quasi-periodic kernel for the time trend, again with the eclipses masked. In both cases (squared-exponential and quasi-periodic kernels) the trend with position determined from the data between the eclipses was used to interpolate a correction to the data during the eclipses. f These light curves are shown in Figs. \[lcplot1\], \[lcplot2a\], \[lcplot2b\] and \[lcplot3\].

![image](Figs/lcplot1.png)

![image](Figs/lcplot2a.png)

![image](Figs/lcplot2b.png)

![image](Figs/lcplot3.png)

WASP archive photometry
-----------------------

The WASP project has obtained over 580 billion photometric observations for more than 30 million bright stars during a survey that has discovered more than 150 transiting exoplanets since observations started in May 2004 [@2006PASP..118.1407P]. WASP photometry is available for many of the systems in Table \[lcinfo\], but is of much lower quality than the K2 photometry. Nevertheless, WASP photometry has enabled us to determine or refine the orbital period for long-period binaries where only two or three eclipses have been observed by the Kepler K2 mission.

![image](Figs/201161715fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201246763fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201253025fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201379113fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201382417fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201408204fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201488365fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201576812fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201648133fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201665500fit-eps-converted-to.pdf){width="49.00000%"}

![image](Figs/201705526fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/201723461fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/202674012fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/EPIC202674012_rvfit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/202843085fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/203361171fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/203371239fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/203543668fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/203610780fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/203636784fit-eps-converted-to.pdf){width="49.00000%"}

![image](Figs/203728604fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/204407880fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/204748201fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/204822807fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/204760247fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/204760247rvfit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/204870619fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205170307fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205020466fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205020466rvfit-eps-converted-to.pdf){width="49.00000%"}

![image](Figs/205546169fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205703649fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205919993fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205919993rvfit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/205982900fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206066862fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206066909fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206084435fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206109641fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206212261fit-eps-converted-to.pdf){width="49.00000%"}

![image](Figs/206241558fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206288770fit-eps-converted-to.pdf){width="49.00000%"} ![image](Figs/206433263fit-eps-converted-to.pdf){width="49.00000%"}

The two WASP instruments are located at the 