All Tables

Table 1: Instrument modes and exposure times.
Table 2: Fits to the 0.2-10 keV X-ray continuum, the Fe K $\alpha$ emission line region and the 0.32-2.07 keV RGS continuum.
Table 3: The rest wavelengths ( $\lambda _{\rm rest}$ ), observed wavelengths ( $\lambda _{\rm obs}$ ), equivalent widths ( EW), blueshifts ( $v_{\rm blue}$ ), fluxes, velocity widths ( $v_{\rm broad}$ , FWHM) and range of log $\xi$ (log $\xi _{\rm max}$ ) where the ion is most abundant of absorption (top section) and emission lines (bottom section) in the RGS spectrum of NGC 7469; rms errors are quoted throughout, except for log $\xi _{\rm max}$ where the error bars give the range where the ion has a higher relative abundance than adjacent ionisation states. Blueshifts are not given for lines whose equivalent width is consistent with zero. Also listed are rest wavelengths, blueshifts, fluxes, velocity widths and log $\xi _{\rm max}$ for the broad and narrow O VI emission lines observed by FUSE (Kriss et al. 2003).
Table 4: Estimates of the ionisation parameter of the warm emitter using the ratio of the fluxes of O VIII Ly $\alpha$ and O VII He $\alpha$ emission lines. The fluxes were fitted assuming an O VIII absorbing column of 10 $^{\rm 17.3}$ cm $^{\rm -2}$ and an O VII column of 10 $^{\rm 16.5}$ cm $^{\rm -2}$ , both blueshifted by -900 km s $^{\rm -1}$ . The O VIII Ly $\alpha$ and O VII He $\alpha$ emission lines were assumed to have a blueshift of -400 km s $^{\rm -1}$ and zero intrinsic width, for fitting purposes.