Constraining the geometry and kinematics of the quasar broad emission line region using gravitational microlensing. I. Models and simulations

TL;DR

This study uses simulations to analyze how gravitational microlensing affects quasar broad emission line profiles, providing diagnostic tools to distinguish BLR models based on observed distortions.

Contribution

It introduces a simulation framework combining BLR models with microlensing maps to identify observable signatures that differentiate BLR geometries and kinematics.

Findings

Line profile distortions can be reproduced and attributed to microlensing effects.

Microlensing magnification constrains BLR and continuum source sizes.

Diagnostic diagrams can discriminate between different BLR models.

Abstract

Recent studies have shown that line profile distortions are commonly observed in gravitationally lensed quasar spectra. We investigate the effect of gravitational microlensing on quasar broad emission line profiles and their underlying continuum, combining the emission from simple representative BLR models with generic microlensing magnification maps. Specifically, we considered Keplerian disk, polar, and equatorial wind BLR models of various sizes. The effect of microlensing has been quantified with four observables: $\mu^{BLR}$, the total magnification of the broad emission line; $\mu^{cont}$, the magnification of the underlying continuum; as well as red/blue, RBI and wings/core, WCI, indices that characterize the line profile distortions. The simulations showed that distortions of line profiles, such as those recently observed in lensed quasars, can indeed be reproduced and attributed to the differential effect of microlensing on spatially separated regions of the BLR. While the magnification of the emission line $\mu^{BLR}$ sets an upper limit on the BLR size and, similarly, the magnification of the continuum $\mu^{cont}$ sets an upper limit on the size of the continuum source, the line profile distortions mainly depend on the BLR geometry and kinematics. We thus built (WCI,RBI) diagrams that can serve as diagnostic diagrams to discriminate between the various BLR models on the basis of quantitative measurements. It appears that a strong microlensing effect puts important constraints on the size of the BLR and on its distance to the high-magnification caustic. In that case, BLR models with different geometries and kinematics are more prone to produce distinctive line profile distortions for a limited number of caustic configurations, which facilitates their discrimination.