Bars in Disk‐dominated and Bulge‐dominated Galaxies at<i>z</i>∼ 0: New Insights from ∼3600 SDSS Galaxies

Barazza, Fabio D.; Jogee, Shardha; Marinova, Irina

doi:10.1086/526510

Cited by 232 publications

(362 citation statements)

References 96 publications

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“…4 is such an object. We find that ∼34% (652 objects) of the sample galaxies have i > 60 • , which is similar to results for other samples (Jogee et al 2004;Barazza et al 2008), that are comparable in size and where the same method has been applied.…”

Section: The Detection and Characterization Of Barssupporting

confidence: 86%

“…While it is still unknown why a specific disk galaxy hosts a bar and an apparently similar galaxy is unbarred, it is clear that a significant fraction of bright disk galaxies appears barred in optical observations (Eskridge et al 2000;Marinova & Jogee 2007;Reese et al 2007;Barazza et al 2008). In studies carried out in the near-infrared (NIR) or in both, NIR and optical, the NIR bar fractions are typically higher (Knapen 1999;Eskridge et al 2000;Laurikainen et al 2004;Menéndez-Delmestre et al 2007;Marinova & Jogee 2007).…”

Section: Introductionmentioning

confidence: 99%

“…By adopting this approach, strong bars were detected twice as frequently in near-infrared data than optical data (Eskridge et al 2000) and the bar fraction was found to increase between Sc galaxies and later types (Odewahn 1996). Apart from visual classification, a quantitative characterization of bars has been attempted using for instance, the gravitational torque method (Block et al 2002;Laurikainen et al 2002;Buta et al 2005), Fourier dissection Laurikainen et al 2006), and ellipse fits to the galaxy isophotes (Regan & Elmegreen 1997;Abraham et al 1999;Sheth et al 2000Sheth et al , 2002Sheth et al , 2008Knapen et al 2000;Erwin & Sparke 2002;Erwin 2005;Jogee et al 2002aJogee et al ,b, 2004Whyte et al 2002;Elmegreen et al 2004;Reese et al 2007;Menéndez-Delmestre et al 2007;Marinova & Jogee 2007;Barazza et al 2008). These methods provide measurements of the bar length and shape and enable the impact of the bar on the disk to be assessed.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: The Detection and Characterization Of Barssupporting

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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show abstract

“…This bar has a size of 6 kpc, i.e. quite large, since 72% of barred galaxies in a sample of 2000 galaxies from the SDSS have a size smaller than this (Barazza et al 2008). This bar also has an extremely blue color, that is consistent with a starburst, i.e.…”

Section: Introductionmentioning

confidence: 99%

A giant bar induced by a merger event at z = 0.4?

Peirani¹,

Hammer

Flores

et al. 2009

A&A

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Context. Disk galaxies are the most common galaxy population in the local universe. However, the formation of their disks and structures -in particular their bars -is still a matter of debate. Aims. We present a physical model of the formation of J033239.72-275154.7, a galaxy observed at z = 0.41 that contains a large, young bar of size 6 kpc. The study of this system is particularly interesting to the understanding of the connection between mergers and bars, as well as the properties and fate of this system in relation to disk galaxy formation. Methods. We compare the morphological and kinematic properties of J033239.72-275154.7, the latter obtained by the GIRAFFE spectrograph, to those derived from the merger of two spiral galaxies described by idealized N-body simulations, including a star formation prescription. Results. We found that the general morphological shape and most of the dynamical properties of the object can be well reproduced by a model in which the satellite is initially placed in a retrograde orbit and the mass ratio of the system is 1:3. In this scenario, a bar forms in the host galaxy after the first passage of the satellite, where a significant fraction of the available gas is consumed in an induced burst. In its later evolution, however, we find that J033239.72-275154.7, whose major progenitor was an Sab galaxy, will probably become a S0 galaxy. This is mainly due to the violent relaxation and the angular momentum loss experienced by the host galaxy during the merger process, which is caused by the adopted orbital parameters. This result suggests that the building of the Hubble sequence is influenced significantly by the last major collision. In the present case, the merger leads to a severe damage of the disk of the progenitor, leading to an evolution towards a more bulge-dominated galaxy. Conclusions.

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“…Roughly 30-40% of the spiral galaxies have a pronounced bar in optical wavelengths and if we take into account weaker bars, the fraction rises up to 60% (de Vaucouleurs 1963;Sellwood & Wilkinson 1993;Marinova & Jogee 2007;Barazza, Jogee & Marinova 2008;Sheth et al 2008;Aguerri, Méndez-Abreu & Corsini 2009;Nair & Abraham 2010;Masters et al 2011). Kinematic data shows the presence of strong non-circular gas motions in bars (e.g.…”

Section: Introductionmentioning

confidence: 99%

On the morphology of dust lanes in galactic bars

Sánchez-Menguiano¹,

Pérez²,

Zurita³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The aim of our study is to use dynamical simulations to explore the influence of two important dynamical bar parameters, bar strength and bar pattern speed, on the shape of the bar dust lanes. To quantify the shape of the dust lanes we have developed a new systematic method to measure the dust lane curvature. Previous numerical simulations have compared the curvature of bar dust lanes with the bar strength, predicting a relation between both parameters which has been supported by observational studies but with a large spread. We take into account the bar pattern speed to explore, simultaneously, the effect of both parameters on the dust lane shape.To that end, we separate our galactic bars in fast bars (1 < R < 1.4) and slow bars (R > 1.4), obtaining, as previous simulations, an inverse relation between the dust lane curvature and the bar strength for fast bars. For the first time, we extend the study to slow bars, finding a constant curvature as a function of the bar strength. As a result, we conclude that weak bars with straight dust lanes are candidates for slow bars. Finally, we have analysed a pilot sample of ten S 4 G galaxies, obtaining dust lane curvatures lying within the range covered by the simulations.

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Bars in Disk‐dominated and Bulge‐dominated Galaxies atz∼ 0: New Insights from ∼3600 SDSS Galaxies

Cited by 232 publications

References 96 publications

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

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

A giant bar induced by a merger event at z = 0.4?

On the morphology of dust lanes in galactic bars

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