Rings and spirals in barred galaxies â II. Ring and spiral morphology

Athanassoula, E.; Romero-Gómez, M.; Bosma, A.; Masdemont, Josep J.

doi:10.1111/j.1365-2966.2009.15583.x

Cited by 95 publications

(87 citation statements)

References 42 publications

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“…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. S 4 G will cover the full range of galaxies with varying spiral arm strengths and galactic structures.…”

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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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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516

501

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“…Athanassoula 2005;Debattista et al 2006;Roškar et al 2008aRoškar et al , 2012Athanassoula et al 2009aAthanassoula et al ,b, 2010, simulations run in a cosmological context allow us to study the environmental effects of evolution, including the impact of satellite-host interactions through to the quiescent, settled, disc phase (e.g. Katz & Gunn 1991;Navarro & Benz 1991;Katz et al 1992;Navarro & White 1994;Steinmetz & Muller 1995;Steinmetz & Navarro 2002;Abadi et al 2003).…”

Section: Introductionmentioning

confidence: 99%

The imprint of satellite accretion on the chemical and dynamical properties of disc galaxies

Ruiz-Lara

Few

Gibson

et al. 2016

A&A

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Aims. We study the effects of the cosmological assembly history on the chemical and dynamical properties of the discs of spiral galaxies as a function of radius. Methods. We made use of the simulated Milky Way mass, fully-cosmological discs from Ramses Disc Environment Study (RaDES). We analysed their assembly history by examining the proximity of satellites to the galactic disc, instead of their merger trees, to better gauge which satellites impact the disc. We presented stellar age and metallicity profiles, age-metallicity relation (AMR), age-velocity dispersion relation (AVR), and stellar age distribution (SAD) in several radial bins for the simulated galaxies. Results. Assembly histories can be divided into three different stages: i) a merger dominated phase, when a large number of mergers with mass ratios of ∼1:1 take place (lasting ∼3.2 ± 0.4 Gyr on average); ii) a quieter phase, when ∼1:10 mergers take place (lasting ∼4.4 ± 2.0 Gyr); and iii) a secular phase where the few mergers that take place have mass ratios below 1:100, which do not affect the disc properties (lasting ∼5.5 ± 2.0 Gyr). The first two phases are able to kinematically heat the disc and produce a disc that is chemically mixed over its entire radial extension. Phase 2 ends with a final merger event (at time t jump ) marking the onset of important radial differences in the AMR, AVR, and SAD. Conclusions. Inverted AMR trends in the outer parts of discs, for stars younger than t jump , are found as the combined effect of radial motions and star formation in satellites temporarily located in these outer parts. U-shaped stellar age profiles change to an old plateau (∼10 Gyr) in the outer discs for the entire RaDES sample. This shape is a consequence of inside-out growth of the disc, radial motions of disc stars (inwards and outwards), and the accretion of old stars from satellites. We see comparable age profiles even when ignoring the influence of stellar migration due to the presence of early in situ star formation in the outer regions of the galaxy.

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“…Bars may redistribute stars in the galaxy disk, leading to disk breaks in the disk profile (e.g., Debattista et al 2006;Radburn-Smith et al 2012;Muñoz-Mateos et al 2013;Kim et al 2014, hereafter Paper I). Bars drive the formation of inner rings and outer rings (Buta & Combes 1996;Buta et al 2003;Romero-Gómez et al 2006;Athanassoula et al 2009aAthanassoula et al , 2009b and possibly spiral density waves (Buta et al 2009;Salo et al 2010). Simulations show that bars may evolve over time by transferring angular momentum from the baryons to the outer disk and/or halo (Sellwood 1980;Debattista & Sellwood 1998;Athanassoula 2002Athanassoula , 2003Valenzuela & Klypin 2003;Martinez-Valpuesta et al 2006;Begelman & Shlosman 2009;Saha et al 2012).…”

Section: Introductionmentioning

confidence: 99%

THE MASS PROFILE AND SHAPE OF BARS IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S⁴G): SEARCH FOR AN AGE INDICATOR FOR BARS

Kim

Sheth

Gadotti

et al. 2015

ApJ

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We have measured the radial light profiles and global shapes of bars using two-dimensional 3.6 μm image decompositions for 144 face-on barred galaxies from the Spitzer Survey of Stellar Structure in Galaxies. The bar surface brightness profile is correlated with the stellar mass and bulge-to-total (B/T) ratio of their host galaxies. Bars in massive and bulge-dominated galaxies (B/T > 0.2) show a flat profile, while bars in less massive, disk-dominated galaxies (B/T ∼ 0) show an exponential, disk-like profile with a wider spread in the radial profile than in the bulge-dominated galaxies. The global two-dimensional shapes of bars, however, are rectangular/boxy, independent of the bulge or disk properties. We speculate that because bars are formed out of disks, bars initially have an exponential (disk-like) profile that evolves over time, trapping more disk stars to boxy bar orbits. This leads bars to become stronger and have flatter profiles. The narrow spread of bar radial profiles in more massive disks suggests that these bars formed earlier (z > 1), while the disk-like profiles and a larger spread in the radial profile in less massive systems imply a later and more gradual evolution, consistent with the cosmological evolution of bars inferred from observational studies. Therefore, we expect that the flatness of the bar profile can be used as a dynamical age indicator of the bar to measure the time elapsed since the bar formation. We argue that cosmic gas accretion is required to explain our results on bar profile and the presence of gas within the bar region.

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Rings and spirals in barred galaxies â II. Ring and spiral morphology

Cited by 95 publications

References 42 publications

TheSpitzerSurvey of Stellar Structure in Galaxies

TheSpitzerSurvey of Stellar Structure in Galaxies

The imprint of satellite accretion on the chemical and dynamical properties of disc galaxies

THE MASS PROFILE AND SHAPE OF BARS IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S⁴G): SEARCH FOR AN AGE INDICATOR FOR BARS

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Rings and spirals in barred galaxies â II. Ring and spiral morphology

Cited by 95 publications

References 42 publications

TheSpitzerSurvey of Stellar Structure in Galaxies

TheSpitzerSurvey of Stellar Structure in Galaxies

The imprint of satellite accretion on the chemical and dynamical properties of disc galaxies

THE MASS PROFILE AND SHAPE OF BARS IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G): SEARCH FOR AN AGE INDICATOR FOR BARS

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Product

Resources

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Rings and spirals in barred galaxies â II. Ring and spiral morphology

THE MASS PROFILE AND SHAPE OF BARS IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S⁴G): SEARCH FOR AN AGE INDICATOR FOR BARS