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Direct detection of thermal emission from nearby hot Jupiters has greatlyadvanced our knowledge of extrasolar planets in recent years. Since hot Jupitersystems can be regarded as analogs of high contrast binaries, ground-basedinfrared long baseline interferometers have the potential to resolve them anddetect their thermal emission with precision closure phase - a method that isimmune to the systematic errors induced by the Earth's atmosphere. In thiswork, we present closure phase studies toward direct detection of nearby hotJupiters using the CHARA interferometer array outfitted with the MIRCinstrument. We carry out closure phase simulations and conduct a large numberof observations for the best candidate {\upsion} And. Our experiments suggestthe method is feasible with highly stable and precise closure phases. However,we also find much larger systematic errors than expected in the observations,most likely caused by dispersion across different wavelengths. We find thatusing higher spectral resolution modes (e.g., R=150) can significantly reducethe systematics. By combining all calibrators in an observing run together, weare able to roughly recalibrate the lower spectral resolution data, allowing usto obtain upper limits of the star-planet contrast ratios of {\upsion} And bacross the H band. The data also allow us to get a refined stellar radius of1.625\pm0.011 R\odot. Our best upper limit corresponds to a contrast ratio of2.1\times10^3:1 with 90% confidence level at 1.52{\mu}m, suggesting that we arestarting to have the capability of constraining atmospheric models of hotJupiters with interferometry. With recent and upcoming improvements ofCHARA/MIRC, the prospect of detecting emission from hot Jupiters with closurephases is promising.

Toward Direct Detection of Hot Jupiters with Precision Closure Phase: Calibration Studies and First Results from the CHARA Array