in 



observations with the above 40, p= 0",9 or the doubfopa- 

 rallax from 166 observations = r',8. 



The above 40 observations give' the mean ''' 



N. P.D.Jan. 1, 1813, 51'2rj'0",94 



13 observations in August and September, 



*S14 - - 51 23 0,51 



The former determination - 51 23 84 



If we reckon the observations near six o'clock in the even- 

 ing, we may consider the determination of the parallax of 

 a Ljr® as resting on 205 observations of that star. 



a Aquilas. 



I was able to obtain only 10 observations of this star in 

 1814, near the time when the zenith distance from parallax 

 appears least, I have therefore joined with these 11 observa- 

 tions when the zenith distance is near its mean quantity. In 

 this way the errors of observation have a greater influence 

 on account of the smallness of the co-efficient of p. The 

 result * gives a parallax greater thaia before, but being com- 

 bined with the former one, the conclusion is not materially ' 

 different. It sufficiently establishes the great parallax ot 

 a Aquilae. 



* If tl»e 10 observations only had been used, the result would hare agreed very nearly 

 mlk the fonner result. 



