Table 3
Slope of best least-square fit to the cumulative distribution of the clusters of inner and outer region of M 33 galaxy.
| Sample | Region | 1st fit | 2nd fit | |
| slope ± σ | slope ± σ | |||
|
|
||||
| (a) | inner | −0.44 ± 0.02 | −1.12 ± 0.06 | |
| ,, | outer | −0.84 ± 0.03 | − | |
| (b) | inner | −0.42 ± 0.02 | −1.38 ± 0.11 | |
| ,, | outer | −0.88 ± 0.03 | − | |
| (c) | inner | −0.32 ± 0.02 | −1.40 ± 0.07 | |
| ,, | outer | −0.68 ± 0.04 | − | |
| (d) | inner | −0.38 ± 0.02 | −1.12 ± 0.06 | |
| ,, | outer | −0.78 ± 0.02 | − | |
Notes. The sample “a” (24 μm sources (915)) and “d” (selected YSCs (648)) represents the cumulative distribution of the clusters as a function of 24 μm flux whereas the sample “b” (8 μm sources (833)) and “c” (selected YSCs (648)) represents the cumulative distribution of the clusters as a function of LTIR and Lbol respectively. The 1st and 2nd fit represents the fitting in the lower and higher flux (or luminosity) ranges.
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