The Palo Verde reactor neutrino oscillation experiment
Identifieur interne : 000432 ( Main/Corpus ); précédent : 000431; suivant : 000433The Palo Verde reactor neutrino oscillation experiment
Auteurs : F. Boehm ; J. Busenitz ; M. Dugger ; G. Gratta ; J. Hanson ; H. Henrikson ; J. Kornis ; D. Lawrence ; K. B. Lee ; D. Michael ; L. Miller ; V. M. Novikov ; A. Piepke ; B. Ritchie ; D. Tracy ; A. Vital ; P. Vogel ; Y. F. Wang ; J. WolfSource :
- Nuclear Physics B (Proceedings Supplements) [ 0920-5632 ] ; 1999.
Abstract
Our collaboration is operating a segmented scintillation detector, containing 11.3 tons of 0.1% Gd loaded liquid scintillator, at 750, 888 and 889 m distance from three nuclear power reactors. Goal of the experiment is to search for neutrino oscillations in disappearance mode. The anti-neutrino capture on the proton serves as detection reaction. The experiment is expected to reach a sensitivity of Δm2 > 1.3 · 10−3 eV2 and sin22Θ > 0.1. Our range of sensitivity is tuned to test the νμ ↔ νe solution of the atmospheric neutrino anomaly as reported by the Kamiokande experiment. Assembly of the detector in an underground lab, with 32 mw.e. effective overburden, is completed. Since June 1998 we are taking data a full reactor power. Detector design and performance are discussed.
Url:
DOI: 10.1016/S0920-5632(99)00413-2
Links to Exploration step
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Vital</name><affiliation><mods:affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</mods:affiliation></affiliation></author><author><name sortKey="Vogel, P" sort="Vogel, P" uniqKey="Vogel P" first="P." last="Vogel">P. Vogel</name><affiliation><mods:affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Wang, Y F" sort="Wang, Y F" uniqKey="Wang Y" first="Y. F." last="Wang">Y. F. Wang</name><affiliation><mods:affiliation>Physics Department, Stanford University, Stanford CA 94305, USA</mods:affiliation></affiliation></author><author><name sortKey="Wolf, J" sort="Wolf, J" uniqKey="Wolf J" first="J." last="Wolf">J. Wolf</name><affiliation><mods:affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Nuclear Physics B (Proceedings Supplements)</title><title level="j" type="abbrev">NUPHBP</title><idno type="ISSN">0920-5632</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1999">1999</date><biblScope unit="volume">77</biblScope><biblScope unit="issue">1–3</biblScope><biblScope unit="page" from="166">166</biblScope><biblScope unit="page" to="170">170</biblScope></imprint><idno type="ISSN">0920-5632</idno></series><idno type="istex">917D20C2E23FA57CC9E5B314D9900A0D19A5B6E5</idno><idno type="DOI">10.1016/S0920-5632(99)00413-2</idno><idno type="PII">S0920-5632(99)00413-2</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0920-5632</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Our collaboration is operating a segmented scintillation detector, containing 11.3 tons of 0.1% Gd loaded liquid scintillator, at 750, 888 and 889 m distance from three nuclear power reactors. Goal of the experiment is to search for neutrino oscillations in disappearance mode. The anti-neutrino capture on the proton serves as detection reaction. The experiment is expected to reach a sensitivity of Δm2 > 1.3 · 10−3 eV2 and sin22Θ > 0.1. Our range of sensitivity is tuned to test the νμ ↔ νe solution of the atmospheric neutrino anomaly as reported by the Kamiokande experiment. Assembly of the detector in an underground lab, with 32 mw.e. effective overburden, is completed. Since June 1998 we are taking data a full reactor power. Detector design and performance are discussed.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>F. Boehm</name><affiliations><json:string>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</json:string></affiliations></json:item><json:item><name>J. 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Novikov</name><affiliations><json:string>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</json:string></affiliations></json:item><json:item><name>A. Piepke</name><affiliations><json:string>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</json:string></affiliations></json:item><json:item><name>B. Ritchie</name><affiliations><json:string>Physics Department, Arizona State University, Tempe AZ 85287, USA</json:string></affiliations></json:item><json:item><name>D. Tracy</name><affiliations><json:string>Physics Department, Stanford University, Stanford CA 94305, USA</json:string></affiliations></json:item><json:item><name>A. Vital</name><affiliations><json:string>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</json:string></affiliations></json:item><json:item><name>P. Vogel</name><affiliations><json:string>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</json:string></affiliations></json:item><json:item><name>Y.F. Wang</name><affiliations><json:string>Physics Department, Stanford University, Stanford CA 94305, USA</json:string></affiliations></json:item><json:item><name>J. Wolf</name><affiliations><json:string>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>Part 4. Long baseline experiments</value></json:item></subject><language><json:string>eng</json:string></language><originalGenre><json:string>Full-length article</json:string></originalGenre><abstract>Our collaboration is operating a segmented scintillation detector, containing 11.3 tons of 0.1% Gd loaded liquid scintillator, at 750, 888 and 889 m distance from three nuclear power reactors. 