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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    <subfield code="a">&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;
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;
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;
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;
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