Abstract. In this paper we discuss the methods developed for the production of the INTEGRAL/SPI instrument response. The response files were produced using a suite of Monte Carlo simulation software developed at NASA/GSFC based on the GEANT-3 package available from CERN. The production of the INTEGRAL/SPI instrument response also required the development of a detailed computer mass model for SPI. We discuss our extensive investigations into methods to reduce both the computation time and storage requirements for the SPI response. We also discuss corrections to the simulated response based on our comparison of ground and inflight calibration data with MGEANT simulations.

We have obtained Fourier-resolved spectra of the black hole binary 4U 1543-47 in the canonical states (high/soft, very high, intermediate, and low/hard) observed in this source during the decay of an outburst that took place in 2002. Our objective is to investigate the variability of the spectral components generally used to describe the energy spectra of black hole systems, namely a disk component, a power-law component attributed to Comptonization by a hot corona, and the contribution of the iron line due to reprocessing of the high-energy (E k 7 keV ) radiation. We find that (1) the disk component is not variable on timescales shorter than $100 s, (2) the reprocessing emission as manifest by the variability of the Fe K line responds to the primary radiation variations down to timescales of $70 ms in the high and very high states, but longer than 2 s in the low state, (3) the low-frequency QPOs are associated with variations of the X-ray power-law spectral component and not to the disk component, and (4) the spectra corresponding to the highest Fourier frequency are the hardest (show the flatter spectra) at a given spectral state. These results question models that explain the observed power spectra as due to modulations of the accretion rate alone, as such models do not provide any apparent reason for a Fourier frequency dependence of the power-law spectral indices.

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