38
between azimuthally averaged star formation levels and galaxy center. The radii
are normalized using the D
25
radius given in the RC3 de Vaucouleurs
et
al.
1991.
As seen in the gure, each shows healthy activity far from the galaxy center. Star
formation is not organized around a centralized location or a central peak value.
Surface brightness maps indicate that the locations of peak surface brightness lie
in the bright FUV complexes at various distances from the galaxy center. Ta-
ble 4.1 summarizes the location of peak values for each galaxy in relation to the
galaxy center. Peak values in Sextans A and IC2574 are found in locations that
are 75 and 91 of the total D
25
radius, illustrating that the brightest peak
cannot automatically be interpreted as the galaxy center.
Galaxy
D
25
D
25
Peak
FUV
Location
Location
0
kpc mag arcsec
,2
kpc Normalized
HoII
7
:
0
94 7.04
18.9
0.8
0.23
IC2574
13
:
0
18 11.7
17.5
5.3
0.91
Sextans A 5
:
0
88 2.40
18.9
0.9
0.75
Table 4.1. Peak FUV Surface Brightness in Relation to Galaxy Center
It is interesting to note that IC2574 and HoII, which lie at the same distance,
have identical peak surface brightness levels. The di erence between peak and
central surface brightness value for each is also similar,
2.6 magnitudes. Sextans
A does not show a similar relationship between its peak and central value. Due
to the small sample, the implications of this nding are unknown and may be
entirely coincidental.
Since the FUV surface brightness pro les presented here are the rst published
for this type of galaxy in this bandpass, a comparison of the pro les to galaxies
of similar type type is not possible. This sample shows several di erent charac-
teristics and it is probable that other FUV light pro les of late-type, low surface
brightness galaxies would be just as heterogeneous. At this point, the results
