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dc.contributor.authorMunoz-Mateso, Juan Carlos
dc.contributor.authorSheth, Kartik
dc.contributor.authorGil de Paz, Armando
dc.contributor.authorMeidt, Sharon
dc.contributor.authorAthanassoula, Evangelie
dc.contributor.authorBosma, Albert
dc.contributor.authorComeron, Sebastien
dc.contributor.authorElmegreen, Debra M.
dc.contributor.authorElmegreen, Bruce G.
dc.contributor.authorMizusawa, Trisha
dc.date.accessioned2013-10-02T13:55:13Z
dc.date.available2013-10-02T13:55:13Z
dc.date.issued2013-07-01
dc.identifier.citationMuñoz-Mateos, J. C., Sheth, K., Gil De Paz, A., Meidt, S., Athanassoula, E., Bosma, A., . . . Zaritsky, D. (2013). The impact of bars on disk breaks as probed by S4G imaging. Astrophysical Journal, 771(1)en_US
dc.identifier.urihttp://hdl.handle.net/11141/72
dc.description.abstractWe have analyzed the radial distribution of old stars in a sample of 218 nearby face-on disks, using deep 3.6μm images from the Spitzer Survey of Stellar Structure in Galaxies. In particular, we have studied the structural properties of those disks with a broken or down-bending profile. We find that, on average, disks with a genuine single-exponential profile have a scale length and a central surface brightness which are intermediate to those of the inner and outer components of a down-bending disk with the same total stellar mass. In the particular case of barred galaxies, the ratio between the break and the bar radii (Rbr/Rbar) depends strongly on the total stellar mass of the galaxy. For galaxies more massive than 1010M , the distribution is bimodal, peaking at Rbr/Rbar ∼ 2 and ∼3.5. The first peak, which is the most populated one, is linked to the outer Lindblad resonance of the bar, whereas the second one is consistent with a dynamical coupling between the bar and the spiral pattern. For galaxies below 1010M , breaks are found up to ∼10Rbar, but we show that they could still be caused by resonances given the rising nature of rotation curves in these low-mass disks. While not ruling out star formation thresholds, our results imply that radial stellar migration induced by non-axisymmetric features can be responsible not only for those breaks at ∼2Rbar, but also for many of those found at larger radii.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttp://aas.org/publications/aas-copyright-policyen_US
dc.titleThe impact of bars on disk breaks as probed by S⁴G imagingen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/0004-637X/771/1/59 10.3847/0004-637X/818/1/101


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