@Article{DurretMAACCMSU:2016:SeFiLa,
author = "Durret, F. and M{\'a}rquez, I. and Acebr{\'o}n, A. and Adami, C.
and Cabrera-Lavers, A. and Capelato, Hugo Vicente and Martinet, N.
and Sarron, F. and Ulmer, M. P.",
affiliation = "{Sorbonne Universit{\'e}s} and {Instituto de Astrof{\'{\i}}sica
de Andaluc{\'{\i}}a} and {Aix Marseille Universit{\'e}} and
{Aix Marseille Universit{\'e}} and {Instituto de
Astrof{\'{\i}}sica de Canarias} and {Instituto Nacional de
Pesquisas Espaciais (INPE)} and {Sorbonne Universit{\'e}s} and
{Sorbonne Universit{\'e}s} and {Northwestern University}",
title = "Searching for filaments and large-scale structure around DAFT/FADA
clusters",
journal = "Astronomy \& Astrophysics",
year = "2016",
volume = "588",
pages = "A69",
month = "Apr.",
keywords = "Galaxies: clusters: general, Large scale structure of Universe.",
abstract = "Context. Clusters of galaxies are located at the intersection of
cosmic filaments and are still accreting galaxies and groups along
these preferential directions. However, because of their
relatively low contrast on the sky, filaments are difficult to
detect (unless a large amount of spectroscopic data are
available), and unambiguous detections have been limited until now
to relatively low redshifts (z< \∼ 0.3). Aims. This project
is aimed at searching for extensions and filaments around
clusters, traced by galaxies selected to be at the cluster
redshift based on the red sequence. In the 0.4 <z< 0.9 redshift
range of our sample, clusters are believed to be already well
formed, but still to be accreting material along filaments.
Methods. We have searched for extensions and filaments around the
thirty clusters of the DAFT/FADA survey for which we had deep wide
field photometric data. For each cluster, based on a
colour-magnitude diagram, we selected galaxies that were likely to
belong to the red sequence, and hence to be at the cluster
redshift, and built density maps. By computing the background for
each of these maps and drawing 3\σ contours, we estimated
the elongations of the structures detected in this way. Whenever
possible, we identified the other structures detected on the
density maps with clusters listed in NED. Results. We find clear
elongations in twelve clusters out of thirty, with sizes that can
reach up to 7.6 Mpc. Eleven other clusters have neighbouring
structures, but the zones linking them are not detected in the
density maps at a 3\σ level. Three clusters show no extended
structure and no neighbours, and four clusters are of too low
contrast to be clearly visible on our density maps. Conclusions.
The simple method we have applied appears to work well to show the
existence of filaments and/or extensions around a number of
clusters in the redshift range 0.4 <z< 0.9. We plan to apply it to
other large cluster samples such as the clusters detected in the
CFHTLS and SDSS-Stripe 82 surveys in the near future.",
doi = "10.1051/0004-6361/201527655",
url = "http://dx.doi.org/10.1051/0004-6361/201527655",
issn = "0004-6361 and 1432-0746",
language = "en",
targetfile = "1_durret_searching.pdf",
urlaccessdate = "15 jun. 2024"
}