The Distribution of Bar and Spiral Arm Strengths in Disk Galaxies

Buta, R.; Vasylyev, S.; Salo, H.; Laurikainen, Eija

doi:10.1086/431251

Cited by 103 publications

(174 citation statements)

References 68 publications

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“…Eskridge et al 2000;Block et al 2002;Buta et al 2005;MJ07;Laurikainen et al 2004Laurikainen et al , 2007. Thus, there are numerous complementary results that we can use or compare with.…”

Section: Osubsgsmentioning

confidence: 99%

“…In § 2, we define our complete sample of 143 bright (M B ≤ −19.3) low-to-moderately inclined (i ≤ 70 • ) spirals from the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al 2002), which is widely used as the local reference sample for bright spirals by numerous studies (e.g., Eskridge et al 2000;Block et al 2002;Buta et al 2005;MJ07 ;Laurikainen et al 2004Laurikainen et al , 2007. In § 3, we perform 2D bulge-disk and bulge-disk-bar decompositions of H-band images using GALFIT (Peng et al 2002), and derive fractional light ratios (B/T , Bar/T , Disk/T ), as well as Sérsic indices and half light radii or scale lengths.…”

Section: Introductionmentioning

confidence: 99%

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BULGEnANDB/TIN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS

Weinzirl

Jogee

Khochfar

et al. 2009

ApJ

316

382

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We use the bulge Sérsic index n and bulge-to-total ratio (B/T ) to explore the fundamental question of how bulges form. We perform 2D bulge-disk-bar decomposition on H-band images of 143 bright, high mass (M ⋆ ≥ 1.0 × 10 10 M ⊙ ) low-to-moderately inclined (i < 70 • ) spirals. Our results are: (1) Our H-band bar fraction (∼ 58%) is consistent with that from ellipse fits. (5) We compare the results with predictions from a set of ΛCDM models. In the models, a high mass spiral can have a bulge with a present-day low B/T ≤ 0.2 only if it did not undergo a major merger since z ≤ 2. The predicted fraction (∼ 1.6%) of high mass spirals, which have undergone a major merger since z ≤ 4 and host a bulge with a present-day low B/T ≤ 0.2, is a factor of over thirty smaller than the observed fraction (∼ 66%) of high mass spirals with B/T ≤ 0.2. Thus, contrary to common perception, bulges built via major mergers since z ≤ 4 seriously fail to account for the bulges present in ∼ 66% of high mass spirals. Most of these present-day low B/T ≤ 0.2 bulges are likely to have been built by a combination of minor mergers and/or secular processes since z ≤ 4.

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“…Eskridge et al 2000;Block et al 2002;Buta et al 2005;MJ07;Laurikainen et al 2004Laurikainen et al , 2007. Thus, there are numerous complementary results that we can use or compare with.…”

Section: Osubsgsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

BULGEnANDB/TIN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS

Weinzirl

Jogee

Khochfar

et al. 2009

ApJ

316

382

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“…Different methods are adopted to determine these quantities. In particular, the bar strength can be measured using the gravitational torque exerted by the bar (Block et al 2002;Buta et al 2005), the maximum ellipticity of the bar (Martin 1995;Jogee et al 1999;Knapen et al 2000;Laine et al 2002;Marinova & Jogee 2007;Barazza et al 2008), Fourier decomposition (Elmegreen et al 1996), and visual estimates of strength (Eskridge et al 2002). As described in Sect.…”

Section: The Properties Of the Barsmentioning

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%

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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“…Several groups have estimated bar frequency from observations (Block et al 2002;Laurikainen et al 2004;Buta et al 2005) and, in the bar strength histogram, found a dearth of weak bars, with an extended wing of strong bars. In TC07, we estimated the bar frequency in a sample of pure stellar galaxy discs.…”

Section: Statistics Of Bar Frequencymentioning

confidence: 99%

Evolution of spiral galaxies in modified gravity

Tiret

Combes

2008

A&A

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The stability of spiral galaxies is compared in modified Newtonian Dynamics (MOND) and Newtonian dynamics with dark matter. We extend our previous simulations that involved pure stellar discs without gas, to deal with the effects of gas dissipation and star formation. We also vary the interpolating µ-function between the MOND and Newtonian regime. Bar formation is studied and compared in both dynamics, from initial conditions identical in visible component morphology and kinematics (same density profile, rotation curve, and velocity dispersion). One first result is that the MOND galaxy evolution is not affected by the choice of the µ-function, it develops bars with the same frequency and strength. The choice of the µ-function significantly changes the equivalent Newton models, in changing the dark matter to visible mass ratio and, therefore, changing the stability. The introduction of gas shortens the timescale for bar formation in the Newton model, but is not significantly shortened in the MOND model, since it was already small. As a consequence, with gas, the MOND and DM bar frequency histograms are now more similar than without gas. The thickening of the plane occurs through vertical resonance with the bar and peanut formation, and even more quickly with gas. Since the mass gets more concentrated with gas, the radius of the peanut is smaller, and the appearance of the pseudo-bulge is more boxy. The bar strength difference is moderated by saturation, and feedback effects, like the bar weakening or destruction by gas inflow due to gravity torques. Averaged over a series of models representing the Hubble sequence, the MOND models have still more bars, and stronger bars, than the equivalent Newton models, better fitting the observations. Gas inflows driven by bars produce accumulations at rings or pseudo-rings at Lindblad resonances, and MOND models can reproduce observed morphologies quite well, as was found before in the Newtonian dynamics.

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The Distribution of Bar and Spiral Arm Strengths in Disk Galaxies

Cited by 103 publications

References 68 publications

BULGEnANDB/TIN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS

BULGEnANDB/TIN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS

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

Evolution of spiral galaxies in modified gravity

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