scholarly journals Surveying the Local Supercluster Plane

2018 ◽  
Vol 73 (2) ◽  
pp. 124-141 ◽  
Author(s):  
O. G. Kashibadze ◽  
I. D. Karachentsev ◽  
V. E. Karachentseva
Keyword(s):  
Local Supercluster

scholarly journals A new catalogue of multiple galaxies in the Local Supercluster

2000 ◽  
Vol 174 ◽  
pp. 40-45
Author(s):  
D. I. Makarov ◽  
I. D. Karachentsev
Keyword(s):  
New Approach ◽  
Galaxy Groups ◽  
Closed Orbits ◽  
Crossing Time ◽  
Local Supercluster ◽  
Virial Mass ◽  
Nearby Galaxies ◽  
The Individual ◽  
Group Member ◽  
Harmonic Radius

AbstractA new approach is suggested which makes use of the individual properties of galaxies, for the identification of small galaxy groups in the Local Supercluster. The criterion is based on the assumption of closed orbits of the companions around the dominating group member within a zero velocity sphere.The criterion is applied to a sample of 6321 nearby galaxies with radial velocities V0 ≤ 3000 km s−1. These 3472 galaxies have been assigned to 839 groups that include 55% of the sample considered. For the groups identified by the new algorithm (with k ≥ 5 members) the median velocity dispersion is 86 km s−1, the median harmonic radius is 247 kpc, the median crossing time is 0.08(1/H), and the median virial-mass-to-light ratio is 56 M⊙/L⊙.

The Dynamics of the Local Supercluster

1983 ◽  
Vol 6 ◽  
pp. 749-750 ◽  
Author(s):  
John P. Huchra
Keyword(s):  
Primary Reason ◽  
Local Supercluster ◽  
The Universe

The primary reason for studying the dynamics of the local supercluster is for use as a local cosmological test (Silk 1974 Ap. J. 193, 525, Peebles 1976, Ap. J. 205, 318). In addit ion, the measurement of the mass enclosed in the local supercluster provides one of the best measurements of the M/L of galaxy systems on very large scales - a test of the hypothesis that M/L increases with radius for galaxy systems and thus a measure of the unseen matter (neutrino?) content of the universe.

Joint Commission Meeting on the Local Supercluster and its Environment

1983 ◽  
pp. 745-760
Author(s):  
R. Brent Tully ◽  
John P. Huchra ◽  
E. E. Salpeter ◽  
G. O. Abell ◽  
J. Einasto ◽  
...  
Keyword(s):  
Joint Commission ◽  
Local Supercluster

scholarly journals Contributions to the Local Gravitational Field from beyond the Local Supercluster

1987 ◽  
Vol 117 ◽  
pp. 435-443
Author(s):  
A. Yahil
Keyword(s):  
Gravitational Field ◽  
Background Radiation ◽  
Nonlinear Effects ◽  
Linear Perturbation ◽  
Density Parameter ◽  
Microwave Background ◽  
Dipole Component ◽  
Local Supercluster ◽  
Microwave Background Radiation ◽  
Linear Perturbation Theory

IRAS 60μ sources are used to map the local (≲200h−1 Mpc, Ho =100h km s−1 Mpc−1) gravitational field, and to determine its dipole component, on the assumption that the infrared radiation traces the matter. The dipole moment is found to point in the direction of the anisotropy of the microwave background radiation. Comparison of the two anisotropies, using linear perturbation theory, yields an estimate of the cosmological density parameter, Ω =0.85±0.16, with nonlinear effects increasing Ωo by ∼15%. The quadrupolar tidal field within the Local Supercluster, due presumably to the same density inhomogeneities, is detected in a kinematical study of the velocity field.

scholarly journals The Orientation of Galaxies in Nearby Galaxy Groups

2004 ◽  
Vol 217 ◽  
pp. 116-117
Author(s):  
P. Flin ◽  
M. Biernacka ◽  
J. Krywult
Keyword(s):  
Statistical Analysis ◽  
Milky Way ◽  
Random Distribution ◽  
Local Group ◽  
Dwarf Galaxies ◽  
Nearby Galaxy ◽  
Groups Of Galaxies ◽  
Galaxy Groups ◽  
Isotropic Distribution ◽  
Local Supercluster

The statistical analysis of six nearby groups of galaxies, connected with the Milky Way, M31, M81, M101, NGC5128 and NGC5236 shows an isotropic distribution of galaxy planes, similarly to galaxies within the Local Group. Also planes of galaxies in the nearby (Vr < 500 km s−1) region of the Local Supercluster exhibit random distribution, disregarding their membership to groups. The result shows that strong environmental effects observed among dwarf galaxies do not change generally random distribution of galaxy planes in this region.

scholarly journals Superclustering of Galaxies

1974 ◽  
Vol 63 ◽  
pp. 79-92 ◽  
Author(s):  
G. O. Abell
Keyword(s):  
Power Spectrum ◽  
Spectrum Analysis ◽  
Covariance Function ◽  
Size Dependence ◽  
Large Deviation ◽  
Power Spectrum Analysis ◽  
Clusters Of Galaxies ◽  
Surface Distribution ◽  
Local Supercluster ◽  
Internal Velocity

Evidence for superclustering of galaxies includes the local supercluster, the large deviation of the observed surface distribution of clusters of galaxies from a random one, the cell size dependence of the index of clumpiness, the results of covariance function tests for correlations between different cluster centers and between clusters and individual galaxies, and a power-spectrum analysis. All tests give results that indicate or are compatible with the existence of inhomogeneities in the distribution of matter in space with linear diameters of 50 to 100 Mpc. If these are dynamically stable superclusters, they probably have internal velocity dispersions in the range 1000 to 3000 km s-1. The possible effects of superclustering on dynamical studies of individual clusters are discussed briefly.

scholarly journals The Physical Properties of Large Scale Systems from Optical Observations

1978 ◽  
Vol 79 ◽  
pp. 253-262
Author(s):  
G. O. Abell
Keyword(s):  
Physical Properties ◽  
Large Scale ◽  
Local Group ◽  
Optical Observations ◽  
Local Inhomogeneity ◽  
Large Scale Systems ◽  
Local Supercluster

Holmberg's (1937) analysis of the distribution of double and multiple galaxies provided what may have been the first hint of a local inhomogeneity of greater scale than that of the Local Group. the idea of a Local Supercluster was subsequently revived by de Vaucouleurs (1953, 1956, 1958). the analyses of others, as well as the continuing study of de Vaucouleurs himself (1976 and references cited therein) have now effectively established the reality of the Local Supercluster. Several other more remote inhomogeneities, or “clouds” of galaxies, were described by Shane and Wirtanen (1954). the writer (Abell 1958) found the distribution of rich clusters to be clumpy, and published a finding list of several apparent superclusters (Abell 1961).

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