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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 709852.0, MPI für Astronomie / Publikationen_mpia
The star formation history of CALIFA galaxies: Radial structures
Authors:González Delgado, R. M.; Pérez, E.; Cid Fernandes, R.; García-Benito, R.; de Amorim, A. L.; Sánchez, S. F.; Husemann, B.; Cortijo-Ferrero, C.; López Fernández, R.; Sánchez-Blázquez, P.; Bekeraite, S.; Walcher, C. J.; Falcón-Barroso, J.; Gallazzi, A.; van de Ven, G.; Alves, J.; Bland-Hawthorn, J.; Kennicutt, R. C.; Kupko, D.; Lyubenova, M.; Mast, D.; Mollá, M.; Marino, R. A.; Quirrenbach, A.; Vílchez, J. M.; Wisotzki, L.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:Astronomy and Astrophysics
Volume:562
Start Page:id. A47 (25 pp)
Audience:Not Specified
Abstract / Description:We have studied the radial structure of the stellar mass surface density (mu*) and stellar population age as a function of the total stellar mass and morphology for a sample of 107 galaxies from the CALIFA survey. We applied the fossil record method based on spectral synthesis techniques to recover the star formation history (SFH), resolved in space and time, in spheroidal and disk dominated galaxies with masses from 109 to 1012 M&sun;. We derived the half-mass radius, and we found that galaxies are on average 15% more compact in mass than in light. The ratio of half-mass radius to half-light radius (HLR) shows a dual dependence with galaxy stellar mass; it decreases with increasing mass for disk galaxies, but is almost constant in spheroidal galaxies. In terms of integrated versus spatially resolved properties, we find that the galaxy-averaged stellar population age, stellar extinction, and mu* are well represented by their values at 1 HLR. Negative radial gradients of the stellar population ages are present in most of the galaxies, supporting an inside-out formation. The larger inner (<=1 HLR) age gradients occur in the most massive (1011 M&sun;) disk galaxies that have the most prominent bulges; shallower age gradients are obtained in spheroids of similar mass. Disk and spheroidal galaxies show negative mu* gradients that steepen with stellar mass. In spheroidal galaxies, mu* saturates at a critical value (~7 × 102 M&sun;/pc2 at 1 HLR) that is independent of the galaxy mass. Thus, all the massive spheroidal galaxies have similar local mu* at the same distance (in HLR units) from the nucleus. The SFH of the regions beyond 1 HLR are well correlated with their local mu*, and follow the same relation as the galaxy-averaged age and mu*; this suggests that local stellar mass surface density preserves the SFH of disks. The SFH of bulges are, however, more fundamentally related to the total stellar mass, since the radial structure of the stellar age changes with galaxy mass even though all the spheroid dominated galaxies have similar radial structure in mu*. Thus, galaxy mass is a more fundamental property in spheroidal systems, while the local stellar mass surface density is more important in disks. Table 1 and appendices are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201322011/olm">http://www.aanda.org</A>
Free Keywords:galaxies: evolution; galaxies: stellar content; galaxies: structure; galaxies: fundamental parameters; galaxies: bulges; galaxies: spiral
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-6361 %R 10.1051/0004-6361/201322011
URL:http://cdsads.u-strasbg.fr/abs/2014A%26A...562A..4...
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