All Tables

Table 1: Summary of the data used to build the spectral energy distribution of Q0056-363. C03: Cutri et al. (2003). M03: Monet et al. (2003). UVW2 is the OM filter used during the present XMM-Newton observation. G99: Grupe et al. (1999). INES: Merged Log of IUE Observations (NASA-ESA, 1999).
Table 2: Best-fitting spectral parameters in the 2.5-12 keV energy range for an absorbed ( $N_{\rm H}=1.88\times 10^{20}$ cm^-2) power-law (PL) component plus a line profile: GA: Gaussian profile; and DISKLINE and LAOR: profile line emitted by a relativistic accretion disk for a non-rotating BH and a maximally rotating BH, respectively (Fabian et al. 1989; Laor 1991). The line fluxes are expressed in erg cm^-2 s¹. We assume an emissivity law q equal to -2. (a): $R_{\rm in}=6~R_{\rm g}$ and $R_{\rm out}=1~000~R_{\rm g}$ , inclination = 30 $^{\circ }$ . (b): $R_{\rm in}=1.26~R_{\rm g}$ and $R_{\rm out}=400~R_{\rm g}$ , inclination = 30 $^{\circ }$ . (c): The energy of the line has been fixed to 6.4 keV (see text).
Table 3: Best-fitting spectral parameters in the 0.3-12 keV energy range. COMPTT: Comptonization of soft photons in a hot plasma (Titarchuk 1994), and DISKLINE: profile line emitted by a relativistic accretion disk around a non-rotating BH (Fabian et al. 1989).