摘要
Radial colour gradients within galaxies arise from gradients of stellar age, metallicity, and dust reddening. Large samples of colour gradients from wide-area imaging surveys can complement smaller integral-field spectroscopy data sets and can be used to constrain galaxy formation models. Here, we measure colour gradients for low-redshift galaxies (z < 0.1) using photometry from the DESI Legacy Imaging Survey DR9. Our sample comprises ~93 000 galaxies with spectroscopic redshifts and ~574 000 galaxies with photometric redshifts. We focus on gradients across a radial range 0.5R <sub>eff</sub> to R <sub>eff</sub> , which corresponds to the inner disc of typical late-type systems at low redshift. This region has been the focus of previous statistical studies of colour gradients and has recently been explored by spectroscopic surveys such as MaNGA. We find that the colour gradients of most galaxies in our sample are negative (redder towards the centre), consistent with the literature. We investigate empirical relationships between colour gradient, average g − r and r − z colour, M <sub>r</sub> , M <sub>★</sub> , and sSFR. Trends of gradient strength with M <sub>r</sub> (M <sub>★</sub> ) show an inflection around M <sub>r</sub> ~ −21 (log <sub>10</sub> M <sub>★</sub> /M <sub>☉</sub> ~ 10.5). Below this mass, colour gradients become steeper with increasing M <sub>★</sub> , whereas colour gradients in more massive galaxies become shallower. We find that positive gradients (bluer stars at smaller radii) are typical for galaxies of M <sub>★</sub> ~ 10 <sup>8</sup> M <sub>☉</sub> . We compare our results to age and metallicity gradients in two data sets derived from fits of different stellar population libraries to MaNGA spectra, but find no clear consensus explanation for the trends we observe. Both MaNGA data sets seem to imply a significant contribution from dust reddening, in particular, to explain the flatness of colour gradients along the red sequence.