The star formation history of CALIFA galaxies: Radial structures
- Author(s)
- R. M. González Delgado, Enrique Pérez, R. Cid Fernandes, R. García-Benito, André Luiz de Amorim, S. F. Sánchez, B. Husemann, C. Cortijo-Ferrero, R. López Fernández, P. Sánchez-Blázquez, S. Bekeraite, C. J. Walcher, J. Falcón-Barroso, A. Gallazzi, G. van de Ven, J. Alves, J. Bland-Hawthorn, R. C. Kennicutt, D. Kupko, M. Lyubenova, D. Mast, M. Mollá, R. A. Marino, A. Quirrenbach, J. M. Vílchez, L. Wisotzki
- Abstract
We have studied the radial structure of the stellar mass surface density
(μ∗) 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⊙. 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 μ∗ 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⊙) disk
galaxies that have the most prominent bulges; shallower age gradients
are obtained in spheroids of similar mass. Disk and spheroidal galaxies
show negative μ∗ gradients that steepen with
stellar mass. In spheroidal galaxies, μ∗ saturates
at a critical value (~7 × 102
M⊙/pc2 at 1 HLR) that is independent of the
galaxy mass. Thus, all the massive spheroidal galaxies have similar
local μ∗ at the same distance (in HLR units) from
the nucleus. The SFH of the regions beyond 1 HLR are well correlated
with their local μ∗, and follow the same relation
as the galaxy-averaged age and μ∗; 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 μ∗. 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 www.aanda.org
- Organisation(s)
- Department of Astrophysics
- External organisation(s)
- Centro de Investigaciones Energeticas Medioambientales y Tecnológica, Max-Planck-Institut für Astronomie, The University of Sydney, Universidade Federal de Santa Catarina, University of Cambridge, Instituto de Astrofísica de Andalucía (CSIC), INAF - Osservatorio Astrofisico di Arcetri, Leibniz-Institut für Astrophysik Potsdam, Universidad Autónoma de Madrid, Institute of Astrophysics of the Canary Islands, University of La Laguna, University of Copenhagen, Landessternwarte Königstuhl (LSW)
- Journal
- Astronomy & Astrophysics
- Volume
- 562
- No. of pages
- 25
- ISSN
- 0004-6361
- DOI
- https://doi.org/10.1051/0004-6361/201322011
- Publication date
- 02-2014
- Peer reviewed
- Yes
- Austrian Fields of Science 2012
- 103003 Astronomy, 103004 Astrophysics
- Keywords
- ASJC Scopus subject areas
- Astronomy and Astrophysics, Space and Planetary Science
- Portal url
- https://ucrisportal.univie.ac.at/en/publications/47f9f64e-c2d3-488c-a3e1-6ad629e7bf9d