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Mapping the Jagiellonian Field of Galaxies

The analysis of two-dimensional galaxy distribution in the Jagiellonian Field (JF) was carried out by the wavelet technique. The positions of galaxies were taken from the Revised Jagiellonian Field Catalogue (RJFC) based on digitized scans of the JF original photographic plates. We discuss briefly the procedure of star/galaxy separation applied by us to the RJFC, the algorithm and the first results of mapping of the selected parts of the RJFC. 1. What is the Revised Jagiellonian Field Catalogue of Galaxies? The region of the original Jagiellonian Field (JF) sky survey (Rudnicki, Dworak, & Flin 1973) was selected by Zwicky (Zwicky 1962) as a region which is enriched by clusters of galaxies and contains a small number of the brighter galaxies. The JF sky survey (photographic plates in three colors with coordinates of center α = 1120, δ = +35◦26′ (2000.0) taken with the 1.25 m Palomar Schmidt telescope) coincides with the CGCG field No. 185. The central part of the JF (4◦ × 4◦) was scanned and automatically processed by the COSMOS machine. This procedure allows one to digitize the images on the plate and to receive a set of parameters fitting the inertia ellipse to each image (e.g., Stobie 1980; MacGillivray & Stobie 1984). Constructing a modern complete galaxy catalogue in the JF region, we decided to carry out an automated procedure of star/galaxy separation on the digitized images. We experimented with the possible combinations of parameters usually applied for such purposes on similar photographic data (e.g., Hewett 1981; Heydon-Dumbleton, Collins, & MacGillivray 1989; Odewahn et al. 1992; Weir, Fayyad, & Djorgovski 1995 with a brief review of discrimination philosophy). Before applying the procedure, all small objects with the COSMOS area parameter smaller than 60 (in increments) were removed from our sample and about 35,000 objects remained to be analyzed. Among the possible discriminators only three gave a clear separation of the loci of stars and galaxies. There were plots presenting the dependence on the logarithm of image area denoted as log(area), the width of Gaussian fit (S) and the intensity weighted second moment (Kw) versus COSMOS image magnitude