The Bar Pattern Speed of NGC 1433 Estimated via Sticky-Particle Simulations

Treuthardt, P.; Salo, H.; Rautiainen, P.; Buta, Ronald J.

doi:10.1088/0004-6256/136/1/300

Cited by 24 publications

(26 citation statements)

References 39 publications

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“…Our model does well to approximate the shape and extent of the inner and outer ring. The outer ring appears to be due to gas trapped in ‘banana’ orbits and circulating around the L 4 and L 5 Lagrangian regions, as was seen in the simulation models of NGC 1433 (Treuthardt et al 2008). The observed image of NGC 4593 also shows an apparent ‘plume’, similar to those seen in NGC 1433, near the leading edge of the bar and in the upper left quadrant of the B ‐band image.…”

Section: Discussionmentioning

confidence: 62%

“…In doing so, we varied Ω p by allowing to increase from 1.0 by increments of 0.1. Treuthardt et al (2008) investigated the morphological effects of differing the gravitational potential used in the simulations of NGC 1433. They found that the different M / L models of Bell & de Jong (2001) had little effect on the modelled morphology of the galaxy.…”

Section: Discussionmentioning

confidence: 99%

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On the link between central black holes, bar dynamics and dark matter haloes in spiral galaxies

Treuthardt

Seigar

Sierra

et al. 2012

Monthly Notices of the Royal Astronomical Society

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The discovery of a relationship between supermassive black hole (SMBH) mass and spiral arm pitch angle (P) is evidence that SMBHs are tied to the overall secular evolution of a galaxy. The discovery of SMBHs in late‐type galaxies with little or no bulge suggests that an underlying correlation between the dark matter halo concentration and SMBH mass (MBH) exists, rather than between the bulge mass and MBH. In this paper we measure P using a two‐dimensional fast Fourier transform and estimate the bar pattern speeds of 40 barred spiral galaxies from the Carnegie‐Irvine Galaxy Survey. The pattern speeds were derived by estimating the gravitational potentials of our galaxies from Ks‐band images and using them to produce dynamical simulation models. The pattern speeds allow us to identify those galaxies with low central dark halo densities, or fast rotating bars, while P provides an estimate of MBH. We find that a wide range of MBH exists in galaxies with low central dark matter halo densities, which appears to support other theoretical results. We also find that galaxies with low central dark halo densities appear to follow more predictable trends in P versus de Vaucouleurs morphological type (T) and bar strength versus T than barred galaxies in general. The empirical relationship between MBH and total gravitational mass of a galaxy (Mtot) allows us to predict the minimum Mtot that will be observationally measured of our fast bar galaxies. These predictions will be investigated in a subsequent paper.

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Section: Discussionmentioning

confidence: 62%

Section: Discussionmentioning

confidence: 99%

On the link between central black holes, bar dynamics and dark matter haloes in spiral galaxies

Treuthardt

Seigar

Sierra

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“… NGC 1433 . A prototypical ringed barred galaxy (Treuthardt et al 2008), with a morphological type (R′)SB(r)ab. It has a circumnuclear ring with a diameter about 0.1 times the size of the bar (at r ∼ 19 arcsec, Crocker, Baugus & Buta 1996; Hameed & Devereuz 1999; Buta et al 2001; Comerón et al 2009) and an outer pseudo‐ring about twice the diameter of the bar.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Star formation history of barred disc galaxies

