Stellar populations of bulges in 14 cluster disc galaxies★
L. Morelli
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Department of Astronomy, Católica de Chile, Pontificia Universidad, Vicuna Mackenna 4860, Casilla 306, Santiago 22, Chile
Search for more papers by this authorE. Pompei
European Southern Observatory, 3107 Alonso de Cordova, Santiago, Chile
Search for more papers by this authorA. Pizzella
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Search for more papers by this authorJ. Méndez-Abreu
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
INAF – Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Search for more papers by this authorE. M. Corsini
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Search for more papers by this authorL. Coccato
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany
Search for more papers by this authorR. P. Saglia
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany
Search for more papers by this authorM. Sarzi
Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB
Search for more papers by this authorF. Bertola
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Search for more papers by this authorL. Morelli
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Department of Astronomy, Católica de Chile, Pontificia Universidad, Vicuna Mackenna 4860, Casilla 306, Santiago 22, Chile
Search for more papers by this authorE. Pompei
European Southern Observatory, 3107 Alonso de Cordova, Santiago, Chile
Search for more papers by this authorA. Pizzella
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Search for more papers by this authorJ. Méndez-Abreu
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
INAF – Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Search for more papers by this authorE. M. Corsini
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Search for more papers by this authorL. Coccato
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany
Search for more papers by this authorR. P. Saglia
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany
Search for more papers by this authorM. Sarzi
Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB
Search for more papers by this authorF. Bertola
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, I-35122 Padova, Italy
Search for more papers by this authorBased on observations made with ESO Telescopes at the La Silla observatory under programmes 70.B-0486 and 71.B-0202.
ABSTRACT
Photometry and long-slit spectroscopy are presented for 14 S0 and spiral galaxies of the Fornax, Eridanus and Pegasus cluster, and NGC 7582 group. The structural parameters of the galaxies are derived from the R-band images by performing a two-dimensional photometric decomposition of the surface brightness distribution. This is assumed to be the sum of the contribution of a bulge and disc component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. The rotation curves and velocity dispersion profiles are measured from the spectra obtained along the major axis of galaxies. The radial profiles of the Hβ, Mg and Fe line-strength indices are presented too. Correlations between the central values of Mg2, 〈Fe〉, Hβ and σ are found. The age, metallicity and α/Fe enhancement of the stellar population in the centre and at the radius where bulge and disc give the same contribution to the total surface brightness are obtained using stellar population models with variable element abundance ratios. Three classes of bulges are identified. The youngest bulges (∼2 Gyr) with ongoing star formation, intermediate-age bulges (4–8 Gyr) have solar metallicity, and old bulges (∼10 Gyr) have high metallicity. Most of the sample bulges display solar α/Fe enhancement, no gradient in age and a negative gradient of metallicity. The presence of negative gradient in the metallicity radial profile favours a scenario with bulge formation via dissipative collapse. This implies strong inside-out formation that should give rise to a negative gradient in the α/Fe enhancement too. But, no gradient is measured in the [α/Fe] radial profiles for all the galaxies, except for NGC 1366. In this galaxy there is a kinematically decoupled component, which is younger than the rest of host bulge. It possibly formed by enriched material probably acquired via interaction or minor merging. The bulge of NGC 1292 is the most reliable pseudo-bulge of our sample. The properties of its stellar population are consistent with a slow build-up within a scenario of secular evolution.
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