2001A&A...378..345H


Query : 2001A&A...378..345H

2001A&A...378..345H - Astronomy and Astrophysics, volume 378, 345-360 (2001/11-1)

Kinematics of the local universe. IX. The Perseus-Pisces supercluster and the Tolman-Bondi model.

HANSKI M.O., THEUREAU G., EKHOLM T. and TEERIKORPI P.

Abstract (from CDS):

The matter distribution around the Perseus-Pisces (PP) supercluster is studied by comparing peculiar velocities given by the Kinematics of the local universe (KLUN) galaxy sample to those predicted by Tolman-Bondi (TB) models. To restrict the TB solutions we first solve the mass of the densest part of PP. This part is identified as a sphere at (l,b)=(140.2°, -22.0°), d ≃50h–1Mpc having a radius of 15h–1Mpc. This sphere surrounds the main part of the PP ridge and four most prominent clusters of the region. Using virial-like mass estimators we calculate the cluster masses and obtain the upper and lower limits for the mass inside the 15h–1Mpc sphere: MPP=4-7h–1*1015M. This corresponds to a mass overdensity δPP≃4, or ρPP=1-2ρcr. Mass to light ratios of the clusters are M/L=200-600hM/L, giving mass density ratio Ω0=0.1-0.3, if the value of M/L is assumed to be representative elsewhere in the universe. We estimate a radial density distribution around the PP core using two toy models and a smoothed density distribution observed for IRAS galaxies. The cosmological density parameters (Ω0, ΩΛ) and the PP mass are free parameters in the TB calculations. The KLUN velocities, obtained by Tully-Fisher relation and the normalized distance method, are adjusted by the Local Group (LG) infall velocity towards PP. Comparison of the TB velocities to KLUN data points indicates that the infall velocity vinf<100km/s. Allowing MPP to vary within the limits given above we get constraints for the value of Ω0; Ω0=0.2-0.4 are prefered to the more extreme values, Ω0=0.1 or 1. A choice of either ΩΛ=1-Ω0 or 0 do not cause any significant changes in the results. The validity of the TB model in complex environments is studied with an N-body simulation. There we see that the radially averaged velocity fields around simulated clusters are compatible with the corresponding TB velocities. This confirms the applicability of the TB model around large galaxy concentrations, providing that smoothed density and radially averaged velocity fields are used.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: Pers-Pisc supercluster - cosmology: theory - large-scale structure of the universe

CDS comments: in ref list Diaferio 1999MNRAS.307..537D instead of 307.552

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME PSC CL ClG 00 58 25.0 +30 39 11           ~ 127 1
2 NAME Pisces I G 01 03 56.6 +21 53 41   16.18 14.3     ~ 373 0
3 EQ 0121+331 G 01 24 43 +33 21.6           ~ 2 0
4 LEDA 197586 G 01 24 47.1930488064 +33 20 40.022492964           ~ 4 0
5 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 675 1
6 NAME PER SUPERCL SCG 02 33.2 +41 37           ~ 389 1
7 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2093 1
8 NAME Corona Borealis SCG 15 25 +29.5           ~ 123 0

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2022.05.25-22:10:41

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