All Tables

Table 1: The exposure time and the observation details for the Chandra and HST observations of NGC 5548. ACIS stands for the Advanced CCD Imaging Spectrometer and HRC for High Resolution Camera. The E140M grating covers the wavelength range between 1150-1730 Å, the E230M grating between 1607-3119 Å.
Table 2: The best fit parameters for the continuum for the earlier RGS observation (Steenbrugge et al. 2003) and the present HETGS and LETGS observations of NGC 5548. The parameters for the HETGS and LETGS are for the best fit model including the three slab components with the outflow velocities frozen to the UV values.
Table 3: Parameters for six ions measured using model A. The first row gives the component number as listed in the UV. The second row lists the outflow velocity v, which was frozen to the UV values, the third row lists the velocity broadening $\sigma _{\rm X-ray}$ as derived from the X-ray spectra. In the fourth row the velocity broadening $\sigma _{\rm UV}$ = FWHM/2.35, where FWHM is the measured and resolved Full Width Half Maximum of the UV absorption lines (Crenshaw et al. 2003). All are in km s^-1. For the -530 km s^-1 component we added the velocity broadening of components 2 to 4. We list the logarithms of the column densities in m^-2. For comparison we also list the C IV and N V column densities as measured by Crenshaw et al. (2003).
Table 4: The best fit column densities using model B for the ions for which the outflow velocity and velocity broadening are well constrained. The outflow velocity v and the rms velocity broadening $\sigma$ are listed as well as the ionization parameters $\xi$ and U for which the ion has its maximum column density. The column densities are from the fit including the broad emission lines (Sect. 3.6).
Table 5: The best fit results for a model with three xabs components fitting all elements but iron, which was fit separately with a slab model (model C). To fit the full blend we froze the velocity broadening to 200 km s^-1 and the outflow velocity to -530 km s^-1.
Table 6: The best fit values for model D, using one warm component and fitting iron separately as a slab component.
Table 7: Narrow emission lines. The Equivalent Width ( EW) as measured with the LETGS, except for the Mg XI, Al XIII and Si XIII forbidden lines (MEG), and flux are listed. In the last column the ionization parameter, $\xi$ , where the ion has the highest column density is given. Forbidden lines are indicated by f, intercombination lines by i. Below the line the C V and O VII RRC are listed. The rest wavelengths are taken from Drake (1988).
Table 8: Parameters of the Fe K $\alpha$ line from the present HEG spectrum (2002), previous HEG spectrum (2000; Yaqoob et al. 2001), and EPIC spectrum (2001; Pounds et al. 2003). The FWHM is given in km s^-1, the flux in ph m^-2 s^-1.
Table 9: Flux of the broad emission lines, from the simultaneous LETGS, MEG and HEG fit. The wavelength was frozen to the rest wavelength of the line, while the FWHM was frozen to 8000 km s^-1. The lines for which upper limits are detected were not used in the further analysis of the data.
Table 10: Comparison of the best fit parameters for the LETGS and HETGS spectra between 1.5 and 24 Å. The labeling of the different components follows Kaastra et al. (2002a).
Table 11: Features in the difference spectrum of the 1999 and 2002 LETGS data. We list Gaussian centroids $\lambda$ (in the restframe of NGC 5548), $\sigma$ and peak value p; peaks are expressed as a fraction of the 2002 spectrum at the same energy.
Table 12: Fits with a finite number of ionization components to the column densities of all elements but iron derived with model B, assuming solar abundances. The number of ionization components is indicated by N. In the last column we give the significance according to an F-test of the added component.
Table 13: Fits with a finite number of ionization components to the iron column densities for the RGS data (Steenbrugge et al. 2003). The number of ionization components is indicated by N. In the last column we give the significance according to an F-test of the added component.
Table 14: The upper limit to the opening angle as calculated from Eq. (4) for the five outflow velocities measured in the UV, over the ionization range observed in the Chandra spectra. The angles are given in sr.
Table A.1: The best fit column densities (in m^-2) as measured using model B. The outflow velocity (in km s^-1) was taken from Table 4 or a function of ionization and frozen. The velocity broadening (in km s^-1) was also frozen during the fit. In the last two columns we list the ionization parameter (in 10^-9 W m) for which the ion has its maximum column density. The column densities quoted are for those measured in the fit including the broad emission lines (Sect. 3.6). All ions with uncertain column densities are indicated by * (see Sect. 3.3).