Cosmic dynamics in the era of Extremely Large Telescopes
Identifieur interne : 008859 ( Main/Exploration ); précédent : 008858; suivant : 008860Cosmic dynamics in the era of Extremely Large Telescopes
Auteurs : J. Liske [Allemagne] ; A. Grazian [Italie] ; E. Vanzella [Italie] ; M. Dessauges [Suisse] ; M. Viel [Italie, Royaume-Uni] ; L. Pasquini [Allemagne] ; M. Haehnelt [Royaume-Uni] ; S. Cristiani [Italie] ; F. Pepe [Suisse] ; G. Avila [Allemagne] ; P. Bonifacio [Italie, France] ; F. Bouchy [France] ; H. Dekker [Allemagne] ; B. Delabre [Allemagne] ; S. D'Odorico [Allemagne] ; V. D'Odorico [Italie] ; S. Levshakov [Russie] ; C. Lovis [Suisse] ; M. Mayor [Suisse] ; P. Molaro [Italie] ; L. Moscardini [Italie] ; M. T. Murphy [Royaume-Uni, Australie] ; D. Queloz [Suisse] ; P. Shaver [Allemagne] ; S. Udry [Suisse] ; T. Wiklind [États-Unis] ; S. Zucker [Israël]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-05-21.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Cosmologie, Simulation.
English descriptors
- KwdEn :
- Absorber, Absorption line, Absorption line lists, Absorption lines, Adelberger, Aguirre, Alternative models, Atness, Available metal lines, Blue dots, Brightness distribution, Cardassian, Colour, Column density, Comoving, Constraint, Cosmic dynamics, Cosmological, Cosmological model, Cosmological redshift, Cosmology, Dark energy, Different redshifts, Doppler shift, Dtobs, Dynamics, Ellipse, Emission lines, Equal time allocation, Expansion history, Forest line lists, Forest region, Forest spectrum, Form factor, Friedman, Friedman equation, Galactic feedback, General relativity, Gnedin, Grid, Haehnelt, Hashed region, High redshift, Hubble, Integration time, Intergalactic matter, Journal compilation, Large telescopes, Late times, Lett, Linder, Line lists, Liske, Lower limit, Lyman alpha forest, Metal lines, Metric, Mnras, Models, Monte Carlo methods, Nqso, Optical depth, Other hand, Other methods, Overall accuracy, Overall value, Parameter, Parameter space, Peculiar acceleration, Peculiar motion, Peculiar motions, Peculiar velocities, Peculiar velocity, Photometry, Photon, Photon noise, Phys, Physical properties, Pixel, Pixel size, Previous section, Qsos, Quasars, Quintessence, Radial velocity shifts, Rauch, Real line lists, Red shift, Redshift, Redshift bins, Redshift difference, Redshift drift, Redshift drift experiment, Redshift evolution, Redshift range, Schaye, Sdss, Signal-to-noise ratio, Simcoe, Simulation, Snia, Solid line, Spectral features, Steidel, Target selection, Theuns, Tobs, Total integration time, Universal expansion, Universe expansion, Velocity shift, Viel, Weak lensing, Zhang, Zqso.
- Teeft :
- Absorber, Absorption line lists, Absorption lines, Adelberger, Aguirre, Alternative models, Atness, Available metal lines, Blue dots, Cardassian, Colour, Column density, Comoving, Constraint, Cosmic dynamics, Cosmological, Cosmological model, Dark energy, Different redshifts, Doppler shift, Dtobs, Ellipse, Emission lines, Equal time allocation, Expansion history, Forest line lists, Forest region, Forest spectrum, Form factor, Friedman, Friedman equation, Galactic feedback, General relativity, Gnedin, Grid, Haehnelt, Hashed region, High redshift, Hubble, Integration time, Journal compilation, Large telescopes, Late times, Lett, Linder, Line lists, Liske, Lower limit, Metal lines, Metric, Mnras, Nqso, Optical depth, Other hand, Other methods, Overall accuracy, Overall value, Parameter, Parameter space, Peculiar acceleration, Peculiar motion, Peculiar motions, Peculiar velocities, Peculiar velocity, Photometry, Photon, Photon noise, Phys, Physical properties, Pixel, Pixel size, Previous section, Qsos, Quintessence, Radial velocity shifts, Rauch, Real line lists, Redshift, Redshift bins, Redshift difference, Redshift drift, Redshift drift experiment, Redshift evolution, Redshift range, Schaye, Sdss, Simcoe, Simulation, Snia, Solid line, Spectral features, Steidel, Target selection, Theuns, Tobs, Total integration time, Universal expansion, Velocity shift, Viel, Weak lensing, Zhang, Zqso.
