Stellar mass distribution of S4G disk galaxies and signatures of bar-induced secular evolution

2016/07/31 by S. Díaz-García, Simón Díaz-García, H. Salo +3 · 1 citation
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Disc #Galaxies: Formation, Evolution, Phenomena #Galaxy #Photometry (optics) #Space Technology and Applications #Stellar density #Stellar dynamics #Stellar mass #Stellar rotation #Stellar structure #Thick disk #Young stellar object #astro-ph.GA

paper · pdf · doi:10.1051/0004-6361/201628683

published as A&A 596, A84 (2016) · 22 pages, 19 figures, accepted for publication in A&A (July 24, 2016)

arxiv created 2016/08/23 · openalex created_date 2016/08/23 · openalex publication_date 2016/08/23 · arxiv updated 2016/12/07 · openalex updated_date 2026/08/05

Abstract

Context. Models of galaxy formation in a cosmological framework need to be tested against observational constraints, such as the average stellar density profiles (and their dispersion) as a function of fundamental galaxy properties (e.g. the total stellar mass). Simulation models predict that the torques produced by stellar bars efficiently redistribute the stellar and gaseous material inside the disk, pushing it outwards or inwards depending on whether it is beyond or inside the bar corotation resonance radius. Bars themselves are expected to evolve, getting longer and narrower as they trap particles from the disk and slow down their rotation speed.

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Cited by

• The dynamical state of bars in cluster dwarf galaxies: The cases of NGC 4483 and NGC 4516