Fundamental constants and high‐resolution spectroscopy
Identifieur interne : 001A60 ( Istex/Corpus ); précédent : 001A59; suivant : 001A61Fundamental constants and high‐resolution spectroscopy
Auteurs : P. Bonifacio ; H. Rahmani ; J. B. Whitmore ; M. Wendt ; M. Centurion ; P. Molaro ; R. Srianand ; M. T. Murphy ; P. Petitjean ; I. I. Agafonova ; S. D'Odorico ; T. M. Evans ; S. A. Levshakov ; S. Lopez ; C. J. A. P. Martins ; D. Reimers ; G. VladiloSource :
- Astronomische Nachrichten [ 0004-6337 ] ; 2014-01.
Abstract
Absorption‐line systems detected in high resolution quasar spectra can be used to compare the value of dimensionless fundamental constants such as the fine‐structure constant, α, and the proton‐to‐electron mass ratio, μ = mp/me, as measured in remote regions of the Universe to their value today on Earth. In recent years, some evidence has emerged of small temporal and also spatial variations in α on cosmological scales which may reach a fractional level of ≈ 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high‐resolution (R ≈ 60000) and high signal‐to‐noise ratio (S/N ≈ 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for Δα /α is obtained for the absorber at zabs = 1.6919 towards HE 2217‐2818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in α in this system is +1.3 ± 2.4stat ± 1.0sys ppm if Al II λ 1670 Å and three FeII transitions are used, and +1.1 ± 2.6stat ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on α ‐variation from an individual absorber and reveals no evidence for variation in α at the 3‐ppm precision level (1σ confidence). The expectation at this sky position of the recently‐reported dipolar variation of α is (3.2–5.4) ± 1.7 ppm depending on dipole model used and this constraint of Δα /α at face value is not supporting this expectation but not inconsistent with it at the 3σ level. For the proton‐to‐electron mass ratio the analysis of the H2 absorption lines of the zabs ≈ 2.4018 damped Lyα system towards HE 0027–1836 provides Δμ /μ = (–7.6 ± 8.1stat ± 6.3sys) ppm which is also consistent with a null variation. The cross‐correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter‐order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
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DOI: 10.1002/asna.201312005
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Evans</name><affiliation><mods:affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Levshakov, S A" sort="Levshakov, S A" uniqKey="Levshakov S" first="S. A." last="Levshakov">S. A. Levshakov</name><affiliation><mods:affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</mods:affiliation></affiliation><affiliation><mods:affiliation>St. Petersburg Electrotechnical University 'LETI', Prof. Popov Str. 5, 197376 St. Petersburg, Russia</mods:affiliation></affiliation></author><author><name sortKey="Lopez, S" sort="Lopez, S" uniqKey="Lopez S" first="S." last="Lopez">S. Lopez</name><affiliation><mods:affiliation>Departamento de Astronomia, Universidad de Chile, Casilla 36‐D, Santiago, Chile</mods:affiliation></affiliation></author><author><name sortKey="Martins, C J A P" sort="Martins, C J A P" uniqKey="Martins C" first="C. J. A. P." last="Martins">C. J. A. P. Martins</name><affiliation><mods:affiliation>Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150‐762 Porto, Portugal</mods:affiliation></affiliation></author><author><name sortKey="Reimers, D" sort="Reimers, D" uniqKey="Reimers D" first="D." last="Reimers">D. Reimers</name><affiliation><mods:affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</mods:affiliation></affiliation></author><author><name sortKey="Vladilo, G" sort="Vladilo, G" uniqKey="Vladilo G" first="G." last="Vladilo">G. Vladilo</name><affiliation><mods:affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:8CE857EC50B3A01C41C2725277EAD30FA29EC3A1</idno><date when="2014" year="2014">2014</date><idno type="doi">10.1002/asna.201312005</idno><idno type="url">https://api.istex.fr/document/8CE857EC50B3A01C41C2725277EAD30FA29EC3A1/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001A60</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001A60</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main" xml:lang="en">Fundamental constants and high‐resolution spectroscopy<ref type="note" target="#fn1"></ref></title><author><name sortKey="Bonifacio, P" sort="Bonifacio, P" uniqKey="Bonifacio P" first="P." last="Bonifacio">P. Bonifacio</name><affiliation><mods:affiliation>GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: Piercarlo.Bonifacio@obspm.fr</mods:affiliation></affiliation><affiliation><mods:affiliation>Correspondence address: GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</mods:affiliation></affiliation></author><author><name sortKey="Rahmani, H" sort="Rahmani, H" uniqKey="Rahmani H" first="H." last="Rahmani">H. Rahmani</name><affiliation><mods:affiliation>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India</mods:affiliation></affiliation></author><author><name