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Faint Galaxy Number-Counts

  • N. Metcalfe
  • T. Shanks
  • R. Fong
  • J. Gardner
  • N. Roche
Conference paper
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUS, volume 171)

Abstract

Observers studying the cosmology and evolutionary history of our Universe through the statistical properties of “normal” galaxies have four main tools at their disposal. (1) The number-redshift relation. Although a very powerful diagnostic, spectroscopic surveys are currently limited to B < 24m and significantly incomplete in the range, 23m < B < 24m. (2) Galaxy number-magnitude counts. Although by themselves, they cannot constrain models as tightly as spectroscopy, they can be measured ~ 4m fainter, where cosmological effects are expected to be significant. (3) Galaxy colours over a wide wavelength range, which provide additional constraints. (4) The dependence of galaxy clustering with magnitude. ω(θ) can be measured to the limit of the counts.

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References

  1. Jones, L.R., Fong, R., Shanks, T., Ellis, R.S., Peterson, B.A., 1991, MNRAS, 249, 481ADSGoogle Scholar
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  6. Stevenson, P.R.F., Shanks, T., Fong, R., 1986, in Chiosi, C., Renzini, A., eds, Spectral Evolution of Galaxies. Reidel, Dordrecht, p. 439CrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1996

Authors and Affiliations

  • N. Metcalfe
    • 1
  • T. Shanks
    • 1
  • R. Fong
    • 1
  • J. Gardner
    • 1
  • N. Roche
    • 2
  1. 1.Physics DeptDurham UniversityDurhamUK
  2. 2.Johns Hopkins UniversityBaltimoreUSA

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