@Article{TortoraLaNaRoFeCa:2014:SyVaCe,
author = "Tortora, C. and La Barbera, F. and Napolitano, N. R. and
Romanowsky, A. J. and Ferreras, I. and Carvalho, Reinaldo Ramos
de",
affiliation = "INAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello,
16Napoli, Italy and INAF-Osservatorio Astronomico di Capodimonte,
Salita Moiariello, 16Napoli, Italy and INAF-Osservatorio
Astronomico di Capodimonte, Salita Moiariello, 16Napoli, Italy and
Department of Physics and Astronomy, San Jos{\'e} State
UniversitySan Jose, CA, United States; University of California
Observatories, 1156 High StreetSanta Cruz, CA, United States and
Mullard Space Science Laboratory, University College London,
Holmbury St Mary, DorkingSurrey, United Kingdom and {Instituto
Nacional de Pesquisas Espaciais (INPE)}",
title = "Systematic variations of central mass density slopes in early-type
galaxies",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2014",
volume = "445",
number = "1",
pages = "115--127",
keywords = "elliptical, lenticular, cD, galaxies, evolution.",
abstract = "We study the total density distribution in the central regions
(<~1 effective radius, Re) of earlytype galaxies (ETGs), using
data from SPIDER and ATLAS3D. Our analysis extends the range of
galaxy stellar mass (M*) probed by gravitational lensing, down to
~10^10M. We model each galaxy with two components (dark matter
halo + stars), exploring different assumptions for the dark matter
halo profile (i.e. NFW, NFW-contracted, and Burkert profiles), and
leaving stellar mass-to-light (M*/L) ratios as free fitting
parameters to the data. For all plausible halo models, the
best-fitting M*/L, normalized to that for a Chabrier initial mass
function, increases systematically with galaxy size and mass. For
anNFWprofile, the slope of the total mass profile is
non-universal, independently of several ingredients in the
modelling (e.g. halo contraction, anisotropy, and rotation
velocity in ETGs). For the most massive (M* ~ 10^11.5M) or largest
(Re ~ 15 kpc) ETGs, the profile is isothermal in the central
regions (~Re/2), while for the low-mass (M* ~ 10^10.2M) or
smallest (Re ~ 0.5 kpc) systems, the profile is steeper than
isothermal, with slopes similar to those for a constant-M/L
profile. For a steeper concentration- mass relation than that
expected from simulations, the correlation of density slope with
galaxy mass tends to flatten, while correlations with Re and
velocity dispersions are more robust. Our results clearly point to
a 'non-homology' in the total mass distribution of ETGs, which
simulations of galaxy formation suggest may be related to a
varying role of dissipation with galaxy mass.",
doi = "10.1093/mnras/stu1616",
url = "http://dx.doi.org/10.1093/mnras/stu1616",
issn = "0035-8711",
label = "scopus 2015-01 TortoraLaNaRoFeCa:2014:SyVaCe",
language = "en",
targetfile = "MNRAS-2014-Tortora-115-27.pdf",
urlaccessdate = "27 abr. 2024"
}