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

We present an investigation of clumpy galaxies in the Hubble Ultra Deep Field at 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. The...

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Bibliographic Details
Published in:The Astrophysical journal 2017-03, Vol.837 (1), p.6
Main Authors: Soto, Emmaris, Mello, Duilia F. de, Rafelski, Marc, Gardner, Jonathan P., Teplitz, Harry I., Koekemoer, Anton M., Ravindranath, Swara, Grogin, Norman A., Scarlata, Claudia, Kurczynski, Peter, Gawiser, Eric
Format: Article
Language:English
Subjects:
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Broadband
Clumps
Coalescing
Disks
ENERGY SPECTRA
FAR ULTRAVIOLET RADIATION
Field cameras
GALACTIC EVOLUTION
GALAXIES
galaxies: evolution
galaxies: formation
galaxies: star formation
galaxies: structure
Gravitation theory
GRAVITATIONAL INSTABILITY
Hubble deep field
Hubble Space Telescope
MASS
PHOTOMETRY
PHYSICAL PROPERTIES
SPACE
Space telescopes
Spectral energy distribution
Star & galaxy formation
STAR EVOLUTION
Star formation
STARS
Stars & galaxies
Stellar age
Stellar mass
TELESCOPES
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Summary:We present an investigation of clumpy galaxies in the Hubble Ultra Deep Field at 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.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa5da3