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After a long-lasting period of quiescence of about a decade, the source V1118Ori, one of the most representative members of the EXor variables, is nowoutbursting. Since the initial increase of the near-infrared flux of about 1mag (JHK bands) registered on 2015 September 22, the source brightness hasremained fairly stable. We estimate DeltaV about 3 mag with respect to thequiescence phase. An optical/near-IR low-resolution spectrum has been obtainedwith the Large Binocular Telescope instruments MODS and LUCI2, and comparedwith a spectrum of similar spectral resolution and sensitivity level takenduring quiescence. Together with the enhancement of the continuum, the outburstspectrum presents a definitely higher number of emission lines, in particularHI recombination lines of the Balmer, Paschen, and Brackett series, along withbright permitted lines of several species, forbidden atomic lines, and COro-vibrational lines. Both mass accretion and mass loss rates havesignificantly increased (by to about an order of magnitude, mass accretion rate= 1.2-4.8 10^-8 M_sun/yr, mass loss rate = 0.8-2 10^-9 M_sun/yr) with respectto the quiescence phase. If compared with previous outbursts, the present oneappears less energetic. Alternatively, it could already be in the fading phase(with the maximum brightness level reached when the source was not visible),or, viceversa, still in the rising phase.

On the 2015 outburst of the EXor variable star V1118 Ori