The Distribution in Space of Clusters of Galaxies

Kiang, T.; Saslaw, William C.

doi:10.1093/mnras/143.2.129

Cited by 38 publications

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“…It starts on small length scales having short dynamical timescales and gradually spreads to larger scales. This is a development of early ideas of continuous clustering (Kiang 1967;Kiang & Saslaw 1969;Saslaw 1972).…”

Section: Discussionmentioning

confidence: 99%

Gravitational Phase Transitions in the Cosmological Many-Body System

Saslaw

Ahmad

2010

ApJ

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Gravitational many-body clustering of particles (e.g., galaxies) in an expanding universe may be regarded as a form of phase transition. We calculate its properties here and find that it differs in several ways from usual laboratory phase transitions. The cosmological case is never complete since it takes longer to evolve dynamically on larger spatial scales. To examine this, we calculate the effects of higher order corrections on the thermodynamic properties and distribution functions (which are known to agree with observations). The additional higher order terms are subdominant and decrease as the number of particles in the system increases. We also propose an order parameter for this hierarchical phase transition and discuss its relation to the Yang-Lee theory of phase transitions. These results also help to quantify earlier ideas of "continuous clustering."

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Section: Discussionmentioning

confidence: 99%

Gravitational Phase Transitions in the Cosmological Many-Body System

Saslaw

Ahmad

2010

ApJ

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“…[I was not aware of it then, but there already was a considerable literature on the galaxy correlation function, including Katz & Mulders (1942);Zwicky (1942); Neyman & Scott (1952);Limber (1954); Rubin (1954);Layzer (1956) ;Neyman, Scott & Shane (1956); Irvine (1961); Kiang (1967); Kiang & Saslaw (1969);and Totsuji & Kihara (1969).] To me the choice was between that and its transform, a power spectrum.…”

Section: Statistical Measures Of Cosmic Structurementioning

confidence: 99%

Seeing Cosmology Grow

Peebles

2012

Annu. Rev. Astron. Astrophys.

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The modest science of cosmology I encountered a half century ago has grown into big science. I comment on steps in this development I think I understand because I was there or, in some cases, wish I had been. Wonderful insights-or lucky guesses-and elegant deductions from measurements were accompanied by the usual mix of unlucky guesses and disregard of unwelcome evidence. I say "usual" because I suspect the course of development of any other natural science is similarly erratic. An example in cosmology is Einstein's homogeneous Universe, which was largely accepted as a working hypothesis when there was scant evidence and seriously challenged after we had a reasonable case for homogeneity. Similar mixes of insight and inattention led to the eventual identification of the 3K microwave background, the demonstration that large-scale structure grew by the gravitational instability of the expanding Universe, and the completion of a tight network of cosmological tests. A half century ago, we had little idea what would become of what we were doing in cosmology. We have a better picture now, but I expect there to be more surprises.

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“…The methods used most are i) the dispersion-subdivision test (Zwicky 1952) -Zwicky & Rudnicki (1966, Karpowicz (1967aKarpowicz ( ,b, 1970aKarpowicz ( ,b, 1971c; ii) the analysis of the index of dumpiness (Neyman & Scott 1952, Neyman et al 1954) -Kiang (1967. Kalinkov (1974b), iii) x-squared test - Abell (1958), Abell & Seligman (1965, Gusak (1969), Fullerton & Hoover (1972), Kalinkov (1974b); iv) the correlation and power spectrum analysis -Karachentsev (1966), Kiang (1967), Kiang & Saslaw (1969), Yu & Peebles (1969), Fullerton & Hoover (1972), Peebles ( , 1975, Hauser & Peebles (1973), Peebles & Hauser (1974), Peebles & Groth (1975), Kalinkov (1973bKalinkov ( , 1974aKalinkov ( ,b, 1975, Kalinkov & Janeva (1976), Kalinkov et al (1975a,c,d); v) the distances to the nearest neighbours - Bogart & Wagoner (1973), Kalinkov (1974b). Some other methods have also been applied -e.g.…”

Section: Methods and Resultsmentioning

confidence: 99%

“…It is based on the ideas and results from Neyman et al (1954), Abell (1958), Slakter (1966 and Kiang & Saslaw (1969). This is in fact a generalized x -squared test for searching for characteristic sizes, especially for second-order clusters.…”

Section: Methods Of Comparison Between Observed and Expected Distribumentioning

confidence: 99%

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The Existence of High-Order Clusters of Galaxies

Kalinkov

1977

Highlights astron.

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The problem of the existence of high-order clustering of galaxies is a basic one in extragalactic astronomy and cosmology. In a conventional formulation this problem consists of indicating the largest configurations in the spatial distribution of galaxies.All treatments are carried out generally on the material presented in the catalogues of Abell (1958) and Zwicky et al. (1961-1968). However catalogues of the Jagellonian type (Rudnicki et al. 1973) may turn out to be extremely valuable. The nature of the observational material demonstrates that only statistical methods may be applied effectively. It is already clear that the expected effects are not large even if high-order clustering is a basic property in the Universe.

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The Distribution in Space of Clusters of Galaxies

Cited by 38 publications

References 0 publications

Gravitational Phase Transitions in the Cosmological Many-Body System

Gravitational Phase Transitions in the Cosmological Many-Body System

Seeing Cosmology Grow

The Existence of High-Order Clusters of Galaxies

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