The Environment of Barred Galaxies in the Low-Redshift Universe

Lin, Ye; Sodi, Bernardo Cervantes; Li, Cheng; Wang, Lixin; Wang, Enci

doi:10.1088/0004-637x/796/2/98

Cited by 31 publications

(37 citation statements)

References 87 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: 89%

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: 89%

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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“…Therefore, we conclude that the bar fraction enhancement in interacting clusters is probably not due to enhanced galaxy-galaxy interactions in such clusters. Moreover, we note that several previous studies also disfavour bar formation due to galaxy-galaxy interactions on a similar basis 3,23,24 .…”

supporting

confidence: 70%

Observational evidence for bar formation in disk galaxies via cluster–cluster interaction

Yoon

Lee

et al. 2019

Nat Astron

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Bars are an elongated structure that extends from the centre of galaxies, and about one-third of disk galaxies are known to possess bars 1,2,3 . These bars are thought to form either through a physical process inherent in galaxies 4,5,6 , or through an external process such as galaxygalaxy interactions 7,8,9 . However, there are other plausible mechanisms of bar formation that still need to be observationally tested.Here we present the observational evidence that bars can form via cluster-cluster interaction 10 . We examined 105 galaxy clusters at redshift 0.015 < z < 0.060 that are selected from the Sloan Digital Sky Survey data, and identified 16 interacting clusters. We find that the barred diskdominated galaxy fraction is about 1.5 times higher in interacting clusters than in clusters with no clear signs of ongoing interaction (42% versus 27%). Our result indicates that bars can form through a large-scale violent phenomenon, and cluster-cluster interaction should be considered an important mechanism of bar formation.We used a volume-limited sample of galaxies with log(M star /M ) ≥ 10.0 in the MPA-JHU catalogue, and selected 105 clusters with M 200 > 7 × 10 13 M in the redshift range of 0.015 < z < 0.060. Here, M star is the galaxy stellar mass, M the mass of Sun and M 200 the cluster halo mass (see Methods). Of these, 16 clusters were found to be in pairs or have substructures (see Methods) and are defined here as interacting clusters. Figure 1 shows examples of the surface number density maps, velocities, and spatial distributions for galaxies of clusters in isolation, in pairs, and with substructures.As detailed in Methods, we detected bars in the cluster member galaxies using a quantitative method that searches for an elongated structure that has a large ellipticity for several consecutive isophotal ellipses but a sudden drop beyond a certain radius, and a nearly constant position angle over only the high-ellipticity region. We complemented the bar classification with a visual inspection to exclude false classifications and add bar galaxies that were not detected by the automated method. This process also examines the radial surface brightness profiles of galaxies, from which we derived the bulge-tototal light ratio (B/T ) of each galaxy. Example images of barred and non-barred galaxies are presented in Fig. 2.The bar fraction of interacting clusters and noninteracting clusters as a function of B/T is shown in Fig. 3a. We find that the bar fraction is several times higher for galaxies with B/T ≤ 0.5 (hereafter, disk-dominated galaxies) than those with B/T > 0.5, in agreement with results from previous studies 2,11,12 . The results of previous numerical simulations also support the finding that the formation or maintenance of bars is prohibited in galaxies with high B/T or high central mass concentrations 13,14,15 . It is also known that bar formation can be suppressed in galaxies that are dynamically hot (random motions of stars are dominant) or have high velocity dispersions 4,5 . Given that bars are...

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“…Notwithstanding this, the case would fall into the category of the objects whose bar has been strongly suppressed. As mentioned above, some studies claim that the global effect of the gravitational perturbers could be summarised in a growth/formation inhibition (Li et al 2009;Lin et al 2014). It is interesting to compare our results to similar recent findings obtained by Moetazedian et al (2017), who detailed the effect of low-mass satellites on the bar growth in a barunstable galaxy.…”

Section: Discussionsupporting

confidence: 85%

External versus internal triggers of bar formation in cosmological zoom-in simulations

Zana

Dotti

Capelo

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The emergence of a large-scale stellar bar is one of the most striking features in disc galaxies. By means of state-of-the-art cosmological zoom-in simulations, we study the formation and evolution of bars in Milky Way-like galaxies in a fully cosmological context, including the physics of gas dissipation, star formation, and supernova feedback. Our goal is to characterise the actual trigger of the non-axisymmetric perturbation that leads to the strong bar observable in the simulations at z = 0, discriminating between an internal/secular versus an external/tidal origin. To this aim, we run a suite of cosmological zoom-in simulations altering the original history of galaxy-satellite interactions at a time when the main galaxy, though already bar-unstable, does not feature any non-axisymmetric structure yet. We find that the main effect of a late minor merger and of a close fly-by is to delay the time of bar formation and those two dynamical events are not directly responsible for the development of the bar and do not alter significantly its global properties (e.g. its final extension). We conclude that, once the disc has grown to a mass large enough to sustain global non-axisymmetric modes, then bar formation is inevitable.

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The Environment of Barred Galaxies in the Low-Redshift Universe

Cited by 31 publications

References 87 publications

A numerical study of interactions and stellar bars

A numerical study of interactions and stellar bars

Observational evidence for bar formation in disk galaxies via cluster–cluster interaction

External versus internal triggers of bar formation in cosmological zoom-in simulations

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