INTRODUCTION 
III 
SCOPE OF THE CATALOGUE. 
This Preliminary General Catalogue contains the computed positions and the 
motions, for the epoch 1900, of 6188 stars that are regarded as specially important. 
That the stars ordinarily visible to the naked eye are of special interest would 
probably be generally admitted without serious protest, not only because that is 
the class of stars which most attracts attention and with which we are best ac¬ 
quainted, but also because it is extremely probable that these stars are in general 
among our nearer neighbors. On the whole they have been more frequently and 
accurately observed in the past than any of the fainter classes of stars. The present 
Catalogue contains about 4030 stars rated upon the natural, or historic, scale herein 
adopted as of the sixth magnitude, or brighter. Of these the count shows 1919 
in the Northern and 2111 in the Southern hemisphere. These numbers are 
approximate only, since they are somewhat dependent upon the treatment of double 
stars; and because they are still more dependent on the uncertainties in determining 
the brightness of the stars. 
Of the remaining 2158 stars — all fainter than sixth magnitude — a few are 
included because of their proximity to brighter stars; others because they were 
observed by Bradley (though a very few Bradley-stars have been omitted); and 
still others because they are among the stars whose positions, though not observed 
by Bradley, were determined with a considerable degree of accuracy previous to 
1850. For all these stars it was possible to determine their motions with greater 
accuracy than that which attaches to the generality of faint stars not included in 
this Catalogue. Therefore, these stars are especially interesting for two reasons 
among others: First, on account of the relative accuracy of their computed 
motion, present and prospective, they afford suitable material from which to secure 
enlargement of the existing lists of standard stars; secondly, these, together with 
the great majority of the stars visible to the naked eye, furnish the best available 
means for critical tests upon certain points that may come into consideration 
relative to systematic motions of the stars. 
HISTORY AND DESIGN OF THIS WORK. 
Perhaps the easiest way to describe the place in the line of sidereal research 
which this work is designed to fill, as well as to indicate the ideas and purposes upon 
which it is founded, is to note in a cursory way successive steps in its evolution. 
Many years ago a plan was formed at the Dudley Observatory for a critical 
discussion of the motions of all stars to which have been attributed, with reasonable 
probability, motions as great as 10" per century. The work progressed very slowly 
at first, in the intervals of other employments; but as it proceeded the conviction 
grew that the problems for which we need a knowledge of stellar motions require 
comprehensive (not fragmentary) treatment, if a given, large amount of labor is 
to be expended to the best advantage. Thus, it is even more important that stellar 
motions shall be free from systematic errors than that they shall be merely precise 
in the differential sense. But if that be so, the most responsible part of a work 