Abstract
The redshifts of all cosmologically distant sources are expected to experience a small, systematic drift as a function of time due to the evolution of the Universe's expansion rate. A measurement of this effect would represent a direct and entirely model‐independent determination of the expansion history of the Universe over a redshift range that is inaccessible to other methods. Here we investigate the impact of the next generation of Extremely Large Telescopes on the feasibility of detecting and characterizing the cosmological redshift drift. We consider the Lyα forest in the redshift range 2 < z < 5 and other absorption lines in the spectra of high‐redshift QSOs as the most suitable targets for a redshift drift experiment. Assuming photon‐noise‐limited observations and using extensive Monte Carlo simulations we determine the accuracy to which the redshift drift can be measured from the Lyα forest as a function of signal‐to‐noise ratio and redshift. Based on this relation and using the brightness and redshift distributions of known QSOs we find that a 42‐m telescope is capable of unambiguously detecting the redshift drift over a period of ∼20 yr using 4000 h of observing time. Such an experiment would provide independent evidence for the existence of dark energy without assuming spatial flatness, using any other cosmological constraints or making any other astrophysical assumption.
Url:
- https://api.istex.fr/document/64EBFEC6FCD1141D09AD31FF17F738AA98D21BE5/fulltext/pdf
- https://api.istex.fr/document/B5997F64EE928B24A12DFB080E997ED33636870D/fulltext/pdf
DOI: 10.1111/j.1365-2966.2008.13090.x
Affiliations:
- Allemagne, Australie, France, Israël, Italie, Royaume-Uni, Russie, Suisse, États-Unis
- Angleterre, Angleterre de l'Est, Latium, Maryland, Provence-Alpes-Côte d'Azur, Émilie-Romagne, Île-de-France
- Bologne, Cambridge, Marseille, Meudon, Rome
- Université de Bologne, Université de Cambridge
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Le document en format XML
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Levshakov</name><affiliation wicri:level="1"><country xml:lang="fr">Russie</country><wicri:regionArea>Department of Theoretical Astrophysics, Ioffe Physico‐Technical Institute, 194021 St Petersburg</wicri:regionArea><wicri:noRegion>194021 St Petersburg</wicri:noRegion></affiliation></author><author><name sortKey="Lovis, C" sort="Lovis, C" uniqKey="Lovis C" first="C." last="Lovis">C. Lovis</name><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny</wicri:regionArea><wicri:noRegion>1290 Sauverny</wicri:noRegion></affiliation></author><author><name sortKey="Mayor, M" sort="Mayor, M" uniqKey="Mayor M" first="M." last="Mayor">M. Mayor</name><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny</wicri:regionArea><wicri:noRegion>1290 Sauverny</wicri:noRegion></affiliation></author><author><name sortKey="Molaro, P" sort="Molaro, P" uniqKey="Molaro P" first="P." last="Molaro">P. Molaro</name><affiliation wicri:level="1"><country xml:lang="fr">Italie</country><wicri:regionArea>INAF – Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143 Trieste</wicri:regionArea><wicri:noRegion>34143 Trieste</wicri:noRegion></affiliation></author><author><name sortKey="Moscardini, L" sort="Moscardini, L" uniqKey="Moscardini L" first="L." last="Moscardini">L. Moscardini</name><affiliation wicri:level="4"><country xml:lang="fr">Italie</country><wicri:regionArea>Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna</wicri:regionArea><orgName type="university">Université de Bologne</orgName><placeName><settlement type="city">Bologne</settlement><region nuts="2" type="region">Émilie-Romagne</region></placeName></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Italie</country><wicri:regionArea>INFN – National Institute for Nuclear Physics, Sezione di Bologna, viale Berti Pichat 6/2, 40127 Bologna</wicri:regionArea><wicri:noRegion>40127 Bologna</wicri:noRegion></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 wicri:level="4"><orgName type="university">Université de Cambridge</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Cambridge</settlement><region type="country">Angleterre</region><region type="région" nuts="1">Angleterre de l'Est</region></placeName></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122</wicri:regionArea><wicri:noRegion>VIC 3122</wicri:noRegion></affiliation></author><author><name sortKey="Queloz, D" sort="Queloz, D" uniqKey="Queloz D" first="D." last="Queloz">D. Queloz</name><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny</wicri:regionArea><wicri:noRegion>1290 