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How the stellar flicker noise affects the characterization of planetary transits ?

Sulis Sophia

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        <dct:identifier rdf:datatype="">0000-0001-8783-526X</dct:identifier>
        <foaf:name>Sulis Sophia</foaf:name>
            <foaf:name>Laboratoire d'astrophysique de Marseille</foaf:name>
    <dct:title>How the stellar flicker noise affects the characterization of planetary transits ?</dct:title>
    <dct:issued rdf:datatype="">2021</dct:issued>
    <dcat:keyword>exoplanet, stellar activity, characterization</dcat:keyword>
    <dct:issued rdf:datatype="">2021-10-06</dct:issued>
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    <dct:description>&lt;p&gt;Stellar activity is known to limit exoplanet detection and characterization. Among this activity, stellar convection (``flicker&amp;#39;&amp;#39;) evolves during the typical transit timescales (~ hours) and affects the inferred transit parameters.&lt;br&gt; We generated realistic simulations of transiting exoplanets based on solar HMI data. These simulations include planets from 1 to 10 Earth radii with different transit geometries. These simulations comprising hundreds of light curves are available to the community :;br&gt; We analyzed the data using standard MCMC methods assuming the noise is white and Gaussian (WGN), or a Gaussian Process (GP). We show that, in both cases, the resulting planet parameters can be affected by biases,&lt;br&gt; which leads to biased planetary radius measurements. This demonstrates the need to develop robust stellar noise modeling to achieve PLATO&amp;#39;s goal of characterizing exoplanets transiting solar-like stars.&lt;br&gt; Next steps of this study will be to investigate&lt;br&gt; i) how other noise sources (e.g., flares, spots and faculae) affect the inferred exoplanet parameters,&lt;br&gt; ii) which noise modeling allows to derive the most accurate transit parameters.&lt;/p&gt;</dct:description>
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