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(Abridge) Bars are very common in the centre of the disc galaxies, and theydrive the evolution of their structure. A volume-limited sample of 2106 discgalaxies extracted from the Sloan Digital Sky Survey Data Release 5 was studiedto derive the bar fraction, length, and strength as a function of themorphology, size, local galaxy density, light concentration, and colour of thehost galaxy. The bars were detected using the ellipse fitting method andFourier analysis method. The ellipse fitting method was found to be moreefficient in detecting bars in spiral galaxies. The fraction of barred galaxiesturned out to be 45%. A bar was found in 29% of the lenticular galaxies, in 55%and 54% of the early- and late-type spirals, respectively. The bar length(normalised by the galaxy size) of late-type spirals is shorter than inearly-type or lenticular ones. A correlation between the bar length and galaxysize was found with longer bars hosted by larger galaxies. The bars of thelenticular galaxies are weaker than those in spirals. Moreover, the unimodaldistribution of the bar strength found for all the galaxy types argues againsta quick transition between the barred and unbarred statues. There is nodifference between the local galaxy density of barred and unbarred galaxies.Besides, neither the length nor strength of the bars are correlated with thelocal density of the galaxy neighbourhoods. In contrast, a statisticalsignificant difference between the central light concentration and colour ofbarred and unbarred galaxies was found. Bars are mostly located in lessconcentrated and bluer galaxies. These results indicate that the properties ofbars are strongly related to those of their host galaxies, but do not depend onthe local environment.

The population of barred galaxies in the local universe I. Detection and characterisation of bars