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On the basis of 16 years of spectroscopic observations of the four componentsof the gravitationally lensed broad absorption line (BAL) quasar H1413+117,covering the ultraviolet to visible rest-frame spectral range, we analyze thespectral differences observed in the P Cygni-type line profiles and have usedthe microlensing effect to derive new clues to the BAL profile formation. Weconfirm that the spectral differences observed in component D can be attributedto a microlensing effect lasting at least a decade. We show that microlensingmagnifies the continuum source in image D, leaving the emission line regionessentially unaffected. We interpret the differences seen in the absorptionprofiles of component D as the result of an emission line superimposed onto anearly black absorption profile. We also find that the continuum source and apart of the broad emission line region are likely de-magnified in component C,while components A and B are not affected by microlensing. We show thatmicrolensing of the continuum source in component D has a chromatic dependencecompatible with the thermal continuum emission of a standard Shakura-Sunyaevaccretion disk. Using a simple decomposition method to separate the part of theline profiles affected by microlensing and coming from a compact region fromthe part unaffected by this effect and coming from a larger region, wedisentangle the true absorption line profiles from the true emission lineprofiles. The extracted emission line profiles appear double-peaked, suggestingthat the emission is occulted by a strong absorber, narrower in velocity thanthe full absorption profile, and emitting little by itself. We propose that theoutflow around H1413+117 is constituted by a high-velocity polar flow and adenser, lower velocity disk seen nearly edge-on.

Microlensing in H1413+117 : disentangling line profile emission and absorption in a broad absorption line quasar