Sauverny</wicri:noRegion></affiliation></author><author><name sortKey="Shaver, P" sort="Shaver, P" uniqKey="Shaver P" first="P." last="Shaver">P. Shaver</name><affiliation wicri:level="1"><country xml:lang="fr">Allemagne</country><wicri:regionArea>European Southern Observatory, Karl‐Schwarzschild‐Str. 2, 85748 Garching</wicri:regionArea><wicri:noRegion>85748 Garching</wicri:noRegion><wicri:noRegion>85748 Garching</wicri:noRegion></affiliation></author><author><name sortKey="Udry, S" sort="Udry, S" uniqKey="Udry S" first="S." last="Udry">S. Udry</name><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny</wicri:regionArea><wicri:noRegion>1290 Sauverny</wicri:noRegion></affiliation></author><author><name sortKey="Wiklind, T" sort="Wiklind, T" uniqKey="Wiklind T" first="T." last="Wiklind">T. Wiklind</name><affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218</wicri:regionArea><placeName><region type="state">Maryland</region></placeName></affiliation><affiliation></affiliation></author><author><name sortKey="Zucker, S" sort="Zucker, S" uniqKey="Zucker S" first="S." last="Zucker">S. Zucker</name><affiliation wicri:level="1"><country xml:lang="fr">Israël</country><wicri:regionArea>Department of Geophysics and Planetary Sciences, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978</wicri:regionArea><wicri:noRegion>Tel Aviv 69978</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">386</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="1192">1192</biblScope><biblScope unit="page" to="1218">1218</biblScope><biblScope unit="page-count">27</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2008-05-21">2008-05-21</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absorber</term><term>Absorption line</term><term>Absorption line lists</term><term>Absorption lines</term><term>Adelberger</term><term>Aguirre</term><term>Alternative models</term><term>Atness</term><term>Available metal lines</term><term>Blue dots</term><term>Brightness distribution</term><term>Cardassian</term><term>Colour</term><term>Column density</term><term>Comoving</term><term>Constraint</term><term>Cosmic dynamics</term><term>Cosmological</term><term>Cosmological model</term><term>Cosmological redshift</term><term>Cosmology</term><term>Dark energy</term><term>Different redshifts</term><term>Doppler shift</term><term>Dtobs</term><term>Dynamics</term><term>Ellipse</term><term>Emission lines</term><term>Equal time allocation</term><term>Expansion history</term><term>Forest line lists</term><term>Forest region</term><term>Forest spectrum</term><term>Form factor</term><term>Friedman</term><term>Friedman equation</term><term>Galactic feedback</term><term>General relativity</term><term>Gnedin</term><term>Grid</term><term>Haehnelt</term><term>Hashed region</term><term>High redshift</term><term>Hubble</term><term>Integration time</term><term>Intergalactic matter</term><term>Journal compilation</term><term>Large telescopes</term><term>Late times</term><term>Lett</term><term>Linder</term><term>Line lists</term><term>Liske</term><term>Lower limit</term><term>Lyman alpha forest</term><term>Metal lines</term><term>Metric</term><term>Mnras</term><term>Models</term><term>Monte Carlo methods</term><term>Nqso</term><term>Optical depth</term><term>Other hand</term><term>Other methods</term><term>Overall accuracy</term><term>Overall value</term><term>Parameter</term><term>Parameter space</term><term>Peculiar acceleration</term><term>Peculiar motion</term><term>Peculiar motions</term><term>Peculiar velocities</term><term>Peculiar velocity</term><term>Photometry</term><term>Photon</term><term>Photon noise</term><term>Phys</term><term>Physical properties</term><term>Pixel</term><term>Pixel size</term><term>Previous section</term><term>Qsos</term><term>Quasars</term><term>Quintessence</term><term>Radial velocity shifts</term><term>Rauch</term><term>Real line lists</term><term>Red shift</term><term>Redshift</term><term>Redshift bins</term><term>Redshift difference</term><term>Redshift drift</term><term>Redshift drift experiment</term><term>Redshift evolution</term><term>Redshift range</term><term>Schaye</term><term>Sdss</term><term>Signal-to-noise ratio</term><term>Simcoe</term><term>Simulation</term><term>Snia</term><term>Solid line</term><term>Spectral features</term><term>Steidel</term><term>Target selection</term><term>Theuns</term><term>Tobs</term><term>Total integration time</term><term>Universal expansion</term><term>Universe expansion</term><term>Velocity shift</term><term>Viel</term><term>Weak