  We analyzed the CIV line profile distortions due to microlensing in two
quasars, J1339 and J1138. J1339 shows a strong, asymmetric line profile
deformation, while J1138 shows a more modest, symmetric deformation. To probe
the CIV broad line region (BLR), we compared the observed line profile
deformations to simulated ones. The simulations are based on three simple BLR
models, a Keplerian disk (KD), an equatorial wind (EW), and a polar wind (PW),
of various sizes, inclinations, and emissivities. We find that the line profile
deformations can be reproduced with the simple BLR models under consideration,
with no need for more complex geometries or kinematics. The models with disk
geometries (KD and EW) are preferred, while the PW model is definitely less
likely. For J1339, we find the CIV BLR half-light radii to be $r_{1/2} =$ 5.1
$^{+4.6}_{-2.9}$ light-days and $r_{1/2} =$ 6.7 $^{+6.0}_{-3.8}$ light-days
from spectra obtained in 2014 and 2017, respectively. They do agree within
uncertainties. For J1138, the amplitude of microlensing is smaller and more
dependent on the macro-magnification factor. From spectra obtained in 2005
(single epoch), we find $r_{1/2} =$ 4.9 $^{+4.9}_{-2.7}$ light-days and
$r_{1/2}= $ 12 $^{+13}_{-8}$ light-days for two extreme values of the
macro-magnification factor. Combining these new measurements with those
previously obtained for the quasars Q2237$+$0305 and J1004$+$4112, we show that
the BLR radii estimated from microlensing do follow the CIV radius--luminosity
relation obtained from reverberation mapping, although the microlensing radii
seem to be systematically smaller, which could indicate either a selection bias
or a real offset (abridged).