sortKey="Whitmore, J B" sort="Whitmore, J B" uniqKey="Whitmore J" first="J. B." last="Whitmore">J. B. Whitmore</name><affiliation><mods:affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Wendt, M" sort="Wendt, M" uniqKey="Wendt M" first="M." last="Wendt">M. Wendt</name><affiliation><mods:affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>Institut für Physik und Astronomie, Universität Potsdam, 14476 Golm, Germany</mods:affiliation></affiliation></author><author><name sortKey="Centurion, M" sort="Centurion, M" uniqKey="Centurion M" first="M." last="Centurion">M. Centurion</name><affiliation><mods:affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</mods:affiliation></affiliation></author><author><name sortKey="Molaro, P" sort="Molaro, P" uniqKey="Molaro P" first="P." last="Molaro">P. Molaro</name><affiliation><mods:affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</mods:affiliation></affiliation></author><author><name sortKey="Srianand, R" sort="Srianand, R" uniqKey="Srianand R" first="R." last="Srianand">R. Srianand</name><affiliation><mods:affiliation>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India</mods:affiliation></affiliation></author><author><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name><affiliation><mods:affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Petitjean, P" sort="Petitjean, P" uniqKey="Petitjean P" first="P." last="Petitjean">P. Petitjean</name><affiliation><mods:affiliation>Universite Paris 6, Institut d'Astrophysique de Paris, CNRS UMR 7095, 98bis bd Arago, 75014 Paris, France</mods:affiliation></affiliation></author><author><name sortKey="Agafonova, I I" sort="Agafonova, I I" uniqKey="Agafonova I" first="I. I." last="Agafonova">I. I. Agafonova</name><affiliation><mods:affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</mods:affiliation></affiliation></author><author><name sortKey="D Odorico, S" sort="D Odorico, S" uniqKey="D Odorico S" first="S." last="D'Odorico">S. D'Odorico</name><affiliation><mods:affiliation>ESO Karl, Schwarzschild‐Str. 2 85741 Garching, Germany</mods:affiliation></affiliation></author><author><name sortKey="Evans, T M" sort="Evans, T M" uniqKey="Evans T" first="T. M." last="Evans">T. M. Evans</name><affiliation><mods:affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Levshakov, S A" sort="Levshakov, S A" uniqKey="Levshakov S" first="S. A." last="Levshakov">S. A. Levshakov</name><affiliation><mods:affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</mods:affiliation></affiliation><affiliation><mods:affiliation>St. Petersburg Electrotechnical University 'LETI', Prof. Popov Str. 5, 197376 St. Petersburg, Russia</mods:affiliation></affiliation></author><author><name sortKey="Lopez, S" sort="Lopez, S" uniqKey="Lopez S" first="S." last="Lopez">S. Lopez</name><affiliation><mods:affiliation>Departamento de Astronomia, Universidad de Chile, Casilla 36‐D, Santiago, Chile</mods:affiliation></affiliation></author><author><name sortKey="Martins, C J A P" sort="Martins, C J A P" uniqKey="Martins C" first="C. J. A. P." last="Martins">C. J. A. P. Martins</name><affiliation><mods:affiliation>Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150‐762 Porto, Portugal</mods:affiliation></affiliation></author><author><name sortKey="Reimers, D" sort="Reimers, D" uniqKey="Reimers D" first="D." last="Reimers">D. Reimers</name><affiliation><mods:affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</mods:affiliation></affiliation></author><author><name sortKey="Vladilo, G" sort="Vladilo, G" uniqKey="Vladilo G" first="G." last="Vladilo">G. Vladilo</name><affiliation><mods:affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Astronomische Nachrichten</title><title level="j" type="alt">ASTRONOMISCHE NACHRICHTEN</title><idno type="ISSN">0004-6337</idno><idno type="eISSN">1521-3994</idno><imprint><biblScope unit="vol">335</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="83">83</biblScope><biblScope unit="page" to="91">91</biblScope><biblScope unit="page-count">9</biblScope><publisher>WILEY‐VCH Verlag</publisher><pubPlace>Berlin</pubPlace><date type="published" when="2014-01">2014-01</date></imprint><idno type="ISSN">0004-6337</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0004-6337</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Absorption‐line systems detected in high resolution quasar spectra can be used to compare the value of dimensionless fundamental constants such as the fine‐structure constant, α, and the proton‐to‐electron mass ratio, μ = mp/me, as measured in remote regions of the Universe to their value today on Earth. In recent years, some evidence has emerged of small temporal and also spatial variations in α on cosmological scales which may reach a fractional level of ≈ 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high‐resolution (R ≈ 60000) and high signal‐to‐noise ratio (S/N ≈ 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for Δα /α is obtained for the absorber