THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. II. SEPARATING LUMINOUS AND DARK MATTER IN CLUSTER CORES

We present stellar and dark matter (DM) density profiles for a sample of seven massive, relaxed galaxy clusters derived from strong and weak gravitational lensing and resolved stellar kinematic observations within the centrally located brightest cluster galaxies (BCGs). In Paper I of the series, we...

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Bibliographic Details
Published in:The Astrophysical journal 2013-03, Vol.765 (1), p.1-12
Main Authors: Newman, Andrew B, Treu, Tommaso, Ellis, Richard S, Sand, David J
Format: Article
Language:English
Subjects:
Adiabatic flow
Astronomical models
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
Dark matter
DENSITY
Galactic clusters
GALAXIES
GALAXY CLUSTERS
GRAVITATIONAL LENSES
MASS
Mathematical models
NONLUMINOUS MATTER
SPATIAL DISTRIBUTION
STARS
Texts
VISIBLE RADIATION
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Summary:We present stellar and dark matter (DM) density profiles for a sample of seven massive, relaxed galaxy clusters derived from strong and weak gravitational lensing and resolved stellar kinematic observations within the centrally located brightest cluster galaxies (BCGs). In Paper I of the series, we demonstrated that the total density profile derived from these data, which span three decades in radius, is consistent with numerical DM-only simulations at radii [> ~]5-10 kpc, despite the significant contribution of stellar material in the core. Here, we decompose the inner mass profiles of these clusters into stellar and dark components. Parameterizing the DM density profile as a power law [rho] sub(DM) [is proportional to] r super(- beta ) on small scales, we find a mean slope [left angle bracket] beta [right angle bracket] = 0.50 + or - 0.10(random)(ProQuest: Formulae and/or non-USASCII text omitted)(systematic). Alternatively, cored Navarro-Frenk-White (NFW) profiles with (ProQuest: Formulae and/or non-USASCII text omitted) provide an equally good description. These density profiles are significantly shallower than canonical NFW models at radii [
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/765/1/25