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

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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]

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


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© European Southern Observatory (ESO) 1999

Online publication: November 3, 1999
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