Bibcode
Muñoz-Mateos, Juan Carlos; Sheth, Kartik; Gil de Paz, Armando; Meidt, Sharon; Athanassoula, E.; Bosma, Albert; Comerón, Sébastien; Elmegreen, Debra M.; Elmegreen, Bruce G.; Erroz-Ferrer, S.; Gadotti, Dimitri A.; Hinz, Joannah L.; Ho, Luis C.; Holwerda, Benne; Jarrett, Thomas H.; Kim, Taehyun; Knapen, J. H.; Laine, Jarkko; Laurikainen, Eija; Madore, Barry F.; Menendez-Delmestre, Karin; Mizusawa, Trisha; Regan, Michael; Salo, Heikki; Schinnerer, Eva; Seibert, Mark; Skibba, Ramin; Zaritsky, Dennis
Referencia bibliográfica
The Astrophysical Journal, Volume 771, Issue 1, article id. 59, 30 pp. (2013).
Fecha de publicación:
7
2013
Revista
Número de citas
108
Número de citas referidas
101
Descripción
We have analyzed the radial distribution of old stars in a sample of 218
nearby face-on disks, using deep 3.6 μm 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 (R br/R bar) depends strongly on the
total stellar mass of the galaxy. For galaxies more massive than
1010 M ☉, the distribution is bimodal,
peaking at R br/R bar ~ 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 1010 M ☉, breaks are found up to ~10 R
bar, 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 ~2 R bar, but
also for many of those found at larger radii.
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