J/A+A/581/A103 CALIFA survey across the Hubble sequence (Gonzalez+, 2015)
The CALIFA survey across the Hubble sequence.
Spatially resolved stellar population properties in galaxies.
Gonzalez Delgado R.M., Garcia-Benito R., Perez E., Cid Fernandes R.,
De Amorim A.L., Cortijo-Ferrero C., Lacerda E.A.D., Lopez Fernandez R.,
Vale-Asari N., Sanchez S.F., Molla M., Ruiz-Lara T., Sanchez-Blazquez P.,
Walcher C.J., Alves J., Aguerri J.A.L., Bekeraite S., Bland-Hawthorn J.,
Galbany L., Gallazzi A., Husemann B., Iglesias-Paramo J., Kalinova V.,
Lopez-Sanchez A.R., Marino R.A., Marquez I., Masegosa J., Mast D.,
Mendez-Abreu J., Mendoza A., Del Olmo A., Perez I., Quirrenbach A.,
Zibetti S., (the collaboration Califa)
<Astron. Astrophys., 581, A103-103 (2015)>
=2015A&A...581A.103G 2015A&A...581A.103G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Models
Keywords: techniques: spectroscopic - Galaxy: evolution -
Galaxy: stellar content - galaxies: structure -
Galaxy: fundamental parameters - galaxies: spiral
Abstract:
Various different physical processes contribute to the star formation
and stellar mass assembly histories of galaxies. One important
approach to understanding the significance of these different
processes on galaxy evolution is the study of the stellar population
content of today's galaxies in a spatially resolved manner. The aim of
this paper is to characterize in detail the radial structure of
stellar population properties of galaxies in the nearby universe,
based on a uniquely large galaxy sample, considering the quality and
coverage of the data. The sample under study was drawn from the CALIFA
survey and contains 300 galaxies observed with integral field
spectroscopy. These cover a wide range of Hubble types, from spheroids
to spiral galaxies, while stellar masses range from M*∼109 to
7x1011M☉. We apply the fossil record method based on spectral
synthesis techniques to recover the following physical properties for
each spatial resolution element in our target galaxies: the stellar
mass surface density (µ*), stellar extinction (AV),
light-weighted and mass-weighted ages (L, M), and
mass-weighted metallicity (<logZ*>M). To study mean trends with
overall galaxy properties, the individual radial profiles are stacked
in seven bins of galaxy morphology (E, S0, Sa, Sb, Sbc, Sc, and Sd).
We confirm that more massive galaxies are more compact, older, more
metal rich, and less reddened by dust. Additionally, we find that
these trends are preserved spatially with the radial distance to the
nucleus. Deviations from these relations appear correlated with Hubble
type: earlier types are more compact, older, and more metal rich for a
given M*, which is evidence that quenching is related to morphology,
but not driven by mass. Negative gradients of L are
consistent with an inside-out growth of galaxies, with the largest
L gradients in Sb-Sbc galaxies. Further, the mean stellar
ages of disks and bulges are correlated and with disks covering a
wider range of ages, and late-type spirals hosting younger disks.
However, age gradients are only mildly negative or flat beyond R∼2HLR
(half light radius), indicating that star formation is more uniformly
distributed or that stellar migration is important at these distances.
The gradients in stellar mass surface density depend mostly on stellar
mass, in the sense that more massive galaxies are more centrally
concentrated. Whatever sets the concentration indices of galaxies
obviously depends less on quenching/morphology than on the depth of
the potential well. There is a secondary correlation in the sense that
at the same M* early-type galaxies have steeper gradients. The
µ* gradients outside 1HLR show no dependence on Hubble type. We
find mildly negative <logZ*>M gradients, which are shallower than
predicted from models of galaxy evolution in isolation. In general,
metallicity gradients depend on stellar mass, and less on morphology,
hinting that metallicity is affected by both - the depth of the
potential well and morphology/quenching. Thus, the largest
<logZ*>M gradients occur in Milky Way-like Sb-Sbc galaxies, and
are similar to those measured above the Galactic disk. Sc spirals show
flatter <logZ*>M gradients, possibly indicating a larger
contribution from secular evolution in disks. The galaxies from the
sample have decreasing-outward stellar extinction; all spirals show
similar radial profiles, independent from the stellar mass, but redder
than E and S0. Overall, we conclude that quenching processes act in
manners that are independent of mass, while metallicity and galaxy
structure are influenced by mass-dependent processes.
Description:
The observations were carried out with the Potsdam Multi-Aperture
Spectrometer 112, PMAS in the PPaK mode 137 at the 3.5m telescope of
Calar Alto observatory. PPaK contains 382 fibers of 2.7" diameter
each, and a 74"x64" FoV 73. Each galaxy is observed with two
spectral settings, V500 and V1200, with spectral resolutions ∼6Å
(FWHM) and 2.3Å, respectively. The V500 grating covers from 3745 to
7300Å, while the V1200 covers 3650-4840Å.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 90 300 Stellar population properties: CBe base model
tablec2.dat 90 300 Stellar population properties: GMe base model
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See also:
J/A+A/582/A21 : CALIFA merging galaxies (mis)alignments
(Barrera-Ballesteros+, 2015)
Byte-by-byte Description of file: tablec1.dat tablec2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- CALIFA CALIFA identification number
5- 19 A15 --- Name NED name
21- 25 A5 --- Type Morphological type
27- 31 F5.2 [Msun] logM* Stellar mass
33- 36 F4.2 [Msun/pc2] logmu*0 Stellar mass surface brightness
38- 41 F4.2 [Msun/pc2] lognmu*HLR Stellar mass surface brightness at R=1HLR
43- 46 F4.2 mag AV0 Stellar extinction at R=0
48- 51 F4.2 mag AVHLR Stellar extinction at R=1HLR
53- 57 F5.2 [yr] logage0 Mean stellar age (luminosity weighted)
at R=0
59- 63 F5.2 [yr] logageHLR Mean stellar age (luminosity weighted)
at R=1HLR
65- 69 F5.2 Sun logZM0 Mettallicity of the stellar population
(mass weighted) at R=0
71- 75 F5.2 Sun logZ0MHLR Mettallicity of the stellar population
(mass weighted) at R=1HLR
77- 81 I5 pc HLR Half-light radius
83- 86 I4 pc HMR Half-mass radius
88- 90 F3.1 --- C concentration index (R90/r50)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 25-Nov-2015