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Herschel–ATLAS: counterparts from the ultraviolet–near‐infrared in the science demonstration phase catalogue

Identifieur interne : 002B22 ( Istex/Corpus ); précédent : 002B21; suivant : 002B23

Herschel–ATLAS: counterparts from the ultraviolet–near‐infrared in the science demonstration phase catalogue

Auteurs : D. J. B. Smith ; L. Dunne ; S. J. Maddox ; S. Eales ; D. G. Bonfield ; M. J. Jarvis ; W. Sutherland ; S. Fleuren ; E. E. Rigby ; M. A. Thompson ; I. K. Baldry ; S. Bamford ; S. Buttiglione ; A. Cava ; D. L. Clements ; A. Cooray ; S. Croom ; A. Dariush ; G. De Zotti ; S. P. Driver ; J. S. Dunlop ; J. Fritz ; D. T. Hill ; A. Hopkins ; R. Hopwood ; E. Ibar ; R. J. Ivison ; D. H. Jones ; L. Kelvin ; L. Leeuw ; J. Liske ; J. Loveday ; B. F. Madore ; P. Norberg ; P. Panuzzo ; E. Pascale ; M. Pohlen ; C. C. Popescu ; M. Prescott ; A. Robotham ; G. Rodighiero ; D. Scott ; M. Seibert ; R. Sharp ; P. Temi ; R. J. Tuffs ; P. Van Der Werf ; E. Van Kampen

Source :

RBID : ISTEX:A0DF6586BAE8156157D7A336C1BD91E5D2E6B5C1

English descriptors

Abstract

We present a technique to identify optical counterparts of 250‐μm‐selected sources from the Herschel–ATLAS survey. Of the 6621 250 μm > 32‐mJy sources in our science demonstration catalogue we find that ∼60 per cent have counterparts brighter than r = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability R > 0.8. This is approximately 37 per cent of the full 250‐μm catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250‐μm‐selected Herschel–ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at z ≈ 0.25 ± 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the r‐band limit have z > 1. We also suggest a method for selecting populations of strongly lensed high‐redshift galaxies. Our identifications are matched to UV–NIR photometry from the GAMA survey, and these data are available as part of the Herschel–ATLAS public data release.

