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Aguerri, J. A. L.; Prieto, M.; Varela, A. M.; Muñoz–Tuñón, C.

doi:10.1023/a:1017582222580

Cited by 61 publications

(126 citation statements)

References 7 publications

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“…We use the two methods presented in Wozniak et al (1995) and Aguerri et al (2000) to derive a B for UGC 628.…”

Section: The Bar Semi-major Axismentioning

confidence: 99%

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A slow bar in a dark matter dominated galaxy

Chemin¹,

Hernandez²

2009

A&A

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Aims. We report on an estimate of the bar pattern speed Ω p for the low surface brightness spiral galaxy UGC 628. Methods. We applied the Tremaine-Weinberg method to high resolution Hα velocity and integrated emission maps of this dark matter dominated galaxy. Observations were made at the CFHT using the optical Fabry-Perot interferometer, FaNTOmM.Results. The Tremaine-Weinberg method estimates a bar pattern speed of (11.3 ± 2.0) km s −1 kpc −1 for UGC 628, which is among the lowest values found for a spiral galaxy. The corotation radius R c of the bar and the gaseous disc is R c = 9.8 +2.9 −2.0 kpc, implying a ratio R = R c /a B of 2.0 +0.5 −0.3 , where a B is the bar radius. The ratio is well beyond the usual range of values, 1.0 ≤ R ≤ 1.4, found for fast bars of high surface brightness barred galaxies. This implies that the bar in UGC 628 is slow. Conclusions. As shown through the use of numerical simulations, fast bars survive when the inner mass distribution of galaxies is dominated by the baryons over the dark matter. Our result suggests that the presence of slow bars in galaxies is likely related to the dominance of dark matter over the mass distribution.

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“…We use the two methods presented in Wozniak et al (1995) and Aguerri et al (2000) to derive a B for UGC 628.…”

Section: The Bar Semi-major Axismentioning

confidence: 99%

“…Aguerri et al (2000) define the bar as having the radial range where I B /I IB > 0.5[max(I B /I IB ) − min(I B /I IB )] + min(I B /I IB ). In this expression I B = I 0 +I 2 +I 4 +I 6 is the bar intensity, with I m being the even Fourier coefficients of order m, and I IB = I 0 − I 2 + I 4 − I 6 is the interbar intensity.…”

Section: The Bar Semi-major Axismentioning

confidence: 99%

A slow bar in a dark matter dominated galaxy

Chemin¹,

Hernandez²

2009

A&A

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“…They are (i) the well-known Tremaine-Winberg method (Tremaine & Weinberg 1984); its later modification to include multiple density wave patterns (Meidt et al 2008a(Meidt et al , 2008b combines photometric data with velocities derived from long-slit spectra placed parallel to the galaxy major axis (Kent 1987;Merrifield & Kruijken 1995;Gerssen et al 1999;Debattista et al 2002;Aguerri et al 2003;Corsini et al 2003;Debattista & Williams 2004;Rand & Wallin 2004;Zimmer et al 2004;Hernandez et al 2005;Fathi et al 2009;Corsini 2011, and references therein, Aguerri et al 2015). (ii) the gravitational potential distribution to reproduce the velocity map (Sanders & Tubbs 1980;England et al 1990;Garcia-Burillo et al 1993;Piñol-Ferrer et al 2014); (iii) the morphologies of the non-circular velocity map of the gas in the galaxy can be used (Canzian 1993;Rand 1995;Sempere et al 1995;Canzian & Allen 1997;Font et al 2011Font et al , 2014aFont et al , 2014b; (iv) finally, numerical simulations of barred galaxies are another method (Lindblad et al 1996;Laine & Heller 1999;Aguerri et al 2001;Weiner et al 2001;Pérez et al 2004;Rautiainen et al 2005Rautiainen et al , 2008Treuthardt et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most Slowly

Font

Beckman

Martínez-Valpuesta

et al. 2017

ApJ

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We have used Spitzer images of a sample of 68 barred spiral galaxies in the local universe to make systematic measurements of bar length and bar strength. We combine these with precise determinations of the corotation radii associated with the bars, taken from our previous study, which used the phase change from radial inflow to radial outflow of gas at corotation, based on high-resolution two-dimensional velocity fields in Hα taken with a FabryPérot spectrometer. After presenting the histograms of the derived bar parameters, we study their dependence on the galaxy morphological type and on the total stellar mass of the host galaxy, and then produce a set of parametric plots. These include the bar pattern speed versus bar length, the pattern speed normalized with the characteristic pattern speed of the outer disk versus the bar strength, and the normalized pattern speed versus , the ratio of corotation radius to bar length. To provide guidelines for our interpretation, we used recently published simulations, including disk and dark matter halo components. Our most striking conclusion is that bars with values of  < 1.4, previously considered dynamically fast rotators, can be among the slowest rotators both in absolute terms and when their pattern speeds are normalized. The simulations confirm that this is because as the bars are braked, they can grow longer more quickly than the outward drift of the corotation radius. We conclude that dark matter halos have indeed slowed down the rotation of bars on Gyr timescales.

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“…Fourier techniques are also commonly used to measure the bar torque (e.g. Aguerri et al 2000;Buta, Block & Knapen 2003;Martínez-Valpuesta, Shlosman & Heller 2006).…”

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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Cited by 61 publications

References 7 publications

A slow bar in a dark matter dominated galaxy

A slow bar in a dark matter dominated galaxy

Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most Slowly

On the morphology of dust lanes in galactic bars

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