Sébastien Comerón, Bruce G. Elmegreen, Heikki Salo, Eija Laurikainen, E. Athanassoula, Albert Bosma, Johan H. Knapen, Dimitri A. Gadotti, Kartik Sheth, Joannah L. Hinz, Michael W. Regan, Armando Gil de Paz, Juan-Carlos Muñoz-Mateos, Karín Menéndez-Delmestre, Mark Seibert, Taehyun Kim, Trisha Mizusawa, Jarkko Laine, Luis C. Ho, Benne Holwerda
Breaks in the radial luminosity profiles of galaxies have been until now mostly studied averaged over discs. Here we study separately breaks in thin and thick discs in 70 edge-on galaxies using imaging from the Spitzer Survey of Stellar Structure in Galaxies. We built luminosity profiles of the thin and the thick discs parallel to midplanes and we found that thin discs often truncate (77%). Thick discs truncate less often (31%), but when they do, their break radius is comparable with that in the thin disc. This suggests either two different truncation mechanisms - one of dynamical origin affecting both discs simultaneously and another one only affecting the thin disc - or a single mechanism that creates a truncation in one disc or in both depending on some galaxy property. Thin discs apparently antitruncate in around 40% of galaxies. However, in many cases, these antitruncations are an artifact caused by the superposition of a thin disc and a thick disc with the latter having a longer scale length. We estimate the real thin disc antitruncation fraction to be less than 15%. We found that the ratio of the thick and thin stellar disc mass is roughly constant (0.2120 km/s, but becomes much larger at smaller velocities. We hypothesize that this is due to a combination of a high efficiency of supernova feedback and a slower dynamical evolution in lower-mass galaxies causing stellar thin discs to be younger and less massive than in higher-mass galaxies.
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http://arxiv.org/abs/1209.1513
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