![]() 2007), and how and where the star-forming process shuts down. Radial star formation gradients are crucial for determining how stellar mass is built up in galaxies as they evolve along the star-forming main sequence (e.g. We finally discuss the striking findings that SFR scales with stellar mass density in the inner parts of galaxies, and that dust content is high in the outer parts despite low stellar mass surface densities there.ĭust, extinction, galaxies: formation – galaxies: high-redshift, galaxies: photometry, galaxies: star formation 1 INTRODUCTION They are also consistent with the sSFR profiles and, if assuming a radially constant gas-to-dust ratio, gas profiles in recent hydrodynamic models. Both sets of profiles agree well with previous radial sSFR and (continuum) A V measurements. sSFR gradients are nearly flat without central quenching signatures, except for M ⋆ > 10 10.5 M ⊙, where central declines of 20–25 per cent are observed. With our calibration, the resulting A V profiles fall much more slowly than stellar mass profiles over the measured radial range. Colour gradient directions are nearly parallel to the Calzetti extinction vector, indicating that dust plays a more important role than stellar population variations. The resulting colour gradients, covering a radial range of 0.2–2.0 effective radii, increase strongly with galaxy mass and with global A V. Using a multi-wavelength multi-aperture photometry catalogue based on CANDELS (Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey), UVI colour profiles of 1328 galaxies are stacked in stellar mass and redshift bins. ![]() ![]() By replacing J with I band, a new calibration method suitable for use with ACS+WFC3 data is created (i.e. ![]() We start with the standard UVJ-based method to estimate dust extinction and specific star formation rate (sSFR). This paper uses radial colour profiles to infer the distributions of dust, gas and star formation in z = 0.4–1.4 star-forming main-sequence galaxies. ![]()
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