2005A&A...443..271S

The effect of rotation on the Frequency Ratio Method (Moya et al., 2005A&A...432..189M) is examined. Its applicability to observed frequencies of rotating γ Doradus stars is discussed taking into account the following aspects: the use of a perturbative approach to compute adiabatic oscillation frequencies; the effect of rotation on the observational Brunt-Vaeisaelae integral determination and finally, the problem of disentangling multiplet-like structures from frequency patterns due to the period spacing expected for high-order gravity modes in asymptotic regime. This analysis reveals that the FRM produces reliable results for objects with rotational velocities up to 70km/s, for which the FRM intrinsic error increases one order of magnitude with respect to the typical FRM errors given in Moya et al. (2005A&A...432..189M). Our computations suggest that, given the spherical degree l identification, the FRM may be discriminating for m=0 modes, in the sense that the method avoids any misinterpretation induced by the presence of rotationally split multiplet-like structures, which reinforces the robustness of the method. However, if l is unknown, such discrimination is not ensured. In order to check the FRM in presence of slow-moderate rotation, we have applied it to the three observed frequencies of the slowly rotating (vsin i=29km/s) γ Doradus star HD48501.