Poster Open Access

Transit Timing in the Kepler Field with PLATO: The case for 24 cameras on the Kepler Field

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


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    <dct:title>Transit Timing in the Kepler Field with PLATO: The case for 24 cameras on the Kepler Field</dct:title>
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    <dct:description>&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;</dct:description>
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