Context : Breaks in the surface brightness profiles in the outer regions of galactic discs are thought to have formed by various internal ( e.g .
bar resonances ) and external ( e.g .
galaxy merging ) processes .
By studying the disc breaks we aim to better understand what processes are responsible for the evolution of the outer discs of galaxies , and galaxies in general .

Aims : We use a large well-defined sample to study how common the disc breaks are , and whether their properties depend on galaxy mass .
By using both optical and infrared data we study whether the observed wavelength affects the break features as a function of galaxy mass and Hubble type .

Methods : We studied the properties of galaxy discs using radial surface brightness profiles of 753 galaxies , obtained from the 3.6 \mu m images of the Spitzer Survey of Stellar Structure in Galaxies ( S ^ { 4 } G ) , and the K _ { s } -band data from the Near InfraRed S0-Sa galaxy Survey ( NIRS0S ) , covering a wide range of galaxy morphologies ( -2 \leq T \leq 9 ) and stellar masses ( 8.5 \lesssim \log _ { 10 } ( M _ { * } / M _ { \sun } ) \lesssim 11 ) .
In addition , optical Sloan Digital Sky Survey ( SDSS ) or Liverpool telescope data was used for 480 of these galaxies .

Results : We find that in low-mass galaxies the single exponential profiles ( Type I ) are most common , and that their fraction decreases with increasing galaxy stellar mass .
The fraction of down-bending ( Type II ) profiles increases with stellar mass , possibly due to more common occurrence of bar resonance structures .
The up-bending ( Type III ) profiles are also more common in massive galaxies .
The observed wavelength affects the scalelength of the disc of every profile type .
Especially the scalelength of the inner disc ( h _ { i } ) of Type II profiles increases from infrared to u -band on average by a factor of \sim 2.2 .
Consistent with the previous studies , but with a higher statistical significance , we find that Type II outer disc scalelengths ( h _ { o } ) in late-type and low mass galaxies ( T > 4 , \log _ { 10 } ( M _ { * } / M _ { \sun } ) \lesssim 10.5 ) are shorter in bluer wavelengths , possibly due to stellar radial migration populating the outer discs with older stars .
In Type III profiles h _ { o } are larger in the u band , hinting to the presence of young stellar population in the outer disc .
While the observed wavelength affects the disc parameters , it does not significantly affect the profile type classification in our sample .
Our results indicate that the observed wavelength is a significant factor when determining the profile types in very low mass dwarf galaxies , for which more Type II profiles have been previously found using optical data .

Conclusions :