81 
measured radiances about the sun. If the angular asymmetry exceeds 10%, those pairs are removed from the 
inversion process. If the integrated asymmetry exceeds 10% or there are not a sufficient number of data 
points, the data are not inverted. The inversion routine used is that of Nakajima, (1983) and has a number 
of options that will be implemented over time. 
The principle plane data are processed using the same inversion however only data on the zenith 
side from the solar disc are used in the inversion due to asymmetry induced by the ground reflectance. The 
principle plane window has identical capabilities as the almucantar window. The test for the quality of the 
data is simply the smoothness of the curve. 
wave < m) t(<sun>> 
Almucantar 
II 1619 
X 
n 070 
X 670 
■ “ i 
A 440 
device 
3 
wave<u> t(<sun>) t(sun> t<sky> 
err 
1019 0 
3185 0 
.3195 0.2594 
0.0087 
070 0 
4242 0 
.4238 0.3530 
0.0080 
870 0 
6913 0 
.7064 0.6015 
0.0494 
440 1 
4473 1 
.4913 1.3666 
0.1100 
waves 
wexp<sun> 
wexp<sky> 
440/070 
1.8001 
1.9856 
440/670 
1.7572 
1.9516 
670/070 
1.8692 
2.0403 
440/1019 
1.8025 
1.9787 
870/1019 
1.8128 
1.9489 
Figure 3, A successful inversion of almucantar radiances during clear (3a) and hazy 
(3b) conditions is possible when the data are symmetric about the sun (upper 
left plot within window). Inversions produce a volume size distribution with 
good accuracy from 0.1 pm to about 3 pm aerosol radii. The aerosol optical 
thickness and phase function (right side of window) from the aureole inversion 
are also computed using Nakajima's (1983) code.