SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 μm
Wang,Wei-Hao1; Lin,Wei-Ching1,2; Lim,Chen-Fatt1,3; Smail,Ian4; Chapman,Scott C.5; Zheng,Xian Zhong6; Shim,Hyunjin7; Kodama,Tadayuki8; Almaini,Omar9; Ao,Yiping6,8; Blain,Andrew W.10; Bourne,Nathan11; Bunker,Andrew J.12,13; Chang,Yu-Yen1; Chao,Dani C.-Y.14; Chen,Chian-Chou15; Clements,David L.16; Conselice,Christopher J.9; Cowley,William I.17; Dannerbauer,Helmut18,19; Dunlop,James S.11; Geach,James E.20; Goto,Tomotsugu14; Jiang,Linhua21; Ivison,Rob J.11,15; Jeong,Woong-Seob22,23; Kohno,Kotaro24,25; Kong,Xu26; Lee,Chien-Hsu27; Lee,Hyung Mok28; Lee,Minju8,29; Micha?owski,Micha? J.30; Oteo,Iván11,15; Sawicki,Marcin31; Scott,Douglas32; Shu,Xin Wen33; Simpson,James M.1; Tee,Wei-Leong1,2; Toba,Yoshiki1; Valiante,Elisabetta34; Wang,Jun-Xian26; Wang,Ran21; Wardlow,Julie L.4
Source PublicationThe Astrophysical Journal
AbstractAbstract The SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES) is a three-year JCMT Large Program aiming to reach the 450 μm confusion limit in the COSMOS-CANDELS region to study a representative sample of the high-redshift far-infrared galaxy population that gives rise to the bulk of the far-infrared background. We present the first-year data from STUDIES. We reached a 450 μm noise level of 0.91?mJy for point sources at the map center, covered an area of 151?arcmin2, and detected 98 and 141 sources at 4.0σ and 3.5σ, respectively. Our derived counts are best constrained in the 3.5–25?mJy regime using directly detected sources. Below the detection limits, our fluctuation analysis further constrains the slope of the counts down to 1 mJy. The resulting counts at 1–25 mJy are consistent with a power law having a slope of ?2.59 (±0.10 for 3.5–25 mJy, and ? 0.7 + 0.4 for 1–3.5 mJy). There is no evidence of a faint-end termination or turnover of the counts in this flux density range. Our counts are also consistent with previous SCUBA-2 blank-field and lensing-cluster surveys. The integrated surface brightness from our counts down to 1 mJy is 90.0?±?17.2 Jy deg?2, which can account for up to 83 ? 16 + 15 % of the COBE?450 μm background. We show that Herschel counts at 350 and 500 μm are significantly higher than our 450 μm counts, likely caused by its large beam and source clustering. High angular resolution instruments like SCUBA-2 at 450 μm are therefore highly beneficial for measuring the luminosity and spatial density of high-redshift dusty galaxies.
Keywordgalaxies: high-redshift galaxies: evolution submillimeter: galaxies cosmology: cosmic background radiation
WOS IDIOP:0004-637X-850-1-aa911b
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), No. 1, Section 4, Roosevelt Rd., Taipei 10617, Taiwan;
2.Institute of Physics, National Taiwan University, Taipei 10617, Taiwan
3.Institute of Astrophysics, National Taiwan University, Taipei 10617, Taiwan
4.Centre for Extragalactic Astronomy, Department of Physics, Durham University, Durham DH1 3LE, UK
5.Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS B3H 3J5 Canada
6.Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China
7.Department of Science Education, Kyungpook National University, Bukgu, Daegu 41566, Korea
8.National Astronomical Observatory of Japan (NAOJ), Mitaka, Tokyo 181-8588, Japan
9.School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD, UK
10.Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK
11.Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UK
12.Department of Physics, University of Oxford, Oxford OX13RH, UK
13.Kavli Institute for the Physics and Mathematics of the Universe, Kashiwa, 277-8583, Japan
14.Institute of Astronomy, National Tsing Hua University, Hsinchu 30013, Taiwan
15.European Southern Observatory, Garching, Germany
16.Astrophysics Group, Imperial College London, Blackett Laboratory, London SW7 2AZ, UK
17.Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
18.Instituto de Astrofísica de Canarias (IAC), Tenerife, Spain
19.Universidad de La Laguna, Dpto. Astroísica, Tenerife, Spain
20.Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatield AL10 9AB, UK
21.Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
22.Korea Astronomy and Space Science Institute, Yuseong-gu, Daejeon 34055, Korea
23.University of Science and Technology, Yuseong-gu, Daejeon 34113, Korea
24.Institute of Astronomy, University of Tokyo, Mitaka, Tokyo 181-0015, Japan
25.Research Center for the Early Universe, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
26.Department of Astronomy, University of Science and Technology of China, Hefei, Anhui 230026, China
27.Subaru Telescope, NAOJ, Hilo, HI 96720, USA
28.Department of Physics and Astronomy, Seoul National University, Seoul 08826, Korea
29.Department of Astronomy, Graduate School of Science, The University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
30.Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, 60-286 Poznań, Poland
31.Department of Astronomy & Physics, Saint Mary’s University, Halifax, B3J 3Z4, Canada
32.Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada
33.Department of Physics, Anhui Normal University, Wuhu, Anhui, 241000, China
34.School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
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Wang,Wei-Hao,Lin,Wei-Ching,Lim,Chen-Fatt,et al. SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 μm[J]. The Astrophysical Journal,2017,850(1).
APA Wang,Wei-Hao.,Lin,Wei-Ching.,Lim,Chen-Fatt.,Smail,Ian.,Chapman,Scott C..,...&Wardlow,Julie L..(2017).SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 μm.The Astrophysical Journal,850(1).
MLA Wang,Wei-Hao,et al."SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 μm".The Astrophysical Journal 850.1(2017).
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