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tokens: for the independent frequencies are also quoted. Formal errors on the amplitudes are ± 0.3 mmag in u and ± 0.2 mmag in v , y , B , and R . These formal errors are known to underestimate the real errors by about a factor of 2 (Handler et al. 2000 ; JHS ). The S/N quoted is for the data set used to create Fig. 3 . The detected signals are separated in groups of independent pressure and mixed modes (numerical subscripts), gravity modes (letter subscripts), as well as first-, second-, and third-order combination frequencies, respectively. The residuals from this solution were searched for other signals that may be intrinsic to the star. We analysed the amplitude-scaled residuals in the different filters (whereby the u data were divided by 1.5, the v and B data are divided by 1.05, and the R data are multiplied by 1.05 to scale them to amplitudes similar to that in the y filter), and using different combinations of data sets. Even though some interesting possibilities for further intrinsic pulsation frequencies offered themselves, we prefer to err on the side of caution and stop the frequency search at this point. Nevertheless, it is interesting to note that the residual scatter in the light curves (6.4 mmag per point in u , 5.2 mmag per point in v , 4.5 mmag per point in y , 5.5 mmag per orbit in B , and 4.2 mmag per orbit in R ) is larger than the precision of the observations. This may be partly explicable by data reduction imperfections, but residual intrinsic stellar variability is also likely involved. 4 MODE IDENTIFICATION BRITE-Constellation was designed to obtain multicolour time series photometry specifically to provide identifications of the spherical degree l of the modes of pulsating stars (Weiss et al. 2014 ). Daszyńska-Daszkiewicz ( 2008 ) provided diagnostic diagrams to perform such mode identifications from a comparison of the amplitude ratios and phase shifts between the two BRITE passbands. The four strongest modes of ν Eri are, both spectroscopically and photometrically, uniquely identified (De Ridder et al. 2004 ; Handler et al. 2004 ; Daszyńska-Daszkiewicz Walczak 2010 ): the strongest mode is radial (spherical degree l = 0) and the high-amplitude triplet consists of dipole modes ( l = 1). In Fig. 4 , the observed uvyBR amplitude ratios are compared to theoretical predictions for the used Strömgren and BRITE passbands for these four modes. Figure 4. Identification of the spherical degree of the four strongest pulsation modes of ν Eri. The filled circles with error bars are the observed amplitude ratios, in order of increasing wavelength u / u , v / u , B / u , y / u , and R / u . The full lines are theoretical predictions for radial modes, the dashed lines for dipole modes, the dashed–dotted lines for quadrupole modes, the dotted lines for l = 3 modes, and the dashed–dot–dot–dotted lines are for l = 4. The thin error bars delineate the uncertainties in the theoretical amplitude ratios. The theoretical amplitude ratios were