All Tables

Table 1: Log of the X-ray pointings on 4U 1954+31 analyzed in this paper.
Table 2: Best-fit parameters for the X-ray spectra of 4U 1954+31 from the pointed observations described in this paper. In all models in which a Fe emission line is needed in the fit, its width is fixed at the value $\sigma = 0.1$ keV. Frozen parameters are written between square brackets. Luminosities are not corrected for the intervening absorptions and are computed assuming a distance d = 1.7 kpc (Masetti et al. 2006a); in the cases in which the X-ray data could not completely cover the X-ray interval of interest for the luminosity determination, an extrapolation of the best-fit model is applied. Errors are at 90% confidence level for a single parameter of interest. Observations are reported in chronological order from left to right.
Table 3: List of the 6.5 keV Fe emission line EWs, assuming a fixed line width of 0.1 keV, for the various X-ray observations covering that spectral energy. Errors and upper limits are at a 90% confidence level. Pointings are listed in chronological order from top to bottom.
Table A.1: Comparison of the X-ray fluxes (expressed in erg cm^-2 s^-1) of EY Cyg and 4U 1954+31 in the 7-30 keV and in the 15-150 keV bands, together with their percentage ratio, as measured during the BeppoSAX pointing described in Sect. 2.1.