  X-ray radiation, in particular radiation between 0.1 keV and 10 keV, is
evident from both point-like sources, such as compact objects and T-Tauri young
stellar objects, and extended emission from hot, cooling gas, such as in
supernova remnants. The X-ray radiation is absorbed by nearby gas, providing a
source of both heating and ionization. While protoplanetary chemistry models
now often include X-ray emission from the central young stellar object,
simulations of star-forming regions have yet to include X-ray emission coupled
to the chemo-dynamical evolution of the gas. We present an extension of the
{\sc TreeRay} reverse raytrace algorithm implemented in the {\sc Flash}
magneto-hydrodynamic code which enables the inclusion of X-ray radiation from
0.1 keV $< E_{\gamma} <$ 100 keV, dubbed {\rm XrayTheSpot}. {\sc XrayTheSpot}
allows for the use of an arbitrary number of bins, minimum and maximum
energies, and both temperature-independent and temperature-dependent
user-defined cross sections, along with the ability to include both point and
extended diffuse emission and is coupled to the thermochemical evolution. We
demonstrate the method with several multi-bin benchmarks testing the radiation
transfer solution and coupling to the thermochemistry. Finally, we show two
example star formation science cases for this module: X-ray emission from
protostellar accretion irradiating an accretion disk and simulations of
molecular clouds with active chemistry, radiation pressure, protostellar
radiation feedback from infrared to X-ray radiation.