at zabs = 1.6919 towards HE 2217‐2818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in α in this system is +1.3 ± 2.4stat ± 1.0sys ppm if Al II λ 1670 Å and three FeII transitions are used, and +1.1 ± 2.6stat ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on α ‐variation from an individual absorber and reveals no evidence for variation in α at the 3‐ppm precision level (1σ confidence). The expectation at this sky position of the recently‐reported dipolar variation of α is (3.2–5.4) ± 1.7 ppm depending on dipole model used and this constraint of Δα /α at face value is not supporting this expectation but not inconsistent with it at the 3σ level. For the proton‐to‐electron mass ratio the analysis of the H2 absorption lines of the zabs ≈ 2.4018 damped Lyα system towards HE 0027–1836 provides Δμ /μ = (–7.6 ± 8.1stat ± 6.3sys) ppm which is also consistent with a null variation. The cross‐correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter‐order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>P. Bonifacio</name><affiliations><json:string>GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</json:string><json:string>E-mail: Piercarlo.Bonifacio@obspm.fr</json:string><json:string>Correspondence address: GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</json:string></affiliations></json:item><json:item><name>H. Rahmani</name><affiliations><json:string>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India</json:string></affiliations></json:item><json:item><name>J.B. Whitmore</name><affiliations><json:string>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>M. Wendt</name><affiliations><json:string>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</json:string><json:string>Institut für Physik und Astronomie, Universität Potsdam, 14476 Golm, Germany</json:string></affiliations></json:item><json:item><name>M. Centurion</name><affiliations><json:string>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</json:string></affiliations></json:item><json:item><name>P. Molaro</name><affiliations><json:string>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</json:string></affiliations></json:item><json:item><name>R. Srianand</name><affiliations><json:string>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India</json:string></affiliations></json:item><json:item><name>M.T. Murphy</name><affiliations><json:string>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>P. Petitjean</name><affiliations><json:string>Universite Paris 6, Institut d'Astrophysique de Paris, CNRS UMR 7095, 98bis bd Arago, 75014 Paris, France</json:string></affiliations></json:item><json:item><name>I.I. Agafonova</name><affiliations><json:string>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</json:string></affiliations></json:item><json:item><name>S. D'Odorico</name><affiliations><json:string>ESO Karl, Schwarzschild‐Str. 2 85741 Garching, Germany</json:string></affiliations></json:item><json:item><name>T.M. Evans</name><affiliations><json:string>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</json:string></affiliations></json:item><json:item><name>S.A. Levshakov</name><affiliations><json:string>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</json:string><json:string>St. Petersburg Electrotechnical University 'LETI', Prof. Popov Str. 5, 197376 St. Petersburg, Russia</json:string></affiliations></json:item><json:item><name>S. Lopez</name><affiliations><json:string>Departamento de Astronomia, Universidad de Chile, Casilla 36‐D, Santiago, Chile</json:string></affiliations></json:item><json:item><name>C.J.A.P. Martins</name><affiliations><json:string>Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150‐762 Porto, Portugal</json:string></affiliations></json:item><json:item><name>D. Reimers</name><affiliations><json:string>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</json:string></affiliations></json:item><json:item><name>G. Vladilo</name><affiliations><json:string>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>atomic processes</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>cosmology: observations</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>elementary particles</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>line: formation</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>quasars: absorption lines</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>techniques: spectroscopic</value></json:item></subject><articleId><json:string>ASNA201312005</json:string></articleId><arkIstex>ark:/67375/WNG-Q2J2KX52-G</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>Absorption‐line systems detected in high resolution quasar spectra can be used to compare the value of dimensionless fundamental constants such as the fine‐structure constant, α, and the proton‐to‐electron mass ratio, μ = mp/me, as measured in remote regions of the Universe to their value today on Earth. In recent years, some evidence has emerged of small temporal and also spatial variations