  We present the analysis of archival XMM-Newton and Chandra observations of CH
Cyg, one of the most studied symbiotic stars (SySts). The combination of the
high-resolution XMM-Newton RGS and Chandra HETG X-ray spectra allowed us to
obtain reliable estimates of the chemical abundances and to corroborate the
presence of multi-temperature X-ray-emitting gas. Spectral fitting of the
medium-resolution XMM-Newton MOS (MOS1+MOS2) spectrum required the use of an
additional component not seen in previous studies in order to fit the 2.0-4.0
keV energy range. Detailed spectral modelling of the XMM-Newton MOS data
suggests the presence of a reflection component, very similar to that found in
active galactic nuclei. The reflection component is very likely produced by an
ionised disk (the accretion disk around the white dwarf) and naturally explains
the presence of the fluorescent Fe emission line at 6.4 keV while also
contributing to the soft and medium energy ranges. The variability of the
global X-ray properties of CH Cyg are discussed as well as the variation of the
three Fe lines around the 6-7 keV energy range. We conclude that reflection
components are needed to model the hard X-ray emission and may be present in
most $\beta/\delta$-type SySt.
