2,486 research outputs found
Covariance matrices for halo number counts and correlation functions
We study the mean number counts and two-point correlation functions, along
with their covariance matrices, of cosmological surveys such as for clusters.
In particular, we consider correlation functions averaged over finite redshift
intervals, which are well suited to cluster surveys or populations of rare
objects, where one needs to integrate over nonzero redshift bins to accumulate
enough statistics. We develop an analytical formalism to obtain explicit
expressions of all contributions to these means and covariance matrices, taking
into account both shot-noise and sample-variance effects. We compute low-order
as well as high-order (including non-Gaussian) terms. We derive expressions for
the number counts per redshift bins both for the general case and for the small
window approximation. We estimate the range of validity of Limber's
approximation and the amount of correlation between different redshift bins. We
also obtain explicit expressions for the integrated 3D correlation function and
the 2D angular correlation. We compare the relative importance of shot-noise
and sample-variance contributions, and of low-order and high-order terms. We
check the validity of our analytical results through a comparison with the
Horizon full-sky numerical simulations, and we obtain forecasts for several
future cluster surveys.Comment: 37 page
Evolution of the X-ray Profiles of Poor Clusters from the XMM-LSS Survey
A sample consisting of 27 X-ray selected galaxy clusters from the XMM-LSS
survey is used to study the evolution in the X-ray surface brightness profiles
of the hot intracluster plasma. These systems are mostly groups and poor
clusters, with temperatures 0.6-4.8 keV, spanning the redshift range 0.05 to
1.05. Comparing the profiles with a standard beta-model motivated by studies of
low redshift groups, we find 54% of our systems to possess a central excess,
which we identify with a cuspy cool core. Fitting beta-model profiles, allowing
for blurring by the XMM point spread function, we investigate trends with both
temperature and redshift in the outer slope (beta) of the X-ray surface
brightness, and in the incidence of cuspy cores. Fits to individual cluster
profiles and to profiles stacked in bands of redshift and temperature indicate
that the incidence of cuspy cores does not decline at high redshifts, as has
been reported in rich clusters. Rather such cores become more prominent with
increasing redshift. Beta shows a positive correlation with both redshift and
temperature. Given the beta-T trend seen in local systems, we assume that
temperature is the primary driver for this trend. Our results then demonstrate
that this correlation is still present at z~0.3, where most of our clusters
reside.Comment: Accepted for publication in MNRAS. 15 pages, 12 figure
Structure Detection in Low Intensity X-Ray Images
In the context of assessing and characterizing structures in X-ray images, we
compare different approaches. Most often the intensity level is very low and
necessitates a special treatment of Poisson statistics. The method based on
wavelet function histogram is shown to be the most reliable one. We also
present a multi-resolution filtering method based on the wavelet coefficients
detection. Comparative results are presented by means of a simulated cluster of
galaxies.Comment: 11 pages, 9 figures, to appear in Astronomy & Astrophysic
Du modalisateur au marqueur de ponctuation des actions : le cas de bon
Bon, est un mot du discours qui reçoit des interprétations variées suivant le contexte conversationnel. Nous tentons de décrire les propriétés associées aux différents emplois de bon sur les plans syntagmatique, pragmatique et structurel du discours. L’analyse fait ressortir deux fonctions discursives principales : le modalisateur et le marqueur de structuration de la conversation (MSC) (Roulet & al., 1985). L’examen du fonctionnement de ce marqueur discursif révèle qu’il est possible de rassembler autour d’une même valeur sémantico-pragmatique l’ensemble de ces emplois : le marqueur de ponctuation oral qui scande et délimite les activités verbales et non verbales (cognitive, énonciative ou physique) des participants à la conversation.Certains words like bon in French are subject to various interpretations according to context in which they appear. A description of the syntagmatic, pragmatic and discursive properties associated with the different uses of bon is presented. Two values of bon are examined: the modifier and the discourse marker (Roulet & al., 1985). A general semantico-pragmatic value is proposed to account for the various roles associated with bon in conversation: an "action punctuation marker" that scands and delimites the verbal and non verbal (cognitive, utterance or physical) activities of the participants
Fauna africana oligocena y nuevas formas endémicas entre los micromamÃferos de Mallorca (Nota preliminar)
Abstract not availabl
The X-CLASS - redMaPPer galaxy cluster comparison: I. Identification procedures
We performed a detailed and, for a large part interactive, analysis of the
matching output between the X-CLASS and redMaPPer cluster catalogues. The
overlap between the two catalogues has been accurately determined and possible
cluster positional errors were manually recovered. The final samples comprise
270 and 355 redMaPPer and X-CLASS clusters respectively. X-ray cluster matching
rates were analysed as a function of optical richness. In a second step, the
redMaPPer clusters were correlated with the entire X-ray catalogue, containing
point and uncharacterised sources (down to a few 10^{-15} erg s^{-1} cm^{-2} in
the [0.5-2] keV band). A stacking analysis was performed for the remaining
undetected optical clusters. Main results show that neither of the wavebands
misses any massive cluster (as coded by X-ray luminosity or optical richness).
After correcting for obvious pipeline short-comings (about 10% of the cases
both in optical and X-ray), ~50% of the redMaPPer (down to a richness of 20)
are found to coincide with an X-CLASS cluster; when considering X-ray sources
of any type, this fraction increases to ~ 80%; for the remaining objects, the
stacking analysis finds a weak signal within 0.5 Mpc around the cluster optical
centers. The fraction of clusters totally dominated by AGN-type emission
appears to be of the order of a few percent. Conversely ~ 40% of the X-CLASS
clusters are identified with a redMaPPer (down to a richness of 20) - part of
the non-matches being due to the fact that the X-CLASS sample extends further
out than redMaPPer (z<1 vs z<0.6); extending the correlation down to a richness
of 5, raises the matching rate to ~ 65%.Comment: 15 pages, 20 figures, 2 table
The cosmological analysis of X-ray cluster surveys V. The potential of cluster counts in the range
Cosmological studies have now entered Stage IV according to the Dark Energy
Task Force prescription, thanks to new missions (Euclid, Rubin Observatory,
SRG/eROSITA) that are expected to provide the required ultimate accuracy in the
dark energy (DE) equation of state (EoS). However, none of these projects have
the power to systematically unveil the galaxy cluster population at .
There therefore remains the need for an ATHENA-like mission to run independent
cosmological investigations and scrutinise the consistency between the results
from the and epochs. We study the constraints on the DE EoS and
on primordial non-Gaussanities for typical X-ray cluster surveys executed by
ATHENA. We consider two survey designs: 50 deg at 80ks (survey A) and 200
deg at 20ks (survey B). We analytically derive cluster counts in a space of
observable properties, and predict the cosmological potential of the
corresponding samples with a Fisher analysis. The achieved depth allows us to
unveil the halo mass function down to the group scale out to . We predict
the detection of thousands of clusters down to a few 10, in particular 940 and 1400 clusters for surveys A and B,
respectively, at . Such samples will allow a detailed modelling of the
evolution of cluster physics along with a standalone cosmological analysis. Our
results suggest that survey B has the optimal design as it provides greater
statistics. Remarkably, high- clusters, despite representing 15% or less of
the full samples, allow a significant reduction of the uncertainty on the
cosmological parameters: is reduced by a factor of 2.3 and by a factor of 3. Inventorying the high- X-ray cluster
population can play a crucial role in ensuring overall cosmological
consistency. This will be the major aim of future new-generation ATHENA-like
missions.Comment: Accepted for publication in A&A, 17 pages, 18 figure
- …