lensing</term><term>Zhang</term><term>Zqso</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Bruit photonique</term><term>Cosmologie</term><term>Distribution brillance</term><term>Dynamique</term><term>Déplacement vers le rouge</term><term>Déplacement vers le rouge cosmologique</term><term>Energie sombre</term><term>Expansion univers</term><term>Forêt Lyman alpha</term><term>Matière intergalactique</term><term>Modèle</term><term>Méthode Monte Carlo</term><term>Quasar</term><term>Raie absorption</term><term>Rapport signal bruit</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Absorber</term><term>Absorption line lists</term><term>Absorption lines</term><term>Adelberger</term><term>Aguirre</term><term>Alternative models</term><term>Atness</term><term>Available metal lines</term><term>Blue dots</term><term>Cardassian</term><term>Colour</term><term>Column density</term><term>Comoving</term><term>Constraint</term><term>Cosmic dynamics</term><term>Cosmological</term><term>Cosmological model</term><term>Dark energy</term><term>Different redshifts</term><term>Doppler shift</term><term>Dtobs</term><term>Ellipse</term><term>Emission lines</term><term>Equal time allocation</term><term>Expansion history</term><term>Forest line lists</term><term>Forest region</term><term>Forest spectrum</term><term>Form factor</term><term>Friedman</term><term>Friedman equation</term><term>Galactic feedback</term><term>General relativity</term><term>Gnedin</term><term>Grid</term><term>Haehnelt</term><term>Hashed region</term><term>High redshift</term><term>Hubble</term><term>Integration time</term><term>Journal compilation</term><term>Large telescopes</term><term>Late times</term><term>Lett</term><term>Linder</term><term>Line lists</term><term>Liske</term><term>Lower limit</term><term>Metal lines</term><term>Metric</term><term>Mnras</term><term>Nqso</term><term>Optical depth</term><term>Other hand</term><term>Other methods</term><term>Overall accuracy</term><term>Overall value</term><term>Parameter</term><term>Parameter space</term><term>Peculiar acceleration</term><term>Peculiar motion</term><term>Peculiar motions</term><term>Peculiar velocities</term><term>Peculiar velocity</term><term>Photometry</term><term>Photon</term><term>Photon noise</term><term>Phys</term><term>Physical properties</term><term>Pixel</term><term>Pixel size</term><term>Previous section</term><term>Qsos</term><term>Quintessence</term><term>Radial velocity shifts</term><term>Rauch</term><term>Real line lists</term><term>Redshift</term><term>Redshift bins</term><term>Redshift difference</term><term>Redshift drift</term><term>Redshift drift experiment</term><term>Redshift evolution</term><term>Redshift range</term><term>Schaye</term><term>Sdss</term><term>Simcoe</term><term>Simulation</term><term>Snia</term><term>Solid line</term><term>Spectral features</term><term>Steidel</term><term>Target selection</term><term>Theuns</term><term>Tobs</term><term>Total integration time</term><term>Universal expansion</term><term>Velocity shift</term><term>Viel</term><term>Weak lensing</term><term>Zhang</term><term>Zqso</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Cosmologie</term><term>Simulation</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The redshifts of all cosmologically distant sources are expected to experience a small, systematic drift as a function of time due to the evolution of the Universe's expansion rate. A measurement of this effect would represent a direct and entirely model‐independent determination of the expansion history of the Universe over a redshift range that is inaccessible to other methods. Here we investigate the impact of the next generation of Extremely Large Telescopes on the feasibility of detecting and characterizing the cosmological redshift drift. We consider the Lyα forest in the redshift range 2 < z < 5 and other absorption lines in the spectra of high‐redshift QSOs as the most suitable targets for a redshift drift experiment. Assuming photon‐noise‐limited observations and using extensive Monte Carlo simulations we determine the accuracy to which the redshift drift can be measured from the Lyα forest as a function of signal‐to‐noise ratio and redshift. Based on this relation and using the brightness and redshift distributions of known QSOs we find that a 42‐m telescope is capable of unambiguously detecting the redshift drift over a period of ∼20 yr using 4000 h of observing time. Such an experiment would provide independent evidence for the existence of dark energy without assuming spatial flatness, using any other cosmological constraints or making any other astrophysical assumption.