  We present new results from optical photometric and spectroscopic
observations of the eruptive pre-main sequence star V2493 Cyg (HBC 722). The
object has continued to undergo significant brightness variations over the past
few months and is an ideal target for follow-up observations. We carried out
CCD BVRI photometric observations in the field of V2493 Cyg ("Gulf of Mexico")
from August 1994 to April 2012, i.e. at the pre-outburst states and during the
phases of the outburst. We acquired high, medium, and low resolution
spectroscopy of V2493 Cyg during the outburst. To study the pre-outburst
variability of the target and construct its historical light curve, we searched
for archival observations in photographic plate collections. Both CCD and
photographic observations were analyzed using 15 comparison stars in the field
of V2493 Cyg. The pre-outburst photographic and CCD photometric observations of
V2493 Cyg show low-amplitude light variations typical of T Tauri stars. The
recent photometric data show a slow light decrease from October 2010 to June
2011 followed by an increase in brightness that continued until early 2012. The
spectral observations of V2493 Cyg are typical of FU Orionis stars absorption
spectra with strong P Cyg profiles of H alpha and Na I D lines. On the basis of
photometric monitoring performed over the past two years, the spectral
properties at the maximal light, as well as the shape of long-term light
curves, we confirm that the observed outburst of V2493 Cyg is of FU Orionis
type.