Url:
DOI: 10.1111/j.1365-2966.2011.18827.x

Links to Exploration step

ISTEX:A0DF6586BAE8156157D7A336C1BD91E5D2E6B5C1

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<name sortKey="Popescu, C C" sort="Popescu, C C" uniqKey="Popescu C" first="C. C." last="Popescu">C. C. Popescu</name>
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<name sortKey="Prescott, M" sort="Prescott, M" uniqKey="Prescott M" first="M." last="Prescott">M. Prescott</name>
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<name sortKey="Scott, D" sort="Scott, D" uniqKey="Scott D" first="D." last="Scott">D. Scott</name>
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<mods:affiliation>Department of Physics and Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, BC V6T 1Z1, Canada</mods:affiliation>
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<name sortKey="Seibert, M" sort="Seibert, M" uniqKey="Seibert M" first="M." last="Seibert">M. Seibert</name>
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<mods:affiliation>Leiden Observatory, Leiden University, PO Box 9513, NL ‐ 2300 RA Leiden, the Netherlands</mods:affiliation>
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<name sortKey="Thompson, M A" sort="Thompson, M A" uniqKey="Thompson M" first="M. A." last="Thompson">M. A. Thompson</name>
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<name sortKey="Croom, S" sort="Croom, S" uniqKey="Croom S" first="S." last="Croom">S. Croom</name>
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<affiliation>
<mods:affiliation>SISSA, Via Bonomea 265, I‐34136 Trieste, Italy</mods:affiliation>
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<name sortKey="Hill, D T" sort="Hill, D T" uniqKey="Hill D" first="D. T." last="Hill">D. T. Hill</name>
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<name sortKey="Hopkins, A" sort="Hopkins, A" uniqKey="Hopkins A" first="A." last="Hopkins">A. Hopkins</name>
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<name sortKey="Hopwood, R" sort="Hopwood, R" uniqKey="Hopwood R" first="R." last="Hopwood">R. Hopwood</name>
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<mods:affiliation>Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AA</mods:affiliation>
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<name sortKey="Ibar, E" sort="Ibar, E" uniqKey="Ibar E" first="E." last="Ibar">E. Ibar</name>
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<name sortKey="Ivison, R J" sort="Ivison, R J" uniqKey="Ivison R" first="R. J." last="Ivison">R. J. Ivison</name>
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<affiliation>
<mods:affiliation>Uk Astronomy Technology Centre, Royal Observatory, Edinburgh EH9 3HJ</mods:affiliation>
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<name sortKey="Jones, D H" sort="Jones, D H" uniqKey="Jones D" first="D. H." last="Jones">D. H. Jones</name>
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<mods:affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</mods:affiliation>
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<name sortKey="Kelvin, L" sort="Kelvin, L" uniqKey="Kelvin L" first="L." last="Kelvin">L. Kelvin</name>
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<mods:affiliation>SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS</mods:affiliation>
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<name sortKey="Leeuw, L" sort="Leeuw, L" uniqKey="Leeuw L" first="L." last="Leeuw">L. Leeuw</name>
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<mods:affiliation>SETI Institute, 515 N. Whisman Avenue, Mountain View, CA 94043, USA</mods:affiliation>
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<author>
<name sortKey="Liske, J" sort="Liske, J" uniqKey="Liske J" first="J." last="Liske">J. Liske</name>
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<mods:affiliation>European Southern Observatory, Karl‐Schwarzschild‐Strasse 2, D‐85748 Garching bei München, Germany</mods:affiliation>
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</author>
<author>
<name sortKey="Loveday, J" sort="Loveday, J" uniqKey="Loveday J" first="J." last="Loveday">J. Loveday</name>
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<mods:affiliation>Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH</mods:affiliation>
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<name sortKey="Madore, B F" sort="Madore, B F" uniqKey="Madore B" first="B. F." last="Madore">B. F. Madore</name>
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<mods:affiliation>Observatories of the Carnegie Institution, 813 Santa Barbera St., Pasadena, CA 91101, USA</mods:affiliation>
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<name sortKey="Norberg, P" sort="Norberg, P" uniqKey="Norberg P" first="P." last="Norberg">P. Norberg</name>
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<mods:affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ</mods:affiliation>
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<name sortKey="Panuzzo, P" sort="Panuzzo, P" uniqKey="Panuzzo P" first="P." last="Panuzzo">P. Panuzzo</name>
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<mods:affiliation>CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F‐91191 Gif‐sur‐Yvette, France</mods:affiliation>
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<name sortKey="Pascale, E" sort="Pascale, E" uniqKey="Pascale E" first="E." last="Pascale">E. Pascale</name>
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<mods:affiliation>School of Physics & Astronomy, Cardiff University, Queen Buildings, The Parade, Cardiff CF24 3AA</mods:affiliation>
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<name sortKey="Pohlen, M" sort="Pohlen, M" uniqKey="Pohlen M" first="M." last="Pohlen">M. Pohlen</name>
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<mods:affiliation>School of Physics & Astronomy, Cardiff University, Queen Buildings, The Parade, Cardiff CF24 3AA</mods:affiliation>
