and [omega]^{2} Scorpionis; about as far to the right of Antares is the
star [sigma] Scorpionis, and immediately above this is the
fifth-magnitude star 19.) The nebula we seek lies between 19 and
[omega], nearer to 19 (about two-fifths of the way towards [omega]).
This nebula is described by Sir W. Herschel as "the richest and most
condensed mass of stars which the firmament offers to the contemplation
of astronomers."

There are two other objects conveniently situated for observation, which
the observer may now turn to. The first is the great cluster in the
sword-hand of Perseus (see Plate 4), now lying about 28° above the
horizon between N.E. and N.N.E. The stars [gamma] and [delta] Cassiopeiæ
(see Map 3 of Frontispiece) point towards this cluster, which is rather
farther from [delta] than [delta] from [gamma], and a little south of
the produced line from these stars. The cluster is well seen with the
naked eye, even in nearly full moonlight. In a telescope of moderate
power this cluster is a magnificent object, and no telescope has yet
revealed its full glory. The view in Plate 5 gives but the faintest
conception of the glories of [chi] Persei. Sir W. Herschel tried in
vain to gauge the depths of this cluster with his most powerful
telescope. He spoke of the most distant parts as sending light to us
which must have started 4000 or 5000 years ago. But it appears
improbable that the cluster has in reality so enormous a longitudinal
extension compared with its transverse section as this view would imply.
On the contrary, I think we may gather from the appearance of this
cluster, that stars are far less uniform in size than has been commonly
supposed, and that the mere irresolvability of a cluster is no proof of
excessive distance. It is unlikely that the faintest component of the
cluster is farther off than the brightest (a seventh-magnitude star) in
the proportion of more than about 20 to 19, while the ordinary estimate