Table 4
Statistics of the break types in the surface brightness profiles of the infrared data.
| All galaxies (N = 753) | Low mass bin (N = 372) | High mass bin (N = 381) | ||||||
| Type | Fraction | Bar fraction | Type | Fraction | Bar fraction | Type | Fraction | Bar fraction |
|
|
||||||||
| I | 30 ± 2% (228) | 73 ± 3 % | I | 35 ± 2% (131) | 73 ± 4 % | I | 25 ± 2% (97) | 72 ± 5 % |
| II.i | 6 ± 1% (43) | 100 ± 0 % | II.i | 6 ± 1% (21) | 100 ± 0 % | II.i | 6 ± 1% (22) | 100 ± 0 % |
| II | 44 ± 2% (335) | 72 ± 2 % | II | 38 ± 3% (143) | 66 ± 4 % | II | 50 ± 3% (192) | 76 ± 3 % |
| III | 25 ± 2% (189) | 51 ± 4 % | III | 26 ± 2% (98) | 50 ± 5 % | III | 24 ± 2% (91) | 53 ± 5 % |
Notes. The profile types are divided to low and high mass bins by the median mass in the Hubble type bins as shown in Fig. 1. We also give the bar fractions for each profile type. The uncertainties are calculated using binomial statistics, and denote the ± 1σ uncertainties. Some galaxies show two breaks in their discs and are counted twice in the statistics, explaining why the overall percentages can be above 100%.
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