Some remarks on the angular momenta of galaxies, their clusters and superclusters

Godlowski, Wlodzimierz; Szydłowski, Marek; Флин, П.

doi:10.1007/s10714-005-0046-7

Cited by 25 publications

(35 citation statements)

References 34 publications

(31 reference statements)

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“…We emphasize however, that the above observational results about lack of alignment of galaxies for poor clusters, as well as evidence for such alignment in the rich galaxy clusters (Godłowski, Szydłowski & Flin (2005), Aryal et al (2007), see also Godłowski, 2011 for later improved analysis) clearly shows that angular momentum of galaxy groups and clusters increases with their richness. The problem of clusters angular momenta in context of their mutual interactions as well as those with dark matter haloes has been discussed by Hahn et al (2007) based on the results of computer simulations.…”

Section: Discussionmentioning

confidence: 65%

The non-Gaussian distribution of galaxy gravitational fields

Stephanovich

Godlowski

2017

Res. Astron. Astrophys.

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We perform a theoretical analysis of the observational dependence between angular momentum of the galaxy clusters and their mass (richness), based on the method introduced in our previous paper. For that we obtain the distribution function of astronomical objects (like galaxies and/or smooth halos of different kinds) gravitational fields due to their tidal interaction. Within the statistical method of Chandrasekhar we are able to show that the distribution function is determined by the form of interaction between objects and for multipole (tidal) interaction it is never Gaussian. Our calculation permits to demonstrate how the alignment of galaxies angular momenta depend on the cluster richness. The specific form of the corresponding dependence is due to assumptions made about cluster morphology. Our approach also predicts the time evolution of stellar objects angular momenta within CDM and ΛCDM models. Namely, we have shown that angular momentum of galaxies increases with time.

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Section: Discussionmentioning

confidence: 65%

The non-Gaussian distribution of galaxy gravitational fields

Stephanovich

Godlowski

2017

Res. Astron. Astrophys.

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“…Godlowski et al (2003) described Li (1988) model and showed the relation between the angular momenta and the masses of the large scale structures. This relationship was observationally tested by several authors (Godlowski et al 2005, Hu et al 2006, Aryal & Saurer 2006, Aryal et al 2007, 2008, Godlowski et al 2010, Godlowski 2012 and found the vanishing angular momenta for less massive structures and non-vanishing for larger structures. Aryal et al (2013) studied preferred alignments of angular momentum vectors of galaxies in six rotating clusters (A954, A1139, A1399, A2162, A2169, and A2366) that are dynamically stable and have a single peak in 1D-3D number density maps.…”

Section: Introductionmentioning

confidence: 94%

Preferred alignments of angular momentum vectors of galaxies in six dynamically unstable Abell clusters

Yadav

Aryal

Saurer

2017

Res. Astron. Astrophys.

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A spatial orientation of angular momentum vectors of galaxies in six dynamically unstable Abell clusters (S1171, S0001, A1035, A1373, A1474 and A4053) is studied. For this, two-dimensional observed parameters (e.g., positions, diameters, position angles) are converted into three-dimensional rotation axes of the galaxy using 'position angle -inclination' method. The expected isotropic distribution curves for angular momentum vectors are obtained by performing random simulations. The observed and expected distributions are compared using several statistical tests. No preferred alignments of angular momentum vectors of galaxies are noticed in all six dynamically unstable clusters supporting hierarchy model of galaxy formation. These clusters have a larger value of velocity dispersion. However, local effects are noticed in the clusters that have substructures in the 1D-3D number density maps.

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“…Godlowski et al (2003) derived a relation between angular momentum and the mass of a galaxy using the "Li model" (Li 1998) and tested this relation for Tully's galaxy group (Godlowski et al 2005). For that group, no preferred alignment of SVs of galaxies is noticed.…”

Section: Discussionmentioning

confidence: 99%

Coexistence of chiral symmetry restoration and random orientation of galaxies

Aryal

Paudel

Saurer

2007

A&A

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We studied the chiral symmetry restoration and the spatial orientation of 2288 spiral and spiral barred galaxies that have radial velocities (RV) less than 5000 km s −1 . A random direction of the rotation of galaxies is assumed in order to classify the structural modes. The distribution of spin vector and spin vector projections of leading and trailing arm galaxies in the total sample and subsamples are studied. We use chi-square, auto-correlation and Fourier tests in order to discriminate the preferred alignments from the random alignments. A good correlation between the random alignment and the chiral symmetry is noticed in the Local Supercluster (RV < 3000 km s −1 ) and in galaxies nearby the Local Supercluster (3000 < RV (km s −1 ) ≤ 5000). Spiral galaxies show a similar result. The barred spirals show an opposite trend to that observed for the spirals. Nearby the Local Supercluster, we noticed a preferred spatial alignment and non-chiral property in the leading and trailing arm spiral barred galaxies. Our result predicts that the progressive loss of chirality might have some connection with the rotationally supported (spirals, barred spirals) and randomized (lenticulars, ellipticals) systems. Thus, we suspect that the dynamical processes in the cluster evolution give rise to a dynamical loss of chirality.

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Some remarks on the angular momenta of galaxies, their clusters and superclusters

Cited by 25 publications

References 34 publications

The non-Gaussian distribution of galaxy gravitational fields

The non-Gaussian distribution of galaxy gravitational fields

Preferred alignments of angular momentum vectors of galaxies in six dynamically unstable Abell clusters

Coexistence of chiral symmetry restoration and random orientation of galaxies

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