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USA</affiliation></author><author xml:id="author-18"><persName><forename type="first">Y.F.</forename><surname>Wang</surname></persName><affiliation>Physics Department, Stanford University, Stanford CA 94305, USA</affiliation></author><author xml:id="author-19"><persName><forename type="first">J.</forename><surname>Wolf</surname></persName><affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</affiliation></author></analytic><monogr><title level="j">Nuclear Physics B (Proceedings Supplements)</title><title level="j" type="abbrev">NUPHBP</title><idno type="pISSN">0920-5632</idno><idno type="PII">S0920-5632(00)X0038-2</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1999"></date><biblScope unit="volume">77</biblScope><biblScope unit="issue">1–3</biblScope><biblScope unit="page" from="166">166</biblScope><biblScope unit="page" to="170">170</biblScope></imprint></monogr><idno type="istex">917D20C2E23FA57CC9E5B314D9900A0D19A5B6E5</idno><idno type="DOI">10.1016/S0920-5632(99)00413-2</idno><idno type="PII">S0920-5632(99)00413-2</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>1999</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>Our collaboration is operating a segmented scintillation detector, containing 11.3 tons of 0.1% Gd loaded liquid scintillator, at 750, 888 and 889 m distance from three nuclear power reactors. Goal of the experiment is to search for neutrino oscillations in disappearance mode. The anti-neutrino capture on the proton serves as detection reaction. The experiment is expected to reach a sensitivity of Δm2 > 1.3 · 10−3 eV2 and sin22Θ > 0.1. Our range of sensitivity is tuned to test the νμ ↔ νe solution of the atmospheric neutrino anomaly as reported by the Kamiokande experiment. Assembly of the detector in an underground lab, with 32 mw.e. effective overburden, is completed. Since June 1998 we are taking data a full reactor power. Detector design and performance are discussed.</p></abstract><textClass><keywords scheme="keyword"><list><head>article-category</head><item><term>Part 4. Long baseline experiments</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="1999">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/917D20C2E23FA57CC9E5B314D9900A0D19A5B6E5/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Elsevier, elements deleted: tail"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//ES//DTD journal article DTD version 4.5.2//EN//XML" URI="art452.dtd" name="istex:docType"></istex:docType><istex:document><converted-article version="4.5.2" docsubtype="fla"><item-info><jid>NUPHBP</jid><aid>99004132</aid><ce:pii>S0920-5632(99)00413-2</ce:pii><ce:doi>10.1016/S0920-5632(99)00413-2</ce:doi><ce:copyright type="unknown" year="1999"></ce:copyright><ce:doctopics><ce:doctopic><ce:text>Part 4. Long baseline experiments</ce:text></ce:doctopic></ce:doctopics></item-info><head><ce:title>The Palo Verde reactor neutrino oscillation experiment</ce:title><ce:presented>Presented by Andreas Piepke on behalf of the Palo Verde Collaboration</ce:presented><ce:author-group><ce:author><ce:given-name>F.</ce:given-name><ce:surname>Boehm</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>J.</ce:given-name><ce:surname>Busenitz</ce:surname><ce:cross-ref refid="AFF2"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>M.</ce:given-name><ce:surname>Dugger</ce:surname><ce:cross-ref refid="AFF3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>G.</ce:given-name><ce:surname>Gratta</ce:surname><ce:cross-ref refid="AFF4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>J.</ce:given-name><ce:surname>Hanson</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>H.</ce:given-name><ce:surname>Henrikson</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>J.</ce:given-name><ce:surname>Kornis</ce:surname><ce:cross-ref refid="AFF2"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>D.</ce:given-name><ce:surname>Lawrence</ce:surname><ce:cross-ref refid="AFF3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>K.B.</ce:given-name><ce:surname>Lee</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>D.</ce:given-name><ce:surname>Michael</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>L.</ce:given-name><ce:surname>Miller</ce:surname><ce:cross-ref refid="AFF4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>V.M.</ce:given-name><ce:surname>Novikov</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>A.</ce:given-name><ce:surname>Piepke</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>B.</ce:given-name><ce:surname>Ritchie</ce:surname><ce:cross-ref refid="AFF3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>D.</ce:given-name><ce:surname>Tracy</ce:surname><ce:cross-ref refid="AFF4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>A.</ce:given-name><ce:surname>Vital</ce:surname><ce:cross-ref refid="AFF2"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>P.</ce:given-name><ce:surname>Vogel</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Y.F.</ce:given-name><ce:surname>Wang</ce:surname><ce:cross-ref refid="AFF4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>J.