Poster Open Access

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

Sulis Sophia

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  <identifier identifierType="DOI">10.5281/zenodo.5552619</identifier>
      <creatorName>Sulis Sophia</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0001-8783-526X</nameIdentifier>
      <affiliation>Laboratoire d'astrophysique de Marseille</affiliation>
    <title>How the stellar flicker noise affects the characterization of planetary transits ?</title>
    <subject>exoplanet, stellar activity, characterization</subject>
    <date dateType="Issued">2021-10-06</date>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
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    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.5552618</relatedIdentifier>
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    <rights rightsURI="">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
    <description descriptionType="Abstract">&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;</description>
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