摘要
ApJ 955 106 (2023) Giant star-forming clumps are a prominent feature of star-forming galaxies (SFGs) and contain important clues on galaxy formation and evolution. However, basic demographics of clumps and their host galaxies remain uncertain. Using the HST/WFC3 F275W images from the Ultraviolet Imaging of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (UVCANDELS), we detect and analyze giant star-forming clumps in galaxies at 0.5≤z≤1, connecting two epochs when clumps are common (at cosmic high-noon, z∼2) and rare (in the local universe). We construct a clump sample whose rest-frame 1600 luminosity is 3 times higher than the most luminous local HII regions (M _(UV) ≤ - 16 AB). In our sample, 35±3 %of low-mass galaxies (log[M _(*) /M _(⊙) ]<10) are clumpy (i.e., containing at least one off-center clump). This fraction changes to 22±3 %and 22±4 %for intermediate (10≤log[M _(*) /M _(⊙) ]≤10.5) and high-mass (log[M _(*) /M _(⊙) ]>10.5) galaxies in agreement with previous studies. When compared to similar-mass non-clumpy SFGs, low- and intermediate-mass clumpy SFGs tend to have higher SFRs and bluer rest-frame U-V colors, while high-mass clumpy SFGs tend to be larger than non-clumpy SFGs. However, clumpy and non-clumpy SFGs have similar Sérsic index, indicating a similar underlying density profile. Furthermore, we investigate how UV luminosity of star-forming regions correlates with the physical properties of host galaxies. On average, more luminous star-forming regions reside in more luminous, smaller, and/or higher-specific SFR galaxies and are found closer to their hosts' galactic center.