SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 mu m
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; Blain, Andrew W.10; Bourne, Nathan11; Bunker, Andrew J.12,13; Chang, Yu-Yen1; Chao, Dani C. -Y.14,35; Chen, Chian-Chou15; Clements, David L.16; Conselice, Christopher J.; 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, Minju29; Michalowski, Michal J.30; Oteo, Ivan11,15; 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.
Corresponding AuthorWang, Wei-Hao(
AbstractThe SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES) is a three-year JCMT Large Program aiming to reach the 450 mu m 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 mu m noise level of 0.91 mJy for point sources at the map center, covered an area of 151 arcmin(2), and detected 98 and 141 sources at 4.0 sigma and 3.5 sigma, 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 (+0.4)(-0.7) 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 mu m background. We show that Herschel counts at 350 and 500 mu m are significantly higher than our 450 mu m counts, likely caused by its large beam and source clustering. High angular resolution instruments like SCUBA-2 at 450 mu m 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
Indexed BySCI
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000415297500017
Citation statistics
Cited Times:13[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Corresponding AuthorWang, Wei-Hao
Affiliation1.Acad Sinica Inst Astron & Astrophys, 1 Sect 4,Roosevelt Rd, Taipei, Taiwan
2.Natl Taiwan Univ, Inst Phys, Taipei 10617, Taiwan
3.Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan
4.Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England
5.Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada
6.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China
7.Kyungpook Natl Univ, Dept Sci Educ, Daegu 41566, South Korea
8.Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan
9.Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England
10.Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England
11.Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland
12.Univ Oxford, Dept Phys, Oxford OX1 3RH, England
13.Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan
14.Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan
15.European Southern Observ, Garching, Germany
16.Imperial Coll London, Blackett Lab, Astrophys Grp, London SW7 2AZ, England
17.Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands
18.IAC, Tenerife, Spain
19.Univ La Laguna, Dept Astrois, Tenerife, Spain
20.Univ Hertfordshire, Ctr Astrophys Res, Sch Phys Astron & Math, Hatield AL10 9AB, England
21.Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
22.Korea Astron & Space Sci Inst, Daejeon 34055, South Korea
23.Univ Sci & Technol, Daejeon 34113, South Korea
24.Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan
25.Univ Tokyo, Res Ctr Early Universe, Bunkyo, Tokyo 1130033, Japan
26.Univ Sci & Technol China, Dept Astron, Hefei 230026, Anhui, Peoples R China
27.Subaru Telescope, NAOJ, Hilo, HI 96720 USA
28.Seoul Natl Univ, Dept Phys & Astron, Seoul 08826, South Korea
29.Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo, Tokyo 1130033, Japan
30.Adam Mickiewicz Univ, Astron Observ Inst, Fac Phys, PL-60286 Poznan, Poland
31.St Marys Univ, Dept Astron & Phys, Halifax B3J 3Z4, NS, Canada
32.Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada
33.Anhui Normal Univ, Dept Phys, Wuhu 241000, Anhui, Peoples R China
34.Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales
35.Max Planck Inst Astrophys, D-85740 Garching, Germany
Recommended Citation
GB/T 7714
Wang, Wei-Hao,Lin, Wei-Ching,Lim, Chen-Fatt,et al. SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 mu m[J]. ASTROPHYSICAL JOURNAL,2017,850(1):17.
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 mu m.ASTROPHYSICAL JOURNAL,850(1),17.
MLA Wang, Wei-Hao,et al."SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 mu m".ASTROPHYSICAL JOURNAL 850.1(2017):17.
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