The $K2$ & $TESS$ Synergy I: Updated Ephemerides and Parameters for K2-114, K2-167, K2-237, & K2-261. (arXiv:2007.00678v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ikwut_Ukwa_M/0/1/0/all/0/1">Mma Ikwut-Ukwa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_J/0/1/0/all/0/1">Joseph E. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bieryla_A/0/1/0/all/0/1">Allyson Bieryla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderburg_A/0/1/0/all/0/1">Andrew Vanderburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mocnik_T/0/1/0/all/0/1">Teo Mocnik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kane_S/0/1/0/all/0/1">Stephen R. Kane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quinn_S/0/1/0/all/0/1">Samuel N. Quinn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colon_K/0/1/0/all/0/1">Knicole D. Colón</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_G/0/1/0/all/0/1">George Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eastman_J/0/1/0/all/0/1">Jason D. Eastman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_C/0/1/0/all/0/1">Chelsea X. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">David W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dotson_J/0/1/0/all/0/1">Jessie Dotson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">Jon M. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">George R. Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seager_S/0/1/0/all/0/1">Sara Seager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderspek_R/0/1/0/all/0/1">Roland K. Vanderspek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">Joshua N. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barclay_T/0/1/0/all/0/1">Thomas Barclay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barentsen_G/0/1/0/all/0/1">Geert Barentsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berta_Thompson_Z/0/1/0/all/0/1">Zachory Berta-Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charbonneau_D/0/1/0/all/0/1">David Charbonneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dragomir_D/0/1/0/all/0/1">Diana Dragomir</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daylan_T/0/1/0/all/0/1">Tansu Daylan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gunther_M/0/1/0/all/0/1">Maximilian Gunther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hedges_C/0/1/0/all/0/1">Christina Hedges</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henze_C/0/1/0/all/0/1">Christopher E. Henze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDermott_S/0/1/0/all/0/1">Scott McDermott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlieder_J/0/1/0/all/0/1">Joshua E. Schlieder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quintana_E/0/1/0/all/0/1">Elisa V. Quintana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_J/0/1/0/all/0/1">Jeffrey C. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Twicken_J/0/1/0/all/0/1">Joseph D. Twicken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yahalomi_D/0/1/0/all/0/1">Daniel A. Yahalomi</a>
Although the $TESS$ primary mission observed the northern and southern
ecliptic hemispheres, generally avoiding the ecliptic, and the $Kepler$ space
telescope during the $K2$ mission could only observe near the ecliptic, many of
the $K2$ fields extend far enough from the ecliptic plane that sections overlap
with $TESS$ fields. Using photometric observations from both $K2$ and $TESS$,
combined with archival spectroscopic observations, we globally modeled four
known planetary systems discovered by $K2$ that were observed in the first year
of the primary $TESS$ mission. Specifically, we provide updated ephemerides and
system parameters for K2-114 b, K2-167 b, K2-237 b, and K2-261 b. These were
some of the first $K2$ planets to be observed by $TESS$ in the first year and
include three Jovian sized planets and a sub-Neptune with orbital periods less
than 12 days. In each case, the updated ephemeris significantly reduces the
uncertainty in prediction of future times of transit, which is valuable for
planning observations with the James Webb Space Telescope and other future
facilities. The $TESS$ extended mission is expected to observe about half of
the $K2$ fields, providing the opportunity to perform this type of analysis on
a larger number of systems.
Although the $TESS$ primary mission observed the northern and southern
ecliptic hemispheres, generally avoiding the ecliptic, and the $Kepler$ space
telescope during the $K2$ mission could only observe near the ecliptic, many of
the $K2$ fields extend far enough from the ecliptic plane that sections overlap
with $TESS$ fields. Using photometric observations from both $K2$ and $TESS$,
combined with archival spectroscopic observations, we globally modeled four
known planetary systems discovered by $K2$ that were observed in the first year
of the primary $TESS$ mission. Specifically, we provide updated ephemerides and
system parameters for K2-114 b, K2-167 b, K2-237 b, and K2-261 b. These were
some of the first $K2$ planets to be observed by $TESS$ in the first year and
include three Jovian sized planets and a sub-Neptune with orbital periods less
than 12 days. In each case, the updated ephemeris significantly reduces the
uncertainty in prediction of future times of transit, which is valuable for
planning observations with the James Webb Space Telescope and other future
facilities. The $TESS$ extended mission is expected to observe about half of
the $K2$ fields, providing the opportunity to perform this type of analysis on
a larger number of systems.
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