Bar pattern speeds in CALIFA galaxies

Cuomo, V.; Lee, Yun Hee; Buttitta, Chiara; Aguerri, J. A. L.; Corsini, E. M.; Morelli, L.

doi:10.1051/0004-6361/202040261

Cited by 19 publications

(18 citation statements)

References 129 publications

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“…Figure 4 shows four example galaxies with three bar length measurements overlaid on their images. We present the positions of the tip of the bar measured from ellipse fitting (red), Fourier analysis (green), and force ratio (blue) on the images, in the same manner as Cuomo et al (2021). When we investigate the bar length measurements on images one by one, all three measurements are compatible for galaxies with simple structures such as shown in Figure 4(a).…”

Section: Bar Length and Resonancementioning

confidence: 90%

“…Because bars do not end with sharp edges, it is not trivial to define the full length. Although there have been lots of efforts to find the best way to determine the length of a bar, each method has its own strengths and weaknesses (Athanassoula & Misiriotis 2002;Michel-Dansac & Wozniak 2006;Cuomo et al 2021). The widely used way is to measure the radius where the ellipticity, , or the normalized Fourier amplitude, A 2 , profile reaches a maximum, at R or R A2 even though it cannot estimate the full length of the bar (Wozniak et al 1995;Athanassoula & Misiriotis 2002;Laurikainen & Salo 2002a,b).…”

Section: Corotation Radius Versus Bar Lengthmentioning

confidence: 99%

“…The widely used way is to measure the radius where the ellipticity, , or the normalized Fourier amplitude, A 2 , profile reaches a maximum, at R or R A2 even though it cannot estimate the full length of the bar (Wozniak et al 1995;Athanassoula & Misiriotis 2002;Laurikainen & Salo 2002a,b). Similarly, we can define the bar radius where the radial profile of the transverseto-radial force ratio has a plateau or a maximum peak, R Q b (Lee et al 2020;Cuomo et al 2021).…”

Section: Corotation Radius Versus Bar Lengthmentioning

confidence: 99%

“…Five galaxies are rejected because they have no R CR intersected by Ω bar in their angular velocity curves because of their rapid pattern speeds. Ultrafast bars with R ≤ 1 cannot exist theoretically, but they have existed in observations (Cuomo et al 2019(Cuomo et al , 2021Guo et al 2019). The possibility of real ultrafast bars was raised also by Zhang & Buta (2007).…”

Section: Corotation Radius Versus Bar Lengthmentioning

confidence: 99%

“…Red, green, and blue crosses indicate bar positions at R bar measured by ellipse fitting (R ), and Fourier analysis (RA2), and force ratio (R Qb ), respectively. The bar positions are determined by analyzing force ratio maps from R bar measured by each method (Lee et al 2020;Cuomo et al 2021). The middle row shows the relation between the bar pattern speed and the frequency curves for each class.…”

Section: Bar Pattern Speed Versus Frequency Curvesmentioning

confidence: 99%

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Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies

Lee,

Park,

Hwang

et al. 2021

Preprint

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We test the idea that bar pattern speeds decrease with time owing to angular momentum exchange with a dark matter halo. If this process actually occurs, then the locations of the corotation resonance and other resonances should generally increase with time. We therefore derive the angular velocity Ω and epicyclic frequency κ as functions of galactocentric radius for 85 barred galaxies using photometric data. Mass maps are constructed by assuming a dynamical mass-to-light ratio and then solving the Poisson equation for the gravitatonal potential. The location of Lindblad resonances and the corotation resonance radius are then derived using the standard precession frequency curves in conjunction with bar pattern speeds recently estimated from the Tremaine-Weinberg method as applied to Integral Field Spectroscopy (IFS) data. Correlations between physical properties of bars and their host galaxies indicate that bar length and the corotation radius depend on the disk circular velocity while bar strength and pattern speed do not. As the bar pattern speed decreases, bar strength, length, and corotation radius incease, but when bars are subclassified into fast, medium, and slow domains, no significant change in bar length is found. Only a hint of an increase of bar strength from fast to slow bars is found. These results suggest that bar length in galaxies undergoes little evolution, being instead determined mainly by the size of their host galaxy.

