Physical Properties of Sub-galactic Clumps at 0.5 \${\textbackslash}leq z {\textbackslash}leq\$ 1.5 in the UVUDF. Soto, E., de Mello, D. F., Rafelski, M., Gardner, J. P., Teplitz, H. I., Koekemoer, A. M., Ravindranath, S., Grogin, N. A., Scarlata, C., Kurczynski, P., & Gawiser, E. ArXiv e-prints, 1702:arXiv:1702.03038, February, 2017. ![Physical Properties of Sub-galactic Clumps at 0.5 \${\textbackslash}leq z {\textbackslash}leq\$ 1.5 in the UVUDF [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We present an investigation of clumpy galaxies in the Hubble Ultra Deep Field at 0.5 \${\textbackslash}leq z {\textbackslash}leq\$ 1.5 in the rest-frame far-ultraviolet (FUV) using HST WFC3 broadband imaging in F225W, F275W, and F336W. An analysis of 1,404 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) utilizing the SED-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 \${\textbackslash}sim\$4% to the host galaxy mass, with total clump contributions to the host galaxy stellar mass ranging widely from less than 1% up to 93%. Clumps in the outskirts of galaxies are typically younger, with higher star formation rates, 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.
@article{soto_physical_2017,
title = {Physical {Properties} of {Sub}-galactic {Clumps} at 0.5 \${\textbackslash}leq z {\textbackslash}leq\$ 1.5 in the {UVUDF}},
volume = {1702},
url = {http://adsabs.harvard.edu/abs/2017arXiv170203038S},
abstract = {We present an investigation of clumpy galaxies in the Hubble Ultra Deep
Field at 0.5 \${\textbackslash}leq z {\textbackslash}leq\$ 1.5 in the rest-frame far-ultraviolet (FUV)
using HST WFC3 broadband imaging in F225W, F275W, and F336W. An analysis
of 1,404 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) utilizing the SED-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 \${\textbackslash}sim\$4\% to the host
galaxy mass, with total clump contributions to the host galaxy stellar
mass ranging widely from less than 1\% up to 93\%. Clumps in the outskirts
of galaxies are typically younger, with higher star formation rates,
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.},
urldate = {2017-02-15},
journal = {ArXiv e-prints},
author = {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},
month = feb,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:1702.03038},
}
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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) utilizing the SED-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 \\${\\textbackslash}sim\\$4% to the host galaxy mass, with total clump contributions to the host galaxy stellar mass ranging widely from less than 1% up to 93%. Clumps in the outskirts of galaxies are typically younger, with higher star formation rates, 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.","urldate":"2017-02-15","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Soto"],"firstnames":["Emmaris"],"suffixes":[]},{"propositions":["de"],"lastnames":["Mello"],"firstnames":["Duilia","F."],"suffixes":[]},{"propositions":[],"lastnames":["Rafelski"],"firstnames":["Marc"],"suffixes":[]},{"propositions":[],"lastnames":["Gardner"],"firstnames":["Jonathan","P."],"suffixes":[]},{"propositions":[],"lastnames":["Teplitz"],"firstnames":["Harry","I."],"suffixes":[]},{"propositions":[],"lastnames":["Koekemoer"],"firstnames":["Anton","M."],"suffixes":[]},{"propositions":[],"lastnames":["Ravindranath"],"firstnames":["Swara"],"suffixes":[]},{"propositions":[],"lastnames":["Grogin"],"firstnames":["Norman","A."],"suffixes":[]},{"propositions":[],"lastnames":["Scarlata"],"firstnames":["Claudia"],"suffixes":[]},{"propositions":[],"lastnames":["Kurczynski"],"firstnames":["Peter"],"suffixes":[]},{"propositions":[],"lastnames":["Gawiser"],"firstnames":["Eric"],"suffixes":[]}],"month":"February","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:1702.03038","bibtex":"@article{soto_physical_2017,\n\ttitle = {Physical {Properties} of {Sub}-galactic {Clumps} at 0.5 \\${\\textbackslash}leq z {\\textbackslash}leq\\$ 1.5 in the {UVUDF}},\n\tvolume = {1702},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv170203038S},\n\tabstract = {We present an investigation of clumpy galaxies in the Hubble Ultra Deep \nField at 0.5 \\${\\textbackslash}leq z {\\textbackslash}leq\\$ 1.5 in the rest-frame far-ultraviolet (FUV)\nusing HST WFC3 broadband imaging in F225W, F275W, and F336W. An analysis\nof 1,404 galaxies yields 209 galaxies that host 403 kpc-scale clumps.\nThese host galaxies appear to be typical star-forming galaxies, with an\naverage of 2 clumps per galaxy and reaching a maximum of 8 clumps. We\nmeasure the photometry of the clumps, and determine the mass, age, and\nstar formation rates (SFR) utilizing the SED-fitting code FAST. We find\nthat clumps make an average contribution of 19\\% to the total rest-frame\nFUV flux of their host galaxy. Individually, clumps contribute a median\nof 5\\% to the host galaxy SFR and an average of \\${\\textbackslash}sim\\$4\\% to the host\ngalaxy mass, with total clump contributions to the host galaxy stellar\nmass ranging widely from less than 1\\% up to 93\\%. Clumps in the outskirts\nof galaxies are typically younger, with higher star formation rates,\nthan clumps in the inner regions. The results are consistent with clump\nmigration theories in which clumps form through violent gravitational\ninstabilities in gas-rich turbulent disks, eventually migrate toward the\ncenter of the galaxies, and coalesce into the bulge.},\n\turldate = {2017-02-15},\n\tjournal = {ArXiv e-prints},\n\tauthor = {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},\n\tmonth = feb,\n\tyear = {2017},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:1702.03038},\n}\n\n","author_short":["Soto, E.","de Mello, D. F.","Rafelski, M.","Gardner, J. P.","Teplitz, H. I.","Koekemoer, A. M.","Ravindranath, S.","Grogin, N. 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