Forum Springer Astron. Astrophys.
Forum Whats New Search Orders

Astron. Astrophys. 351, L15-L18 (1999)

Previous Section Next Section Title Page Table of Contents

2. Observations and data analysis

The observations used for the analysis are listed in Table 1. For the timing analysis in the [FORMULA] keV energy range the RXTE /PCA (Bradt, Swank & Rothschild 1993) data in the `binned' and `event' modes containing X-ray events below and above 13 keV respectively were used. We generated power density spectra (PDS) in the [FORMULA] Hz frequency range accumulated in the 4 s time intervals (Leahy et al. 1983). The PDS were linearly rebinned into 0.25 Hz bins. The white-noise level due to Poissonian statistics corrected for the dead-time effects was subtracted. For the determination of the QPO centroid frequencies the PDS were fitted to the analytic model consisting of a Lorentzian profile and a power law continuum in the [FORMULA] Hz frequency range (typical error of the derived value of the QPO frequency is [FORMULA] Hz).


Table 1. The list of RXTE /PCA observations of GRS 1915+105 used for the analysis.

Previous Section Next Section Title Page Table of Contents

© European Southern Observatory (ESO) 1999

Online publication: November 3, 1999