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The Origins of UV–optical Color Gradients in Star-forming Galaxies at z?~?2: Predominant Dust Gradients but Negligible sSFR Gradients
Liu,F. S.1,2; Jiang,Dongfei1,3; Faber,S. M.2; Koo,David C.2; Yesuf,Hassen M.2; Tacchella,Sandro4; Mao,Shude5,6,7; Wang,Weichen8; Guo,Yicheng2; Fang,Jerome J.2,9; Barro,Guillermo2,10; Zheng,Xianzhong3,11; Jia,Meng1; Tong,Wei1; Liu,Lu1; Meng,Xianmin6
2017-07-14
Source PublicationThe Astrophysical Journal Letters
ISSN2041-8205
Volume844Issue:1
AbstractAbstract The rest-frame UV–optical (i.e., NUV ? B) color is sensitive to both low-level recent star formation (specific star formation rate—sSFR) and dust. In this Letter, we extend our previous work on the origins of NUV???B color gradients in star-forming galaxies (SFGs) at to those at . We use a sample of 1335 large (semimajor axis radius ) SFGs with extended UV emission out to in the mass range at in the CANDELS/GOODS-S and UDS fields. We show that these SFGs generally have negative NUV???B color gradients (redder centers), and their color gradients strongly increase with galaxy mass. We also show that the global rest-frame FUV???NUV color is approximately linear with , which is derived by modeling the observed integrated FUV to NIR spectral energy distributions of the galaxies. Applying this integrated calibration to our spatially resolved data, we find a negative dust gradient (more dust extinguished in the centers), which steadily becomes steeper with galaxy mass. We further find that the NUV???B color gradients become nearly zero after correcting for dust gradients regardless of galaxy mass. This indicates that the sSFR gradients are negligible and dust reddening is likely the principal cause of negative UV–optical color gradients in these SFGs. Our findings support that the buildup of the stellar mass in SFGs at Cosmic Noon is self-similar inside .
Keywordgalaxies: high-redshift galaxies: photometry galaxies: star formation
DOI10.3847/2041-8213/aa7cf5
Language英语
WOS IDIOP:2041-8205-844-1-aa7cf5
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/23872
Collection中国科学院紫金山天文台
Affiliation1.College of Physical Science and Technology, Shenyang Normal University, Shenyang 110034, China; fsliu@synu.edu.cn
2.University of California Observatories and the Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
3.Purple Mountain Observatory, Chinese Academy of Sciences, 2 West-Beijing Road, Nanjing 210008, China
4.Department of Physics, Institute for Astronomy, ETH Zurich, CH-8093 Zurich, Switzerland
5.Physics Department and Tsinghua Centre for Astrophysics, Tsinghua University, Beijing 100084, China
6.National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Beijing 100012, China
7.Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester M13 9PL, UK
8.Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
9.Orange Coast College, Costa Mesa, CA 92626, USA
10.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
11.Chinese Academy of Sciences South America Center for Astronomy, China-Chile Joint Center for Astronomy, Camino El Observatorio 1515, Las Condes, Santiago, Chile
Recommended Citation
GB/T 7714
Liu,F. S.,Jiang,Dongfei,Faber,S. M.,等. The Origins of UV–optical Color Gradients in Star-forming Galaxies at z?~?2: Predominant Dust Gradients but Negligible sSFR Gradients[J]. The Astrophysical Journal Letters,2017,844(1).
APA Liu,F. S..,Jiang,Dongfei.,Faber,S. M..,Koo,David C..,Yesuf,Hassen M..,...&Meng,Xianmin.(2017).The Origins of UV–optical Color Gradients in Star-forming Galaxies at z?~?2: Predominant Dust Gradients but Negligible sSFR Gradients.The Astrophysical Journal Letters,844(1).
MLA Liu,F. S.,et al."The Origins of UV–optical Color Gradients in Star-forming Galaxies at z?~?2: Predominant Dust Gradients but Negligible sSFR Gradients".The Astrophysical Journal Letters 844.1(2017).
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