</div></front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>France</li><li>Israël</li><li>Italie</li><li>Royaume-Uni</li><li>Russie</li><li>Suisse</li><li>États-Unis</li></country><region><li>Angleterre</li><li>Angleterre de l'Est</li><li>Latium</li><li>Maryland</li><li>Provence-Alpes-Côte d'Azur</li><li>Émilie-Romagne</li><li>Île-de-France</li></region><settlement><li>Bologne</li><li>Cambridge</li><li>Marseille</li><li>Meudon</li><li>Rome</li></settlement><orgName><li>Université de Bologne</li><li>Université de Cambridge</li></orgName></list><tree><country name="Allemagne"><noRegion><name sortKey="Liske, J" sort="Liske, J" uniqKey="Liske J" first="J." last="Liske">J. Liske</name></noRegion><name sortKey="Avila, G" sort="Avila, G" uniqKey="Avila G" first="G." last="Avila">G. Avila</name><name sortKey="D Odorico, S" sort="D Odorico, S" uniqKey="D Odorico S" first="S." last="D'Odorico">S. D'Odorico</name><name sortKey="Dekker, H" sort="Dekker, H" uniqKey="Dekker H" first="H." last="Dekker">H. Dekker</name><name sortKey="Delabre, B" sort="Delabre, B" uniqKey="Delabre B" first="B." last="Delabre">B. Delabre</name><name sortKey="Pasquini, L" sort="Pasquini, L" uniqKey="Pasquini L" first="L." last="Pasquini">L. Pasquini</name><name sortKey="Shaver, P" sort="Shaver, P" uniqKey="Shaver P" first="P." last="Shaver">P. Shaver</name></country><country name="Italie"><region name="Latium"><name sortKey="Grazian, A" sort="Grazian, A" uniqKey="Grazian A" first="A." last="Grazian">A. Grazian</name></region><name sortKey="Bonifacio, P" sort="Bonifacio, P" uniqKey="Bonifacio P" first="P." last="Bonifacio">P. Bonifacio</name><name sortKey="Cristiani, S" sort="Cristiani, S" uniqKey="Cristiani S" first="S." last="Cristiani">S. Cristiani</name><name sortKey="D Odorico, V" sort="D Odorico, V" uniqKey="D Odorico V" first="V." last="D'Odorico">V. D'Odorico</name><name sortKey="Molaro, P" sort="Molaro, P" uniqKey="Molaro P" first="P." last="Molaro">P. Molaro</name><name sortKey="Moscardini, L" sort="Moscardini, L" uniqKey="Moscardini L" first="L." last="Moscardini">L. Moscardini</name><name sortKey="Moscardini, L" sort="Moscardini, L" uniqKey="Moscardini L" first="L." last="Moscardini">L. Moscardini</name><name sortKey="Vanzella, E" sort="Vanzella, E" uniqKey="Vanzella E" first="E." last="Vanzella">E. Vanzella</name><name sortKey="Viel, M" sort="Viel, M" uniqKey="Viel M" first="M." last="Viel">M. Viel</name></country><country name="Suisse"><noRegion><name sortKey="Dessauges, M" sort="Dessauges, M" uniqKey="Dessauges M" first="M." last="Dessauges">M. Dessauges</name></noRegion><name sortKey="Lovis, C" sort="Lovis, C" uniqKey="Lovis C" first="C." last="Lovis">C. Lovis</name><name sortKey="Mayor, M" sort="Mayor, M" uniqKey="Mayor M" first="M." last="Mayor">M. Mayor</name><name sortKey="Pepe, F" sort="Pepe, F" uniqKey="Pepe F" first="F." last="Pepe">F. Pepe</name><name sortKey="Queloz, D" sort="Queloz, D" uniqKey="Queloz D" first="D." last="Queloz">D. Queloz</name><name sortKey="Udry, S" sort="Udry, S" uniqKey="Udry S" first="S." last="Udry">S. Udry</name></country><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Viel, M" sort="Viel, M" uniqKey="Viel M" first="M." last="Viel">M. Viel</name></region><name sortKey="Haehnelt, M" sort="Haehnelt, M" uniqKey="Haehnelt M" first="M." last="Haehnelt">M. Haehnelt</name><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name></country><country name="France"><region name="Île-de-France"><name sortKey="Bonifacio, P" sort="Bonifacio, P" uniqKey="Bonifacio P" first="P." last="Bonifacio">P. Bonifacio</name></region><name sortKey="Bouchy, F" sort="Bouchy, F" uniqKey="Bouchy F" first="F." last="Bouchy">F. Bouchy</name><name sortKey="Bouchy, F" sort="Bouchy, F" uniqKey="Bouchy F" first="F." last="Bouchy">F. Bouchy</name></country><country name="Russie"><noRegion><name sortKey="Levshakov, S" sort="Levshakov, S" uniqKey="Levshakov S" first="S." last="Levshakov">S. Levshakov</name></noRegion></country><country name="Australie"><noRegion><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name></noRegion></country><country name="États-Unis"><region name="Maryland"><name sortKey="Wiklind, T" sort="Wiklind, T" uniqKey="Wiklind T" first="T." last="Wiklind">T. Wiklind</name></region></country><country name="Israël"><noRegion><name sortKey="Zucker, S" sort="Zucker, S" uniqKey="Zucker S" first="S." last="Zucker">S. Zucker</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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