A Nearly-Constant Clustering Amplitude for Faint Galaxies

Details A Nearly-Constant Clustering Amplitude for Faint Galaxies A Nearly-Constant Clustering Amplitude for Faint Galaxies

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...191.8712b&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #87.12; Bulletin of the American Astronomical Society, Vol. 29, p.1355

Astronomy and Astrophysics

Astronomy

Scientific paper

The angular clustering of faint field galaxies is investigated using deep imaging (I ~ 25) obtained with the 10-m Keck--I telescope. The autocorrelation function is consistent with omega (theta ) ~ theta (-0.8) , and we find no compelling evidence for a flattening of the power law index at the faintest magnitude limits. Results from a number of independent observational studies are combined in order to investigate the variation of the correlation amplitude with median I-magnitude. At I_med 23 the results obtained by different studies are all in rough agreement and indicate that for I_med > 22 the correlation amplitude declines far less steeply than would be expected from an extrapolation of the trend in the brighter samples. In particular, at I_med ~ 24 our data indicate omega (theta ) to be a factor ~ 7 higher than the extrapolation. A flattening of the correlation amplitude at faint magnitude limits is a general feature of models in which the redshift distribution of the faint field population contains a substantial fraction of objects at z > 1 and in order to reproduce the apparent abrupt flattening of the amplitude of omega (theta ) observed at the faintest limits, of order 50% of the galaxies in a sample with I_med ~ 24 must be at z > 1.

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