2004 TT357: A potential contact binary in the Trans-Neptunian belt

We report photometric observations of the trans-Neptunian object 2004~TT$_{357}$ obtained in 2015 and 2017 using the 4.3~m Lowell's Discovery Channel Telescope. We derive a rotational period of 7.79$\pm$0.01~h and a peak-to-peak lightcurve amplitude of 0.76$\pm$0.03~mag. 2004 TT$_{357}$ displays a large variability that can be explained by a very elongated single object or can be due to a contact/close binary. The most likely scenario is that 2004 TT$_{357}$ is a contact binary. If it is in hydrostatic equilibrium, we find that the lightcurve can be explained by a system with a mass ratio q$_{min}$=0.45$\pm$0.05, and a density of $\rho_{min}$=2g cm$^{-3}$, or less likely a system with q$_{max}$=0.8$\pm$0.05, and $\rho_{max}$=5g cm$^{-3}$. Considering a single triaxial ellipsoid in hydrostatic equilibrium, we derive a lower limit to the density of 0.78g cm$^{-3}$, and an elongation (a/b) of 2.01 assuming an equatorial view. From Hubble Space Telescope data, we report no resolved companion orbiting 2004 TT$_{357}$. Despite an expected high fraction of contact binaries in the trans-Neptunian belt, 2001 QG$_{298}$ is the unique confirmed contact binary in the trans-Neptunian belt, and 2004 TT$_{357}$ is only the second candidate to this class of systems, with 2003 SQ$_{317}$.