Physical Properties of Sub-galactic Clumps at 0.5 ≤ Z ≤ 1.5 in the UVUDF

Journal Article · Wed Mar 01 04:00:00 EST 2017 · Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/AA5DA3· OSTI ID:22869297

Soto, Emmaris; Mello, Duilia F. de ^[1]; Rafelski, Marc; Koekemoer, Anton M.; Ravindranath, Swara; Grogin, Norman A. ^[2]; Gardner, Jonathan P. ^[3]; Teplitz, Harry I. ^[4]; Scarlata, Claudia ^[5]; Kurczynski, Peter; Gawiser, Eric ^[6]

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1. Physics Department The Catholic University of America 620 Michigan Avenue NE Washington, DC 20064 (United States)
2. Space Telescope Science Institute 3700 San Martin Drive Baltimore, MD 21218 (United States)
3. NASA Goddard Space Flight Center Observational Cosmology Laboratory Greenbelt, MD 20771 (United States)
4. Infrared Processing and Analysis Center, Caltech Pasadena, CA 91125 (United States)
5. Minnesota Institute of Astrophysics and School of Physics and Astronomy University of Minnesota Minneapolis, MN 55455 (United States)
6. Department of Physics and Astronomy Rutgers University Piscataway, NJ 08854 (United States)

We present an investigation of clumpy galaxies in the Hubble Ultra Deep Field at 0.5⩽z⩽1.5 in the rest-frame far-ultraviolet (FUV) using Hubble Space Telescope Wide Field Camera 3 broadband imaging in F225W, F275W, and F336W. An analysis of 1404 galaxies yields 209 galaxies that host 403 kpc scale clumps. These host galaxies appear to be typical star-forming galaxies, with an average of 2 clumps per galaxy and reaching a maximum of 8 clumps. We measure the photometry of the clumps and determine the mass, age, and star formation rates (SFR) using the spectral energy distribution fitting code FAST. We find that clumps make an average contribution of 19% to the total rest-frame FUV flux of their host galaxy. Individually, clumps contribute a median of 5% to the host galaxy SFR and an average of ∼4% to the host galaxy mass, with total clump contributions to the host galaxy stellar mass ranging widely from lower than 1% up to 93%. Clumps in the outskirts of galaxies are typically younger, with higher SFRs, than clumps in the inner regions. The results are consistent with clump migration theories in which clumps form through violent gravitational instabilities in gas-rich turbulent disks, eventually migrate toward the center of the galaxies, and coalesce into the bulge.

• OSTI ID: 22869297
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 837; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ENERGY SPECTRA
FAR ULTRAVIOLET RADIATION
GALACTIC EVOLUTION
GALAXIES
GRAVITATIONAL INSTABILITY
MASS
PHOTOMETRY
PHYSICAL PROPERTIES
SPACE
STAR EVOLUTION
STARS
TELESCOPES