Faint Galaxy Counts and the Angular Correlation Function

Details Faint Galaxy Counts and the Angular Correlation Function Faint Galaxy Counts and the Angular Correlation Function

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.5602c&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #56.02; Bulletin of the American Astronomical Society, Vol. 26, p.1407

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Density fluctuations in the Universe on 10 to 50 Mpc scales provide important constraints on cosmological models. These fluctuations can be probed by measuring the angular correlation function for galaxies on 1 to 5 degree scales. To determine this function, we have taken a grid of CCD images of fields with a separation of 0.8 degrees, allowing us to probe these large angular scales with a 10' x 10' CCD. The images were taken by our collaborators at La Palma using the 2.5 meter Isaac Newton Telescope. We estimate that our images should go a factor of three deeper than the APM survey. These fields were selected to be well above the galactic disk and in a region of low far-infrared emission on the IRAS survey to avoid interstellar extinction as much as possible. The observations were made near the zenith to reduce atmospheric extinction. Effects of extinction were further reduced by taking R band images. Photometry and classification have been done using the FOCAS package in IRAF. In addition to the angular correlation function, the data provides us with galaxy counts, which give somewhat weaker constraints on possible cosmological scenarios. Our galaxy counts compare well to the literature (Metcalfe, et al. 1991). Preliminary results will be presented.

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