The Evolution of Galaxies Resolved in Space and Time: A View of Inside-Out Growth From the Califa Survey

Pérez, E.; Fernandes, R. Cid; Delgado, R. M. González; García-Benito, R.; Sánchez, S. F.; Husemann, B.; Mast, D.; Rodón, J. R.; Kupko, D.; Backsmann, N.; Amorim, A. L. de; Ven, Glenn van de; Walcher, Jakob; Wisotzki, L.; Cortijo-Ferrero, C.

doi:10.1088/2041-8205/764/1/l1

Cited by 235 publications

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“…This ratio also shows a dual dependence with M : it decreases with increasing mass for disk galaxies, and becomes almost constant in spheroidal galaxies. These results are a signpost of the inside-out growth previously found by Pérez et al (2013).…”

Section: Discussionsupporting

confidence: 83%

“…This ratio is lower than 1 (Fig. 3), a fingerprint of the inside-out growth found by Pérez et al (2013). Figure 19 shows how the radial profiles of log age M decrease outward for all the Hubble types.…”

Section: Califa View Of the Inside-out Growth Of Galaxiesmentioning

confidence: 83%

“…The ratio between the HMR and the HLR (a M 50 /a L 50 ) reflects the spatial variation of the SFH in a galaxy. This ratio is lower than 1 in almost all cases (González Delgado et al 2014c), a signpost of the inside-out growth found by Pérez et al (2013). Figure 3 shows the relation between a M 50 /a L 50 and Hubble type (left panel), and galaxy stellar mass (right panel).…”

Section: The Hmr/hlrmentioning

confidence: 84%

“…Our method to extract stellar population properties from datacubes has been explained and applied to CALIFA in Pérez et al (2013), Cid Fernandes et al (2013, and González Delgado et al (2014c,a). In short, we analyze the data with the  code (Cid Fernandes et al 2005), which fits an observed spectrum (O λ ) in terms of a model (M λ ) built by a nonparametric linear combination of N simple stellar populations (SSP) from a base spanning different ages (t) and metallicities (Z).…”

Section: Stellar Population Analysis: Differences With Respect To Prementioning

confidence: 99%

“…Pérez et al (2013) studied the stellar mass growth as a function of the radius and cosmic time in galaxies with 10 10 M 5 × 10 11 M , and showed that the nuclei grow faster than the inner 0.5 HLR, which, in turn, grow faster than the outer 1 HLR. This conclusion is supported by the stellar age radial profiles presented in González Delgado et al (2014c), and confirmed here in Fig.…”

Section: Califa View Of the Inside-out Growth Of Galaxiesmentioning

confidence: 99%

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The CALIFA survey across the Hubble sequence

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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 7 × 10 11 M . 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 (A V ), light-weighted and mass-weighted ages ( log age L , log age M ), and mass-weighted metallicity ( log Z 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 log age L are consistent with an inside-out growth of galaxies, with the largest log age 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 ∼ 2 HLR (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 1 HLR show no dependence on Hubble type. We find mildly negative log Z 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....

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Section: Discussionsupporting

confidence: 83%

Section: Califa View Of the Inside-out Growth Of Galaxiesmentioning

confidence: 83%

Section: The Hmr/hlrmentioning

confidence: 84%