@Article{OldWPGMSTBYCMSSCBPLS:2018:ImDySu,
author = "Old, L. and Wojtak, R. and Pearce, F. R. and Gray, M. E. and
Mamon, G. A. and Sif{\'o}n, C. and Tempel, E. and Biviano, A. and
Yee, H. K. C. and Carvalho, Reinaldo Ramos de and M{\"u}ller, V.
and Sepp, T. and Skibba, R. A. and Croton, D. and Bamford, S. P.
and Power, C. and von der Linden, A. and Saro, A.",
affiliation = "{University of Toronto} and {Stanford University} and {University
of Nottingham} and {University of Nottingham} and {Sorbonne
Universit{\'e}s} and {Princeton University} and {Leibniz-Institut
f{\"u}r Astrophysik Potsdam (AIP)} and {INAF-Osservatorio
Astronomico di Trieste} and {University of Toronto} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Leibniz-Institut
f{\"u}r Astrophysik Potsdam (AIP)} and {Tartu Observatory} and
{University of California} and {Swinburne University of
Technology} and {University of Nottingham} and {University of
Western Australia} and {Stony Brook University} and
{INAF-Osservatorio Astronomico di Trieste}",
title = "Galaxy cluster mass reconstruction project - III: the impact of
dynamical substructure on cluster mass estimates",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2018",
volume = "475",
number = "1",
pages = "853--866",
keywords = "Cosmological parameters, Galaxies: Clusters: General, Galaxies:
Groups: General, Galaxies: Haloes, Galaxies: Kinematics and
dynamics, Large-scale structure of Universe.",
abstract = "With the advent of wide-field cosmological surveys, we are
approaching samples of hundreds of thousands of galaxy clusters.
While such large numbers will help reduce statistical
uncertainties, the control of systematics in cluster masses is
crucial. Here we examine the effects of an important source of
systematic uncertainty in galaxy-based cluster mass estimation
techniques: the presence of significant dynamical substructure.
Dynamical substructure manifests as dynamically distinct subgroups
in phase-space, indicating an 'unrelaxed' state. This issue
affects around a quarter of clusters in a generally selected
sample. We employ a set of mock clusters whose masses have been
measured homogeneously with commonly used galaxy-based mass
estimation techniques (kinematic, richness, caustic, radial
methods). We use these to study how the relation between
observationally estimated and true cluster mass depends on the
presence of substructure, as identified by various popular
diagnostics.We find that the scatter for an ensemble of clusters
does not increase dramatically for clusters with dynamical
substructure. However, we find a systematic bias for all methods,
such that clusters with significant substructure have higher
measured masses than their relaxed counterparts. This bias depends
on cluster mass: the most massive clusters are largely unaffected
by the presence of significant substructure, but masses are
significantly overestimated for lower mass clusters, by ~10 per
cent at 1014 and \≳20 per cent for \≲1013.5. The use
of cluster samples with different levels of substructure can
therefore bias certain cosmological parameters up to a level
comparable to the typical uncertainties in current cosmological
studies.",
doi = "10.1093/mnras/stx3241",
url = "http://dx.doi.org/10.1093/mnras/stx3241",
issn = "0035-8711 and 1365-2966",
label = "self-archiving-INPE-MCTIC-GOV-BR",
language = "en",
urlaccessdate = "27 abr. 2024"
}