The Intercomparison of Star Catalogs. III. Comparing the AGK3, the AGK3U, the ACRS (Part 1), and the PPM to the General Catalog

Details The Intercomparison of Star Catalogs. III. Comparing the AGK3, the AGK3U, the ACRS (Part 1), and the PPM to the General Catalog The Intercomparison of Star Catalogs. III. Comparing the AGK3, the AGK3U, the ACRS (Part 1), and the PPM to the General Catalog

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...451..768d&link_type=abstract

Astrophysical Journal v.451, p.768

Astronomy and Astrophysics

Astronomy

2

Astrometry, Catalogs, Methods: Analytical, Reference Systems

Scientific paper

We have extended our work on the search for rapidly varying systematics in star catalogs to the large-scale catalogs mentioned in the title. Essential to our task is a procedure for minimizing catalog-to-catalog differences and a reference catalog to use as a comparison standard. For the former the method of infinitely overlapping circles continues to be utilized while for the latter we can no longer use the successor to the Fourth Fundamental Catalogue, the Basic FK5. For the Basic FK5, even if supplemented with the FK5 Extension, will have only a small, bright overlap with these much larger, fainter reaching star catalogs. Hence, we have turned to the General Catalogue as a reference. The average intersection set is now ˜20,000 stars. In addition, because heretofore unknown problems of a systematic nature within General Catalogue might lead us to false conclusions, we have also used the AGK3RN as a intermediate test case [the version of the reference catalog (AGK3R) for the AGK3 with proper motions]. Finally, the AGK3U appears best according to our central limit theorem tests. However, because of the relatively few observations per coordinate in these catalogs, as opposed to those in fundamental catalogs, the true statistical meaning of this result is somewhat muddled. The theory developed in Paper I will be extended in the next paper in this series in an effort to partially overcome the problematic issue of the small average number of observations per position.

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