J/MNRAS/474/2094ivo://CDS.VizieR/J/MNRAS/474/2094doi:10.26093/cds/vizier.74742094CDSAngus R.Morton T.Aigrain S.Foreman-Mackey D.Rajpaul V.2024-08-18T20:17:10Z2021-03-04T09:50:38ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsVariability in the light curves of spotted, rotating stars is often non-sinusoidal and quasi-periodic - spots move on the stellar surface and have finite lifetimes, causing stellar flux variations to slowly shift in phase. A strictly periodic sinusoid therefore cannot accurately model a rotationally modulated stellar light curve. Physical models of stellar surfaces have many drawbacks preventing effective inference, such as highly degenerate or high-dimensional parameter spaces. In this work, we test an appropriate effective model: a Gaussian Process with a quasi-periodic covariance kernel function. This highly flexible model allows sampling of the posterior probability density function of the periodic parameter, marginalizing over the other kernel hyperparameters using a Markov Chain Monte Carlo approach. To test the effectiveness of this method, we infer rotation periods from 333 simulated stellar light curves, demonstrating that the Gaussian process method produces periods that are more accurate than both a sine-fitting periodogram and an autocorrelation function method. We also demonstrate that it works well on real data, by inferring rotation periods for 275 Kepler stars with previously measured periods. We provide a table of rotation periods for these and many more, altogether 1102 Kepler objects of interest, and their posterior probability density function samples. Because this method delivers posterior probability density functions, it will enable hierarchical studies involving stellar rotation, particularly those involving population modelling, such as inferring stellar ages, obliquities in exoplanet systems, or characterizing star-planet interactions. The code used to implement this method is available online (https://github.com/RuthAngus/GProtation/).2018MNRAS.474.2094Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/474/2094CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/133 : Kepler Input Catalog (Kepler Mission Team, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/474/2094https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/474/2094http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/474/2094https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/474/2094https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/474/2094http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/474/2094GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/474/2094/table5 (Rotation periods and Kepler input catalogue (KIC) properties for 1102 Kepler objects of interest)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/474/2094/table5?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/474/2094/table5?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/474/2094/table5?GETtext/xml+votable180.050000true286.808491449.31641420.0055555555555555564/922 933-935 945 5/3645-3647 3683 3693-3695 3704 3706 3729-3731 3776-3778 3785-3789 3792 6/14567 14573 14575 14578-14579 14730-14731 14738 14744 14746 14750-14751 14768-14770 14792 14794-14795 14828 14830 14914-14915 15040-15041 15043-15045 15057 15059-15062 15116 15118-15119 15136-15137 15139 15160 15172-15174 15176 15178 15200 15232https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/474/2094?format=asciidefaultJ/MNRAS/474/2094/table5Rotation periods and Kepler input catalogue (KIC) properties for 1102 Kepler objects of interestSimbadNameSimbad column added by the CDSmeta.idcharKOIKOI numbermeta.id;meta.mainintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[Fe/H]? KIC metallicityphys.abund.Zfloatnullablee_[Fe/H]? Lower uncertainty on the KIC metallicitystat.error;phys.abund.FefloatnullableE_[Fe/H]? Upper uncertainty on the KIC metallicitystat.error;stat.maxfloatnullablelogg? KIC surface gravitylog(cm.s**-2)phys.gravityfloatnullablee_logg? Lower uncertainty on the KIC surface gravitylog(cm.s**-2)stat.errorfloatnullableE_logg? Upper uncertainty on the KIC surface gravitylog(cm.s**-2)stat.error;stat.maxfloatnullablePerStellar rotation perioddtime.perioddoublee_PerLower uncertainty on the stellar rotation perioddstat.errordoubleE_PerUpper uncertainty on the stellar rotation perioddstat.error;stat.maxdoubleTeff? KIC effective temperatureKphys.temperature.effectivefloatnullablee_Teff? Lower uncertainty on the KIC effective temperatureKstat.error;phys.temperature.effectivefloatnullableE_Teff? Upper uncertainty on the KIC effective temperatureKstat.error;stat.maxfloatnullable_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main