  In this paper, we present an intercomparison study of two quasars, SDSS
J145618.32+340037.2 and SDSS J215331.50-025514.1, which have proximate damped
Lya systems (PDLAs) with residual flux upon the Lya absorption trough. Though
they both have residual flux as luminous as $10^{43}erg/s$, their PDLAs are
quite different in, e.g., HI column density, metal line absorption strength,
high-ionization absorption lines as well as residual flux strength. For J1456,
the HI column density is $20.6\pm0.2$, with za=2.3138, nearly identical to the
quasar redshift (z=2.3142) determined from the [OIII] emission line. The
metallicity of this system is typical of DLAs and there is high ionization
therein, suggesting that the PDLA system is multiphase, putting it in the
quasar environment. For J2153, we measure the HI column density to be
$21.5\pm0.1$ at za=3.511, slightly redshifted with respect to the quasar
(z=3.490) measured from CIII]. The metallicity of this system is quite low and
there is a lack of significant high-ionization absorption lines therein,
suggesting that the system is beyond the quasar host galaxy. The residual flux
is wide (1000 km/s) in J1456, with a significance of $8\sigma$, while also wide
(1500 km/s) but with a smaller significance of $3\sigma$ in J2153. Among many
explanations, we find that Lya fuzz or resonant scattering can be used to
explain the residual flux in the two sources while partial coverage cannot be
excluded for J1456. By comparing these two cases, together with similar cases
reported previously, we suggest that the strength of the residual flux is
related to properties such as metallicity and high-ionization absorption lines
of PDLAs. The residual flux recorded upon the PDLA absorption trough opens a
window for us to see the physical conditions and processes of the quasar
environment, and their profile and strength further remind us of their spatial
scales.
