Onderstaande tekst is niet 100% betrouwbaar

Table io.

Gal. lat. § t) £

— 90°to-4oc — 2.4 —238 +148

— 40° to — 200 — 1.8 - 27.3 + 18.3

— 20° to + 200 — 0.4 — 28.6 + 15 6 + 20° to + 40° _ 1.5 _ 26.2 + ,7.4 + 40° to + 90° — 1.0 — 27 9 4- 16.6

All stars together — m —26.8 -f- 16.2

From these we derive the coordinates of the apexgiven in the following table.

Table ii.

Gal" lat" A D RA RD pk

— 90° to - 40° 264°.3 + 3<°-7 —3° 3 +o°.s 1.9 4.4

— 40° to — jo° 266°.2 + 33°.8 — ,».4 + 2».6 ,.9 3.3

— 20° tO + 20° 2Ó9°.2 +28°.6 -f i°.6 — 2°.6 98 7.5 + 20°t0+40° 266°.7 +33°.5 — o°.9 + 2*3 3.3 3.2 + 4Q°to +90° 2ó7°.9 +3°°.7 -f 0°.3 — o°.5 2.1 4.2

All stars together 2670.7 +3i°.2 2oo 22.6

The values of A and D from all stars together have been obtained by adding the equations for the individual groups and by solving the resulting system of equations

By subtracting the values of A and D obtained from all stars together from those given by the individual groups the residuals denoted respectively by Ra and Rd have been found. A decided trend cannot well be recognised in them. Supposing the difïferences to be purely accidental we may derive the rnean errors from the residuals. For that purpose weights have been given to the individual values of A and D, which are respectively equal to a hundredth part of the coefficients A and C (defined on page 27) in the equations of Bravais. Denoting the mean errors of the values of A and D from all stars together by fA and fD, we get:

(55) eA= — o° 8 fD= — i° 0.

These values are in accordance with those of the means errors derived in Chapter III by means of a comparison of the values of A and D obtained from the zones of different declination; those of D after the reduction of the values of taS to the system of Auwers (see (20) on page 32 and (50) on page 46). There thus seems to be no reason to ascribe any reality to the differences found between the results from zones of different galactic latitude.

Results from groups of different type of spectrum.

In order to see whether a difference between the coordinates of the apex from stars of different type of spectrum can be ascertained, the stars ofBRADLEY of Type I and Type II have been treated separately. The data for the formation

Sluiten