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<name sortKey="Popescu, C C" sort="Popescu, C C" uniqKey="Popescu C" first="C. C." last="Popescu">C. C. Popescu</name>
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<mods:affiliation>Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE</mods:affiliation>
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<author>
<name sortKey="Prescott, M" sort="Prescott, M" uniqKey="Prescott M" first="M." last="Prescott">M. Prescott</name>
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<mods:affiliation>Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD</mods:affiliation>
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<name sortKey="Robotham, A" sort="Robotham, A" uniqKey="Robotham A" first="A." last="Robotham">A. Robotham</name>
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<mods:affiliation>SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS</mods:affiliation>
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<name sortKey="Rodighiero, G" sort="Rodighiero, G" uniqKey="Rodighiero G" first="G." last="Rodighiero">G. Rodighiero</name>
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<mods:affiliation>INAF – Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, I‐35122 Padova, Italy</mods:affiliation>
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</author>
<author>
<name sortKey="Scott, D" sort="Scott, D" uniqKey="Scott D" first="D." last="Scott">D. Scott</name>
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<mods:affiliation>Department of Physics and Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, BC V6T 1Z1, Canada</mods:affiliation>
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<author>
<name sortKey="Seibert, M" sort="Seibert, M" uniqKey="Seibert M" first="M." last="Seibert">M. Seibert</name>
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<mods:affiliation>Observatories of the Carnegie Institution, 813 Santa Barbera St., Pasadena, CA 91101, USA</mods:affiliation>
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<name sortKey="Sharp, R" sort="Sharp, R" uniqKey="Sharp R" first="R." last="Sharp">R. Sharp</name>
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<mods:affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</mods:affiliation>
</affiliation>
</author>
<author>
<name sortKey="Temi, P" sort="Temi, P" uniqKey="Temi P" first="P." last="Temi">P. Temi</name>
<affiliation>
<mods:affiliation>Astrophysics Branch, NASA Ames Research Center, Mail Stop 2456, Moffett Field, CA 94035, USA</mods:affiliation>
</affiliation>
</author>
<author>
<name sortKey="Tuffs, R J" sort="Tuffs, R J" uniqKey="Tuffs R" first="R. J." last="Tuffs">R. J. Tuffs</name>
<affiliation>
<mods:affiliation>Max Planck Institut für Kernphysik (MPIK), Saupfercheckweg, 69117 Heidelberg, Germany</mods:affiliation>
</affiliation>
</author>
<author>
<name sortKey="Van Der Werf, P" sort="Van Der Werf, P" uniqKey="Van Der Werf P" first="P." last="Van Der Werf">P. Van Der Werf</name>
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<mods:affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ</mods:affiliation>
</affiliation>
<affiliation>
<mods:affiliation>Leiden Observatory, Leiden University, PO Box 9513, NL ‐ 2300 RA Leiden, the Netherlands</mods:affiliation>
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<author>
<name sortKey="Van Kampen, E" sort="Van Kampen, E" uniqKey="Van Kampen E" first="E." last="Van Kampen">E. Van Kampen</name>
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<mods:affiliation>European Southern Observatory, Karl‐Schwarzschild‐Strasse 2, D‐85748 Garching bei München, Germany</mods:affiliation>
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<title level="j">Monthly Notices of the Royal Astronomical Society</title>
<idno type="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-09-11">2011-09-11</date>
<biblScope unit="volume">416</biblScope>
<biblScope unit="issue">2</biblScope>
<biblScope unit="page" from="857">857</biblScope>
<biblScope unit="page" to="872">872</biblScope>
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<idno type="ISSN">0035-8711</idno>
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<idno type="DOI">10.1111/j.1365-2966.2011.18827.x</idno>
<idno type="ArticleID">MNR18827</idno>
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<idno type="ISSN">0035-8711</idno>
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<term>methods: statistical</term>
<term>submillimetre: galaxies</term>
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<language ident="en">en</language>
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<front>
<div type="abstract" xml:lang="en">We present a technique to identify optical counterparts of 250‐μm‐selected sources from the Herschel–ATLAS survey. Of the 6621 250 μm > 32‐mJy sources in our science demonstration catalogue we find that ∼60 per cent have counterparts brighter than r = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability R > 0.8. This is approximately 37 per cent of the full 250‐μm catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250‐μm‐selected Herschel–ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at z ≈ 0.25 ± 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the r‐band limit have z > 1. We also suggest a method for selecting populations of strongly lensed high‐redshift galaxies. Our identifications are matched to UV–NIR photometry from the GAMA survey, and these data are available as part of the Herschel–ATLAS public data release.</div>
</front>
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<name>D. J. B. Smith</name>
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<json:string>Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, Hatfield, Herts AL10 9AB</json:string>
