@article{ikarashi_very_2017,
	title = {Very compact millimeter sizes for composite star-forming/{AGN} submillimeter galaxies},
	volume = {1710},
	url = {http://adsabs.harvard.edu/abs/2017arXiv171009021I},
	abstract = {We report the study of far-IR sizes of submillimeter galaxies (SMGs) in 
relation to their dust-obscured star formation rate (SFR) and active
galactic nuclei (AGN) presence, determined using mid-IR photometry. We
determined the millimeter-wave (\${\textbackslash}lambda\_\{{\textbackslash}rm obs\}=1100 {\textbackslash}mu\$m) sizes of
69 ALMA-identified SMGs, selected with \${\textbackslash}geq10\$\${\textbackslash}sigma\$ confidence on
ALMA images (\$F\_\{{\textbackslash}rm 1100 {\textbackslash}mu m\}=1.7\$--7.4 mJy). We found that all the
SMGs are located above an avoidance region in the millimeter size-flux
plane, as expected by the Eddington limit for star formation. In order
to understand what drives the different millimeter-wave sizes in SMGs,
we investigated the relation between millimeter-wave size and AGN
fraction for 25 of our SMGs at \$z=1\$--3. We found that the SMGs for
which the mid-IR emission is dominated by star formation or AGN have
extended millimeter-sizes, with respective median \$R\_\{{\textbackslash}rm c,e\} =
1.6{\textasciicircum}\{+0.34\}\_\{-0.21\}\$ and 1.5\${\textasciicircum}\{+0.93\}\_\{-0.24\}\$ kpc. Instead, the SMGs
for which the mid-IR emission corresponds to star-forming/AGN composites
have more compact millimeter-wave sizes, with median \$R\_\{\vphantom{\}}{\textbackslash}rm
c,e\vphantom{\{}\}=1.0{\textasciicircum}\{+0.20\}\_\{-0.20\}\$ kpc. The relation between millimeter-wave size
and AGN fraction suggests that this size may be related to the
evolutionary stage of the SMG. The very compact sizes for composite
star-forming/AGN systems could be explained by supermassive black holes
growing rapidly during the SMG coalescing, star-formation phase.},
	journal = {ArXiv e-prints},
	author = {Ikarashi, Soh and Caputi, Karina and Ohta, Kouji and Ivison, R. J. and Lagos, Claudia D. P. and Bisigello, Laura and Hatsukade, Bunyo and Aretxaga, Itziar and Dunlop, James S. and Hughes, David H. and Iono, Daisuke and Izumi, Takuma and Kashikawa, Nobunari and Koyama, Yusei and Kawabe, Ryohei and Kohno, Kotaro and Motohara, Kentaro and Nakanishi, Kouichiro and Tamura, Yoichi and Umehata, Hideki and Wilson, Grant W. and Yabe, Kiyoto and Yun, Min S.},
	month = oct,
	year = {2017},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:1710.09021},
}

{"_id":"4cinHMoC2i6PQGCfb","bibbaseid":"ikarashi-caputi-ohta-ivison-lagos-bisigello-hatsukade-aretxaga-etal-verycompactmillimetersizesforcompositestarformingagnsubmillimetergalaxies-2017","author_short":["Ikarashi, S.","Caputi, K.","Ohta, K.","Ivison, R. J.","Lagos, C. D. P.","Bisigello, L.","Hatsukade, B.","Aretxaga, I.","Dunlop, J. S.","Hughes, D. H.","Iono, D.","Izumi, T.","Kashikawa, N.","Koyama, Y.","Kawabe, R.","Kohno, K.","Motohara, K.","Nakanishi, K.","Tamura, Y.","Umehata, H.","Wilson, G. W.","Yabe, K.","Yun, M. S."],"bibdata":{"bibtype":"article","type":"article","title":"Very compact millimeter sizes for composite star-forming/AGN submillimeter galaxies","volume":"1710","url":"http://adsabs.harvard.edu/abs/2017arXiv171009021I","abstract":"We report the study of far-IR sizes of submillimeter galaxies (SMGs) in relation to their dust-obscured star formation rate (SFR) and active galactic nuclei (AGN) presence, determined using mid-IR photometry. We determined the millimeter-wave (\\${\\textbackslash}lambda_\\{{\\textbackslash}rm obs\\}=1100 {\\textbackslash}mu\\$m) sizes of 69 ALMA-identified SMGs, selected with \\${\\textbackslash}geq10\\$\\${\\textbackslash}sigma\\$ confidence on ALMA images (\\$F_\\{{\\textbackslash}rm 1100 {\\textbackslash}mu m\\}=1.7\\$–7.4 mJy). We found that all the SMGs are located above an avoidance region in the millimeter size-flux plane, as expected by the Eddington limit for star formation. In order to understand what drives the different millimeter-wave sizes in SMGs, we investigated the relation between millimeter-wave size and AGN fraction for 25 of our SMGs at \\$z=1\\$–3. We found that the SMGs for which the mid-IR emission is dominated by star formation or AGN have extended millimeter-sizes, with respective median \\$R_\\{{\\textbackslash}rm c,e\\} = 1.6{\\textasciicircum}\\{+0.34\\}_\\{-0.21\\}\\$ and 1.5\\${\\textasciicircum}\\{+0.93\\}_\\{-0.24\\}\\$ kpc. Instead, the SMGs for which the mid-IR emission corresponds to star-forming/AGN composites have more compact millimeter-wave sizes, with median \\$R_\\{p̌hantom{\\}}{\\textbackslash}rm c,ep̌hantom{\\{}\\}=1.0{\\textasciicircum}\\{+0.20\\}_\\{-0.20\\}\\$ kpc. The relation between millimeter-wave size and AGN fraction suggests that this size may be related to the evolutionary stage of the SMG. The very compact sizes for composite star-forming/AGN systems could be explained by supermassive black holes growing rapidly during the SMG coalescing, star-formation phase.","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Ikarashi"],"firstnames":["Soh"],"suffixes":[]},{"propositions":[],"lastnames":["Caputi"],"firstnames":["Karina"],"suffixes":[]},{"propositions":[],"lastnames":["Ohta"],"firstnames":["Kouji"],"suffixes":[]},{"propositions":[],"lastnames":["Ivison"],"firstnames":["R.","J."],"suffixes":[]},{"propositions":[],"lastnames":["Lagos"],"firstnames":["Claudia","D.","P."],"suffixes":[]},{"propositions":[],"lastnames":["Bisigello"],"firstnames":["Laura"],"suffixes":[]},{"propositions":[],"lastnames":["Hatsukade"],"firstnames":["Bunyo"],"suffixes":[]},{"propositions":[],"lastnames":["Aretxaga"],"firstnames":["Itziar"],"suffixes":[]},{"propositions":[],"lastnames":["Dunlop"],"firstnames":["James","S."],"suffixes":[]},{"propositions":[],"lastnames":["Hughes"],"firstnames":["David","H."],"suffixes":[]},{"propositions":[],"lastnames":["Iono"],"firstnames":["Daisuke"],"suffixes":[]},{"propositions":[],"lastnames":["Izumi"],"firstnames":["Takuma"],"suffixes":[]},{"propositions":[],"lastnames":["Kashikawa"],"firstnames":["Nobunari"],"suffixes":[]},{"propositions":[],"lastnames":["Koyama"],"firstnames":["Yusei"],"suffixes":[]},{"propositions":[],"lastnames":["Kawabe"],"firstnames":["Ryohei"],"suffixes":[]},{"propositions":[],"lastnames":["Kohno"],"firstnames":["Kotaro"],"suffixes":[]},{"propositions":[],"lastnames":["Motohara"],"firstnames":["Kentaro"],"suffixes":[]},{"propositions":[],"lastnames":["Nakanishi"],"firstnames":["Kouichiro"],"suffixes":[]},{"propositions":[],"lastnames":["Tamura"],"firstnames":["Yoichi"],"suffixes":[]},{"propositions":[],"lastnames":["Umehata"],"firstnames":["Hideki"],"suffixes":[]},{"propositions":[],"lastnames":["Wilson"],"firstnames":["Grant","W."],"suffixes":[]},{"propositions":[],"lastnames":["Yabe"],"firstnames":["Kiyoto"],"suffixes":[]},{"propositions":[],"lastnames":["Yun"],"firstnames":["Min","S."],"suffixes":[]}],"month":"October","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:1710.09021","bibtex":"@article{ikarashi_very_2017,\n\ttitle = {Very compact millimeter sizes for composite star-forming/{AGN} submillimeter galaxies},\n\tvolume = {1710},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv171009021I},\n\tabstract = {We report the study of far-IR sizes of submillimeter galaxies (SMGs) in \nrelation to their dust-obscured star formation rate (SFR) and active\ngalactic nuclei (AGN) presence, determined using mid-IR photometry. We\ndetermined the millimeter-wave (\\${\\textbackslash}lambda\\_\\{{\\textbackslash}rm obs\\}=1100 {\\textbackslash}mu\\$m) sizes of\n69 ALMA-identified SMGs, selected with \\${\\textbackslash}geq10\\$\\${\\textbackslash}sigma\\$ confidence on\nALMA images (\\$F\\_\\{{\\textbackslash}rm 1100 {\\textbackslash}mu m\\}=1.7\\$--7.4 mJy). We found that all the\nSMGs are located above an avoidance region in the millimeter size-flux\nplane, as expected by the Eddington limit for star formation. In order\nto understand what drives the different millimeter-wave sizes in SMGs,\nwe investigated the relation between millimeter-wave size and AGN\nfraction for 25 of our SMGs at \\$z=1\\$--3. We found that the SMGs for\nwhich the mid-IR emission is dominated by star formation or AGN have\nextended millimeter-sizes, with respective median \\$R\\_\\{{\\textbackslash}rm c,e\\} =\n1.6{\\textasciicircum}\\{+0.34\\}\\_\\{-0.21\\}\\$ and 1.5\\${\\textasciicircum}\\{+0.93\\}\\_\\{-0.24\\}\\$ kpc. Instead, the SMGs\nfor which the mid-IR emission corresponds to star-forming/AGN composites\nhave more compact millimeter-wave sizes, with median \\$R\\_\\{\\vphantom{\\}}{\\textbackslash}rm\nc,e\\vphantom{\\{}\\}=1.0{\\textasciicircum}\\{+0.20\\}\\_\\{-0.20\\}\\$ kpc. The relation between millimeter-wave size\nand AGN fraction suggests that this size may be related to the\nevolutionary stage of the SMG. The very compact sizes for composite\nstar-forming/AGN systems could be explained by supermassive black holes\ngrowing rapidly during the SMG coalescing, star-formation phase.},\n\tjournal = {ArXiv e-prints},\n\tauthor = {Ikarashi, Soh and Caputi, Karina and Ohta, Kouji and Ivison, R. J. and Lagos, Claudia D. P. and Bisigello, Laura and Hatsukade, Bunyo and Aretxaga, Itziar and Dunlop, James S. and Hughes, David H. and Iono, Daisuke and Izumi, Takuma and Kashikawa, Nobunari and Koyama, Yusei and Kawabe, Ryohei and Kohno, Kotaro and Motohara, Kentaro and Nakanishi, Kouichiro and Tamura, Yoichi and Umehata, Hideki and Wilson, Grant W. and Yabe, Kiyoto and Yun, Min S.},\n\tmonth = oct,\n\tyear = {2017},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:1710.09021},\n}\n\n","author_short":["Ikarashi, S.","Caputi, K.","Ohta, K.","Ivison, R. J.","Lagos, C. D. P.","Bisigello, L.","Hatsukade, B.","Aretxaga, I.","Dunlop, J. S.","Hughes, D. H.","Iono, D.","Izumi, T.","Kashikawa, N.","Koyama, Y.","Kawabe, R.","Kohno, K.","Motohara, K.","Nakanishi, K.","Tamura, Y.","Umehata, H.","Wilson, G. W.","Yabe, K.","Yun, M. S."],"key":"ikarashi_very_2017","id":"ikarashi_very_2017","bibbaseid":"ikarashi-caputi-ohta-ivison-lagos-bisigello-hatsukade-aretxaga-etal-verycompactmillimetersizesforcompositestarformingagnsubmillimetergalaxies-2017","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2017arXiv171009021I"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["very","compact","millimeter","sizes","composite","star","forming","agn","submillimeter","galaxies","ikarashi","caputi","ohta","ivison","lagos","bisigello","hatsukade","aretxaga","dunlop","hughes","iono","izumi","kashikawa","koyama","kawabe","kohno","motohara","nakanishi","tamura","umehata","wilson","yabe","yun"],"title":"Very compact millimeter sizes for composite star-forming/AGN submillimeter galaxies","year":2017}