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Section: Bar Length and Resonancementioning

confidence: 90%

Section: Corotation Radius Versus Bar Lengthmentioning

confidence: 99%

Section: Corotation Radius Versus Bar Lengthmentioning

confidence: 99%

Section: Corotation Radius Versus Bar Lengthmentioning

confidence: 99%

Section: Bar Pattern Speed Versus Frequency Curvesmentioning

confidence: 99%

See 3 more Smart Citations

Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies

Lee,

Park,

Hwang

et al. 2021

Preprint

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A slow bar in the lenticular barred galaxy NGC 4277

Buttitta

Corsini

Cuomo

et al. 2022

A&A

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Aims. We characterised the properties of the bar hosted in lenticular galaxy NGC 4277, which is located behind the Virgo cluster. Methods. We measured the bar length and strength from the surface photometry obtained from the broad-band imaging of the Sloan Digital Sky Survey and we derived the bar pattern speed from the stellar kinematics obtained from the integral-field spectroscopy performed with the Multi Unit Spectroscopic Explorer at the Very Large Telescope. We also estimated the co-rotation radius from the circular velocity, which we constrained by correcting the stellar streaming motions for asymmetric drift, and we finally derived the bar rotation rate. Results. We found that NGC 4277 hosts a short (Rbar = 3.2−0.6+0.9 kpc), weak (Sbar = 0.21 ± 0.02), and slow (ℛ = 1.8−0.3+0.5) bar and its pattern speed (Ωbar = 24.7 ± 3.4 km s−1 kpc−1) is amongst the best-constrained ones ever obtained with the Tremaine–Weinberg (TW) method with relative statistical errors of ∼0.2. Conclusions. NGC 4277 is the first clear-cut case of a galaxy hosting a slow stellar bar (ℛ > 1.4 at more than a 1σ confidence level) measured with the model-independent TW method. A possible interaction with the neighbour galaxy NGC 4273 could have triggered the formation of such a slow bar and/or the bar could be slowed down due to the dynamical friction with a significant amount of dark matter within the bar region.

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Looking for a needle in a haystack: Measuring the length of a stellar bar

Ghosh,

Di Matteo

2024

A&A

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One of the challenges related to stellar bars is to accurately determine the length of the bar in a disc galaxy. In the literature, a wide variety of methods have been employed to measure the extent of a bar. However, a systematic study on determining the robustness and accuracy of different bar length estimators is still beyond our grasp. Here, we investigate the accuracy and the correlation (if any) between different bar length measurement methods while using an $N$-body model of a barred galaxy, where the bar evolves self-consistently in the presence of a live dark matter halo. We investigate the temporal evolution of the bar length, using different estimators (involving isophotal analysis of de-projected surface brightness distribution and Fourier decomposition of surface density), and we study their robustness and accuracy. We made further attempts to determine correlations among any two of these bar length estimators used here. In the presence of spirals, the bar length estimators that only consider the amplitudes of different Fourier moments (and do not take into account the phase-angle of $m=2$ Fourier moment) systematically overestimate the length of the bar. The strength of dark-gaps (produced by bars) is strongly correlated with the bar length in early rapid growth phase and is only weakly anti-correlated during subsequent quiescent phase of bar evolution. However, the location of dark-gaps is only weakly correlated to the bar length, hence, this information cannot be used as a robust proxy for determining the bar length. In addition, the bar length estimators, obtained using isophotal analysis of de-projected surface brightness distribution, systematically overestimate the bar length. The implications of bar length over(under)estimation in the context of determining fast and slow bars are further discussed in this work.

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Bar pattern speeds in CALIFA galaxies

Cited by 19 publications

References 129 publications

Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies

Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies

A slow bar in the lenticular barred galaxy NGC 4277

Looking for a needle in a haystack: Measuring the length of a stellar bar

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