</ce:given-name><ce:surname>Wolf</ce:surname><ce:cross-ref refid="AFF2"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="AFF1"><ce:label>a</ce:label><ce:textfn>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</ce:textfn></ce:affiliation><ce:affiliation id="AFF2"><ce:label>b</ce:label><ce:textfn>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</ce:textfn></ce:affiliation><ce:affiliation id="AFF3"><ce:label>c</ce:label><ce:textfn>Physics Department, Arizona State University, Tempe AZ 85287, USA</ce:textfn></ce:affiliation><ce:affiliation id="AFF4"><ce:label>d</ce:label><ce:textfn>Physics Department, Stanford University, Stanford CA 94305, USA</ce:textfn></ce:affiliation></ce:author-group><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>Our collaboration is operating a segmented scintillation detector, containing 11.3 tons of 0.1% Gd loaded liquid scintillator, at 750, 888 and 889 m distance from three nuclear power reactors. Goal of the experiment is to search for neutrino oscillations in disappearance mode. The anti-neutrino capture on the proton serves as detection reaction. The experiment is expected to reach a sensitivity of <ce:italic>Δm</ce:italic><ce:sup>2</ce:sup> > 1.3 · 10<ce:sup>−3</ce:sup> eV<ce:sup>2</ce:sup> and <ce:italic>sin</ce:italic><ce:sup>2</ce:sup>2Θ > 0.1. Our range of sensitivity is tuned to test the <ce:italic>ν</ce:italic><ce:inf><ce:italic>μ</ce:italic></ce:inf> ↔ <ce:italic>ν</ce:italic><ce:inf><ce:italic>e</ce:italic></ce:inf> solution of the atmospheric neutrino anomaly as reported by the Kamiokande experiment. Assembly of the detector in an underground lab, with 32 mw.e. effective overburden, is completed. Since June 1998 we are taking data a full reactor power. Detector design and performance are discussed.</ce:simple-para></ce:abstract-sec></ce:abstract></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>The Palo Verde reactor neutrino oscillation experiment</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>The Palo Verde reactor neutrino oscillation experiment</title></titleInfo><name type="personal"><namePart type="given">F.</namePart><namePart type="family">Boehm</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Busenitz</namePart><affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Dugger</namePart><affiliation>Physics Department, Arizona State University, Tempe AZ 85287, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Gratta</namePart><affiliation>Physics Department, Stanford University, Stanford CA 94305, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Hanson</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Henrikson</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Kornis</namePart><affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Lawrence</namePart><affiliation>Physics Department, Arizona State University, Tempe AZ 85287, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K.B.</namePart><namePart type="family">Lee</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Michael</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="family">Miller</namePart><affiliation>Physics Department, Stanford University, Stanford CA 94305, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">V.M.</namePart><namePart type="family">Novikov</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Piepke</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B.</namePart><namePart type="family">Ritchie</namePart><affiliation>Physics Department, Arizona State University, Tempe AZ 85287, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Tracy</namePart><affiliation>Physics Department, Stanford University, Stanford CA 94305, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Vital</namePart><affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Vogel</namePart><affiliation>Division of Physics and Astronomy, Caltech, Pasadena CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Y.F.</namePart><namePart type="family">Wang</namePart><affiliation>Physics Department, Stanford University, Stanford CA 94305, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Wolf</namePart><affiliation>Department of Physics and Astronomy, University of Alabama, Tuscaloosa AL 35487, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="Full-length article"></genre><originInfo><publisher>ELSEVIER</publisher><dateIssued encoding="w3cdtf">1999</dateIssued><copyrightDate encoding="w3cdtf">1999</copyrightDate></originInfo><language><languageTerm type="code" authority="iso639-2b">eng</languageTerm><languageTerm type="code" authority="rfc3066">en</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract lang="en">Our collaboration is operating a segmented scintillation detector, containing 11.3 tons of 0.1% Gd loaded liquid scintillator, at 750, 888 and 889 m distance from three nuclear power reactors. Goal of the experiment is to search for neutrino oscillations in disappearance mode. The anti-neutrino capture on the proton serves as detection reaction. The experiment is expected to reach a sensitivity of Δm2 > 1.3 · 10−3 eV2 and sin22Θ > 0.1. Our range of sensitivity is tuned to test the νμ ↔ νe solution of the atmospheric neutrino anomaly as reported by the Kamiokande experiment. Assembly of the detector in an underground lab, with 32 mw.e. effective overburden, is completed. Since June 1998 we are taking data a full reactor power. Detector design and performance are discussed.</abstract><subject><genre>article-category</genre><topic>Part 4. 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