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(Abridged) We present a spectral analysis of a deep (220 ks) XMM-Newtonobservation of the Phoenix cluster (SPT-CL J2344-4243), which we also combinewith Chandra archival ACIS-I data. We extract CCD and RGS X-ray spectra fromthe core region to search for the signature of cold gas, and constrain the massdeposition rate in the cooling flow which is thought to be responsible of themassive star formation episode observed in the BCG. We find an average massdeposition rate of $\dot M = 620 (-190 +200)_{stat} (-50 +150)_{syst}M_\odot$/yr in the temperature range 0.3-3.0 keV from MOS data. Atemperature-resolved analysis shows that a significant amount of gas isdeposited only above 1.8 keV, while upper limits of the order of hundreds of$M_\odot$/yr can be put in the 0.3-1.8 keV temperature range. From pn data weobtain $\dot M = 210 (-80 +85)_{stat} ( -35 +60)_{syst} M_\odot$/yr, and theupper limits from the temperature-resolved analysis are typically a factor of 3lower than MOS data. In the RGS spectrum, no line emission from ionizationstates below Fe XXIII is seen above $12 \AA$, and the amount of gas coolingbelow $\sim 3$ keV has a best-fit value $\dot M = 122_{-122}^{+343}$$M_{\odot}$/yr. In addition, our analysis of the FIR SED of the BCG based onHerschel data provides $SFR = (530 \pm 50) M_\odot$/yr, significantly lowerthan previous estimates by a factor 1.5. Current data are able to firmlyidentify substantial amount of cooling gas only above 1.8 keV in the core ofthe Phoenix cluster. While MOS data analysis is consistent with values as highas $\dot M \sim 1000$ within $1 \sigma$, pn data provide $\dot M < 500 M_\odot$yr$^{-1}$ at $3\sigma$ c.l. at temperature below 1.8 keV. At present, thisdiscrepancy cannot be explained on the basis of known calibration uncertaintiesor other sources of statistical noise.

New XMM-Newton observation of the Phoenix cluster: properties of the cool core