in α on cosmological scales which may reach a fractional level of ≈ 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high‐resolution (R ≈ 60000) and high signal‐to‐noise ratio (S/N ≈ 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for Δα /α is obtained for the absorber at zabs = 1.6919 towards HE 2217‐2818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in α in this system is +1.3 ± 2.4stat ± 1.0sys ppm if Al II λ 1670 Å and three FeII transitions are used, and +1.1 ± 2.6stat ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on α ‐variation from an individual absorber and reveals no evidence for variation in α at the 3‐ppm precision level (1σ confidence). The expectation at this sky position of the recently‐reported dipolar variation of α is (3.2–5.4) ± 1.7 ppm depending on dipole model used and this constraint of Δα /α at face value is not supporting this expectation but not inconsistent with it at the 3σ level. For the proton‐to‐electron mass ratio the analysis of the H2 absorption lines of the zabs ≈ 2.4018 damped Lyα system towards HE 0027–1836 provides Δμ /μ = (–7.6 ± 8.1stat ± 6.3sys) ppm which is also consistent with a null variation. The cross‐correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter‐order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</abstract><qualityIndicators><score>10</score><pdfWordCount>6043</pdfWordCount><pdfCharCount>33621</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>9</pdfPageCount><pdfPageSize>595 x 842 pts (A4)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>407</abstractWordCount><abstractCharCount>2500</abstractCharCount><keywordCount>6</keywordCount></qualityIndicators><title>Fundamental constants and high‐resolution spectroscopy</title><genre><json:string>article</json:string></genre><host><title>Astronomische Nachrichten</title><language><json:string>unknown</json:string></language><doi><json:string>10.1002/(ISSN)1521-3994</json:string></doi><issn><json:string>0004-6337</json:string></issn><eissn><json:string>1521-3994</json:string></eissn><publisherId><json:string>ASNA</json:string></publisherId><volume>335</volume><issue>1</issue><pages><first>83</first><last>91</last><total>9</total></pages><genre><json:string>journal</json:string></genre><subject><json:item><value>Original Paper</value></json:item></subject></host><ark><json:string>ark:/67375/WNG-Q2J2KX52-G</json:string></ark><publicationDate>2014</publicationDate><copyrightDate>2014</copyrightDate><doi><json:string>10.1002/asna.201312005</json:string></doi><id>8CE857EC50B3A01C41C2725277EAD30FA29EC3A1</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/8CE857EC50B3A01C41C2725277EAD30FA29EC3A1/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/8CE857EC50B3A01C41C2725277EAD30FA29EC3A1/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/8CE857EC50B3A01C41C2725277EAD30FA29EC3A1/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main" xml:lang="en">Fundamental constants and high‐resolution spectroscopy<ref type="note" target="#fn1"></ref></title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>WILEY‐VCH Verlag</publisher><pubPlace>Berlin</pubPlace><availability><licence>Copyright © 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim</licence></availability><date type="published" when="2014-01"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main" xml:lang="en">Fundamental constants and high‐resolution spectroscopy<ref type="note" target="#fn1"></ref></title><title level="a" type="short" xml:lang="en">Fundamental constants and high‐resolution spectroscopy</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">P.</forename><surname>Bonifacio</surname></persName><email>Piercarlo.Bonifacio@obspm.fr</email><affiliation>GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France<address><country key="DE"></country></address></affiliation><affiliation>GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</affiliation></author><author xml:id="author-0001"><persName><forename type="first">H.</forename><surname>Rahmani</surname></persName><affiliation>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">J.B.</forename><surname>Whitmore</surname></persName><affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">M.</forename><surname>Wendt</surname></persName><affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany<address><country key="DE"></country></address></affiliation><affiliation>Institut für Physik und Astronomie, Universität Potsdam, 14476 Golm, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">M.</forename><surname>Centurion</surname></persName><affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">P.</forename><surname>Molaro</surname></persName><affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">R.</forename><surname>Srianand</surname></persName><affiliation>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">M.T.</forename><surname>Murphy</surname></persName><affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">P.