xpected complete
equipment, Planets (totally neglected at Greenwich) were to be
observed. Observations were to be reduced completely, and the
reductions were to be exhibited in an orderly way: this was a novelty
in Astronomy. I considered it so important that I actually proposed
to omit in my publication the original observations, but was dissuaded
by Herschel and others. I sometimes suspended, observations for a
short time, in order to obtain leisure for; the reductions. I had at
first no intention of correcting the places of the fundamental stars
as settled at Greenwich. But I found myself compelled to do so,
because they were not sufficiently accurate; and then I took the
course of observing and reducing as an independent observer, without
reference to any other observatory. I introduced the principle of not
correcting instrumental errors, but measuring them and applying
numerical corrections. I determined my longitude by chronometers, and
my latitude by a repeating circle borrowed from Mr Sheepshanks, which
I used so well that the result; was only half a second in error. The
form of my reductions in the published volume for 1828 is rather
irregular, but the matter is good: it soon attracted attention. In
1829 the process was much the same: I had an assistant, Mr Baldrey.
In 1830 still the same, with the additions:--that I formally gave the
corrections of relative right-ascension of fundamental stars (without
alteration of equinox, which I had not the means of obtaining) to be
used in the year 1831; and that I reduced completely the observed
occultations (with a small error, subsequently corrected). In 1831 the
system of correction of broken transits was improved: the errors of
assumed R.A. of Fundamental Stars were exhibited: Mean Solar Time was
obtained from Sidereal Time by time of Transit of [Symbol: Aries]
(computed by myself): the method of computing occultations was
improved. In 1832 the small Equatoreal was erected, and was soon
employed in observations of the elongation of the 4th Satellite of
Jupiter for determining the mass of Jupiter. The Mural Circle was
erected at the end of the year, but not used. The calculation of
R.A. of Fundamental Stars was made homogeneously with the others:
separate results of all were included in ledgers: a star-catalogue was
formed: all as to the present time (1871). With the Equatoreal the
difference of N.P.D. of Mars and stars was observed.

"With the beginning of 1833 the