Sánchez‐Blázquez

Ocvirk

Gibson³

et al. 2011

Monthly Notices of the Royal Astronomical Society

174

212

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We present the first results of a pilot study aimed at understanding the influence of bars on the evolution of galaxy discs through the study of their stellar content. We examine here the kinematics, star formation history, mass-weighted, luminosity-weighted, and single stellar population (SSP) equivalent ages and metallicities for four galaxies ranging from lenticulars to late-type spirals. The data employed extends to 2-3 disc scalelengths, with S/N(A)>50. Several techniques are explored to derive star formation histories and SSP-equivalent parameters, each of which are shown to be compatible. We demostrate that the age-metallicity degeneracy is highly reduced by using spectral fitting techniques --instead of indices-- to derive these parameters. We found that the majority of the stellar mass in our sample is composed of old (~10 Gyr) stars. This is true in the bulge and the disc region, even beyond two disc scalelengths. In the bulge region, we find that the young, dynamically cold, structures produced by the presence of the bar (e.g., nuclear discs or rings) are responsible for shaping the bulges' age and metallicity gradients. In the disc region, a larger fraction of young stars is present in the external parts of the disc compared with the inner disc. The disc growth is, therefore, compatible with a moderate inside-out formation scenario, where the luminosity weighted age changes from ~10 Gyrs in the centre, to ~4 Gyrs at two disc scalelengths, depending upon the galaxy. For two galaxies, we compare the metallicity and age gradients of the disc major axis with that of the bar, finding very important differences. In particular, the stellar population of the bar is more similar to the bulge than to the disc, indicating that, at least in those two galaxies, bars formed long ago and have survived to the present day. (abridged)Comment: 24 pages, 23 figures, accepted for publication in MNRA

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“…These methods start by computing the gravitational potential of the galaxy that is used to produce hydrodynamical galaxy models, with Ω b as one of the free parameters of the models. Determination of the best value of Ω b is done by matching the modelled and observed surface gas distribution and/or gas velocity field (see, e.g., Sanders & Tubbs 1980;Hunter et al 1988;England et al 1990;Garcia-Burillo et al 1993;Sempere et al 1995a;Lindblad & Kristen 1996;Laine & Heller 1999;Weiner et al 2001;Aguerri et al 2001;Pérez et al 2004;Rautiainen et al 2008;Treuthardt et al 2008). Other methods determine the pattern speed by identifying some morphological galaxy features with Lindblad resonances.…”

Section: Introductionmentioning

confidence: 99%

Bar pattern speeds in CALIFA galaxies

Aguerri

Méndez-Abreu

Falcón-Barroso

et al. 2015

A&A

113

189

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Context. The bar pattern speed (Ω b ) is defined as the rotational frequency of the bar, and it determines the bar dynamics. Several methods have been proposed for measuring Ω b . The non-parametric method proposed by Tremaine & Weinberg (1984, ApJ, 282, L5; TW) and based on stellar kinematics is the most accurate. This method has been applied so far to 17 galaxies, most of them SB0 and SBa types. Aims. We have applied the TW method to a new sample of 15 strong and bright barred galaxies, spanning a wide range of morphological types from SB0 to SBbc. Combining our analysis with previous studies, we investigate 32 barred galaxies with their pattern speed measured by the TW method. The resulting total sample of barred galaxies allows us to study the dependence of Ω b on galaxy properties, such as the Hubble type. Methods. We measured Ω b using the TW method on the stellar velocity maps provided by the integral-field spectroscopy data from the CALIFA survey. Integral-field data solve the problems that long-slit data present when applying the TW method, resulting in the determination of more accurate Ω b . In addition, we have also derived the ratio R of the corotation radius to the bar length of the galaxies. According to this parameter, bars can be classified as fast (R < 1.4) and slow (R > 1.4). Results. For all the galaxies, R is compatible within the errors with fast bars. We cannot rule out (at 95% level) the fast bar solution for any galaxy. We have not observed any significant trend between R and the galaxy morphological type. Conclusions. Our results indicate that independent of the Hubble type, bars have been formed and then evolve as fast rotators. This observational result will constrain the scenarios of formation and evolution of bars proposed by numerical simulations.

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The Bar Pattern Speed of NGC 1433 Estimated via Sticky-Particle Simulations

Cited by 24 publications

References 39 publications

On the link between central black holes, bar dynamics and dark matter haloes in spiral galaxies

On the link between central black holes, bar dynamics and dark matter haloes in spiral galaxies

Star formation history of barred disc galaxies

Bar pattern speeds in CALIFA galaxies

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