</forename><surname>Petitjean</surname></persName><affiliation>Universite Paris 6, Institut d'Astrophysique de Paris, CNRS UMR 7095, 98bis bd Arago, 75014 Paris, France<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">I.I.</forename><surname>Agafonova</surname></persName><affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">S.</forename><surname>D'Odorico</surname></persName><affiliation>ESO Karl, Schwarzschild‐Str. 2 85741 Garching, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0011"><persName><forename type="first">T.M.</forename><surname>Evans</surname></persName><affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0012"><persName><forename type="first">S.A.</forename><surname>Levshakov</surname></persName><affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia<address><country key="DE"></country></address></affiliation><affiliation>St. Petersburg Electrotechnical University 'LETI', Prof. Popov Str. 5, 197376 St. Petersburg, Russia<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">S.</forename><surname>Lopez</surname></persName><affiliation>Departamento de Astronomia, Universidad de Chile, Casilla 36‐D, Santiago, Chile<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0014"><persName><forename type="first">C.J.A.P.</forename><surname>Martins</surname></persName><affiliation>Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150‐762 Porto, Portugal<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0015"><persName><forename type="first">D.</forename><surname>Reimers</surname></persName><affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0016"><persName><forename type="first">G.</forename><surname>Vladilo</surname></persName><affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy<address><country key="DE"></country></address></affiliation></author><idno type="istex">8CE857EC50B3A01C41C2725277EAD30FA29EC3A1</idno><idno type="ark">ark:/67375/WNG-Q2J2KX52-G</idno><idno type="DOI">10.1002/asna.201312005</idno><idno type="unit">ASNA201312005</idno><idno type="toTypesetVersion">file:ASNA.ASNA201312005.pdf</idno></analytic><monogr><title level="j" type="main">Astronomische Nachrichten</title><title level="j" type="alt">ASTRONOMISCHE NACHRICHTEN</title><idno type="pISSN">0004-6337</idno><idno type="eISSN">1521-3994</idno><idno type="book-DOI">10.1002/(ISSN)1521-3994</idno><idno type="book-part-DOI">10.1002/asna.v335.1</idno><idno type="product">ASNA</idno><imprint><biblScope unit="vol">335</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="83">83</biblScope><biblScope unit="page" to="91">91</biblScope><biblScope unit="page-count">9</biblScope><publisher>WILEY‐VCH Verlag</publisher><pubPlace>Berlin</pubPlace><date type="published" when="2014-01"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>Abstract</head><p>Absorption‐line systems detected in high resolution quasar spectra can be used to compare the value of dimensionless fundamental constants such as the fine‐structure constant, <hi rend="italic">α</hi>, and the proton‐to‐electron mass ratio, <hi rend="italic">μ</hi> = m<hi rend="subscript">p</hi>/m<hi rend="subscript">e</hi>, as measured in remote regions of the Universe to their value today on Earth. In recent years, some evidence has emerged of small temporal and also spatial variations in <hi rend="italic">α</hi> on cosmological scales which may reach a fractional level of ≈ 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high‐resolution (<hi rend="italic">R</hi> ≈ 60000) and high signal‐to‐noise ratio (S/N ≈ 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for Δ<hi rend="italic">α</hi> /<hi rend="italic">α</hi> is obtained for the absorber at <hi rend="italic">z</hi><hi rend="subscript">abs</hi> = 1.6919 towards HE 2217‐2818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in <hi rend="italic">α</hi> in this system is +1.3 ± 2.4<hi rend="subscript">stat</hi> ± 1.0<hi rend="subscript">sys</hi> ppm if Al II <hi rend="italic">λ</hi> 1670 Å and three FeII transitions are used, and +1.1 ± 2.6<hi rend="subscript">stat</hi> ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on <hi rend="italic">α</hi> ‐variation from an individual absorber and reveals no evidence for variation in <hi rend="italic">α</hi> at the 3‐ppm precision level (1<hi rend="italic">σ</hi> confidence). The expectation at this sky position of the recently‐reported dipolar variation of <hi rend="italic">α</hi> is (3.2–5.4) ± 1.7 ppm depending on dipole model used and this constraint of Δ<hi rend="italic">α</hi> /<hi rend="italic">α</hi> at face value is not supporting this expectation but not inconsistent with it at the 3<hi rend="italic">σ</hi> level. For the proton‐to‐electron mass ratio the analysis of the H<hi rend="subscript">2</hi> absorption lines of the <hi rend="italic">z</hi><hi rend="subscript">abs</hi> ≈ 2.4018 damped Ly<hi rend="italic">α</hi> system towards HE 0027–1836 provides Δ<hi rend="italic">μ</hi> /<hi rend="italic">μ</hi> = (–7.6 ± 8.1<hi rend="subscript">stat</hi> ± 