( if) 
For the last position the measurement of Hussey in April 1899 
could not be taken into account. Of all the measurements after 
1888.0 the means are taken without regard to personal correction, 
this not being independently deducible and the use of the value 
deduced above for BurRNHAM being prohibited on account of the 
entirely different appearance of the system. 
That the number of the normal positions might not be unneces- 
sarily great I formed normal places by uniting the yearly means 
two by two according to their weights for the whole of the period 
18621880 when the changes in distance were still very slight 
and the motion of the angle therefore pretty regular and moreover 
very small. An exception was only made for the first three, of which 
only one position was formed. In order to simplify still further the 
following computations, the value of log fp was rounded off to 
tenths; these modified values are indicated by log y/p’ to distinguish 
them from the preceding. In this manner the following 21 normal 
deviations were obtained : 
NO. | Date Ag wy N°.| Date A6 |2Yp'| N°] Date Ab |2Yp! 
1 /1863.31 ;—0°154) 0.4 | 8 |1877.75 ,—0°014) 0.5 | 15 |1886.14 |—0°23) 0.3 
2 /1865.71 |—0.020| 0.3 9 |1879.84 |+0.217) 0.6 | 16 [1887.19 |—1.07/ 0.2 
3 1867.76 |—0.212) 0.4 | 10 (1881.17 |4+0.04 0.5 | 17 |1888.970/—0.16) 9.9 
4 |1869.80 |—0.555| 0.4 f 11 (1882.11 |—G.07 0.5 | 18 |1890.275|—1.44| 9.7 
5 |1871.89 |—0.722| 0.3 | 12 |1883.15 |—0.32 0.4 | 19 |1897.004/+4.38) 0.1 
6 1873.94 |—0.582} 0.4] 13 [1884.18 |—0.43 0.4 | 20 |1897.971/4+2.43) 0.3 
0 0. 
Or 
= 
rn 
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vo 
ns) 
1885.19 —0,15 
7 11875.64 an 1898, 844 RA de 0.0 
As has already been stated the observations after the periastron- 
passage could not be treated in the same way as the previous ones, 
because for that part of the orbit the data are far from sufficient 
for a satisfactory deduction of the personal corrections. This statement 
however does not imply that the corrections found before 1888 are 
not at all subject to doubt. Whoever’s task it was to investigate 
the critical problem of these corrections will immediately admit, 
that in a part of the orbit where e.g. two of the observers have a 
predominating influence, there can be no question about a complete 
elimination of the personal errors, even apart from the fact that 
the accidental errors are often many times greater than the constant 
ones. Hence the determination of the latter may be very uncertain, 
