The Central Region in M100: Observations and Modeling

Knapen, Johan H.; Beckman, J.; Heller, Clayton; Shlosman, Isaac; Jong, Roelof S. de

doi:10.1086/176516

Cited by 225 publications

(305 citation statements)

References 55 publications

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“…In addition to internal processes (e.g. AGN feedback, Dubois et al 2013;Gürkan et al 2015;Mullaney et al 2015;Bongiorno et al 2016; bar-driven evolution, Knapen et al 1995;Kormendy & Kennicutt 2004;Sheth et al 2005; morphological quenching, Martig et al 2009; virial gas heating, Birnboim & Dekel 2003;Cattaneo et al 2006;Gabor & Davé 2015;etc. ), interactions with local environments play a significant role in shaping the observed properties of galaxies.…”

Section: Introductionmentioning

confidence: 99%

Connecting optical and X-ray tracers of galaxy cluster relaxation

Roberts

Parker

Hlavacek-Larrondo

2018

Monthly Notices of the Royal Astronomical Society

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Substantial effort has been devoted in determining the ideal proxy for quantifying the morphology of the hot intracluster medium in clusters of galaxies. These proxies, based on X-ray emission, typically require expensive, high-quality X-ray observations making them difficult to apply to large surveys of groups and clusters. Here, we compare optical relaxation proxies with X-ray asymmetries and centroid shifts for a sample of SDSS clusters with high-quality, archival X-ray data from Chandra and XMM-Newton. The three optical relaxation measures considered are: the shape of the member-galaxy projected velocity distribution -measured by the Anderson-Darling (AD) statistic, the stellar mass gap between the most-massive and second-most-massive cluster galaxy, and the offset between the most-massive galaxy (MMG) position and the luminosityweighted cluster centre. The AD statistic and stellar mass gap correlate significantly with X-ray relaxation proxies, with the AD statistic being the stronger correlator. Conversely, we find no evidence for a correlation between X-ray asymmetry or centroid shift and the MMG offset. High-mass clusters (M halo > 10 14.5 M ) in this sample have X-ray asymmetries, centroid shifts, and Anderson-Darling statistics which are systematically larger than for low-mass systems. Finally, considering the dichotomy of Gaussian and non-Gaussian clusters (measured by the AD test), we show that the probability of being a non-Gaussian cluster correlates significantly with X-ray asymmetry but only shows a marginal correlation with centroid shift. These results confirm the shape of the radial velocity distribution as a useful proxy for cluster relaxation, which can then be applied to large redshift surveys lacking extensive X-ray coverage.

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Section: Introductionmentioning

confidence: 99%

Connecting optical and X-ray tracers of galaxy cluster relaxation

Roberts

Parker

Hlavacek-Larrondo

2018

Monthly Notices of the Royal Astronomical Society

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“…These dynamical effects have a wide range of consequences on both the gaseous and stellar content of the galaxy: the central bulge-like stellar component gets heated up (Berentzen et al 1998;Fathi & Peletier 2003;Kormendy & Kennicutt 2004;Athanassoula 2005;Berentzen et al 2007), while gas flows from the outer to the inner regions of the galaxy (Combes & Gerin 1985;Combes & Elmegreen 1993;Maciejewski et al 2002;Regan & Teuben 2004;Baba et al 2010;Masters et al 2012;Kubryk et al 2015). As a result, the radial chemical abundance profile initially flattens (Vila-Costas & Edmunds 1992;Martin & Roy 1994;Matteo et al 2013), and the concentration of gas in the centre of the galaxy increases (Knapen et al 1995;Sakamoto et al 1999). The accumulation of gas in the centre eventually triggers an increase in the star formation rate (SFR) (Devereux 1987 shown that this enhanced star formation activity increases the metallicity of the gas in the central region (Friedli et al 1994;Friedli & Benz 1995), thus explaining the origin of the observed break in the slope of the chemical abundance profiles of barred galaxies (Martin & Roy 1995;Roy & Walsh 1997;Considère et al 2000).…”

Section: Introductionmentioning

confidence: 99%

The mass dependence of star formation histories in barred spiral galaxies

Carles¹,

Martel²,

Ellison³

et al. 2016

Mon. Not. R. Astron. Soc.

