October 5, 2021 Poster Open Access

Jontof-Hutter, Daniel; Lissauer, Jack; Rowe, Jason

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  <identifier identifierType="DOI">10.5281/zenodo.5551125</identifier>
  <creators>
    <creator>
      <creatorName>Jontof-Hutter, Daniel</creatorName>
      <givenName>Daniel</givenName>
      <familyName>Jontof-Hutter</familyName>
      <affiliation>University of the Pacific</affiliation>
    </creator>
    <creator>
      <creatorName>Lissauer, Jack</creatorName>
      <givenName>Jack</givenName>
      <familyName>Lissauer</familyName>
      <affiliation>NASA Ames Research Center</affiliation>
    </creator>
    <creator>
      <creatorName>Rowe, Jason</creatorName>
      <givenName>Jason</givenName>
      <familyName>Rowe</familyName>
      <affiliation>Bishop's University</affiliation>
    </creator>
  </creators>
  <titles>
    <title>Transit Timing in the Kepler Field with PLATO: The case for 24 cameras on the Kepler Field</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2021</publicationYear>
  <dates>
    <date dateType="Issued">2021-10-05</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/5551125</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.5551124</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/plato2021</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="https://creativecommons.org/licenses/by/4.0/legalcode">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">&lt;p&gt;Since TTV signals increase with observational baseline,&amp;nbsp;PLATO&amp;#39;s stare at the&lt;br&gt;
Kepler field will yield transit timing variations with a total baseline that&lt;br&gt;
includes both missions, an important opportunity unique to the&amp;nbsp;PLATO&amp;nbsp;mission.&lt;br&gt;
&lt;br&gt;
We discuss the regimes in period and radius where Kepler and TESS provide&lt;br&gt;
good samples for planet characterization, and highlight where&amp;nbsp;PLATO&amp;nbsp;could&lt;br&gt;
maximize its impact; where Kepler planets are expected to have TTV signals&lt;br&gt;
regardless of their prior detection, and where the TTV periodicity is&lt;br&gt;
comparable to or exceeds the Kepler baseline.&lt;br&gt;
&lt;br&gt;
We argue that&amp;nbsp;PLATO&amp;#39;s impact in characterizing low-mass planets with transit&lt;br&gt;
timing will be significantly enhanced by centering Long-duration Observation&lt;br&gt;
Phases on the Kepler field to ensure that 24 cameras observe Kepler targets,&lt;br&gt;
enabling similar transit timing precision to Kepler. Transit timing&lt;br&gt;
uncertainty scales as ~1/SNR. Hence, having just 6 (or 12) cameras on the&lt;br&gt;
Kepler field instead of 24 would increase transit timing uncertainties by ~2&lt;br&gt;
(or sqrt(2)).&lt;br&gt;
&lt;br&gt;
Finally, we provide some examples of anticipated highlights from&amp;nbsp;PLATO&amp;nbsp;in&lt;br&gt;
characterizing planets with transit timing.&lt;br&gt;
&amp;nbsp;&lt;/p&gt;</description>
  </descriptions>
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