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We present a near-IR study of the EXor variable V1118 Ori, performed byfollowing a slightly declining phase after a recent outburst. In particular,the near-IR (0.8 - 2.3 micron) spectrum, obtained for the first time, shows alarge variety of emission features of the HI and HeI recombination and COovertone. By comparing the observed spectrum with a wind model, a mass lossrate value is derived along with other parameters whose values are typical ofan accreting T Tauri star. In addition, we have used X-ray data from the XMMarchive, taken in two different epochs during the declining phase monitored inIR. X-ray emission (in the range 0.5 - 10 keV) permits to derive severalparameters which confirm the T Tauri nature of the source. In the near-IR theobject maintains a low visual extinction during all the activity phases,confirming that variable extinction does not contribute to brightnessvariations. The lack of both a significant amount of circumstellar material andany evidence of IR cooling from collimated jet/outflow driven by the source,indicates that, at least this member of the EXor class, is in a late stage ofthe Pre-Main Sequence evolution. In the X-ray regime, an evident fading ispresent, detected in the post-outburst phase, that cannot be reconciled withthe presence of any absorbing material. This circumstance, combined with thepersistence (in the pre- and post-outburst phases) of a temperature componentat about 10 MK, suggests that accretion has some influence in regulating thecoronal activity

Evidence for T Tauri-like emission in the EXor V1118 Ori from near-IR and X-ray data