The orientation of galaxies in clusters

Trèvese, D.; Cirimele, G.; Флин, П.

doi:10.1086/116286

Cited by 50 publications

(53 citation statements)

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“…We can now give the astrophysical interpretation of the results obtained in §2.2: the stable equilibrium position of a triaxial galaxy at the center of a triaxial cluster corresponds geometrically to the three principal axes of the galaxy to be collinear -in the same order -with the principal axes of the cluster density distribution. This configuration reproduces in a natural way the observed "strong alignment of the [brightest] galaxy major axis with the long axis of the parent cluster" (Trevese, Cirimele, Flin 1992), already mentioned in the Introduction. In order to estimate the oscillatory periods of a galaxy around its equilibrium position, the numerical values of the TF components in a realistic cluster are needed.…”

Section: Triaxial Galaxies At the Center Of Triaxial Clusterssupporting

confidence: 82%

“…Fong, Stevenson & Shanks (1990) found a moderately significant radial alignment of Es, together with a less significant tendency of Es to be oriented perpendicularly to this direction. The best evidence for alignment is for the Brightest Cluster Ellipticals: Trevese, Cirimele & Flin (1992) described a "strong alignment of the brightest galaxy major axis with the long axis of the parent cluster".…”

Section: Introductionmentioning

confidence: 99%

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Ciotti

Giampieri

1997

Celestial Mechanics and Dynamical Astronomy

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Abstract.We investigate the motion, near the equilibrium configurations, of an initially spinless rigid body subject to an external tidal field. Two cases are considered: when the center of mass of the body is at rest at the equilibrium point of the field generated by a generic mass distribution, and when it is placed on a circular orbit subject to a spherically symmetric potential. A complete analysis of the equilibrium configurations is carried out for both cases. First, we derive the conditions for the stable equilibria, and then we analyze the frequencies of oscillations around the equilibrium positions. In view of these results, we consider the problem of alignment of galaxies in clusters. After estimating the period of the oscillations induced on the galaxies by the tidal field of the cluster, we discuss the possible effect of resonances between stellar orbits inside the galaxy and the oscillations of the galaxy as a whole; this may be a mechanism responsible for producing an intracluster stellar population.

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Section: Triaxial Galaxies At the Center Of Triaxial Clusterssupporting

confidence: 82%

Section: Introductionmentioning

confidence: 99%

Untitled

Ciotti

Giampieri

1997

Celestial Mechanics and Dynamical Astronomy

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“…Nevertheless, it is clear that in isolated Abell clusters of galaxies only the dominant brightest cluster members exhibit the sign of alignment [35,36,37]. However, in very rich galaxy clusters, such as A754 [38], or A1656 [39,40,41] the nonrandom distribution of galaxies has been observed.…”

Section: Resultsmentioning

confidence: 99%

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

2005

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We discuss the relation between angular momenta and masses of galaxy structures base on the Li model of the universe with global rotation. In our previous paper (God lowski et al 2002) it was shown that the model predicts the presence of a minimum in this relation. In the present paper we discuss observational evidence allowing us to verify this relation. We check these theoretical predictions analysing Tully's galaxy grups. We find null angular momentum J = 0 for the masses corresponding to mass of galaxy grups and non-vanishing angular momenta for other galaxies structures. The comparing of alignment in different galactic structures are consistent with obtained theoretical relation J(M ) if we interpret the groving alignment as the increasing angular momenta of galaxies in the large scale.

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“…This is the fourth, and the last one, of a series of papers (Trèvese et al 1992;Flin et al 1995;Trèvese et al 1997) giving the positions, magnitudes ellipticities and orientations of cluster galaxies with magnitudes between m 3 and m 3 + 3, where m 3 is the magnitude of the third brightest galaxy within one Abell radius from the cluster centre. Because the details of the observations and data reduction were given in the previous papers, here in Sect.…”

Section: Introductionmentioning

confidence: 95%