Detalles de publicación
PP 014066
Tracing a high redshift cosmic web with quasar systems
(1)Tartu Observatory, 61602 Tõravere, Estonia,
(2)Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain,
(3)Universidad de La Laguna, Dept. Astrofísica, E-38206 La Laguna, Tenerife, Spain,
(4)School of Physics, Korea Institute for Advanced Study, 85 Hoegiro, Dong-Dae-Mun-Gu, Seoul 130-722, Korea,
(5)Tuorla Observatory, University of Turku, Väisäläntie 20, Piikkiö, Finland,
(6)Estonian Academy of Sciences, EE-10130 Tallinn, Estonia,
(7)Institute of Physics, Tartu University, Tähe 4, 51010 Tartu, Estonia,
(8)ICRANet, Piazza della Repubblica 10, 65122 Pescara, Italy
Context. To understand the formation, evolution, and present-day properties of the cosmic web we need to study it at low and high
redshifts.
Aims. We trace the cosmic web at redshifts that range from 1.0 ≤ z ≤ 1.8 by using the quasar (QSO) data from the SDSS DR7 QSO
catalogue.
Methods. We apply a friend-of-friend (FoF) algorithm to the quasar and random catalogues to determine systems at a series of linking
length, and analyse richness and sizes of these systems.
Results. At the linking lengths l ≤ 30 h −1 Mpc, the number of quasar systems is larger than the number of systems detected in random
catalogues, and the systems themselves have smaller diameters than random systems. The diameters of quasar systems are comparable
to the sizes of poor galaxy superclusters in the local Universe. The richest quasar systems have four members. The mean space density
−3
of quasar systems, ≈ 10 −7 (h −1 Mpc) , is close to the mean space density of local rich superclusters. At intermediate linking lengths
−1
(40 ≤ l ≤ 70 h Mpc), the richness and length of quasar systems are similar to those derived from random catalogues. Quasar system
diameters are similar to the sizes of rich superclusters and supercluster chains in the local Universe. The percolating system, which
penetrate the whole sample volume appears in a quasar sample at a smaller linking length than in random samples (85 h −1 Mpc). At
the linking length 70 h −1 Mpc, the richest systems of quasars have diameters exceeding 500 h −1 Mpc. Quasar luminosities in systems
are not correlated with the system richness.
Conclusions. Quasar system catalogues in our web pages and at the Strasbourg Astronomical Data Center (CDS) serve as a database
for searching for superclusters of galaxies and for tracing the cosmic web at high redshifts.
redshifts.
Aims. We trace the cosmic web at redshifts that range from 1.0 ≤ z ≤ 1.8 by using the quasar (QSO) data from the SDSS DR7 QSO
catalogue.
Methods. We apply a friend-of-friend (FoF) algorithm to the quasar and random catalogues to determine systems at a series of linking
length, and analyse richness and sizes of these systems.
Results. At the linking lengths l ≤ 30 h −1 Mpc, the number of quasar systems is larger than the number of systems detected in random
catalogues, and the systems themselves have smaller diameters than random systems. The diameters of quasar systems are comparable
to the sizes of poor galaxy superclusters in the local Universe. The richest quasar systems have four members. The mean space density
−3
of quasar systems, ≈ 10 −7 (h −1 Mpc) , is close to the mean space density of local rich superclusters. At intermediate linking lengths
−1
(40 ≤ l ≤ 70 h Mpc), the richness and length of quasar systems are similar to those derived from random catalogues. Quasar system
diameters are similar to the sizes of rich superclusters and supercluster chains in the local Universe. The percolating system, which
penetrate the whole sample volume appears in a quasar sample at a smaller linking length than in random samples (85 h −1 Mpc). At
the linking length 70 h −1 Mpc, the richest systems of quasars have diameters exceeding 500 h −1 Mpc. Quasar luminosities in systems
are not correlated with the system richness.
Conclusions. Quasar system catalogues in our web pages and at the Strasbourg Astronomical Data Center (CDS) serve as a database
for searching for superclusters of galaxies and for tracing the cosmic web at high redshifts.