The formation of spiral arms and rings in barred galaxies

Romero-Gómez, M.; Athanassoula, E.; Masdemont, Josep J.; García-Gómez, C.

doi:10.1051/0004-6361:20077504

Cited by 124 publications

(124 citation statements)

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“…This is important since the rings and spirals in barred galaxies are observational properties. So we obtain connections between the parameters in our model and observational results (e.g., Athanassoula et al 2009aAthanassoula et al ,b, 2010Athanassoula et al , 2011Romero-Gómez et al 2006, 2007.…”

Section: Introductionsupporting

confidence: 70%

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Zotos

Jung

2017

Monthly Notices of the Royal Astronomical Society

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The escape dynamics of the stars in a barred galaxy composed of a spherically symmetric central nucleus, a bar, a flat thin disk and a dark matter halo component is investigated by using a realistic three degrees of freedom (3-dof) dynamical model. Modern colour-coded diagrams are used for distinguishing between bounded and escaping motion. In addition, the smaller alignment index (SALI) method is deployed for determining the regular, sticky or chaotic nature of bounded orbits. We reveal the basins of escape corresponding to the escape through the two symmetrical escape channels around the Lagrange points L 2 and L 3 and also we relate them with the corresponding distribution of the escape times of the orbits. Furthermore, we demonstrate how the stable manifolds, around the index-1 saddle points, accurately define the fractal basin boundaries observed in the colour-coded diagrams. The development scenario of the fundamental vertical Lyapunov periodic orbit is thoroughly explored for obtaining a more complete view of the unfolding of the singular behaviour of the dynamics at the cusp values of the parameters. Finally, we examine how the combination of the most important parameters of the bar (such as the semi-major axis and the angular velocity) influences the observed stellar structures (rings and spirals) which are formed by escaping stars guided by the invariant manifolds near the saddle points.

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Section: Introductionsupporting

confidence: 70%

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Zotos

Jung

2017

Monthly Notices of the Royal Astronomical Society

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“…Modal studies by Bertin et al (1989aBertin et al ( , 1989b predict that there should be amplitude variations along the arms from resonances between inward-and outward-moving spiral waves, and the precise amplitude variations have been modeled (Elmegreen & Elmegreen 1984;Elmegreen et al 1989;Elmegreen & Thomasson 1993;Regan & Elmegreen 1997). Most recently, a new theory has been proposed for the formation of rings and spiral arms, which argues in favor of chaotic orbits, confined by invariant manifolds emanating from the L1 and L2 Lagrangian points of a bar (Romero-Gómez et al 2007). Several comparisons between the results of this theory and observations have been carried out successfully (Athanassoula et al 2009a(Athanassoula et al , 2009b and several more will be possible with the S 4 G database.…”

Section: Spiral Armsmentioning

confidence: 99%

TheSpitzerSurvey of Stellar Structure in Galaxies

Sheth¹,

Regan²,

Hinz³

et al. 2010

Publications of the Astronomical Society of the Pacific

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ABSTRACT. The Spitzer Survey of Stellar Structure in Galaxies (S 4 G) is an Exploration Science Legacy Program approved for the Spitzer post-cryogenic mission. It is a volume-, magnitude-, and size-limited (d < 40 Mpc, jbj > 30°, m Bcorr < 15:5, and D 25 > 1 0 ) survey of 2331 galaxies using the Infrared Array Camera (IRAC) at 3.6 and 4.5 μm. Each galaxy is observed for 240 s and mapped to ≥1:5 × D 25 . The final mosaicked images have a typical 1σ rms noise level of 0.0072 and 0:0093 MJy sr À1 at 3.6 and 4.5 μm, respectively. Our azimuthally averaged surface brightness profile typically traces isophotes at μ 3:6μm ðABÞð1σÞ ∼ 27 mag arcsec À2 , equivalent to a stellar mass surface density of ∼1 M ⊙ pc À2 . S 4 G thus provides an unprecedented data set for the study of the distribution of mass and stellar structures in the local universe. This large, unbiased, and extremely deep sample of all Hubble types from dwarfs to spirals to ellipticals will allow for detailed structural studies, not only as a function of stellar mass, but also as a function of the local environment. The data from this survey will serve as a vital testbed for cosmological simulations predicting the stellar mass properties of present-day galaxies. This article introduces the survey and describes the sample selection, the significance of the 3.6 and 4.5 μm bands for this study, and the data collection and survey strategies. We describe the S 4 G data analysis pipeline and present measurements for a first set of galaxies, observed in both the cryogenic and warm mission phases of Spitzer. For every galaxy we tabulate the galaxy diameter, position angle, axial ratio, inclination at μ 3:6μm ðABÞ ¼ 25:5, and 26:5 mag arcsec À2 (equivalent to ≈μ B ðABÞ ¼ 27:2 and 28:2 mag arcsec À2 , respectively). These measurements will form the initial S 4 G catalog of galaxy properties. We also measure the total magnitude and the azimuthally averaged radial profiles of ellipticity, position angle, surface brightness, and color. Finally, using the galaxy-fitting code GALFIT, we deconstruct each galaxy into its main constituent stellar components: the bulge/spheroid, disk, bar, and nuclear point source, where necessary. Together, these data products will provide a comprehensive and definitive catalog of stellar structures, mass, and properties of galaxies in the nearby universe and will enable a variety of scientific investigations, some of which are highlighted in this introductory S 4 G survey paper.

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“…[71,70,79]). Furthermore, due to an exchange of angular momentum between the disc and the dark matter halo, mediated by the bar, the disc becomes more centrally concentrated [7,3].…”

Section: Observed Properties Of Barred Galaxiesmentioning

confidence: 99%

Barred Galaxies: an Observer’s Perspective

Gadotti

2008

Chaos in Astronomy

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Summary. I review both well established and more recent findings on the properties of bars, and their host galaxies, stemming from photometric and spectroscopic observations, and discuss how these findings can be understood in terms of a global picture of the formation and evolution of bars, keeping a connection with theoretical developments. In particular, I show the results of a detailed structural analysis of ≈ 300 barred galaxies in the Sloan Digital Sky Survey, providing physical quantities, such as bar length, ellipticity and boxyness, and bar-to-total luminosity ratio, that can either be used as a solid basis on which realistic models can be built, or be compared against more fundamental theoretical results. I also show correlations that indicate that bars grow longer, thinner and stronger with dynamical age, and that the growth of bars and bulges is connected. Finally, I briefly discuss open questions and possible directions for future research.

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The formation of spiral arms and rings in barred galaxies

Cited by 124 publications

References 50 publications

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

TheSpitzerSurvey of Stellar Structure in Galaxies

Barred Galaxies: an Observer’s Perspective

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