2012MNRAS.426.2137W

High-speed photometric observations of the spectroscopically discovered PG 1159 star SDSSJ034917.41-005917.9 in 2007 and 2009 reveal a suite of pulsation frequencies in the range of 1038–3323 µHz with amplitudes between 3.5 and 18.6mmag. SDSSJ034917.41-005917.9 is therefore a member of the GW Vir class of pulsating pre-white dwarfs. We have identified 10 independent pulsation frequencies that can be fitted by an asymptotic model with a constant period spacing of 23.61±0.21s, presumably associated with a sequence of l = 1 modes. The highest amplitude peak in the suite of frequencies shows evidence for a triplet structure, with a frequency separation of 14.4 µHz. Five of the identified frequencies do not fit the l = 1 sequence, but are, however, well modelled by an independent asymptotic sequence with a constant period spacing of 11.66±0.13s. It is unclear to which l mode these frequencies belong.