English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

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. Usingthe HST/WFC3 F275W images from the Ultraviolet Imaging of the Cosmic AssemblyNear-infrared Deep Extragalactic Legacy Survey (UVCANDELS), we detect andanalyze giant star-forming clumps in galaxies at 0.5 $\leq$ z $\leq$ 1,connecting two epochs when clumps are common (at cosmic high-noon, z $\sim$ 2)and rare (in the local universe). We construct a clump sample whose rest-frame1600 {\AA} luminosity is 3 times higher than the most luminous local HIIregions (M$_{UV} \leq -$16 AB). In our sample, 35 $\pm$ 3$\%$ of low-massgalaxies (log[M$_{*}$/M$_{\odot}$] $<$ 10) are clumpy (i.e., containing atleast one off-center clump). This fraction changes to 22 $\pm$ 3$\%$ and 22$\pm$ 4$\%$ for intermediate (10 $\leq$ log[M$_{*}$/M$_{\odot}$] $\leq$ 10.5)and high-mass (log[M$_{*}$/M$_{\odot}$] $>$ 10.5) galaxies in agreement withprevious studies. When compared to similar-mass non-clumpy SFGs, low- andintermediate-mass clumpy SFGs tend to have higher SFRs and bluer rest-frame U-Vcolors, while high-mass clumpy SFGs tend to be larger than non-clumpy SFGs.However, clumpy and non-clumpy SFGs have similar S\'ersic index, indicating asimilar underlying density profile. Furthermore, we investigate how UVluminosity of star-forming regions correlates with the physical properties ofhost galaxies. On average, more luminous star-forming regions reside in moreluminous, smaller, and/or higher-specific SFR galaxies and are found closer totheir hosts' galactic center.

UV-Bright Star-Forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 $\leq$ z $\leq$ 1