Volume 608, December 2017
|Number of page(s)||11|
|Published online||15 December 2017|
The role of stellar radial motions in shaping galaxy surface brightness profiles
1 Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain
2 Departamento de Astrofísica, Universidad de La Laguna, 38200 La Laguna, Tenerife, Spain
3 Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus de Fuentenueva, 18071 Granada, Spain
4 Instituto Carlos I de Física Teórica y computacional, Universidad de Granada, 18071 Granada, Spain
5 E.A. Milne Centre for Astrophysics, University of Hull, Hull HU6 7RX, UK
6 Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements (JINA-CEE), Indiana 46556, USA
7 Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Cantoblanco, Spain
Received: 1 July 2017
Accepted: 20 September 2017
Aims. The physics driving features such as breaks observed in galaxy surface brightness (SB) profiles remains contentious. Here, we assess the importance of stellar radial motions in shaping their characteristics.
Methods. We use the simulated Milky Way-mass cosmological discs from the Ramses Disc Environment Study (RaDES) to characterise the radial redistribution of stars in galaxies displaying type-I (pure exponentials), II (downbending), and III (upbending) SB profiles. We compare radial profiles of the mass fractions and the velocity dispersions of different sub-populations of stars according to their birth and current location.
Results. Radial redistribution of stars is important in all galaxies regardless of their light profiles. Type-II breaks seem to be a consequence of the combined effects of outward-moving and accreted stars. The former produce shallower inner profiles (lack of stars in the inner disc) and accumulate material around the break radius and beyond, strengthening the break; the latter can weaken or even convert the break into a pure exponential. Further accretion from satellites can concentrate material in the outermost parts, leading to type-III breaks that can coexist with type-II breaks, but situated further out. Type-III galaxies would be the result of an important radial redistribution of material throughout the entire disc, as well as a concentration of accreted material in the outskirts. In addition, type-III galaxies display the most efficient radial redistribution and the largest number of accreted stars, followed by type-I and II systems, suggesting that type-I galaxies may be an intermediate case between types II and III. In general, the velocity dispersion profiles of all galaxies tend to flatten or even increase around the locations where the breaks are found. The age and metallicity profiles are also affected, exhibiting different inner gradients depending on their SB profile, being steeper in the case of type-II systems (as found observationally). The steep type-II profiles might be inherent to their formation rather than acquired via radial redistribution.
Key words: galaxies: evolution / galaxies: spiral / galaxies: stellar content / galaxies: formation / galaxies: structure / methods: numerical
© ESO, 2017
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