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

Soto, Emmaris and de Mello, Duilia F. and Rafelski, Marc and Gardner, Jonathan P. and Teplitz, Harry I. and Koekemoer, Anton M. and Ravindranath, Swara and Grogin, Norman A. and Scarlata, Claudia and Kurczynski, Peter and Gawiser, Eric (2017) Physical Properties of Sub-galactic Clumps at 0.5 ≤ Z ≤ 1.5 in the UVUDF. Astrophysical Journal, 837 (1). Art. No. 6. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170227-123040059

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Abstract

We present an investigation of clumpy galaxies in the Hubble Ultra Deep Field at 05 ≤ 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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa5da3DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa5da3PublisherArticle
https://arxiv.org/abs/1702.03038arXivDiscussion Paper
ORCID:
AuthorORCID
Rafelski, Marc0000-0002-9946-4731
Teplitz, Harry I.0000-0002-7064-5424
Koekemoer, Anton M.0000-0002-6610-2048
Scarlata, Claudia0000-0002-9136-8876
Additional Information:© 2017 The American Astronomical Society. Received 2016 June 17; accepted 2017 January 30; published 2017 February 27. We would like to thank B. Elmegreen for making the UDF clump data from Elmegreen et al. (2013) available for Figure 6. We also thank K. Whitaker for her assistance in mastering FAST, N. Bond, Y. Guo, and C. Leitherer for valuable discussions, and A. Fitzmaurice for her contributions to the earlier stages of this work. This material is based upon work supported by the National Aeronautics and Space Administration under Grant Number NNX13AT09H issued through the NASA Education Minority University Research Education Project (MUREP) through the NASA Harriett G. Jenkins Graduate Fellowship activity. D.F.d.M. was supported by STScI grant number HST-GO-12534.008-A. Facility: HST (WFC/ACS, WFC3/UVIS, WFC3/IR). Software: Source Extractor, IDL.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANNX13AT09H
NASAHST-GO-12534.008-A
Subject Keywords:Galaxies: Evolution; Galaxies: Formation; Galaxies: Star Formation; Galaxies: Structure
Issue or Number:1
Record Number:CaltechAUTHORS:20170227-123040059
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170227-123040059
Official Citation:Emmaris Soto et al 2017 ApJ 837 6
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74551
Collection:CaltechAUTHORS
Deposited By: Melissa Ray
Deposited On:28 Feb 2017 00:09
Last Modified:03 Oct 2019 16:40

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