The galaxy two-point correlation function down to V - 26 magnitudes on 0.5-deg scales

Details The galaxy two-point correlation function down to V - 26 magnitudes on 0.5-deg scales The galaxy two-point correlation function down to V - 26 magnitudes on 0.5-deg scales

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...382...32n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 382, Nov. 20, 1991, p. 32-43.

Astronomy and Astrophysics

Astrophysics

53

Data Correlation, Galactic Clusters, Galactic Evolution, Astrometry, Astronomical Catalogs, Brightness Distribution, Charge Coupled Devices, Red Shift

Scientific paper

The measurement of the galaxy angular two-point correlation function w(theta) down to about 26 mag on scales less than 0.45 deg is extended by using the Palomar 200-inch Four-Shooter CCD-array to image to deep radio-optical survey regions with contiguous mosaics in Gunn gri, yielding a total of about 60,000 faint galaxies down to about 26 mag. The first results for one mosaic in Gunn g is presented. For the range 20-24.5 mag, the amplitude of w(theta) - A(omega) - continues to decrease toward fainter magnitudes. Beyond 25 mag, the present catalogs become graduallly incomplete, and A(omega) starts to rise again while maintaining roughly the same slope. The following possible explanations for this effect are given: (1) differential incompleteness between chips; (2) the systematic selection at the faintest magnitudes of the highest surface brightness galaxies, which are known locally to cluster more strongly than low surface brightness galaxies; and (3) the fact that an increasing fraction of faint objects could be distant subgalactic clumps that still have to merge into single L* galaxies.

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