Please note that eDoc will be permanently shut down in the first quarter of 2021!      Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 731817.0, MPI für Astronomie / Publikationen_mpia
No direct coupling between bending of galaxy disc stellar age and light profiles
Authors:Ruiz-Lara, T.; Pérez, I.; Florido, E.; Sánchez-Blázquez, P.; Méndez-Abreu, J.; Lyubenova, M.; Falcón-Barroso, J.; Sánchez-Menguiano, L.; Sánchez, S. F.; Galbany, L.; García-Benito, R.; González Delgado, R. M.; Husemann, B.; Kehrig, C.; López-Sánchez, Á. R.; Marino, R. A.; Mast, D.; Papaderos, P.; van de Ven, G.; Walcher, C. J.; Zibetti, S.; Team, C.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:1
Start Page:L35
End Page:L39
Audience:Not Specified
Abstract / Description:We study the stellar properties of 44 face-on spiral galaxies from the Calar Alto Legacy Integral Field Area survey via full spectrum fitting techniques. We compare the age profiles with the surface brightness distribution in order to highlight differences between profile types (type I, exponential profile; and II, down-bending profile). We observe an upturn (`U-shape') in the age profiles for 17 out of these 44 galaxies with reliable stellar information up to their outer parts. This `U-shape' is not a unique feature for type II galaxies but can be observed in type I as well. These findings suggest that the mechanisms shaping the surface brightness and stellar population distributions are not directly coupled. This upturn in age is only observable in the light-weighted profiles while it flattens out in the mass-weighted profiles. Given recent results on the outer parts of nearby systems and the results presented in this Letter, one of the most plausible explanations for the age upturn is an early formation of the entire disc (˜10 Gyr ago) followed by an inside-out quenching of the star formation.
Free Keywords:techniques: spectroscopic; galaxies: evolution; galaxies: formation; galaxies: spiral; galaxies: stellar content; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.