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Cepheid investigations using the Kepler space telescope

Identifieur interne : 006479 ( Main/Exploration ); précédent : 006478; suivant : 006480

Cepheid investigations using the Kepler space telescope

Auteurs : R. Szab [Hongrie] ; L. Szabados [Hongrie] ; C. Ngeow [Taïwan] ; R. Smolec [Autriche] ; A. Derekas [Hongrie] ; P. Moskalik [Pologne] ; J. Nuspl [Hongrie] ; H. Lehmann [Allemagne] ; G. F Rész [États-Unis] ; J. Molenda- Akowicz [Pologne] ; S. T. Bryson [États-Unis] ; A. A. Henden [États-Unis] ; D. W. Kurtz ; D. Stello [Australie] ; J. M. Nemec [Canada] ; J. M. Benk [Hongrie] ; L. Berdnikov [Russie] ; H. Bruntt [France] ; N. R. Evans [États-Unis] ; N. A. Gorynya [Russie] ; E. N. Pastukhova [Russie] ; R. J. Simcoe [Russie] ; J. E. Grindlay [États-Unis] ; E. J. Los [États-Unis] ; A. Doane [États-Unis] ; S. G. Laycock [États-Unis] ; D. J. Mink [États-Unis] ; G. Champine [États-Unis] ; A. Sliski [États-Unis] ; G. Handler [Autriche] ; L. L. Kiss [Hongrie] ; Z. Kolláth [Hongrie] ; J. Kovács [Hongrie] ; J. Christensen-Dalsgaard [Danemark] ; H. Kjeldsen [Danemark] ; C. Allen [États-Unis] ; S. E. Thompson [États-Unis] ; J. Van Cleve [États-Unis]

Source :

RBID : ISTEX:C8F5AA1485B53C865437CFE018A5EDC3D2F1568A

English descriptors

Abstract

We report results of initial work done on selected candidate Cepheids to be observed with the Kepler space telescope. Prior to the launch, 40 candidates were selected from previous surveys and data bases. The analysis of the first 322 d of Kepler photometry, and recent ground‐based follow‐up multicolour photometry and spectroscopy allowed us to confirm that one of these stars, V1154 Cyg (KIC 7548061), is indeed a 4.9‐d Cepheid. Using the phase lag method, we show that this star pulsates in the fundamental mode. New radial velocity data are consistent with previous measurements, suggesting that a long‐period binary component is unlikely. No evidence is seen in the ultraprecise, nearly uninterrupted Kepler photometry for non‐radial or stochastically excited modes at the micromagnitude level. The other candidates are not Cepheids, but an interesting mix of possible spotted stars, eclipsing systems and flare stars.

Url:
DOI: 10.1111/j.1365-2966.2011.18342.x


Affiliations:


