468 
Instrument, as in the mean time I had ordered a new and larger 
instrument from the firm of SARTORIUS in Göttingen. At the end of 
1914 I again went to Europe for six months, and on my return in 
the summer of 1915 I was able to take the new instrument with 
me, after it had been subjected to a first examination at the obser- 
vatory in Leiden. 
Although I have since made a considerable number of observations 
with this instrument, it will be better to discuss these in later papers. 
The publication of my occasional observations with the Zurss-telescope, 
in so far as these may prove to be of scientific value, will also be 
better delayed till that of the final discussion of my occultations 
In the following paper I shall therefore confine myself to the deter- 
minations of the coordinates of Matuba and Cabinda. 
2. Determination of the latitude of Matuba. 
In July 1913 [ made a first determination of ‘the latitude of 
Matuba by meridian-zenith-distances, and I afterwards repeated it 
in Febr. and March 1914. A short description of my installation 
there may here be given. 
Matuba is about 400 meters from the coast, and lies more than 
100 meters above sea level. My observatory consists of three apart- 
ments, of which the two outer ones are provided with moveable 
roofs. In these my universal instrument and the equatorial Zurss 
telescope are mounted upon solid piers. Here on the firm 
ground a much greater stability is obtained than at Chiloango. In 
the inner room, which is arranged as a study, stand the chrono- 
meters in a closed cupboard, which is kept dry by calcium chloride. 
The observatory stands free from my house, but is connected with 
it oy a covered passage. 
The first determination of the latitude of my observatory was 
made in 1913 from July 6 to July 22rd, and I proceeded in exactly 
the same way as before in my second determination of the latitude 
of Chiloanga’), i.e. that observations were made exactly in the 
meridian, so that only one pointing could be obtained of each star. 
In order to eliminate as far as possible the systematic division errors 
and the flexure of the telescope, the observations were made in six 
different positions of the vertical circle, namely with the zenith point 
1) Versl. Akad. Amsterdam 17 73—78 ; Proc. 11 (95—101) 1908. 
