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Titan's thick atmosphere is primarily composed of nitrogen and methane.Complex chemistry happening in Titan's atmosphere produces optically thickorganic hazes. These hazes play significant roles in Titan's atmosphere and onits surface, and their optical properties are crucial for understanding manyprocesses happening on Titan. Due to the lack of such information, the opticalconstants of laboratory prepared Titan haze analogues are essential inputs foratmospheric modeling and data analysis of remote sensing observations of Titan.Here, we perform laboratory simulations in a Titan relevant environment,analyze the resulting Titan haze analogues using vacuum Fourier transforminfrared spectroscopy, and calculate the optical constants from the measuredtransmittance and reflectance spectra. We provide a reliable set of opticalconstants of Titan haze analogue in the wavelength range from 0.4 to 3.5 micronand will extend to 28.5 micron in the near future, which can both be used foranalyzing existing and future observational data of Titan. This studyestablishes a feasible method to determine optical constants of haze analoguesof (exo)planetary bodies.

Optical Constants of Titan Haze Analogue from 0.4 to 3.5 {\mu}m: Determined Using Vacuum Spectroscopy