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Bar fractions depend on the properties of the host galaxies, which areclosely related to the formation and evolution of bars. However, observationalstudies do not provide consistent results. We investigate the bar fraction andits dependence on the properties of the host galaxies by using three barclassification methods: visual inspection, ellipse fitting method, and Fourieranalysis. Our volume-limited sample consists of 1,698 spiral galaxies brighterthan $M_{\rm r}=-15.2$ with $z < 0.01$ from SDSS/DR7 visually classified by Annet al. (2015). We first compare the consistency of classification among thethree methods. Automatic classifications detect visually determined stronglybarred galaxies with the concordance of $74\% \sim 85\%$. However, they havesome difficulty in identifying bars, in particular, in bulge-dominatedgalaxies, which affects the distribution of bar fraction as a function of theHubble type. We obtain, for the same sample, different bar fractions of 63%,48%, and 36% by visual inspection, ellipse fitting, and Fourier analysis,respectively. The difference is mainly due to how many weak bars are included.Moreover, we find the different dependence of bar fraction on the Hubble typefor strong versus weak bars: SBs are preponderant in early-type spirals whereasSABs in late-type spirals. This causes a contradictory dependence on hostgalaxy properties when different classification methods are used. We proposethat strong bars and weak bars experience different processes for theirformation, growth, and dissipation by interacting with different inner galacticstructures of early-type and late-type spirals.

Bar Fraction in Early- and Late-type Spirals