All Tables

Table 1: Basic properties of Seyfert-type warm absorbers observed with XMM-Newton and Chandra: object name, morphological type, redshift, log $L_{\rm bol}$ (erg s $^{\rm -1}$ ; with reference if different to that given in the last column), whether the X-ray spectrum is dominated by emission lines (EM), whether the source has a warm absorber (WA), whether a detailed spectral model has been published (Mod), whether the warm absorber is outflowing (Outflow), and reference for the warm absorber model.
Table 2: Equivalent hydrogen columns (log $N_{\rm H}$ ; cm $^{\rm -2}$ ), ionisation parameters (log $\xi$ ; erg cm s $^{\rm -1}$ ) and outflow velocities ( $v_{\rm out}$ ; km s $^{\rm -1}$ ) of the modelled warm absorber phases of objects listed in Table 1.
Table 3: Averaged warm absorber parameters for the sources in Table 2: object name, range in log ionisation parameter ( $\Delta$ log $\xi$ ; erg s $^{\rm -1}$ ), log total equivalent hydrogen column (log $N_{\rm Htot}$ ; cm $^{\rm -2}$ ), log weighted average ionisation parameter (log $\xi$ $_{\rm avg}$ ; erg s $^{\rm -1}$ ), weighted average outflow velocity ( $v_{\rm avg}$ ; km s $^{\rm -1}$ ).
Table 4: Mass outflow rates calculated for each outflowing warm absorber phase using the parameters quoted in Table 2 (Markarian 766 does not have an outflowing warm absorber, but the ionising luminosity is listed as we use it elsewhere): object name, log ionisation parameter (log $\xi$ ; erg cm s $^{\rm -1}$ ), log 1-1000 Ryd ionising luminosity (log $L_{\rm ion}$ ; erg s $^{\rm -1}$ ), X-ray to optical spectral index ( $\alpha _{\rm ox}$ ), percentage of total momentum transfer due to Thomson scattering (% ${\dot M}_{\rm scat}$ ), percentage volume filling factor (% C_v), mass outflow rate per phase ( ${\dot M}_{\rm out}$ ; $M_\odot$ yr $^{\rm -1}$ ), mass accretion rate ( ${\dot M}_{\rm acc}$ ; $M_\odot$ yr $^{\rm -1}$ ), ratio of total mass outflow rate (summed over all phases) to mass accretion rate ( ${\dot M}_{\rm out,total}$ / ${\dot M}_{\rm acc}$ ), kinetic luminosity of outflow (log $L_{\rm KE}$ ; erg s $^{\rm -1}$ ), percentage of $L_{\rm bol}$ represented by $L_{\rm KE}$ (% of $L_{\rm bol}$ ).
Table 5: Comparison of distances within the AGN environment: object name, log ionisation parameter of each phase (log $\xi$ ; erg cm s $^{\rm -1}$ ), black hole mass ( $M_{\rm BH}$ ; 10 $^{\rm 7}$ $M_\odot$ ), distance of BLR from central engine ( $r_{\rm BLR}$ ; pc), distance of torus from central engine ( $r_{\rm torus}$ ; pc), minimum distance of warm absorber from central engine ( $r_{\rm min}$ ; pc), maximum distance of warm absorber from central engine ( $r_{\rm max}$ ; pc), the ratios of the minimum and maximum distances to the BLR and torus distances respectively ( $r_{\rm min}$ / $r_{\rm BLR}$ , $r_{\rm max}$ / $r_{\rm BLR}$ , $r_{\rm min}$ / $r_{\rm torus}$ , $r_{\rm max}$ / $r_{\rm torus}$ ).
Table 6: The results of using the turbulent velocity rather than the outflow velocity to calculate the minimum distance of a warm absorber from the central engine: object name, turbulent velocity ( $v_{\rm min,vturb}$ ; km s $^{\rm -1}$ FWHM), minimum distance of warm absorber from central engine derived from turbulent velocity ( $r_{\rm min,vturb}$ ; pc), the ratios of this minimum distance to the BLR and torus distances respectively ( $r_{\rm min,vturb}$ / $r_{\rm BLR}$ , $r_{\rm min,vturb}$ / $r_{\rm torus}$ ), and the ratio $r_{\rm min,vturb}$ / $r_{\rm min}$ .