All Tables

Table 1: Chandra-LETGS observation log of Mrk 279.
Table 2: Fit parameters of a power-law plus modified blackbody fit to the total spectrum of Mrk 279. The errors on the parameters are only statistical and do not include any systematic uncertainty. The fit was restricted to the 1.9-110 Å range. The spectra were binned by a factor of 10 before spectral fitting.
Table 3: Parameters of the X-ray broad lines from a line-by-line fitting. The line transition, its centroid (in Å), the FWHM in km s^-1 and the rounded correspondent value in Å, the intrinsic line luminosity and the significance are listed (see text for details). Note that for the triplets the FWHM is the result of the blend of the lines.
Table 4: Rest wavelength, along with the observed luminosity and the luminosity predicted by the LOC model of the broad UV lines as measured by FUSE (labeled 1) and HST-STIS (labeled 2). For each observed blended-line, the value of Lum $_{\rm LOC}$ consistently refers to the summed contribution of the lines in the blend.
Table 5: Rest wavelengths and intrinsic luminosity (in units of 10⁴¹ erg s^-1) of the lines in the LETGS (as reported in Table 3) compared with the X-ray line luminosities as predicted by the LOC model (last column) are listed. Note that the observed X-ray line luminosities were not used in the LOC fitting, which was based on UV data only. Here the triplets location has been identified with the wavelength of the forbidden line.
Table 6: Laboratory wavelength, formal EW and outflow velocity for the X-ray absorption lines. The EW and the column densities predicted by models M1 and M2 assume different covering factors for the absorbing gas and are discussed in the text.
Table 7: The two absorption components at the redshift of Mrk 279. For each component we list the value of the ionization parameter $\log\xi$ , the column density $N_{\rm H}$ and the outflow velocity $v_{\rm out}$ .