tokens: wings. If we compare epochs I and II, we can see that the magnified blue wing fades while the red wing enhances. This supports that the separation between the approaching and receding parts of the microlensed region of the BLR is of about a few light-days. In several cases, mainly affecting the shelf-like feature at ∼ λ 1610 and several blends of Fe ii and Fe iii , the impact of microlensing and microlensing variability (see Tables 2 – 5 ) is mag, comparable to the typical microlensing magnification amplitudes observed in the X-ray continuum. It is important to notice that the spectral features mainly affected by intrinsic variability are also the C iv wings, some blends of Fe ii and Fe iii , and the shelf-like feature at ∼ λ 1610. In contrast with microlensing, we have not observed marked asymmetries induced by intrinsic variability in the line profiles. This result supports (within the statistical significance of our relatively limited sample) the hypothesis that the small region sensitive to microlensing is not systematically affected by extinction, beaming, or any other mechanism that may selectively enhance one part of it. Consequently, the asymmetric enhancements observed, in either the blue or red parts of microlensed line profiles, likely originate from an anisotropic distribution of microlensing magnification in the source plane. 3. Discussion 3.1. Microlensing and Kinematics The main result of the previous sections is that the cores of C iv , C iii ], and Mg ii and the wings of the last two lines are only weakly affected by microlensing. However, the wings of C iv can be strongly affected. In other high-ionization emission-line features, such as the Fe iii λλ 2039–2113 blend and the shelf-like feature at ∼ λ 1610, the whole feature may be globally affected by high-magnification microlensing. To discuss these results with more detailed kinematic information than the separation between core and wings, in Figure 6 we have overlapped the averaged line profiles corresponding to C iv , C iii ], Mg ii , and Fe iii λλ 2039–2113. The wings of Mg ii correspond to relatively low velocities as compared with other lines. This is consistent with the weak impact of microlensing on this line. Regarding C iii ] and C iv , the red parts of these lines match very well, except at the lowest intensity level, where the shelf-like feature at ∼ λ 1610 is present in C iv (the blue side of C iii ] is blended with Al iii , Si iii , and Fe ii , and no reasonable comparison can be made). In spite of this remarkable kinematic coincidence, the C iv line can be strongly affected by microlensing, whereas C iii ] seems to be rather insensitive to this effect (see, e.g., the cases of SDSS J1004+4112 and SDSS J1339+1310). In addition, they have a different degree of ionization (C iv is of high ionization and C iii ] of low ionization). These results suggest that both lines are mostly generated in the same region, but that there is also a contribution, exclusive to the
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