Solar-like oscillations in red giants observed with Kepler: influence of increased timespan on global oscillation parameters
Identifieur interne : 004F95 ( PascalFrancis/Curation ); précédent : 004F94; suivant : 004F96Solar-like oscillations in red giants observed with Kepler: influence of increased timespan on global oscillation parameters
Auteurs : S. Hekker [Pays-Bas, Royaume-Uni] ; Y. Elsworth [Royaume-Uni] ; B. Mosser [France] ; T. Kallinger [Belgique] ; W. J. Chaplin [Royaume-Uni] ; J. De Ridder [Belgique] ; R. A. Garcia [France] ; D. Stello [Australie] ; B. D. Clarke [États-Unis] ; J. R. Hall [États-Unis] ; K. A. Ibrahim [États-Unis]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
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Abstract
Context. The length of the asteroseismic timeseries obtained from the Kepler satellite analysed here span 19 months. Kepler provides the longest continuous timeseries currently available, which calls for a study of the influence of the increased timespan on the accuracy and precision of the obtained results. Aims. We aim to investigate how the increased timespan influences the detectability of the oscillation modes, and the absolute values and uncertainties of the global oscillation parameters, i.e., frequency of maximum oscillation power, vmax, and large frequency separation between modes of the same degree and consecutive orders, ?Δv?. Methods. We use published methods to derive vmax and ?Δv? for timeseries ranging from 50 to 600 days and compare these results as a function of method, timespan and ?Δv?. Results. We find that in general a minimum of the order of 400 day long timeseries are necessary to obtain reliable results for the global oscillation parameters in more than 95% of the stars, but this does depend on ?Δv?. In a statistical sense the quoted uncertainties seem to provide a reasonable indication of the precision of the obtained results in short (50-day) runs, they do however seem to be overestimated for results of longer runs. Furthermore, the different definitions of the global parameters used in the different methods have non-negligible effects on the obtained values. Additionally, we show that there is a correlation between vmax and the flux variance. Conclusions. We conclude that longer timeseries improve the likelihood to detect oscillations with automated codes (from ∼60% in 50 day runs to >95% in 400 day runs with a slight method dependence) and the precision of the obtained global oscillation parameters. The trends suggest that the improvement will continue for even longer timeseries than the 600 days considered here, with a reduction in the median absolute deviation of more than a factor of 10 for an increase in timespan from 50 to 2000 days (the currently foreseen length of the mission). This work shows that global parameters determined with high precision - thus from long datasets -using different definitions can be used to identify the evolutionary state of the stars.
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Stello</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Clarke, B D" sort="Clarke, B D" uniqKey="Clarke B" first="B. D." last="Clarke">B. D. Clarke</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Hall, J R" sort="Hall, J R" uniqKey="Hall J" first="J. R." last="Hall">J. R. Hall</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Ibrahim, K A" sort="Ibrahim, K A" uniqKey="Ibrahim K" first="K. A." last="Ibrahim">K. A. Ibrahim</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0411738</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0411738 INIST</idno><idno type="RBID">Pascal:12-0411738</idno><idno type="wicri:Area/PascalFrancis/Corpus">000F26</idno><idno type="wicri:Area/PascalFrancis/Curation">004F95</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Solar-like oscillations in red giants observed with Kepler: influence of increased timespan on global oscillation parameters</title><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Astronomical institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>1 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>University of Birmingham, School of Physics and Astronomy</s1><s2>Edgbaston, Birmingham B 15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Elsworth, Y" sort="Elsworth, Y" uniqKey="Elsworth Y" first="Y." last="Elsworth">Y. Elsworth</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>University of Birmingham, School of Physics and Astronomy</s1><s2>Edgbaston, Birmingham B 15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>LESIA, UMR 8109, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D</s1><s2>3001 Leuven</s2><s3>BEL</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Chaplin, W J" sort="Chaplin, W J" uniqKey="Chaplin W" first="W. J." last="Chaplin">W. J. Chaplin</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>University of Birmingham, School of Physics and Astronomy</s1><s2>Edgbaston, Birmingham B 15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="De Ridder, J" sort="De Ridder, J" uniqKey="De Ridder J" first="J." last="De Ridder">J. De Ridder</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D</s1><s2>3001 Leuven</s2><s3>BEL</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Garcia, R A" sort="Garcia, R A" uniqKey="Garcia R" first="R. A." last="Garcia">R. A. Garcia</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Clarke, B D" sort="Clarke, B D" uniqKey="Clarke B" first="B. D." last="Clarke">B. D. Clarke</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Hall, J R" sort="Hall, J R" uniqKey="Hall J" first="J. R." last="Hall">J. R. Hall</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Ibrahim, K A" sort="Ibrahim, K A" uniqKey="Ibrahim K" first="K. A." last="Ibrahim">K. A. Ibrahim</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Correlations</term><term>Detectability</term><term>Kepler satellite</term><term>Late type stars</term><term>Oscillation modes</term><term>Red giant stars</term><term>Uncertainty</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Géante rouge</term><term>Satellite Kepler</term><term>Détectabilité</term><term>Mode oscillation</term><term>Incertitude</term><term>Corrélation</term><term>Etoile type avancé</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. The length of the asteroseismic timeseries obtained from the Kepler satellite analysed here span 19 months. Kepler provides the longest continuous timeseries currently available, which calls for a study of the influence of the increased timespan on the accuracy and precision of the obtained results. Aims. We aim to investigate how the increased timespan influences the detectability of the oscillation modes, and the absolute values and uncertainties of the global oscillation parameters, i.e., frequency of maximum oscillation power, v<sub>max</sub>, and large frequency separation between modes of the same degree and consecutive orders, ?