Context : Abridged

Aims : The goal of this paper is to quantify the changes on the SF distribution within the disc galaxies in the last \sim 8 Gyr .
We use as a proxy for the SF radial profile the Near-UV surface brightness distributions , allowing suitably for extinction .

Methods : We compare the effective radii ( R _ { eff } ) and concentration of the flux distribution in the rest-frame Near-UV for a sample of 270 galaxies in the range 0 < z < 1 .
This radial distribution is compared to that measured in the rest-frame B -band , which traces older stellar populations .
The analysis is performed using deep , high resolution , multi-band images from GALEX , SDSS , and HST/ACS - GOODS -South .

Results : The relation R _ { eff } ( NUV ) - M _ { \star } suffers a moderate change between z \sim 1 and z \sim 0 , at a fixed stellar mass of 10 ^ { 10 } M _ { \odot } galaxies increase their effective radii by a factor 1.18 \pm 0.06 .
The ratio R _ { eff } ( NUV ) / R _ { eff } ( B ) has increased by \sim 10 % in the same period .
Median profiles in NUV show signs of truncation at \R \sim R _ { eff } , and median colour profiles ( NUV - B ) show a minimum ( a “ bluest ” point ) also around \R \sim 1-1.5 R _ { eff } .
The surface brightness of the discs ( at R _ { eff } ) has decreased by \sim 80 % in NUV , and by \sim 60 % in B since z \sim 1 .
The distributions of NUV flux are more compact at z \sim 1 than nowadays , in terms of the fraction of flux enclosed in a specific radius ( in kpc ) .
The central brightness in B and NUV has increased with respect to the brightness level of the discs , both in B and NUV , indicating perhaps a continuous accumulation of the bulge structure since z \sim 1 , or that they have been left exposed because of the significant decline in the the star-forming activity in the discs .

Conclusions : Our results indicate that the SF surface density has decreased dramatically in discs since z \sim 1 , and this decline has been more intense in the central parts ( \lesssim R _ { eff } ) of the galaxies .
In addition , our data suggest that the bulges/pseudo-bulges have grown in surface brightness with regard to the discs since z \sim 1 .