6.3<hi rend="subscript">sys</hi>) ppm which is also consistent with a null variation. The cross‐correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter‐order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</p></abstract><textClass><keywords xml:lang="en"><term xml:id="kwd1">atomic processes</term><term xml:id="kwd2">cosmology: observations</term><term xml:id="kwd3">elementary particles</term><term xml:id="kwd4">line: formation</term><term xml:id="kwd5">quasars: absorption lines</term><term xml:id="kwd6">techniques: spectroscopic</term></keywords><keywords rend="articleCategory"><term>Original Paper</term></keywords><keywords rend="tocHeading1"><term>Original Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>WILEY‐VCH Verlag</publisherName><publisherLoc>Berlin</publisherLoc></publisherInfo><doi registered="yes">10.1002/(ISSN)1521-3994</doi><issn type="print">0004-6337</issn><issn type="electronic">1521-3994</issn><idGroup><id type="product" value="ASNA"></id></idGroup><titleGroup><title type="main" xml:lang="en" sort="ASTRONOMISCHE NACHRICHTEN">Astronomische Nachrichten</title><title type="short">Astron. 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In recent years, some evidence has emerged of small temporal and also spatial variations in <i>α</i> on cosmological scales which may reach a fractional level of ≈ 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high‐resolution (<i>R</i> ≈ 60000) and high signal‐to‐noise ratio (S/N ≈ 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for Δ<i>α</i> /<i>α</i> is obtained for the absorber at <i>z</i><sub>abs</sub> = 1.6919 towards HE 2217‐2818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in <i>α</i> in this system is +1.3 ± 2.4<sub>stat</sub> ± 1.0<sub>sys</sub> ppm if Al II <i>λ</i> 1670 Å and three FeII transitions are used, and +1.1 ± 2.6<sub>stat</sub> ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on <i>α</i> ‐variation from an individual absorber and reveals no evidence for variation in <i>α</i> at the 3‐ppm precision level (1<i>σ</i> confidence). The expectation at this sky position of the recently‐reported dipolar variation of <i>α</i> is (3.2–5.4) ± 1.7 ppm depending on dipole model used and this constraint of Δ<i>α</i> /<i>α</i> at face value is not supporting this expectation but not inconsistent with it at the 3<i>σ</i> level. For the proton‐to‐electron mass ratio the analysis of the H<sub>2</sub> absorption lines of the <i>z</i><sub>abs</sub> ≈ 2.4018 damped Ly<i>α</i> system towards HE 0027–1836 provides Δ<i>μ</i> /<i>μ</i> = (–7.6 ± 8.1<sub>stat</sub> ± 6.3<sub>sys</sub>) ppm which is also consistent with a null variation. The cross‐correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter‐order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</p></abstract></abstractGroup></contentMeta><noteGroup><note xml:id="fn1"><p>Based on observations obtained with UVES at the the 8.2 m Kueyen ESO telescope programme L185.A‐0745.</p></note></noteGroup></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Fundamental constants and high‐resolution spectroscopy</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Fundamental constants and high‐resolution spectroscopy</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Fundamental constants and high‐resolution spectroscopy</title></titleInfo><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Bonifacio</namePart><affiliation>GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</affiliation><affiliation>E-mail: Piercarlo.Bonifacio@obspm.fr</affiliation><affiliation>Correspondence address: GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, 92190 Meudon, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Rahmani</namePart><affiliation>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.B.</namePart><namePart type="family">Whitmore</namePart><affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Wendt</namePart><affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</affiliation><affiliation>Institut für Physik und Astronomie, Universität Potsdam, 14476 Golm, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Centurion</namePart><affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Molaro</namePart><affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Srianand</namePart><affiliation>Inter‐University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.T.</namePart><namePart type="family">Murphy</namePart><affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Petitjean</namePart><affiliation>Universite Paris 6, Institut d'Astrophysique de Paris, CNRS UMR 7095, 98bis bd Arago, 75014 Paris, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">I.I.</namePart><namePart type="family">Agafonova</namePart><affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">D'Odorico</namePart><affiliation>ESO Karl, Schwarzschild‐Str. 2 85741 Garching, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.M.</namePart><namePart type="family">Evans</namePart><affiliation>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.A.