Preparation of Kepler light curves for asteroseismic analyses
ABSTRACT The Kepler mission is providing photometric data of exquisite quality for the asteroseismic study of different classes of pulsating stars. These analyses place particular demands on the pre‐processing of the data, over a range of time‐scales from minutes to months. Here, we describe process...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society. Letters 2011-06, Vol.414 (1), p.L6-L10 |
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| container_title | Monthly notices of the Royal Astronomical Society. Letters |
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| creator | García, R. A. Hekker, S. Stello, D. Gutiérrez-Soto, J. Handberg, R. Huber, D. Karoff, C. Uytterhoeven, K. Appourchaux, T. Chaplin, W. J. Elsworth, Y. Mathur, S. Ballot, J. Christensen-Dalsgaard, J. Gilliland, R. L. Houdek, G. Jenkins, J. M. Kjeldsen, H. McCauliff, S. Metcalfe, T. Middour, C. K. Molenda-Zakowicz, J. Monteiro, M. J. P. F. G. Smith, J. C. Thompson, M. J. |
| description | ABSTRACT
The Kepler mission is providing photometric data of exquisite quality for the asteroseismic study of different classes of pulsating stars. These analyses place particular demands on the pre‐processing of the data, over a range of time‐scales from minutes to months. Here, we describe processing procedures developed by the Kepler Asteroseismic Science Consortium to prepare light curves that are optimized for the asteroseismic study of solar‐like oscillating stars in which outliers, jumps and drifts are corrected. |
| doi_str_mv | 10.1111/j.1745-3933.2011.01042.x |
| format | Article |
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The Kepler mission is providing photometric data of exquisite quality for the asteroseismic study of different classes of pulsating stars. These analyses place particular demands on the pre‐processing of the data, over a range of time‐scales from minutes to months. Here, we describe processing procedures developed by the Kepler Asteroseismic Science Consortium to prepare light curves that are optimized for the asteroseismic study of solar‐like oscillating stars in which outliers, jumps and drifts are corrected.</description><identifier>ISSN: 1745-3925</identifier><identifier>EISSN: 1745-3933</identifier><identifier>DOI: 10.1111/j.1745-3933.2011.01042.x</identifier><language>eng</language><publisher>Oxford, UK: Blackwell Publishing Ltd</publisher><subject>asteroseismology ; methods: data analysis</subject><ispartof>Monthly notices of the Royal Astronomical Society. Letters, 2011-06, Vol.414 (1), p.L6-L10</ispartof><rights>2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4342-992dcead09f57019e21cab98f9ec0d14fd291016ae53c004a0e9cb05862203313</citedby><cites>FETCH-LOGICAL-c4342-992dcead09f57019e21cab98f9ec0d14fd291016ae53c004a0e9cb05862203313</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1111%2Fj.1745-3933.2011.01042.x$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1111%2Fj.1745-3933.2011.01042.x$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,776,780,1411,27903,27904,45553,45554</link.rule.ids></links><search><creatorcontrib>García, R. A.</creatorcontrib><creatorcontrib>Hekker, S.</creatorcontrib><creatorcontrib>Stello, D.</creatorcontrib><creatorcontrib>Gutiérrez-Soto, J.</creatorcontrib><creatorcontrib>Handberg, R.</creatorcontrib><creatorcontrib>Huber, D.</creatorcontrib><creatorcontrib>Karoff, C.</creatorcontrib><creatorcontrib>Uytterhoeven, K.</creatorcontrib><creatorcontrib>Appourchaux, T.</creatorcontrib><creatorcontrib>Chaplin, W. J.</creatorcontrib><creatorcontrib>Elsworth, Y.</creatorcontrib><creatorcontrib>Mathur, S.</creatorcontrib><creatorcontrib>Ballot, J.</creatorcontrib><creatorcontrib>Christensen-Dalsgaard, J.</creatorcontrib><creatorcontrib>Gilliland, R. L.</creatorcontrib><creatorcontrib>Houdek, G.</creatorcontrib><creatorcontrib>Jenkins, J. M.</creatorcontrib><creatorcontrib>Kjeldsen, H.</creatorcontrib><creatorcontrib>McCauliff, S.</creatorcontrib><creatorcontrib>Metcalfe, T.</creatorcontrib><creatorcontrib>Middour, C. K.</creatorcontrib><creatorcontrib>Molenda-Zakowicz, J.</creatorcontrib><creatorcontrib>Monteiro, M. J. P. F. G.</creatorcontrib><creatorcontrib>Smith, J. C.</creatorcontrib><creatorcontrib>Thompson, M. J.</creatorcontrib><title>Preparation of Kepler light curves for asteroseismic analyses</title><title>Monthly notices of the Royal Astronomical Society. Letters</title><description>ABSTRACT
The Kepler mission is providing photometric data of exquisite quality for the asteroseismic study of different classes of pulsating stars. These analyses place particular demands on the pre‐processing of the data, over a range of time‐scales from minutes to months. Here, we describe processing procedures developed by the Kepler Asteroseismic Science Consortium to prepare light curves that are optimized for the asteroseismic study of solar‐like oscillating stars in which outliers, jumps and drifts are corrected.</description><subject>asteroseismology</subject><subject>methods: data analysis</subject><issn>1745-3925</issn><issn>1745-3933</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><recordid>eNqNkEtPwzAQhC0EEqXwH3zjlOC18_IBJFpBQS2FAw-Ji-U6G3BJm2Kn0P57EoJ6Zi870s6MVh8hFFgIzZzNQ0ijOBBSiJAzgJABi3i42SO93WF_p3l8SI68nzMm0izNeuT8weFKO13bakmrgo5xVaKjpX17r6lZuy_0tKgc1b5GV3m0fmEN1Utdbj36Y3JQ6NLjyd_uk6frq8fhTTC5H90OLyeBiUTEAyl5blDnTBZxykAiB6NnMiskGpZDVORcAoNEYywMY5FmKM2MxVnCORMCRJ-cdr0rV32u0ddqYb3BstRLrNZeZVJCnACIxpl1TtN86x0WauXsQrutAqZaYGquWhaq5aJaYOoXmNo00Ysu-m1L3P47p-6mE97KpiDoCmwDa7Mr0O5DJalIY_UyHanX57GADAZqIH4AmCyAGQ</recordid><startdate>20110611</startdate><enddate>20110611</enddate><creator>García, R. 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The Kepler mission is providing photometric data of exquisite quality for the asteroseismic study of different classes of pulsating stars. These analyses place particular demands on the pre‐processing of the data, over a range of time‐scales from minutes to months. Here, we describe processing procedures developed by the Kepler Asteroseismic Science Consortium to prepare light curves that are optimized for the asteroseismic study of solar‐like oscillating stars in which outliers, jumps and drifts are corrected.</abstract><cop>Oxford, UK</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1111/j.1745-3933.2011.01042.x</doi><tpages>5</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | asteroseismology methods: data analysis |
| title | Preparation of Kepler light curves for asteroseismic analyses |
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