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) =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_*_~10^9^ to 7x10^11^M_{sun}_. 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 ({mu}_*_), stellar extinction (A_V_), light-weighted and mass-weighted ages (_L_, _M_), and mass-weighted metallicity (_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 {mu}_*_ gradients outside 1HLR show no dependence on Hubble type. We find mildly negative _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 _M_ gradients occur in Milky Way-like Sb-Sbc galaxies, and are similar to those measured above the Galactic disk. Sc spirals show flatter _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 ~6{AA} (FWHM) and 2.3{AA}, respectively. The V500 grating covers from 3745 to 7300{AA}, while the V1200 covers 3650-4840{AA}. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablec1.dat 90 300 Stellar population properties: CBe base model tablec2.dat 90 300 Stellar population properties: GMe base model -------------------------------------------------------------------------------- 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 -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 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 (R_90_/r_50_) -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Patricia Vannier [CDS] 25-Nov-2015