Observation and reduction methods of deep Palomar 200 inch 4-Shooter mosaics

Details Observation and reduction methods of deep Palomar 200 inch 4-Shooter mosaics Observation and reduction methods of deep Palomar 200 inch 4-Shooter mosaics

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apjs...96..371n&link_type=abstract

The Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 96, no. 2, p. 371-399

Astronomy and Astrophysics

Astronomy

18

Charge Coupled Devices, Galactic Evolution, Mosaics, Refracting Telescopes, Sky Surveys (Astronomy), Astrometry, Astronomical Photometry, Error Analysis, Point Spread Functions

Scientific paper

We present deep contiguous CCD-mosaics in Gunn gri filters with the Palomar 200 inch 4-Shooter CCD array for two widely separated survey fields, each is approximately 0.45 deg x 0.45 deg in size. We used the FOCAS package to compile multicolor catalogs in each survey field that contain approximately 23,000 galaxies and have 90% completeness limits of gri less than or approximately equal to 24.5 mag (B(sug J) is less than or approximately equal to 25.2 mag). The purpose is to constrain the evolution of galaxy clustering by tracing w(theta) down to BJ is approximately 25 mag. This paper describes the photometric and astrometric reduction methods of our 4-Shooter mosaics and the resulting faint galaxy catalogs. The accuracy of the global photometric zero points is determined from overlapping 4-Shooter frames and the known colors of field main-sequence stars, and amounts to approximately 0.08 mag rms. Astrometric solutions are determined from 10-15 secondary standard stars for each CCD with accurately measured coordinates from recent-epoch Palomar 48 inch Schmidt plates. The CCD frame-to-frame overlap shows that the rms accuracy of each CCD's astrometry is less than or approximately equal to 0.5 sec. Using less than or approximately equal to 8 Point Spread Function (PSF) stars in each CCD, we can distinguish stars from galaxies using object shape parameters down to gri less than or approximately equal to 23 mag. We present the resulting galaxy counts down to Gunn gri less than or approximately equal to 25 mag. The completeness of our galaxy catalogs is determined by comparing our galaxy counts with those from somewhat deeper surveys that cover much smaller areas. The multicolor two-point angular correlation functions for galaxies in these fields are presented in a companion (main journal) paper.

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