2018MNRAS.475..359B

KIC 5123889 was observed by Kepler almost continuously over a 4-yr period in long-cadence mode. The periodogram shows 14 low-frequency peaks spaced at almost exactly equidistant periods that are shown to be dipole gravity modes. Because the period spacing is practically constant, it can be deduced that the internal rotation period is probably in excess of 1 yr, allowing non-rotating models to be used for frequency matching. For a given metallicity and overshoot parameter, there is a strong correlation between the period spacing and the effective temperature in models covering the main-sequence band. The periods of all 14 dipole modes can be matched with the models to a precision of about 0.1 per cent. In addition, 51 peaks with frequencies in the range 1.7-2.8 d^–1 are identified as combinations of the dipole mode frequencies. Four peaks in the frequency range 12.7-18.5 d^–1, two of which have high amplitudes, identify the star as a δ Scuti. An attempt to fit the high frequencies using the restrictions imposed by the dipole gravity modes is not convincing as no unique identification can be made. Combination frequencies involving the δ Scuti frequencies and the dipole modes are also present.