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Title:
SXDF-UDS-CANDELS-ALMA 1.5 arcmin2 deep survey
Authors:
Kohno, K.; Yamaguchi, Y.; Tamura, Y.; Tadaki, K.; Hatsukade, B.; Ikarashi, S.; Caputi, K. I.; Rujopakarn, W.; Ivison, R. J.; Dunlop, J. S.; Motohara, K.; Umehata, H.; Yabe, K.; Wang, W. H.; Kodama, T.; Koyama, Y.; Hayashi, M.; Matsuda, Y.; Hughes, D.; Aretxaga, I.; Wilson, G. W.; Yun, M. S.; Ohta, K.; Akiyama, M.; Kawabe, R.; Iono, D.; Nakanishi, K.; Lee, M.; Makiya, R.
Affiliation:
AA(Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan ), AB(Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan), AC(Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan), AD(Max-Planck-Institut für extraterrestrische Physik (MPE), Garching, Germany), AE(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), AF(Kapteyn Astronomical Institute, University of Groningen, The Netherlands), AG(Kapteyn Astronomical Institute, University of Groningen, The Netherlands), AH(Kavli Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo, Chiba, Japan), AI(European Southern Observatory, Garching, Germany), AJ(Institute for Astronomy, University of Edinburgh, Royal Observatory, UK), AK(Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan), AL(Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan), AM(Kavli Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo, Chiba, Japan), AN(Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Taipei, Taiwan), AO(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), AP(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), AQ(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), AR(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), AS(Instituto Nacional de Astrofsica, Óptica y Electrónica (INAOE), Puebla, Mexico), AT(Instituto Nacional de Astrofsica, Óptica y Electrónica (INAOE), Puebla, Mexico), AU(Department of Astronomy, University of Massachusetts, Amherst, USA), AV(Department of Astronomy, University of Massachusetts, Amherst, USA), AW(Department of Astronomy, Kyoto University, Kyoto, Japan), AX(Astronomical Institute, Tohoku University, Sendai, Japan), AY(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), AZ(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), BA(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), BB(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan), BC(Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan)
Publication:
Galaxies at High Redshift and Their Evolution Over Cosmic Time, IAU Symposium Vol. 319, pp. 92-95
Publication Date:
00/2016
Origin:
CUP
Keywords:
galaxies: starburst, galaxies: high-redshift, submillimeter,
Abstract Copyright:
(c) 2016: Copyright © International Astronomical Union 2016
DOI:
10.1017/S1743921315010364
Bibliographic Code:
2016IAUS..319...92K

Abstract

We have conducted 1.1 mm ALMA observations of a contiguous 105'' × 50'' or 1.5 arcmin2 window in the SXDF-UDS-CANDELS. We achieved a 5sigma sensitivity of 0.28 mJy, giving a flat sensus of dusty star-forming galaxies with L IR ~6×1011 L &sun; (if T dust=40K) up to z ~ 10 thanks to the negative K-correction at this wavelength. We detected 5 brightest sources (S/N>6) and 18 low-significant sources (5>S/N>4 they may contain spurious detections, though). One of the 5 brightest ALMA sources (S 1.1mm = 0.84 +/- 0.09 mJy) is extremely faint in the WFC3 and VLT/HAWK-I images, demonstrating that a contiguous ALMA imaging survey uncovers a faint dust-obscured population invisible in the deep optical/near-infrared surveys. We find a possible [CII]-line emitter at z=5.955 or a low-z CO emitting galaxy within the field, allowing us to constrain the [CII] and/or CO luminosity functions across the history of the universe.
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