Properties of clumps and filaments around galaxy clusters
  We report on the possibility of studying the proprieties of cosmic diffuse
baryons by studying self-gravitating clumps and filaments connected to galaxy
clusters. While filaments are challenging to detect with X-ray observations,
the higher density of clumps makes them visible and a viable tracer to study
the thermodynamical proprieties of baryons undergoing accretion along cosmic
web filaments onto galaxy clusters. We developed new algorithms to identify
these structures and applied them to a set of non-radiative cosmological
simulations of galaxy clusters at high resolution. We find that in those
simulated clusters, the density and temperature of clumps are independent of
the mass of the cluster where they reside. We detected a positive correlation
between the filament temperature and the host cluster mass. The density and
temperature of clumps and filaments also tended to correlate. Both the
temperature and density decrease moving outward. We observed that clumps are
hotter, more massive, and more luminous if identified closer to the cluster
center. Especially in the outermost cluster regions (~3*R500,c or beyond),
X-ray observations might already have the potential to locate cosmic filaments
based on the distribution of clumps and to allow one to study the
thermodynamics of diffuse baryons before they are processed by the intracluster
medium.
