A spatially resolved study of ionized regions in galaxies at different ...

2.4. Discussion 29
19
20
NGC 5471 (m - M = 29.3)
4 Myr
16 Myr
25 Myr
50 Myr
70 Myr
−11
−10
−9
21
−8
m 547M
22
23
−7
−6
M547M
24
−5
25
−4
26
−3
−0.5 0.0 0.5 1.0 1.5
m 547M−m 675W′
Figure 2.8: Final CMD corrected for field star contamination, together with five isochrones from 4
to 70 Myr. The line across the bottom shows the completeness limit at the 50% level as derived from
false star tests. The right-hand side scale gives the absolute magnitudes corresponding to a distance
of 7.2 Mpc.
values not covered by the atmosphere grid, the boundary values have been used with a caution
flag. In terms of the present work, these stars do not modify the results obtained.
In Figure 2.8 we show the final CMD (corrected for field star contamination). The 50%
completeness limit is also plotted, and five isochones from 4 to 70 Myr are shown in colour.
The right hand side scale gives the absolute magnitude corresponding to a distance of 7.2
Mpc.
2.4 Discussion
In this section we discuss the results of the photometry in terms of the integrated properties,
both of the individual clusters defined in section 2.3.1 and of the whole star forming
complex, and in terms of the resolved stellar photometry in the CMD. We attempt to bring
all the results into a coherent picture of the past and present star formation processes in
NGC 5471.