The Distribution of Barred Galaxies in the Virgo Cluster

Andersen, V.

doi:10.1086/117918

Cited by 28 publications

(34 citation statements)

References 25 publications

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“…The pioneering work of Thompson (1981) showed an increased fraction of barred galaxies in the central region of the Coma cluster indicating that tidal interactions trigger bar formation. Similar results were also found in other samples, especially for early-type galaxies (see Giuricin et al 1993;Andersen 1996;Eskridge et al 2000;Barazza et al 2009;Lansbury et al 2014;Lin et al 2014). More recently, Méndez-Abreu et al (2012) showed that the effect of the environment on the bar formation depends on the mass of the galaxy.…”

Section: Introductionsupporting

confidence: 88%

A numerical study of interactions and stellar bars

Martínez-Valpuesta

Aguerri

González-García

et al. 2016

Mon. Not. R. Astron. Soc.

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For several decades it has been known that stellar bars in disc galaxies can be triggered by interactions, or by internal processes such as dynamical instabilities. In this work, we explore the differences between these two mechanisms using numerical simulations. We perform two groups of simulations based on isolated galaxies, one group in which a bar develops naturally, and another group in which the bar could not develop in isolation. The rest of the simulations recreate 1:1 coplanar fly-by interactions computed with the impulse approximation. The orbits we use for the interactions represent the fly-bys in groups or clusters of different masses accordingly to the velocity of the encounter. In the analysis we focus on bars' amplitude, size, pattern speed and their rotation parameter, R = R CR /R bar . The latter is used to define fast (R < 1.4) and slow rotation (R > 1.4). Compared with equivalent isolated galaxies we find that bars affected or triggered by interactions: (i) remain in the slow regime for longer; (ii) are more boxy in face-on views; (iii) they host kinematically hotter discs. Within this set of simulations we do not see strong differences between retrograde or prograde fly-bys. We also show that slow interactions can trigger bar formation.

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Section: Introductionsupporting

confidence: 88%

A numerical study of interactions and stellar bars

Martínez-Valpuesta

Aguerri

González-García

et al. 2016

Mon. Not. R. Astron. Soc.

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“…A similar result was reported by Varela et al (2004). Interestingly, while the fraction of barred disks in clusters or groups is not higher than in the field (Kumai et al 1986;van den Bergh 2002van den Bergh , 2007Marinova et al 2009), Thompson (1981) and Andersen (1996) presented evidence that barred galaxies in the Coma and Virgo clusters are more concentrated toward the cluster centers than unbarred disks.…”

Section: Introductionsupporting

confidence: 72%

“…An analysis of the clustercentric distances of barred galaxies in the Coma cluster (Thompson 1981) showed that a significantly larger fraction of barred galaxies are located at the cluster core than larger clustercentric distances (the adopted core radius for Coma was ∼784 kpc). In a similar study of the Virgo cluster, Andersen (1996) found that the barred disk galaxies are more centrally concentrated than the unbarred disks. For S0 galaxies, the same study found that the distributions of barred and unbarred objects are the same.…”

Section: The Distribution Of Barred Galaxies Within the Clustersmentioning

confidence: 91%

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Barazza¹,

Jablonka

Desai

et al. 2009

A&A

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We present a study of large-scale bars in field and cluster environments out to redshifts of ∼0.8 using a final sample of 945 moderately inclined disk galaxies drawn from the EDisCS project. We characterize bars and their host galaxies and look for relations between the presence of a bar and the properties of the underlying disk. We investigate whether the fraction and properties of bars in clusters are different from their counterparts in the field. The properties of bars and disks are determined by ellipse fits to the surface brightness distribution of the galaxies using HST/ACS images in the F814W filter. The bar identification is based on quantitative criteria after highly inclined (>60 • ) systems have been excluded. The total optical bar fraction in the redshift range z = 0.4−0.8 (median z = 0.60), averaged over the entire sample, is 25% (20% for strong bars). For the cluster and field subsamples, we measure bar fractions of 24% and 29%, respectively. We find that bars in clusters are on average longer than in the field and preferentially found close to the cluster center, where the bar fraction is somewhat higher (∼31%) than at larger distances (∼18%). These findings however rely on a relatively small subsample and might be affected by small number statistics. In agreement with local studies, we find that disk-dominated galaxies have a higher optical bar fraction (∼45%) than bulge-dominated galaxies (∼15%). This result is based on Hubble types and effective radii and does not change with redshift. The latter finding implies that bar formation or dissolution is strongly connected to the emergence of the morphological structure of a disk and is typically accompanied by a transition in the Hubble type. The question whether internal or external factors are more important for bar formation and evolution cannot be answered definitely. On the one hand, the bar fraction and properties of cluster and field samples of disk galaxies are quite similar, indicating that internal processes are crucial for bar formation. On the other hand, we find evidence that cluster centers are favorable locations for bars, which suggests that the internal processes responsible for bar growth are supported by the typical interactions taking place in such environments.

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“…Thompson (1981) found a larger fraction of barred galaxies in the core of the Coma cluster and Giuricin et al (1993) reported a higher recurrence of early-type barred spirals in high local density environments. Later studies of local (Andersen 1996;Eskridge et al 2000) and intermediate-redshift clusters (Barazza et al 2009) showed similar findings and, more recently, Méndez-Abreu et al (2012) proved that by taking into account the different luminosity ranges, it is possible to detect different effects of the environment for luminous and faint galaxies located in clusters or in the field. They propose that interactions in bright disk galaxies that are stable enough against interactions trigger bar formation, while for faint galaxies, interactions are strong enough to heat the disk, inhibiting bar formation.…”

Section: Introductionmentioning

confidence: 69%

The Environment of Barred Galaxies in the Low-Redshift Universe

Lin

Sodi

et al. 2014

ApJ

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We present a study of the environment of barred galaxies using a volume-limited sample of over 30,000 galaxies drawn from the Sloan Digital Sky Survey. We use four different statistics to quantify the environment: the projected two-point cross-correlation function, the background-subtracted number count of neighbor galaxies, the overdensity of the local environment, and the membership of our galaxies to galaxy groups to segregate central and satellite systems. For barred galaxies as a whole, we find a very weak difference in all the quantities compared to unbarred galaxies of the control sample. When we split our sample into early-and late-type galaxies, we see a weak but significant trend for early-type galaxies with a bar to be more strongly clustered on scales from a few 100 kpc to 1 Mpc when compared to unbarred early-type galaxies. This indicates that the presence of a bar in early-type galaxies depends on the location within their host dark matter halos. This is confirmed by the group catalog in the sense that for early-types, the fraction of central galaxies is smaller if they have a bar. For late-type galaxies, we find fewer neighbors within ∼50 kpc around the barred galaxies when compared to unbarred galaxies from the control sample, suggesting that tidal forces from close companions suppress the formation/growth of bars. Finally, we find no obvious correlation between overdensity and the bars in our sample, showing that galactic bars are not obviously linked to the large-scale structure of the universe.

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The Distribution of Barred Galaxies in the Virgo Cluster

Cited by 28 publications

References 25 publications

A numerical study of interactions and stellar bars

A numerical study of interactions and stellar bars

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

The Environment of Barred Galaxies in the Low-Redshift Universe

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