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Faint Galaxy Number-Counts

Published online by Cambridge University Press:  25 May 2016

N. Metcalfe ,
T. Shanks ,
R. Fong ,
J. Gardner  and
N. Roche
N. Metcalfe
Affiliation:
Physics Dept, Durham University, South Parks Road, Durham DE1 3LE, UK
T. Shanks
Affiliation:
Physics Dept, Durham University, South Parks Road, Durham DE1 3LE, UK
R. Fong
Affiliation:
Physics Dept, Durham University, South Parks Road, Durham DE1 3LE, UK
J. Gardner
Affiliation:
Physics Dept, Durham University, South Parks Road, Durham DE1 3LE, UK
N. Roche
Affiliation:
Johns Hopkins University, Baltimore, USA

Extract

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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.

Here we report on the latest Durham count and clustering work.

Type
High Redshift Galaxies
Information
Symposium - International Astronomical Union , Volume 171: New Light on Galaxy Evolution , 1996 , pp. 225 - 228
Copyright
Copyright © Kluwer 1996 

References

Jones, L.R., Fong, R., Shanks, T., Ellis, R.S., Peterson, B.A., 1991, MNRAS, 249, 481 Google Scholar
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Roche, N., Shanks, T., Metcalfe, N., Fong, R., 1994 in MacGillivray, et al., eds, IAU Symp. 161, Astronomy from Wide-Field Imaging. Kluwer, Dordrecht, p. 635 Google Scholar
Stevenson, P.R.F., Shanks, T., Fong, R., 1986, in Chiosi, C., Renzini, A., eds, Spectral Evolution of Galaxies. Reidel, Dordrecht, p. 439 Google Scholar