  The star V2282 Sgr is positionally consistent with a strong Chandra X-ray and
a Spitzer/IRAC MIR source. We derived its long term $I$-band light curve from
the photographic archives of the Asiago and Catania Observatories, covering the
years from 1965 to 1984. CCD $R_C$ photometry in Summer 2009 was re-analyzed.
Optical spectra were secured at Loiano Observatory in 2011 and 2012. J H K
photometry, obtained from several experiments in different epochs was compared
and the Spitzer images were re-analyzed.
  V2282 Sgr was found to be irregular variable in all wavelengths.
Spectroscopically, it shows strong emission features (H Balmer lines, [NII]6584
AA and [OIII]5007/4959 AA) while the Na D doublet is very strong, indicating a
circumstellar envelope. A single thermal energy distribution cannot reproduce
the observed SED, while it can be explained as the sum of a G-type star plus a
variable circumstellar disc, which mimics a class 0/I object. Most likely,
V2282 Sgr is a 1-2 $M_{sun}$ mass pre main sequence star with an accretion
disk.
