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Kinematical Evolution of the Pairwise Velocity Field of Galaxies

Published online by Cambridge University Press:  25 May 2016

Naoki Seto
Affiliation:
Department of Physics, Kyoto University, Kyoto 606-01
Jun'ichi Yokoyama
Affiliation:
Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-01

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It has been a long-standing cosmological issue to explain why the statistical distribution of the radial pairwise peculiar velocity of galaxies has an exponential shape rather than the Gaussian, as suggested by observations and explicitly shown by results of N-body simulations. Previous explanations on the exponential distribution are based on highly nonlinear dynamics of galactic systems (R < 1h –1 Mpc). That is, the exponential feature appears as a result of superposition of Gaussian velocity distributions in clumps with various velocity dispersions. Hence although this model is suitable to account for a symmetric exponential distribution with vanishing mean net relative velocity, a more elaborate treatment is necessary in order to reproduce an asymmetric exponential distribution with its peak at a negative relative velocity as observed in numerical simulations.

Type
IV. Structure Formation and Dark Matter
Copyright
Copyright © Kluwer 1999 

References

Seto, N. and Yokoyama, J. (1998), ApJ, in press (Jan 10 issue, astro-ph/9707312) Google Scholar
Sheth, R. K. (1996), MNRAS, 279, 1311 CrossRefGoogle Scholar
Zurek, W. H. et al. (1994) ApJ, 431, 559 CrossRefGoogle Scholar
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