Hostname: page-component-848d4c4894-x24gv Total loading time: 0 Render date: 2024-06-03T21:25:07.661Z Has data issue: false hasContentIssue false
  • English
  • Français

Dynamics and Interactions of High-Redshift Galaxies

Published online by Cambridge University Press:  25 May 2016

M. Noguchi
M. Noguchi*
Affiliation:
Astronomical Institute, Tohoku University, Aoba, Sendai 980-77, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A large number of high redshift galaxies observed with the Hubble Space Telescope (HST) show anomalous morphology and photometric properties, which may be an indication of evolutionary process in young galaxies. We show here by means of numerical simulations that the copious interstellar gas existing in the disks of rapidly collapsing protogalaxies can bring about these peculiarities. Gravitational instability in a gas-rich disk leads to the formation of massive gas clumps with a typical mass of 109M⊙. These subgalactic clumps make disk galaxy evolution a dynamically energetic and chaotic process, and give a natural explanation for peculiar morphology of high redshift galaxies. Moreover, the present model provides a new picture on the causal relationship between the emergence of quasar activities and the dynamical evolution of host galaxies. The clump-driven evolution model is also capable of explaining the correlations observed among present-day galaxies. Namely, the relative bulge dominance, existence of a thick disk, and a mass of the super-massive black hole situated at the galactic center should all be correlated positively. In contrast to their vigorous evolution in isolated state, primeval disk galaxies do not show any dramatic enhancement of activity or remarkable dynamical response in interaction with another galaxies.

Type
Deep Fields & Evolution
Information
Symposium - International Astronomical Union , Volume 186: Galaxy Interactions at High and Low Redshift , 1999 , pp. 431 - 438
Copyright
Copyright © Kluwer 1999 

References

Barnes, J.E., and Hernquist, L. (1992), Ann. Rev. Astron. Astrophys. 30, 705–742 CrossRefGoogle Scholar
Kormendy, J., and Richstone, D. (1995), Ann. Rev. Astron. Astrophys. 33, 581–624 Google Scholar
Noguchi, M. (1988), Astron. Astrophys. 203, 259–272 Google Scholar
Noguchi, M. (1996), Astrophys. J. 469, 605–622 Google Scholar
Noguchi, M. (1997), submitted Google Scholar
Noguchi, M. (1998), in preparation Google Scholar
Rich, R.M. (1996), in Unsolved Problems of the Milky Way (eds. Blitz, L. & Teuben, P.) 403–410 (IAU Symp. No. 169, Kluwer Academic Publishers, Dordrecht)Google Scholar
Rubin, V.C., Burstein, D., Ford, W.K., and Thonnard, N. (1985), Astrophys. J. 289, 81–104 CrossRefGoogle Scholar
Saio, H., and Yoshii, Y. (1990), Astrophys. J. 363, 40–49 CrossRefGoogle Scholar
Schade, D., Lilly, S.J., Crampton, D., Hammer, F., Le Fèvre, O., and Tresse, L. (1995), Astrophys. J. 451, L1–L4 CrossRefGoogle Scholar
van den Bergh, S., Abraham, R.G., Ellis, R.S., Tanvir, N.R., Santiago, B.X., and Glazebrook, K.G. (1996), Astron. J. 112, 359–368 Google Scholar