<json:string>E-mail: daniel.j.b.smith@gmail.com</json:string>
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<name>L. Dunne</name>
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<name>S. J. Maddox</name>
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<name>S. Eales</name>
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<json:string>School of Physics & Astronomy, Cardiff University, Queen Buildings, The Parade, Cardiff CF24 3AA</json:string>
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<name>D. G. Bonfield</name>
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<json:string>Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, Hatfield, Herts AL10 9AB</json:string>
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<name>M. J. Jarvis</name>
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<json:string>Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, Hatfield, Herts AL10 9AB</json:string>
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<name>W. Sutherland</name>
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<json:string>School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London E1 4NS</json:string>
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<name>S. Fleuren</name>
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<json:string>School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London E1 4NS</json:string>
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<name>E. E. Rigby</name>
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<json:string>Centre for Astronomy and Particle Theory, The School of Physics & Astronomy, Nottingham University, University Park Campus, Nottingham NG7 1HR</json:string>
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<name>A. Cooray</name>
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<json:string>University of California, Ivine, Department of Physics & Astronomy, 4186 Frederick Reines Hall, Irvine, CA 92697‐4575, USA</json:string>
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<name>S. Croom</name>
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<json:string>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia</json:string>
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<name>A. Dariush</name>
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<json:string>School of Physics & Astronomy, Cardiff University, Queen Buildings, The Parade, Cardiff CF24 3AA</json:string>
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<name>G. de Zotti</name>
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<json:string>INAF – Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, I‐35122 Padova, Italy</json:string>
<json:string>SISSA, Via Bonomea 265, I‐34136 Trieste, Italy</json:string>
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<name>S. P. Driver</name>
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<name>J. S. Dunlop</name>
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<json:string>Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ</json:string>
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<name>R. Hopwood</name>
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<name>E. Ibar</name>
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<json:string>Uk Astronomy Technology Centre, Royal Observatory, Edinburgh EH9 3HJ</json:string>
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<name>R. J. Ivison</name>
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<name>D. H. Jones</name>
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<json:string>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</json:string>
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<name>L. Kelvin</name>
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<json:string>SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS</json:string>
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<name>L. Leeuw</name>
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<json:string>SETI Institute, 515 N. Whisman Avenue, Mountain View, CA 94043, USA</json:string>
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<name>J. Liske</name>
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<json:string>European Southern Observatory, Karl‐Schwarzschild‐Strasse 2, D‐85748 Garching bei München, Germany</json:string>
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<name>J. Loveday</name>
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<name>B. F. Madore</name>
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<json:string>Observatories of the Carnegie Institution, 813 Santa Barbera St., Pasadena, CA 91101, USA</json:string>
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<name>P. Norberg</name>
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<json:string>Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ</json:string>
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<name>P. Panuzzo</name>
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<name>E. Pascale</name>
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<json:string>School of Physics & Astronomy, Cardiff University, Queen Buildings, The Parade, Cardiff CF24 3AA</json:string>
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<name>M. Pohlen</name>
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<p>We present a technique to identify optical counterparts of 250‐μm‐selected sources from the Herschel–ATLAS survey. Of the 6621 250 μm > 32‐mJy sources in our science demonstration catalogue we find that ∼60 per cent have counterparts brighter than r = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability R > 0.8. This is approximately 37 per cent of the full 250‐μm catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250‐μm‐selected Herschel–ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at z ≈ 0.25 ± 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the r‐band limit have z > 1. We also suggest a method for selecting populations of strongly lensed high‐redshift galaxies. Our identifications are matched to UV–NIR photometry from the GAMA survey, and these data are available as part of the Herschel–ATLAS public data release.</p>