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We performed a series of 29 gasdynamical simulations of disc galaxies, barred and unbarred, with various stellar masses, to study the impact of the bar on star formation history. Unbarred galaxies evolve very smoothly, with a star formation rate (SFR) that varies by at most a factor of three over a period of 2 Gyr. The evolution of barred galaxies is much more irregular, especially at high stellar masses. In these galaxies, the bar drives a substantial amount of gas toward the centre, resulting in a high SFR, and producing a starburst in the most massive galaxies. Most of the gas is converted into stars, and gas exhaustion leads to a rapid drop of star formation after the starburst. In massive barred galaxies (stellar mass M * > 2 × 10 10 M ⊙ ) the large amount of gas funnelled toward the centre is completely consumed by the starburst, while in lower-mass barred galaxies it is only partially consumed. Gas concentration is thus higher in lower-mass barred galaxies than it is in higher-mass ones. Even though unbarred galaxies funnelled less gas toward their centre, the lower SFR allows this gas to accumulate. At late times, the star formation efficiency is higher in barred galaxies than unbarred ones, enabling these galaxies to maintain a higher SFR with a smaller gas supply. Several properties, such as the global SFR, central SFR, or central gas concentration, vary monotonically with time for unbarred galaxies, but not for barred galaxies. Therefore one must be careful when comparing barred and unbarred galaxies that share one observational property, since these galaxies might be at very different stages of their respective evolution.

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“…Both theory and observations reveal the importance of inner Lindblad resonances (ILRs) in slowing down the radial gas inflow within the inner kiloparsec of barred galaxies (e.g., Schwarz 1984;Combes & Gerin 1985;Shlosman et al 1989;Athanassoula 1992;Sofue 1991;Kenney et al 1992;Knapen et al 1995aKnapen et al , 1995bJogee 2001;Jogee et al 2001). The resulting concentration of molecular gas leads to the formation of nuclear rings on scales of a few hundred parsecs (e.g., review by Buta & Combes 1996).…”

Section: Introductionmentioning

confidence: 99%

Gasdynamics in NGC 5248: Fueling a Circumnuclear Starburst Ring of Super–Star Clusters

Jogee

Shlosman

Laine

et al. 2002

ApJ

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Through observations and modeling, we demonstrate how the recently discovered large-scale bar in NGC 5248 generates spiral structure that extends from 10 kpc down to 100 pc, fuels star formation on progressively smaller scales, and drives disk evolution. Deep inside the bar, two massive molecular spirals cover nearly 180 in azimuth, show streaming motions of 20-40 km s À1 , and feed a starburst ring of super-star clusters at 375 pc. They also connect to two narrow K-band spirals that delineate the UV bright star clusters in the ring. The data suggest that the K-band spirals are young, and the starburst has been triggered by a bar-driven spiral density wave (SDW). The latter may even have propagated closer to the center where a second H ring and a dust spiral are found. The molecular and Hubble Space Telescope data support a scenario where stellar winds and supernovae efficiently clear out gas from dense star-forming regions on timescales less than a few Myr. We have investigated the properties of massive CO spirals within the framework of bar-driven SDWs, incorporating the effect of gas self-gravity. We find good agreement between the model predictions and the observed morphology, kinematics, and pitch angle of the spirals. This combination of observations and modeling provides the best evidence to date for a strong dynamical coupling between the nuclear region and the surrounding disk. It also confirms that a low central mass concentration, which may be common in late-type galaxies, is particularly favorable to the propagation of a bar-driven gaseous SDW deep into the central region of the galaxy, whereas a large central mass concentration favors other processes, such as the formation and decoupling of nuclear bars.

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The Central Region in M100: Observations and Modeling

Cited by 225 publications

References 55 publications

Connecting optical and X-ray tracers of galaxy cluster relaxation

Connecting optical and X-ray tracers of galaxy cluster relaxation

The mass dependence of star formation histories in barred spiral galaxies

Gasdynamics in NGC 5248: Fueling a Circumnuclear Starburst Ring of Super–Star Clusters

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