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We present Spitzer 4.5\micron\ light curve observations, Keck NIRSPEC radialvelocity observations, and LCOGT optical light curve observations ofPTFO~8-8695, which may host a Jupiter-sized planet in a very short orbitalperiod (0.45 days). Previous work by \citet{vaneyken12} and \citet{barnes13}predicts that the stellar rotation axis and the planetary orbital plane shouldprecess with a period of $300 - 600$ days. As a consequence, the observedtransits should change shape and depth, disappear, and reappear with theprecession. Our observations indicate the long-term presence of the transitevents ($>3$ years), and that the transits indeed do change depth, disappearand reappear. The Spitzer observations and the NIRSPEC radial velocityobservations (with contemporaneous LCOGT optical light curve data) areconsistent with the predicted transit times and depths for the $M_\star = 0.34\M_\odot$ precession model and demonstrate the disappearance of the transits. AnLCOGT optical light curve shows that the transits do reappear approximately 1year later. The observed transits occur at the times predicted by astraight-forward propagation of the transit ephemeris. The precession modelcorrectly predicts the depth and time of the Spitzer transit and the lack of atransit at the time of the NIRSPEC radial velocity observations. However, theprecession model predicts the return of the transits approximately 1 monthlater than observed by LCOGT. Overall, the data are suggestive that theplanetary interpretation of the observed transit events may indeed be correct,but the precession model and data are currently insufficient to confirm firmlythe planetary status of PTFO~8-8695b.

Follow-Up Observations of PTFO 8-8695: A 3 MYr Old T-Tauri Star Hosting a Jupiter-mass Planetary Candidate