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<unparsedEditorialHistory>Accepted 2011 March 29. Received 2011 March 17; in original form 2010 July 28</unparsedEditorialHistory>
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<i>Herschel</i>
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<i>Herschel</i>
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<title type="short">Herschel–
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<title type="main">ABSTRACT</title>
<p>We present a technique to identify optical counterparts of 250‐
<span type="mathematics">μ</span>
m‐selected sources from the 
<i>Herschel</i>
–ATLAS survey. Of the 6621 250 
<span type="mathematics">μ</span>
m > 32‐mJy sources in our science demonstration catalogue we find that ∼60 per cent have counterparts brighter than 
<i>r</i>
 = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability 
<i>R</i>
 > 0.8. This is approximately 37 per cent of the full 250‐
<span type="mathematics">μ</span>
m catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250‐
<span type="mathematics">μ</span>
m‐selected 
<i>Herschel</i>
–ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at 
<i>z</i>
 ≈ 0.25 ± 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the 
<i>r</i>
‐band limit have 
<i>z</i>
 > 1. We also suggest a method for selecting populations of strongly lensed high‐redshift galaxies. Our identifications are matched to UV–NIR photometry from the GAMA survey, and these data are available as part of the 
<i>Herschel</i>
–ATLAS public data release.</p>
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<i>Herschel</i>
 is an ESA space observatory with science instruments provided by European‐led Principal Investigator consortia and with important participation from NASA.</p>
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<affiliation>Astrophysics Branch, NASA Ames Research Center, Mail Stop 2456, Moffett Field, CA 94035, USA</affiliation>
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<affiliation>Max Planck Institut für Kernphysik (MPIK), Saupfercheckweg, 69117 Heidelberg, Germany</affiliation>
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<namePart type="given">P.</namePart>
<namePart type="family">van der Werf</namePart>
<affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ</affiliation>
<affiliation>Leiden Observatory, Leiden University, PO Box 9513, NL ‐ 2300 RA Leiden, the Netherlands</affiliation>
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<namePart type="given">E.</namePart>
<namePart type="family">van Kampen</namePart>
<affiliation>European Southern Observatory, Karl‐Schwarzschild‐Strasse 2, D‐85748 Garching bei München, Germany</affiliation>
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<publisher>Blackwell Publishing Ltd</publisher>
<place>
<placeTerm type="text">Oxford, UK</placeTerm>
</place>
<dateIssued encoding="w3cdtf">2011-09-11</dateIssued>
<edition>Accepted 2011 March 29. Received 2011 March 17; in original form 2010 July 28</edition>
<copyrightDate encoding="w3cdtf">2011</copyrightDate>
</originInfo>
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<languageTerm type="code" authority="rfc3066">en</languageTerm>
<languageTerm type="code" authority="iso639-2b">eng</languageTerm>
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<extent unit="figures">13</extent>
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<abstract lang="en">We present a technique to identify optical counterparts of 250‐μm‐selected sources from the Herschel–ATLAS survey. Of the 6621 250 μm > 32‐mJy sources in our science demonstration catalogue we find that ∼60 per cent have counterparts brighter than r = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability R > 0.8. This is approximately 37 per cent of the full 250‐μm catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250‐μm‐selected Herschel–ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at z ≈ 0.25 ± 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the r‐band limit have z > 1. We also suggest a method for selecting populations of strongly lensed high‐redshift galaxies. Our identifications are matched to UV–NIR photometry from the GAMA survey, and these data are available as part of the Herschel–ATLAS public data release.</abstract>
<note type="content">*Herschel is an ESA space observatory with science instruments provided by European‐led Principal Investigator consortia and with important participation from NASA.</note>
<subject lang="en">
<genre>keywords</genre>
<topic>methods: statistical</topic>
<topic>submillimetre: galaxies</topic>
</subject>
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<title>Monthly Notices of the Royal Astronomical Society</title>
</titleInfo>
<genre type="journal">journal</genre>
<identifier type="ISSN">0035-8711</identifier>
<identifier type="eISSN">1365-2966</identifier>
<identifier type="DOI">10.1111/(ISSN)1365-2966</identifier>
<identifier type="PublisherID">MNR</identifier>
<part>
<date>2011</date>
<detail type="volume">
<caption>vol.</caption>
<number>416</number>
</detail>
<detail type="issue">
<caption>no.</caption>
<number>2</number>
</detail>
<extent unit="pages">
<start>857</start>
<end>872</end>
<total>16</total>
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<identifier type="DOI">10.1111/j.1365-2966.2011.18827.x</identifier>
<identifier type="ArticleID">MNR18827</identifier>
<accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</accessCondition>
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<recordOrigin>Blackwell Publishing Ltd</recordOrigin>
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