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We present new results from optical photometric and spectroscopicobservations of the eruptive pre-main sequence star V2493 Cyg (HBC 722). Theobject has continued to undergo significant brightness variations over the pastfew months and is an ideal target for follow-up observations. We carried outCCD 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 thephases of the outburst. We acquired high, medium, and low resolutionspectroscopy of V2493 Cyg during the outburst. To study the pre-outburstvariability of the target and construct its historical light curve, we searchedfor archival observations in photographic plate collections. Both CCD andphotographic observations were analyzed using 15 comparison stars in the fieldof V2493 Cyg. The pre-outburst photographic and CCD photometric observations ofV2493 Cyg show low-amplitude light variations typical of T Tauri stars. Therecent photometric data show a slow light decrease from October 2010 to June2011 followed by an increase in brightness that continued until early 2012. Thespectral observations of V2493 Cyg are typical of FU Orionis stars absorptionspectra with strong P Cyg profiles of H alpha and Na I D lines. On the basis ofphotometric monitoring performed over the past two years, the spectralproperties at the maximal light, as well as the shape of long-term lightcurves, we confirm that the observed outburst of V2493 Cyg is of FU Orionistype.

Optical photometric and spectral study of the new FU Orionis object V2493 Cyg (HBC 722)