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We report on the follow-up $XMM-Newton$ observation of the persistent X-raypulsar CXOU J225355.1+624336, discovered with the CATS@BAR project on archival$Chandra$ data. The source was detected at $f_{\rm X}$(0.5-10 keV) = 3.4$\times10^{-12}$ erg cm$^{-2}$ s$^{-1}$, a flux level which is fully consistent withthe previous observations performed with $ROSAT$, $Swift$, and $Chandra$. Themeasured pulse period $P$ = 46.753(3) s, compared with the previousmeasurements, implies a constant spin down at an average rate $\dot P =5.3\times 10^{-10}$ s s$^{-1}$. The pulse profile is energy dependent, showingthree peaks at low energy and a less structured profile above about 3.5 keV.The pulsed fraction slightly increases with energy. We described thetime-averaged EPIC spectrum with four different emission models: a partiallycovered power law, a cut-off power law, and a power law with an additionalthermal component (either a black body or a collisionally ionized gas). In allcases we obtained equally good fits, so it was not possible to prefer or rejectany emission model on the statistical basis. However, we disfavour the presenceof the thermal components, since their modeled X-ray flux, resulting from aregion larger than the neutron star surface, would largely dominate the X-rayemission from the pulsar. The phase-resolved spectral analysis showed that asimple flux variation cannot explain the source variability and proved that itis characterized by a spectral variability along the pulse phase. The resultsof the $XMM-Newton$ observation confirmed that CXOU J225355.1+624336 is a BeXBwith a low-luminosity ($L_{\rm X} \sim 10^{34-35}$ erg s$^{-1}$), a limitedvariability, and a constant spin down. Therefore, they reinforce the sourceclassification as a persistent BeXB.

A deep $XMM-Newton$ observation of the X-Persei-like binary system CXOU J225355.1+624336