  Close binary systems provide an excellent tool to determine stellar
parameters such as radii and masses with a high degree of precision. Due to the
high rotational velocities, most of these systems exhibit strong signs of
magnetic activity, which has been postulated to be the underlying reason for
radius inflation in many of the components. We aim to extend the sample of
low-mass binary systems with well-known X-ray properties. For this, we analyze
data from a singular XMM-Newton pointing of the close, low-mass eclipsing
binary system BX Tri. The UV light curve is modeled with the eclipsing binary
modeling tool PHOEBE and data acquired with the EPIC cameras is analyzed to
search for hints of orbital modulation. We find clear evidence of orbital
modulation in the UV light curve and show that PHOEBE is fully capable of
modeling data within this wavelength range. Comparison to a theoretical flux
prediction based on PHOENIX models shows that the majority of UV emission is of
photospheric origin. While the X-ray light curve does exhibit strong
variations, the signal-to-noise ratio of the observation is insufficient for a
clear detection of signs of orbital modulation. There is evidence of a
Neupert-like correlation between UV and X-ray data.
