The Astrophysical Journal (Jan 2023)

UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1

  • Alec Martin,
  • Yicheng Guo,
  • Xin Wang,
  • Anton M. Koekemoer,
  • Marc Rafelski,
  • Harry I. Teplitz,
  • Rogier A. Windhorst,
  • Anahita Alavi,
  • Norman A. Grogin,
  • Laura Prichard,
  • Ben Sunnquist,
  • Daniel Ceverino,
  • Nima Chartab,
  • Christopher J. Conselice,
  • Y. Sophia Dai,
  • Avishai Dekel,
  • Jonathan P. Gardner,
  • Eric Gawiser,
  • Nimish P. Hathi,
  • Matthew J. Hayes,
  • Rolf A. Jansen,
  • Zhiyuan Ji,
  • David C. Koo,
  • Ray A. Lucas,
  • Nir Mandelker,
  • Vihang Mehta,
  • Bahram Mobasher,
  • Kalina V. Nedkova,
  • Joel Primack,
  • Swara Ravindranath,
  • Brant E. Robertson,
  • Michael J. Rutkowski,
  • Zahra Sattari,
  • Emmaris Soto,
  • L. Y. Aaron Yung

DOI
https://doi.org/10.3847/1538-4357/aced3e
Journal volume & issue
Vol. 955, no. 2
p. 106

Abstract

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Giant star-forming clumps are a prominent feature of star-forming galaxies (SFGs) and contain important clues on galaxy formation and evolution. However, the basic demographics of clumps and their host galaxies remain uncertain. Using the Hubble Space Telescope/Wide Field Camera 3 F275W images from the Ultraviolet Imaging of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey, 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 Å luminosity is 3 times higher than the most luminous local H ii regions ( M _UV ≤ −16 AB). In our sample, 35% ± 3% of low-mass galaxies (log[ M _∗ / M _⊙ ] 10.5) galaxies, in agreement with previous studies. When compared to similar-mass nonclumpy SFGs, low- and intermediate-mass clumpy SFGs tend to have higher star formation rates (SFRs) and bluer rest-frame U − V colors, while high-mass clumpy SFGs tend to be larger than nonclumpy SFGs. However, clumpy and nonclumpy SFGs have similar Sérsic index, indicating a similar underlying density profile. Furthermore, we investigate how the 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 centers.

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