@Article{LaBarberaVFPPMACRFV:2019:IMRaGr,
author = "La Barbera, Francesco and Vazdekis, A. and Ferreras, I. and
Paquali, A. and Prieto, C. Allende and Mart{\'{\i}}n-Navarro, I.
and Aguado, D. S. and Carvalho, Reinaldo Ramos de and Rembold, S.
and Falc{\'o}n-Barroso, J. and van de Ven, G.",
affiliation = "{INAF – Osservatorio Astronomico di Capodimonte} and {Instituto de
Astrof{\'{\i}}sica de Canarias} and {University College London}
and {Universit{\"a}t Heidelberg} and {Instituto de
Astrof{\'{\i}}sica de Canarias} and {University of California
Observatories} and {University of Cambridge} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Universidade Federal
de Santa Maria (UFSM)} and {Instituto de Astrof{\'{\i}}sica de
Canarias} and {University of Vienna}",
title = "IMF radial gradients in most massive early-type galaxies",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2019",
volume = "489",
number = "3",
pages = "4090--4110",
month = "Nov.",
keywords = "galaxies: elliptical and lenticular, cD, galaxies: formation,
galaxies: fundamental parameters, galaxies: stellar content.",
abstract = "Using new long-slit spectroscopy obtained with X-Shooter at
ESO-VLT, we study, for the first time, radial gradients of optical
and near-infrared initial mass function (IMF)-sensitive features
in a representative sample of galaxies at the very high mass end
of the galaxy population. The sample consists of seven early-type
galaxies (ETGs) at z similar to 0.05, with central velocity
dispersion in the range 300 less than or similar to sigma less
than or similar to 350 km s(-1). Using state-of-the-art stellar
population synthesis models, we fit a number of spectral indices,
from different chemical species (including TiO and Na indices), to
constrain the IMF slope (i.e. the fraction of low-mass stars), as
a function of galactocentric distance, over a radial range out to
similar to 4 kpc. ETGs in our sample show a significant
correlation of IMF slope and surface mass density. The
bottom-heavy population (i.e. an excess of low-mass stars in the
IMF) is confined to central galaxy regions with surface mass
density above similar to 10(10)M(circle dot) kpc (2), or,
alternatively, within a characteristic radius of similar to 2 kpc.
Radial distance, in physical units, and surface mass density are
the best correlators to IMF variations, with respect to other
dynamical (e.g. velocity dispersion) and stellar population (e.g.
metallicity) properties. Our results for the most massive galaxies
suggest that there is no single parameter that fully explains
variations in the stellar IMF, but IMF radial profiles at z
similar to 0 rather result from the complex formation and mass
accretion history of galaxy inner and outer regions.",
doi = "10.1093/mnras/stz2192",
url = "http://dx.doi.org/10.1093/mnras/stz2192",
issn = "0035-8711 and 1365-2966",
language = "en",
targetfile = "barbera_ifm.pdf",
urlaccessdate = "27 abr. 2024"
}