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We obtained the first long, homogenous time-series of V2104Cyg, consisting of679 datapoints, with the uvbybeta photometers of Sierra Nevada and San PedroMartir Observatories with the aim to detect and subsequently interpret theintrinsic frequencies of this previously unstudied variable star, which turnedout to be a Be star. We try to figure out its place among the variable B starson the upper Main Sequence. In order to obtain additional information onphysical parameters we collected a few spectra with the ELODIE and FIESinstruments. We searched for frequencies in the uvby passbands using 2different frequency analysis methods and used the S/N>4 criterion to select thesignificant periodicities. We obtained an estimate of the physical parametersof the underlying B star of spectral type between B5 and B7, by correcting forthe presence of a circumstellar disk, using a formalism based on the strenghtof the Halpha line emission. We detected 3 independent frequencies withamplitudes below 0.01mag, f1 = 4.7126 c/d, f2 = 2.2342 c/d and f3 = 4.671 c/d,and discovered that V2104Cyg is a Be star. The fast rotation (vsini=290+/-10km/s, and 27<i<45) hampered the investigation of the associated pulsationalparameters l. Nevertheless, the most plausible explanation for the observedvariability of this mid-late type Be star is a non-radial pulsation model. Thispaper is based on observations obtained at the Observatorio AstronomicoNacional San Pedro Martir (Mexico), Observatorio de Sierra Nevada (Spain),Observatoire de Haute Provence (France), and on observations made with theNordic Optical Telescope, Observatorio Roque de los Muchachos, La Palma, Spain.

Multiperiodicity in the newly discovered mid-late Be star V2104 Cygni