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J. Brinkmann (NMSU/APO), J.A. Smith (UMich), D.L. Tucker (FNAL), J. Annis (FNAL), J.W. Briggs (UChicago/Yerkes), M. Doi (U. Tokyo), M. Fukugita (U. Tokyo/IAS), J. E. Gunn (Princeton), M. Hamabe (U. Tokyo), S. Ichikawa (NAOJ), T. Ichikawa (Tohoku U.), T.A. McKay (UMich), R. McMillan (NMSU/APO), G. Richards, C.M. Rockosi (UChicago/FNAL), M. Watanabe (NAOJ), SDSS Collaboration
The Sloan Digital Sky Survey (SDSS) has achieved first light. Though still in the engineering shakedown year, the image quality of some of these early runs is useable for science results.
Although similar to the Thuan-Gunn ugriz system, the SDSS u'g'r'i'z' system has wider effective bandwidths and covers almost the entire spectrum from the 3000~Å\/ to 11\,000~Å. This is a new photometric system; therefore, calibration of a network of primary standard stars is needed before the survey science results can be interpreted properly.
Starting in March 1998, we have been using the USNO 40-inch telescope to obtain the primary standard star data used to define the SDSS system. The detector is a UV-coated 1024x1024 SITe CCD with spectra response similar to those used in the SDSS 2.5 m imaging camera telescope recently installed at Apache Point Observatory in New Mexico. The detector on the 20-in telescope is a UV-coated 2048x2048 SITe CCD which was made out of the same batch of silicon as the USNO40's detector.
In this paper, we describe the hardware used to obtain the standard star data. In companion posters, we describe both the software used to obtain and reduce the data (D.L. Tucker et al.) and the data themselves (J.A. Smith).
If you would like more information about this abstract, please follow the link to http://www.sdss.org/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.
The author(s) of this abstract have provided an email address for comments about the abstract: brinkmann@nmsu.edu