2006A&A...459..557S

In this article we present the results of 215h of time-series photometry on the rapidly pulsating subdwarf B star PG 1325+101 (T_eff=35000K, logg=5.8, log N(He)/N(H)=-1.7), obtained during 25 days of observation in Spring 2003 from nine different sites. As in previous observations, the temporal spectrum is dominated by the main peak at 7255.55µHz, with an amplitude of about 2.7% which, however, is dropped to about 1.7% in February 2005. No secondary peaks close to the dominant pulsation mode are clearly detected. In addition, at least fourteen more pulsation frequencies are found: three of them at 7704.92, 9380.17 and 14511.10µHz were already present in the discovery run with small differences in frequency, probably due to 1-day aliasing effects. The peak at 7704.92µHz belongs to a triplet of almost equally spaced frequencies that could be due to rotational splitting and would imply a rotational period of about 1.6 days. Based on the results of this article, a detailed asteroseismic analysis of PG 1325+101 is presented in a separate paper (Charpinet et al., 2006A&A...459..565C, Paper II).