Fundamental constants and high‐resolution spectroscopy
Identifieur interne : 003E01 ( Main/Exploration ); précédent : 003E00; suivant : 003E02Fundamental constants and high‐resolution spectroscopy
Auteurs : P. Bonifacio [France] ; H. Rahmani [Inde] ; J. B. Whitmore [Australie] ; M. Wendt [Allemagne] ; M. Centurion [Italie] ; P. Molaro [Italie] ; R. Srianand [Inde] ; M. T. Murphy [Australie] ; P. Petitjean [France] ; I. I. Agafonova [Russie] ; S. D'Odorico [Allemagne] ; T. M. Evans [Australie] ; S. A. Levshakov [Russie] ; S. Lopez [Chili] ; C. J. A. P. Martins [Portugal] ; D. Reimers [Allemagne] ; G. Vladilo [Italie]Source :
- 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)
Url:
DOI: 10.1002/asna.201312005
Affiliations:
- Allemagne, Australie, Chili, France, Inde, Italie, Portugal, Russie
- Brandebourg, Hambourg, Île-de-France
- Hambourg, Meudon, Paris, Potsdam
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Levshakov</name><affiliation wicri:level="1"><country xml:lang="fr">Russie</country><wicri:regionArea>Ioffe Physical‐Technical Institute, Polytekhnicheskaya, Str. 26, 194021 Saint Petersburg</wicri:regionArea><wicri:noRegion>194021 Saint Petersburg</wicri:noRegion></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Russie</country><wicri:regionArea>St. Petersburg Electrotechnical University 'LETI', Prof. Popov Str. 5, 197376 St. Petersburg</wicri:regionArea><wicri:noRegion>197376 St. Petersburg</wicri:noRegion></affiliation></author><author><name sortKey="Lopez, S" sort="Lopez, S" uniqKey="Lopez S" first="S." last="Lopez">S. Lopez</name><affiliation wicri:level="1"><country xml:lang="fr">Chili</country><wicri:regionArea>Departamento de Astronomia, Universidad de Chile, Casilla 36‐D, Santiago</wicri:regionArea><wicri:noRegion>Santiago</wicri:noRegion></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 wicri:level="1"><country xml:lang="fr">Portugal</country><wicri:regionArea>Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150‐762 Porto</wicri:regionArea><wicri:noRegion>4150‐762 Porto</wicri:noRegion></affiliation></author><author><name sortKey="Reimers, D" sort="Reimers, D" uniqKey="Reimers D" first="D." last="Reimers">D. Reimers</name><affiliation wicri:level="1"><country xml:lang="fr">Allemagne</country><wicri:regionArea>Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg</wicri:regionArea><placeName><settlement type="city">Hambourg</settlement><region type="land" nuts="2">Hambourg</region></placeName></affiliation></author><author><name sortKey="Vladilo, G" sort="Vladilo, G" uniqKey="Vladilo G" first="G." last="Vladilo">G. Vladilo</name><affiliation wicri:level="1"><country xml:lang="fr">Italie</country><wicri:regionArea>Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste</wicri:regionArea><wicri:noRegion>34143 Trieste</wicri:noRegion></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><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>Chili</li><li>France</li><li>Inde</li><li>Italie</li><li>Portugal</li><li>Russie</li></country><region><li>Brandebourg</li><li>Hambourg</li><li>Île-de-France</li></region><settlement><li>Hambourg</li><li>Meudon</li><li>Paris</li><li>Potsdam</li></settlement></list><tree><country name="France"><region name="Île-de-France"><name sortKey="Bonifacio, P" sort="Bonifacio, P" uniqKey="Bonifacio P" first="P." last="Bonifacio">P. 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