearby face‐on spiral galaxy, M83. The observations cover the galactic centre and reach out to ∼6 kpc, thereby spanning a large range of environmental conditions, ideal for testing empirical laws of cluster disruption. The clusters are selected by visual inspection to be centrally concentrated, symmetric and resolved on the images. We find that a large fraction of objects detected by automated algorithms (e.g. SExtractor or daofind) are not clusters, but rather are associations. These are likely to disperse into the field on time‐scales of tens of Myr due to their lower stellar densities and not due to gas expulsion (i.e. they were never gravitationally bound). We split the sample into two discrete fields (inner and outer regions of the galaxy) and search for evidence of environmentally dependent cluster disruption. Colour–colour diagrams of the clusters, when compared to simple stellar population models, already indicate that a much larger fraction of the clusters in the outer field are older by tens of Myr than in the inner field. This impression is quantified by estimating each cluster’s properties (age, mass and extinction) and comparing the age/mass distributions between the two fields. Our results are inconsistent with ‘universal’ age and mass distributions of clusters, and instead show that the ambient environment strongly affects the observed populations.

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Section: Discussion a N D C O N C L U S I O N Ssupporting

confidence: 89%

“…In principle, this result could also be due to a higher extinction in the outer field, but this is not a favoured scenario as (1) the inner regions host more gas/dust per unit surface area (e.g. Crosthwaite et al 2002) and (2) we do not see as many reddened clusters ( V − I > 0.8) in the outer field. In Fig.…”

Section: Tracing Cluster Disruptionmentioning

confidence: 91%

Evidence for environmentally dependent cluster disruption in M83

Bastian

Adamo

Gieles

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

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“…Therefore it must fall toward the center. In fact, both galaxies have high gas densities and active star formation in their bright centers (e. g., Crosthwaite et al 2002;Curran et al 2001a, b).…”

Section: Figurementioning

confidence: 99%

Secular Evolution and the Formation of Pseudobulges in Disk Galaxies

Kormendy¹,

Kennicutt

2004

Annu. Rev. Astron. Astrophys.

1,761

107

2,359

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The Universe is in transition. At early times, galactic evolution was dominated by hierarchical clustering and merging, processes that are violent and rapid. In the far future, evolution will mostly be secular: the slow rearrangement of energy and mass that results from interactions involving collective phenomena such as bars, oval disks, spiral structure, and triaxial dark halos. Both processes are important now. This paper reviews internal secular evolution, concentrating on one important consequence, the buildup of dense central components in disk galaxies that look like classical, merger-built bulges but that were made slowly out of disk gas. We call these pseudobulges.We begin with an "existence proof" -a review of how bars rearrange disk gas into outer rings, inner rings, and stuff dumped onto the center. Simulation results correspond closely to the morphology of barred galaxies. In the simulations, gas transported to small radii reaches high densities that plausibly feed star formation. In the observations, many SB and oval galaxies have dense central concentrations of gas and star formation. Optical colors and spectra often imply young stellar populations. So the formation of pseudobulges is well supported by theory and observations. It is embedded in a broader evolution picture that accounts for much of the richness observed in galaxy structure.If secular processes built dense central components that masquerade as bulges, how can we distinguish them from merger-built bulges? Observations show that pseudobulges retain a memory of their disky origin. 2That is, they have one or more characteristics of disks: (1) flatter shapes than those of classical bulges, (2) correspondingly large ratios of ordered to random velocities indicative of disk dynamics, (3) small velocity dispersions σ with respect to the Faber-Jackson correlation between σ and bulge luminosity, (4) spiral structure or nuclear bars in the "bulge" part of the light profile, (5) nearly exponential brightness profiles, and (6) starbursts. These structures occur preferentially in barred and oval galaxies in which secular evolution should be most rapid. So the cleanest examples of pseudobulges are recognizable.Are their formation timescales plausible? We use measurements of central gas densities and star formation rates to show that pseudobulges of the observed densities form on reasonable timescales of a few billion years.Thus a large variety of observational and theoretical results contribute to a new picture of galaxy evolution that complements hierarchical clustering and merging. Secular evolution consists of more than the aging of stellar populations. Every galaxy is dynamically evolving.

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“…Its beautiful symmetry and prominent spiral arms has earned the moniker, the Southern Pinwheel Galaxy. It is also notable for its extended H i disk, spanning more than a degree along its major axis (Tilanus & Allen 1993;Koribalski et al 2004;Koribalski 2008), and its central nuclear region that is almost exclusively molecular gas (Crosthwaite et al 2002;Lundgren et al 2008). In global terms, the molecular gas contributes about 25% to the total gas content.…”

Section: Case Study Of M 83mentioning

confidence: 99%

EXTENDING THE NEARBY GALAXY HERITAGE WITHWISE: FIRST RESULTS FROM THEWISEENHANCED RESOLUTION GALAXY ATLAS

Jarrett

Masci

Tsai

et al. 2012

The Astronomical Journal

280

166

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The Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at mid-infrared wavelengths 3.4 µm, 4.6 µm, 12 µm and 22 µm. The mission was primarily designed to extract point sources, leaving resolved and extended sources, for the most part, unexplored. Accordingly, we have begun a dedicated WISE Enhanced Resolution Galaxy Atlas (WERGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalogue. Here we demonstrate the first results of the WERGA-project for a sample of 17 galaxies, chosen to be of large angular size, diverse morphology, and covering a range in color, stellar mass and star formation. It includes many wellstudied galaxies, such as M 51, M 81, M 87, M 83, M 101, IC 342. Photometry and surface brightness decomposition is carried out after special super-resolution processing, achieving spatial resolutions similar to that of Spitzer -IRAC. The enhanced resolution method is summarized in the first paper of this two part series. In this second work, we present WISE, Spitzer and GALEX photometric and characterization measurements for the sample galaxies, combining the measurements to study the global properties. We derive star formation rates using the PAH-sensitive 12 µm (W3) fluxes, warm-dust sensitive 22 µm (W4) fluxes, and young massive-star sensitive UV fluxes. Stellar masses are estimated using the 3.4 µm (W1) and 4.6 µm (W2) measurements that trace the dominant stellar mass content. We highlight and showcase the detailed results of M 83, comparing the WISE/Spitzer results with the ATCA Hi gas distribution and GALEX UV emission, tracing the evolution from gas to stars. In addition to the enhanced images, WISE's all-sky coverage provides a tremendous advantage over Spitzer for building a complete nearby galaxy catalog, tracing both stellar mass and star-formation histories. We discuss the construction of a complete mid-infrared catalog of galaxies and its complementary role to study the assembly and evolution of galaxies in the local universe.

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CO in the Disk of the Barred Spiral Galaxy M83: CO (1–0), CO (2–1), and Neutral Gas

Cited by 68 publications

References 69 publications

Evidence for environmentally dependent cluster disruption in M83

Evidence for environmentally dependent cluster disruption in M83

Secular Evolution and the Formation of Pseudobulges in Disk Galaxies

EXTENDING THE NEARBY GALAXY HERITAGE WITHWISE: FIRST RESULTS FROM THEWISEENHANCED RESOLUTION GALAXY ATLAS

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