417 
First set of examples, which I have taken since. 
The moon and Venus (Mar. 1, p.m.) both to right of meri- 
dian (moon’s H.A. 24 hours, Venus's 43 about) give 
error in are 1’. 40° (abt. 3™. 8° 
Vip ule ee) G oi) . - 
Observed dist. 31°. 39. 35"). time); too small, as in the case 
Computed dist. 31°. 41°. 15° cfu Gan ane once 
Also the sun, in the previous example; the planet in this, 
are to the right of the moon: but the moon, in this case, is 
at a much greater altitude. 
But for three cases of Pollux and the moon, the moon in 
this case being to the right of the star, not to the left, as before, 
I obtained 
ils 2. 3. 
Obs. dist. 322.38 alow 30°. 39°. 4° 30°. 33°. 46" 
Comp. dist.| 32°. 37°. 31$" | 30°. 3, S00, Be, BD 
434° 22) AT 
(abt. 1m, 205 time.) | (abt. 2™, 20s time.) | (abt. 1m, 205 time.) 
Tn all these cases the observed distance is too great; but the 
moon and star in the Ist .case were on opposite sides of the 
meridian; in the latter two cases only, the H.A. of the moon 
was considerable. With these I couple a case of Mars and 
the moon (H.A. of Mars 1". 50”, of moon 3". 15™), both to right 
of meridian; because the error agrees with that in the case of 
Pollux in a similar position; the computed distance (but not 
given in the N. A.) at a certain time (Jan. 29, 1876) being 
93°. 29°. 13", and the reduced measured distance 23°. 30°. 6", or 
nearly 1‘ too great. 
In another example (Sept. 7, 1875, p.m.), with the moon and 
sun very low (less than 10°), and the former almost on the 
meridian, I had an error of 1’. 44" are, or 38". 41° time. In this 
case again the observed distance was too small, and the sun, of 
course, to the right of the moon. 
