We present analyses of archival X-ray data obtained from the XMM-Newton satellite and optical photometric data obtained from 1 m class telescopes of ARIES , Nainital of a magnetic cataclysmic variable ( MCV ) Paloma .
Two persistent periods at 156 \pm 1 minutes and 130 \pm 1 minutes are present in the X-ray data , which we interpret as the orbital and spin periods , respectively .
These periods are similar to those obtained from the previous as well as new optical photometric observations .
The soft-X-ray excess seen in the X-ray spectrum of Paloma and the averaged X-ray spectra are well fitted by two-temperature plasma models with temperatures of 0.10 _ { -0.01 } ^ { +0.02 } and 13.0 _ { -0.5 } ^ { +0.5 } keV with an Fe K \alpha line and an absorbing column density of 4.6 \times 10 22 cm -2 .
This material partially covers 60 \pm 2 % of the X-ray source .
We also present the orbital and spin-phase-resolved spectroscopy of Paloma in the 0.3 - 10.0 keV energy band and find that the X-ray spectral parameters show orbital and spin-phase dependencies .
New results obtained from optical and X-ray studies of Paloma indicate that it belongs to a class of a few magnetic CVs that seem to have the characteristics of both the polars and the intermediate polars .