</namePart><namePart type="family">Levshakov</namePart><affiliation>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg, Russia</affiliation><affiliation>St. Petersburg Electrotechnical University 'LETI', Prof. Popov Str. 5, 197376 St. Petersburg, Russia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Lopez</namePart><affiliation>Departamento de Astronomia, Universidad de Chile, Casilla 36‐D, Santiago, Chile</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C.J.A.P.</namePart><namePart type="family">Martins</namePart><affiliation>Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150‐762 Porto, Portugal</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Reimers</namePart><affiliation>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Vladilo</namePart><affiliation>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>WILEY‐VCH Verlag</publisher><place><placeTerm type="text">Berlin</placeTerm></place><dateIssued encoding="w3cdtf">2014-01</dateIssued><dateCaptured encoding="w3cdtf">2013-08-29</dateCaptured><dateValid encoding="w3cdtf">2013-11-01</dateValid><copyrightDate encoding="w3cdtf">2014</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">4</extent><extent unit="tables">2</extent><extent unit="references">56</extent></physicalDescription><abstract lang="en">Absorption‐line systems detected in high resolution quasar spectra can be used to compare the value of dimensionless fundamental constants such as the fine‐structure constant, α, and the proton‐to‐electron mass ratio, μ = mp/me, as measured in remote regions of the Universe to their value today on Earth. In recent years, some evidence has emerged of small temporal and also spatial variations in α on cosmological scales which may reach a fractional level of ≈ 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high‐resolution (R ≈ 60000) and high signal‐to‐noise ratio (S/N ≈ 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for Δα /α is obtained for the absorber at zabs = 1.6919 towards HE 2217‐2818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in α in this system is +1.3 ± 2.4stat ± 1.0sys ppm if Al II λ 1670 Å and three FeII transitions are used, and +1.1 ± 2.6stat ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on α ‐variation from an individual absorber and reveals no evidence for variation in α at the 3‐ppm precision level (1σ confidence). The expectation at this sky position of the recently‐reported dipolar variation of α is (3.2–5.4) ± 1.7 ppm depending on dipole model used and this constraint of Δα /α at face value is not supporting this expectation but not inconsistent with it at the 3σ level. For the proton‐to‐electron mass ratio the analysis of the H2 absorption lines of the zabs ≈ 2.4018 damped Lyα system towards HE 0027–1836 provides Δμ /μ = (–7.6 ± 8.1stat ± 6.3sys) ppm which is also consistent with a null variation. The cross‐correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter‐order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</abstract><note type="content">*Based on observations obtained with UVES at the the 8.2 m Kueyen ESO telescope programme L185.A‐0745.</note><note type="funding">Conseil Scientifique de l'Observatoire de Paris</note><note type="funding">grant DFG Sonderforschungsbereich SFB 676 Teilprojekt C4</note><note type="funding">grant PTDC/FIS/111725/2009 from FCT (Portugal)</note><note type="funding">FCT Research Professorship, contract reference IF/00064/2012</note><note type="funding">Australian Research Council for funding under the Discovery Projects scheme (DP110100866)</note><subject lang="en"><genre>keywords</genre><topic>atomic processes</topic><topic>cosmology: observations</topic><topic>elementary particles</topic><topic>line: formation</topic><topic>quasars: absorption lines</topic><topic>techniques: spectroscopic</topic></subject><relatedItem type="host"><titleInfo><title>Astronomische Nachrichten</title></titleInfo><titleInfo type="abbreviated"><title>Astron. Nachr.</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><subject><genre>article-category</genre><topic>Original Paper</topic></subject><identifier type="ISSN">0004-6337</identifier><identifier type="eISSN">1521-3994</identifier><identifier type="DOI">10.1002/(ISSN)1521-3994</identifier><identifier type="PublisherID">ASNA</identifier><part><date>2014</date><detail type="volume"><caption>vol.</caption><number>335</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>83</start><end>91</end><total>9</total></extent></part></relatedItem><identifier type="istex">8CE857EC50B3A01C41C2725277EAD30FA29EC3A1</identifier><identifier type="ark">ark:/67375/WNG-Q2J2KX52-G</identifier><identifier type="DOI">10.1002/asna.201312005</identifier><identifier type="ArticleID">ASNA201312005</identifier><accessCondition type="use and reproduction" contentType="copyright">Copyright © 2014 WILEY‐VCH Verlag GmbH & Co. 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