A PLEA FOR THE STARS. 67 
To this list I might add such objects as the closely-aggre- 
gated globular cluster known as 47 7oncarz, and the similar, but 
less dense, cluster, Omega Centauri—stupendous objects, with 
adequate optical power, and even faintly resolvable with tele- 
scopes of moderate aperture. 
Several objects of great beauty, just within the range of 
common telescopes, appear to be entirely neglected. Our 6-inch 
and 10-inch telescopes disdain to look at them; and humbler 
observers seem to have quite lost sight of them. Take, e2.¢., 
4949 Are, a lovely double, each about 6 mag., and distant about 
2”. Or take H5246 Judi, each 8 mag., distant about 2”. Or 
take H5319 Gruzs—a very delicate test for a 3%4-inch,—each 8 
mag., and less than 2” apart. What scientific journal ever 
notices them? Crossley is ignorant of them, and Proctor 
acknowledges them not. Even Webb only notices one of the 
three. Their names lie buried in Sir John’s Cape catalogue. 
Their loveliness smiles upon us from the distant heavens in vain. 
A noble field of investigation lies open in those coarser star- 
clusters wherein our southern heavens are so rich, such as H3179 
and H3111 in Avgo, H3660 Ava, and the cluster around Kappa 
Crucis. If the exact places of the larger stars which compose 
these groups could be plotted, and an accurate chart of their 
positions at a given epoch made, it would be very interesting 
hereafter to note any indications of drift, or of such changes as 
the manifest physical connection of the associated stars suggests. 
Mr. Russell, of Sydney, has attempted something of the kind 
with the Kappa Crucis cluster, and his chart is one of the most 
interesting products of that observer’s industry. 
It is true that the difficult work, and most of what may be 
called the strictly original work, of observation lies outside the 
reach of all but large and costly instruments. But how 
ingenious, serviceable, and really original a use may be made of 
instruments of moderate aperture, Mr. J. H. Pope has well 
shown in his paper on Double Star Measurements (Transactions 
of N.Z. Institute for 1878, pp. 141-144). 
And even when the instrument is not of such a character as 
will enable the observer to add anything to the accumulating 
data of astronomical investigation, it will at least enable him to 
understand, appreciate, and form an intelligent opinion upon 
the many interesting questions which Astronomy opens for 
discussion. 
The details of the nebular theory, in its application to such 
planets as Jupiter and Saturn, are not only recognised, but in a 
manner realised, when even a common telescope reveals in the 
one that series of belts whose form, number, tint, and shading 
are so constantly varying that a view of the planet after the 
lapse of a few months is almost startling for its novelty ; and in 
the other, that superb system wherein we discern the evolutionary 
process 77 flagrante, and see in those flights of satellites vestiges 
of the origin of our solar system. 
We talk of the dead moon, and of sun-spots, but to realise 
