J/A+A/614/A40ivo://CDS.VizieR/J/A+A/614/A40doi:10.26093/cds/vizier.36140040CDSPascual-Granado J.Suarez J.C.Garrido R.Moya A.Garcia Hernandez A.,Rodon J.R.Lares-Martiz M.2018-09-18T13:19:45Z2018-06-12T11:30:48ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frvariable-starsasteroseismologyIt is known that the observed distribution of frequencies in CoRoT and Kepler {delta} Scuti stars has no parallelism with any theoretical model. Pre-whitening is a widespread technique in the analysis of time series with gaps from pulsating stars located in the classical instability strip such as {delta} Scuti stars. However, some studies have pointed out that this technique might introduce biases in the results of the frequency analysis. This work aims at studying the biases that can result from pre-whitening in asteroseismology. The results will depend on the intrinsic range and distribution of frequencies of the stars. The periodic nature of the gaps in CoRoT observations, just in the range of the pulsational frequency content of the {delta} Scuti stars, is shown to be crucial to determine their oscillation frequencies, the first step to perform asteroseismology of these objects. Hence, here we focus on the impact of pre-whitening on the asteroseismic characterization of {delta} Scuti stars. We select a sample of 15 {delta} Scuti stars observed by the CoRoT satellite, for which ultra-high quality photometric data have been obtained by its seismic channel. In order to study the impact on the asteroseismic characterization of {delta} Scuti stars we perform the pre-whitening procedure on three datasets: gapped data, linearly interpolated data, and data with gaps interpolated using Autoregressive and Moving Average models (ARMA). The different results obtained show that at least in some cases pre-whitening is not an efficient procedure for the deconvolution of the spectral window. Therefore, in order to reduce the effect of the spectral window to the minimum it is necessary to interpolate with an algorithm that is aimed to preserve the original frequency content, and not only to perform a pre-whitening of the data.2018A&A...614A..40Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/614/A40CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/corot : CoRoT observation log (CoRoT, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/614/A40https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/614/A40http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/614/A40https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/614/A40https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/614/A40http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/614/A40GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/614/A40/list (List of studied stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/614/A40/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/614/A40/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/614/A40/list?GETtext/xml+votable180.050000true103.7088120833-1.07077138890.0055555555555555566/22035 22038 22046 22077 22114 23581 23604 23808 30260 30301 30404-30405 30439 30441https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/614/A40?format=asciidefaultJ/A+A/614/A40/listList of studied starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainARMAName of the table with frequencies in ARMA interpolated datameta.id;meta.filecharlinName of the table with frequencies in linear interpolated datameta.id;meta.filechargappedName of the table with frequencies in gapped interpolated datameta.id;meta.filecharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/614/A40/armaFrequencies in ARMA interpolated data (tables 5-19)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharFreqFrequencyd**-1em.freqdoubleSigniSignificance of frequency (1)stat.fit.goodness;em.freqdoubleAmpAmplitudesrc.var.amplitudedoublePhasePhaseradtime.phasefloatJ/A+A/614/A40/gappedFrequencies in gapped data (tables 35-49)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharFreqFrequencyd**-1em.freqdoubleSigniSignificance of frequency (1)stat.fit.goodness;em.freqdoubleAmpAmplitudesrc.var.amplitudedoublePhasePhaseradtime.phasefloatJ/A+A/614/A40/linearFrequencies in linearly interpolated data (tables 20-34)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharFreqFrequencyd**-1em.freqdoubleSigniSignificance of frequency (1)stat.fit.goodness;em.freqdoubleAmpAmplitudesrc.var.amplitudedoublePhasePhaseradtime.phasefloat