20 
will be required to clear up the difficulties that have occurred 
as to this and other low stars. It is my intention to pursue the 
subject. If an opportunity should be afforded me, by con- 
tinuing the observations, of ultimately succeeding, I hope it will 
be considered that the time consumed has not been mispent. 
As to the parallaxes of stars near the zenith, there cannot I 
think be a doubt, that they have been determined by this enquiry 
to the exactness of a small fraction of a second. 
Table 1. Containing the observations and reductions of « Lyre 
almost explains itself. 
The observations from the commencement to September 20, 1819, 
were all made on the meridian. The mean of the three mi- 
croscopes being taken, and the correction for collimation or index 
error being applied, and also the sum of the equations, the mean 
zenith distance Jan. 1, 1819, is obtained. The refraction is com- 
puted by the internal Thermometer. 
The corrections of the mean of the three microscopes, for 
collimation or index error, were as follows for the single ob- 
servations : 
Face W. 
1818 July 14 Aug. 16 +54,76 
1818 Oct." 16 Nov. 8 +47,81 
1818 Nov. 24 —1819, Feb. 24 +43,67 
1819 July 3 Augt. 27 +46,91 
1819 Aug. 31 Nov. 8 446,35 
