tokens: the AGN luminosity, or the distance from the BH. For simplicity we vary only one of these, the density, while keeping the others fixed. As discussed in following sections, this change, while simple, does serve to illustrate the types of SEDs that will filter through the wind. Changes in the mass-loss rate of the wind can cause changes in the hydrogen density of the equatorial obscurer. We examine the effects of such variations upon the transmitted SED in Figure 3 , which shows three typical SEDs. As the figure shows, the shape of the SED is highly sensitive to the value of the hydrogen density. Figure 3. SED transmitted through equatorial obscurer and incident upon the BLR is shown for three different values of the hydrogen density. The unextinguished SED is also shown. The SED is dramatically dependent on the hydrogen density of the obscurer. High hydrogen densities produce strong absorption in the XUV region and strong emission in the FUV/optical regions. The density and flux parameters chosen here do not matter in detail. The transmitted SED actually depends on the ionization parameter, which is the ratio of the ionizing flux to the hydrogen density (Osterbrock Ferland 2006 ). Increasing the hydrogen density lowers the ionization parameter inversely. Particular values of the density and flux do not matter as long as the ratio giving the ionization parameter is kept constant. As the ionization parameter increases the level of ionization of the gas increases. The gas opacity decreases as the number of bound electrons decreases. The ionization structure changes in ways that produce the three characteristic SEDs shown in Figure 3 . These are the three cases: 1. Case 1 has the lowest density and the highest ionization, and is shown in black. This wind is fully ionized, has no H or He ionization fronts, and nearly fully transmits the entire incident SED. 2. Case 2 has an intermediate density and is shown in blue. This has a He 2+ − He + ionization-front but no H ionization-front. The incident SED is heavily absorbed for the XUV energies, 11 11 We refer to the region 6–13.6 eV (912–2000 Å) as FUV, 13.6–54.4 eV (228–912 Å) as EUV, and 54.4 eV to few hundred eV (less than 228 Å) as XUV. although most of the hydrogen-ionizing radiation is transmitted. 3. Finally, Case 3 is shown with the red line and has the highest density. The wind has both H and He ionization-fronts, and much of the light in the EUV and XUV regions is absorbed. 4. The Response of the BLR to Changes of the Transmitted Continuum We now show how the EWs of the BLR lines in Figure 2 are affected by changes in the transmitted SED of the equatorial obscurer. Figure 4 shows how the EW of the strongest observed lines reacts as the density, n (H), of the equatorial obscurer varies. These changes are due to variations in the SED filtering through the equatorial obscurer. The three general types of SED shown in Figure 3 produce the three different BLR regimes shown in Figure 4 . We
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