Presentation #413.03 in the session Physical Properties of Centaurs & KBOs (iPosters).
In the past, Kuiper Belt photometry has been primarily conducted in the visible and near-infrared range. Initial work with u-band photometry has shown that it can reveal unique surface information, including possibly confirming Haumea family members. In addition, LSST will soon revolutionize u-band photometry for small bodies. We have obtained time-resolved u-band photometry of the Haumea system in order to determine the u-g colors for Haumea, Haumea’s Dark Red Spot (Lacerda 2008), and Haumea’s largest moon Hi’iaka. We obtained these observations using BYU time at the Astronomical Research Consortium 3.5-m telescope at Apache Point Observatory. Using Bayesian parameter inference powered by Markov Chain Monte Carlo, we fit models to the Haumea system photometry including the unresolved contribution of Hi’iaka. We will present our model fits with implications for Haumea’s surface and formation.