TY - JOUR
T1 - UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
AU - Martin, Alec
AU - Guo, Yicheng
AU - Wang, Xin
AU - Koekemoer, Anton M.
AU - Rafelski, Marc
AU - Teplitz, Harry I.
AU - Windhorst, Rogier A.
AU - Alavi, Anahita
AU - Grogin, Norman A.
AU - Prichard, Laura
AU - Sunnquist, Ben
AU - Ceverino, Daniel
AU - Chartab, Nima
AU - Conselice, Christopher J.
AU - Dai, Y. Sophia
AU - Dekel, Avishai
AU - Gardner, Jonathan P.
AU - Gawiser, Eric
AU - Hathi, Nimish P.
AU - Hayes, Matthew J.
AU - Jansen, Rolf A.
AU - Ji, Zhiyuan
AU - Koo, David C.
AU - Lucas, Ray A.
AU - Mandelker, Nir
AU - Mehta, Vihang
AU - Mobasher, Bahram
AU - Nedkova, Kalina V.
AU - Primack, Joel
AU - Ravindranath, Swara
AU - Robertson, Brant E.
AU - Rutkowski, Michael J.
AU - Sattari, Zahra
AU - Soto, Emmaris
AU - Yung, L. Y.Aaron
N1 - Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/10/1
Y1 - 2023/10/1
N2 - 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) 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 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.
AB - 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) 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 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.
UR - http://www.scopus.com/inward/record.url?scp=85173931015&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aced3e
DO - 10.3847/1538-4357/aced3e
M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???
AN - SCOPUS:85173931015
SN - 0004-637X
VL - 955
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 106
ER -