Characterizing Bars at<i>z</i>∼ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift

Marinova, Irina; Jogee, Shardha

doi:10.1086/512355

Cited by 262 publications

(355 citation statements)

References 71 publications

(188 reference statements)

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“…The resulting large errors in the PA would cause inaccurate deprojections. We also note that the statistical results before and after deprojection are very similar (Marinova & Jogee 2007).…”

Section: The Detection and Characterization Of Barssupporting

confidence: 57%

“…We use e bar as a partial measure of the bar strength and a max as an estimate for the semi-major axis of the bar, a bar . A detailed theoretical and empirical justification of this approach is provided in Marinova & Jogee (2007) and Menéndez-Delmestre et al (2007) (see also the discussion in Sect. 5).…”

Section: The Detection and Characterization Of Barsmentioning

confidence: 99%

“…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). These findings indicate that bar detection is affected by dust extinction and that studies completed at different wavelengths cannot be readily compared.…”

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: 57%

Section: The Detection and Characterization Of Barsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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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“…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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Optical multiband surface photometry of a sample of Seyfert galaxies: III. Global, isophotal, and bar parameters

Slavcheva-Mihova

Mihov

2011

Astron Nachr

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This paper is third in a series, studying the optical properties of a sample of Seyfert galaxies. Here we present a homogeneous set of global (ellipticity, position angle, inclination, and total magnitude) and isophotal (semi-major axis and colour indices at 24 V mag arcsec −2 ) parameters of the galaxy sample. We find the following median corrected isophotal colour24 = 1.1 mag arcsec −2 . A set of bar parameters (ellipticity, position angle, semi-major axis corresponding to the ellipticity maximum in the bar region, and length) are also reported; deprojection has been applied to the bar ellipticity, length, and relative length in terms of galaxy isophotal semi-major axis. Regarding bar length estimation, we use a method, based on the relation between the behaviour of the profiles and orbit analysis. The so estimated bar length tightly correlates with the semi-major axis, corresponding to the ellipticity maximum with a median ratio of the former to the latter of 1.22. The median of the deprojected bar ellipticity, length, and relative length are 0.39, 5.44 kpc, and 0.44, respectively. There is a correlation between the deprojected bar length and the corrected isophotal semi-major axis at 24 V mag arcsec −2 . Three of the 17 large-scale bars appear strong, based on the deprojected bar ellipticity as a first-order approximation of bar strength. The deprojected relative bar length does not appear to correlate with the bar ellipticity.

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Characterizing Bars atz∼ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift

Cited by 262 publications

References 71 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

On the morphology of dust lanes in galactic bars

Optical multiband surface photometry of a sample of Seyfert galaxies: III. Global, isophotal, and bar parameters

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