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

Auteurs : Alec Martin (Department of Physics and Astronomy, University of Missouri, Columbia, MO, USA), Yicheng Guo (Department of Physics and Astronomy, University of Missouri, Columbia, MO, USA), Xin Wang (School of Astronomy and Space Science, University of Chinese Academy of Sciences), Anton M. Koekemoer (Space Telescope Science Institute, Baltimore, MD, USA), Marc Rafelski (Space Telescope Science Institute, Baltimore, MD, USA), Harry I. Teplitz (IPAC, Caltech, Pasadena, CA, USA), Rogier A. Windhorst (School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA), Anahita Alavi (IPAC, Caltech, Pasadena, CA, USA), Norman A. Grogin (Space Telescope Science Institute, Baltimore, MD, USA), Laura Prichard (Space Telescope Science Institute, Baltimore, MD, USA), Ben Sunnquist (Space Telescope Science Institute, Baltimore, MD, USA), Daniel Ceverino (Departamento de Fisica Teorica, Modulo 8, Facultad de Ciencias, Universidad Autonoma de Madrid, Madrid, Spain), Nima Chartab (The Observatories of the Carnegie Institution for Science, Pasadena, CA, USA), Christopher J. Conselice (Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester, UK), Y. Sophia Dai (Chinese Academy of Sciences South America Center for Astronomy), Avishai Dekel (Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem, Israel), Johnathan P. Gardner (Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA), Eric Gawiser (Department of Physics and Astronomy Rutgers University Piscataway, NJ, USA), Nimish P. Hathi (Space Telescope Science Institute, Baltimore, MD, USA), Matthew J. Hayes (Stockholm University, Department of Astronomy and Oskar Klein Centre for Cosmoparticle Physics, AlbaNova University Centre, Stockholm, Sweden), Rolf A. Jansen (School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA), Zhiyuan Ji (Steward Observatory, University of Arizona, Tucson, AZ, USA), David C. Koo (UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA), Ray A. Lucas (Space Telescope Science Institute, Baltimore, MD, USA), Nir Mandelker (Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem, Israel), Vihang Mehta (IPAC, Caltech, Pasadena, CA, USA), Bahram Mobasher (Department of Physics and Astronomy, University of California, Riverside, Riverside CA, USA), Kalina V. Nedkova (Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA), Joel Primack (Department of Physics, University of California, Santa Cruz, CA, USA), Swara Ravindranath (Space Telescope Science Institute, Baltimore, MD, USA), Brant E. Robertson (Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA), Michael J. Rutkowski (Department of Physics and Astronomy, Minnesota State University, Mankato, MN, USA), Zahra Sattari (The Observatories of the Carnegie Institution for Science, Pasadena, CA, USA), Emmaris Soto (Computational Physics, Inc., Springfield, VA, USA), L. Y. Aaron Yung (Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA)

arXiv: 2308.00041v1 - DOI (astro-ph.GA)
21 pages, 13 figures, Submitted to ApJ
Licence : CC BY 4.0

Résumé : 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 $\leq$ 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-frame 1600 {\AA} luminosity is 3 times higher than the most luminous local HII regions (M$_{UV} \leq -$16 AB). In our sample, 35 $\pm$ 3$\%$ of low-mass galaxies (log[M$_{*}$/M$_{\odot}$] $<$ 10) are clumpy (i.e., containing at least 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 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 S\'ersic 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.

Soumis à arXiv le 31 Jul. 2023

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