Δv?. Methods. We use published methods to derive v<sub>max</sub> and ?Δv? for timeseries ranging from 50 to 600 days and compare these results as a function of method, timespan and ?Δv?. Results. We find that in general a minimum of the order of 400 day long timeseries are necessary to obtain reliable results for the global oscillation parameters in more than 95% of the stars, but this does depend on ?Δv?. In a statistical sense the quoted uncertainties seem to provide a reasonable indication of the precision of the obtained results in short (50-day) runs, they do however seem to be overestimated for results of longer runs. Furthermore, the different definitions of the global parameters used in the different methods have non-negligible effects on the obtained values. Additionally, we show that there is a correlation between v<sub>max</sub> and the flux variance. Conclusions. We conclude that longer timeseries improve the likelihood to detect oscillations with automated codes (from ∼60% in 50 day runs to >95% in 400 day runs with a slight method dependence) and the precision of the obtained global oscillation parameters. The trends suggest that the improvement will continue for even longer timeseries than the 600 days considered here, with a reduction in the median absolute deviation of more than a factor of 10 for an increase in timespan from 50 to 2000 days (the currently foreseen length of the mission). This work shows that global parameters determined with high precision - thus from long datasets -using different definitions can be used to identify the evolutionary state of the stars.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>544</s2></fA05><fA06><s3>p. 2</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Solar-like oscillations in red giants observed with Kepler: influence of increased timespan on global oscillation parameters</s1></fA08><fA11 i1="01" i2="1"><s1>HEKKER (S.)</s1></fA11><fA11 i1="02" i2="1"><s1>ELSWORTH (Y.)</s1></fA11><fA11 i1="03" i2="1"><s1>MOSSER (B.)</s1></fA11><fA11 i1="04" i2="1"><s1>KALLINGER (T.)</s1></fA11><fA11 i1="05" i2="1"><s1>CHAPLIN (W. J.)</s1></fA11><fA11 i1="06" i2="1"><s1>DE RIDDER (J.)</s1></fA11><fA11 i1="07" i2="1"><s1>GARCIA (R. A.)</s1></fA11><fA11 i1="08" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="09" i2="1"><s1>CLARKE (B. D.)</s1></fA11><fA11 i1="10" i2="1"><s1>HALL (J. R.)</s1></fA11><fA11 i1="11" i2="1"><s1>IBRAHIM (K. A.)</s1></fA11><fA14 i1="01"><s1>Astronomical institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>University of Birmingham, School of Physics and Astronomy</s1><s2>Edgbaston, Birmingham B 15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></fA14><fA14 i1="03"><s1>LESIA, UMR 8109, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D</s1><s2>3001 Leuven</s2><s3>BEL</s3><sZ>4 aut.</sZ><sZ>6 aut.</sZ></fA14><fA14 i1="05"><s1>Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>7 aut.</sZ></fA14><fA14 i1="06"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></fA14><fA14 i1="07"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="08"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ></fA14><fA20><s2>A90.1-A90.11</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000506819320240</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0411738</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>Context. The length of the asteroseismic timeseries obtained from the Kepler satellite analysed here span 19 months. Kepler provides the longest continuous timeseries currently available, which calls for a study of the influence of the increased timespan on the accuracy and precision of the obtained results. Aims. We aim to investigate how the increased timespan influences the detectability of the oscillation modes, and the absolute values and uncertainties of the global oscillation parameters, i.e., frequency of maximum oscillation power, v<sub>max</sub>, and large frequency separation between modes of the same degree and consecutive orders, ?Δv?. Methods. We use published methods to derive v<sub>max</sub> and ?Δv? for timeseries ranging from 50 to 600 days and compare these results as a function of method, timespan and ?Δv?. Results. We find that in general a minimum of the order of 400 day long timeseries are necessary to obtain reliable results for the global oscillation parameters in more than 95% of the stars, but this does depend on ?Δv?. In a statistical sense the quoted uncertainties seem to provide a reasonable indication of the precision of the obtained results in short (50-day) runs, they do however seem to be overestimated for results of longer runs. Furthermore, the different definitions of the global parameters used in the different methods have non-negligible effects on the obtained values. Additionally, we show that there is a correlation between v<sub>max</sub> and the flux variance. Conclusions. We conclude that longer timeseries improve the likelihood to detect oscillations with automated codes (from ∼60% in 50 day runs to >95% in 400 day runs with a slight method dependence) and the precision of the obtained global oscillation parameters. The trends suggest that the improvement will continue for even longer timeseries than the 600 days considered here, with a reduction in the median absolute deviation of more than a factor of 10 for an increase in timespan from 50 to 2000 days (the currently foreseen length of the mission). This work shows that global parameters determined with high precision - thus from long datasets -using different definitions can be used to identify the evolutionary state of the stars.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Géante rouge</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Red giant stars</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Satellite Kepler</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Kepler satellite</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Satélite Kepler</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Détectabilité</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Detectability</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Detectabilidad</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Mode oscillation</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Oscillation modes</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Incertitude</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Uncertainty</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Incertidumbre</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Corrélation</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Correlations</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Etoile type avancé</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Late type stars</s0><s5>32</s5></fC03><fN21><s1>317</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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