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Le document en format XML

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<name sortKey="Christensen Alsgaard, J" sort="Christensen Alsgaard, J" uniqKey="Christensen Alsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name>
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<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>
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<date type="published" when="2011-06-01">2011-06-01</date>
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<term>Acta astron</term>
<term>Additional photometric data</term>
<term>Amplitude</term>
<term>Antonello</term>
<term>Arellano ferro</term>
<term>Astron</term>
<term>Bottom panel</term>
<term>Brightness variation</term>
<term>Cepheid</term>
<term>Cepheid candidates</term>
<term>Cepheid instability strip</term>
<term>Cepheid investigations</term>
<term>Cepheid nature</term>
<term>Cepheids</term>
<term>Cepheids pulsate</term>
<term>Classical cepheids</term>
<term>Contamination index</term>
<term>Data base</term>
<term>Data points</term>
<term>Data sets</term>
<term>Entire table</term>
<term>Error bars</term>
<term>Exposure time</term>
<term>Fourier</term>
<term>Fourier parameter progressions</term>
<term>Fourier parameters</term>
<term>Frequency peaks</term>
<term>Frequency spectrum</term>
<term>Fundamental mode</term>
<term>Galactic</term>
<term>Galactic cepheids</term>
<term>Garden street</term>
<term>Gorynya</term>
<term>Harmonics</term>
<term>Hungarian academy</term>
<term>Individual candidates</term>
<term>Instrumental effects</term>
<term>Instrumental magnitudes</term>
<term>Kepler</term>
<term>Kepler cepheid candidates</term>
<term>Kepler data</term>
<term>Kepler figure</term>
<term>Kepler light curve</term>
<term>Kepler light curves</term>
<term>Kepler magnitude system</term>
<term>Kepler magnitudes</term>
<term>Kepler mission</term>
<term>Kepler observations</term>
<term>Kepler passband</term>
<term>Kepler photometry</term>
<term>Kepler space telescope</term>
<term>Larger number</term>
<term>Light curve</term>
<term>Light curves</term>
<term>Linear cepheid instability strip</term>
<term>Lled squares</term>
<term>Lulin observatory</term>
<term>Mnras</term>
<term>Moffett field</term>
<term>Monthly notices</term>
<term>More details</term>
<term>Multicolour</term>
<term>Multicolour light curves</term>
<term>Multicolour photometry</term>
<term>Nyquist frequency</term>
<term>Observatory</term>
<term>Online version</term>
<term>Optimal aperture</term>
<term>Photometric</term>
<term>Photometric data</term>
<term>Photometric survey</term>
<term>Photometry</term>
<term>Poretti</term>
<term>Progression</term>
<term>Pulsation</term>
<term>Pulsation period</term>
<term>Pulsational</term>
<term>Residual</term>
<term>Sample table</term>
<term>Saturation limit</term>
<term>Separate paper</term>
<term>Solar orbit</term>
<term>Spectroscopic</term>
<term>Spectroscopic binarity</term>
<term>Spectroscopic observations</term>
<term>Survey phase</term>
<term>Szab</term>
<term>Szabados</term>
<term>Telescope</term>
<term>Upper panel</term>
<term>Variable stars</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en">
<term>Acta astron</term>
<term>Additional photometric data</term>
<term>Amplitude</term>
<term>Antonello</term>
<term>Arellano ferro</term>
<term>Astron</term>
<term>Bottom panel</term>
<term>Brightness variation</term>
<term>Cepheid</term>
<term>Cepheid candidates</term>
<term>Cepheid instability strip</term>
<term>Cepheid investigations</term>
<term>Cepheid nature</term>
<term>Cepheids</term>
<term>Cepheids pulsate</term>
<term>Classical cepheids</term>
<term>Contamination index</term>
<term>Data base</term>
<term>Data points</term>
<term>Data sets</term>
<term>Entire table</term>
<term>Error bars</term>
<term>Exposure time</term>
<term>Fourier</term>
<term>Fourier parameter progressions</term>
<term>Fourier parameters</term>
<term>Frequency peaks</term>
<term>Frequency spectrum</term>
<term>Fundamental mode</term>
<term>Galactic</term>
<term>Galactic cepheids</term>
<term>Garden street</term>
<term>Gorynya</term>
<term>Harmonics</term>
<term>Hungarian academy</term>
<term>Individual candidates</term>
<term>Instrumental effects</term>
<term>Instrumental magnitudes</term>
<term>Kepler</term>
<term>Kepler cepheid candidates</term>
<term>Kepler data</term>
<term>Kepler figure</term>
<term>Kepler light curve</term>
<term>Kepler light curves</term>
<term>Kepler magnitude system</term>
<term>Kepler magnitudes</term>
<term>Kepler mission</term>
<term>Kepler observations</term>
<term>Kepler passband</term>
<term>Kepler photometry</term>
<term>Kepler space telescope</term>
<term>Larger number</term>
<term>Light curve</term>
<term>Light curves</term>
<term>Linear cepheid instability strip</term>
<term>Lled squares</term>
<term>Lulin observatory</term>
<term>Mnras</term>
<term>Moffett field</term>
<term>Monthly notices</term>
<term>More details</term>
<term>Multicolour</term>
<term>Multicolour light curves</term>
<term>Multicolour photometry</term>
<term>Nyquist frequency</term>
<term>Observatory</term>
<term>Online version</term>
<term>Optimal aperture</term>
<term>Photometric</term>
<term>Photometric data</term>
<term>Photometric survey</term>
<term>Photometry</term>
<term>Poretti</term>
<term>Progression</term>
<term>Pulsation</term>
<term>Pulsation period</term>
<term>Pulsational</term>
<term>Residual</term>
<term>Sample table</term>
<term>Saturation limit</term>
<term>Separate paper</term>
<term>Solar orbit</term>
<term>Spectroscopic</term>
<term>Spectroscopic binarity</term>
<term>Spectroscopic observations</term>
<term>Survey phase</term>
<term>Szab</term>
<term>Szabados</term>
<term>Telescope</term>
<term>Upper panel</term>
<term>Variable stars</term>
</keywords>
</textClass>
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</teiHeader>
<front>
<div type="abstract" xml:lang="en">We report results of initial work done on selected candidate Cepheids to be observed with the Kepler space telescope. Prior to the launch, 40 candidates were selected from previous surveys and data bases. The analysis of the first 322 d of Kepler photometry, and recent ground‐based follow‐up multicolour photometry and spectroscopy allowed us to confirm that one of these stars, V1154 Cyg (KIC 7548061), is indeed a 4.9‐d Cepheid. Using the phase lag method, we show that this star pulsates in the fundamental mode. New radial velocity data are consistent with previous measurements, suggesting that a long‐period binary component is unlikely. No evidence is seen in the ultraprecise, nearly uninterrupted Kepler photometry for non‐radial or stochastically excited modes at the micromagnitude level. The other candidates are not Cepheids, but an interesting mix of possible spotted stars, eclipsing systems and flare stars.</div>
</front>
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<li>Pologne</li>
<li>Russie</li>
<li>Taïwan</li>
<li>États-Unis</li>
</country>
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<li>Californie</li>
<li>District fédéral central</li>
<li>Hongrie centrale</li>
<li>Massachusetts</li>
<li>Nouvelle-Galles du Sud</li>
<li>Île-de-France</li>
</region>
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<li>Budapest</li>
<li>Meudon</li>
<li>Moscou</li>
<li>Sydney</li>
</settlement>
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<li>Université de Sydney</li>
</orgName>
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<region name="Massachusetts">
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<name sortKey="Allen, C" sort="Allen, C" uniqKey="Allen C" first="C." last="Allen">C. Allen</name>
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<name sortKey="Los, E J" sort="Los, E J" uniqKey="Los E" first="E. J." last="Los">E. J. Los</name>
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<name sortKey="Nemec, J M" sort="Nemec, J M" uniqKey="Nemec J" first="J. M." last="Nemec">J. M. Nemec</name>
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<country name="Russie">
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<name sortKey="Berdnikov, L" sort="Berdnikov, L" uniqKey="Berdnikov L" first="L." last="Berdnikov">L. Berdnikov</name>
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<name sortKey="Bruntt, H" sort="Bruntt, H" uniqKey="Bruntt H" first="H." last="Bruntt">H. Bruntt</name>
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