2015/06/09 by R. M. Gonzáez-Delgado, Delgado, R. M. González, R. García-Benito +25
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.1506.02809
5 pages, 3 figures, Proceedings for "Multi-Object Spectroscopy in the Next Decade: Big Questions, Large Surveys and Wide Fields", Santa Cruz de La Palma, Canary Islands, 2nd to 6th March 2015
arxiv created 2015/06/09 · openalex publication_date 2015/06/09 · arxiv updated 2015/06/10 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We characterize in detail the radial structure of the stellar population properties of 300 galaxies in the nearby universe, observed with integral field spectroscopy in the CALIFA survey. The sample covers a wide range of Hubble types, from spheroidal to spiral galaxies, ranging in stellar masses from M_⋆ ∼ 109 to 7 × 1011 M_\odot. We derive the stellar mass surface density (μ_⋆), light-weighted and mass-weighted ages (⟨ \rm log age⟩ L, ⟨ \rm log age⟩ M), and mass-weighted metallicity (⟨ \rm log Z_⋆⟩ M), applying the spectral synthesis technique. We study the mean trends with galaxy stellar mass, M_⋆, and 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 evidences that quenching is related to morphology, but not driven by mass.