  Stellar black holes (sBHs) are widely believed to exist in the accretion
disks of active galactic nuclei (AGNs). Previous studies often focus on the
transient emission produced by embedded sBHs. Here, we explore the possible
observational consequences of an AGN accretion disk that contains a population
of accreting sBHs. Embedded accreting sBHs change the effective temperature
distribution of the AGN accretion disk by heating gas in the outer regions. Two
possible observational consequences are presented. First, the spectral energy
distribution has a turnover feature at $\sim 4700\ \textrm{\AA}$ when the
supermassive black hole (SMBH) mass is $\sim 10^8\ M_{\odot}$, which can help
explain the observed shallow spectral shape at wavelengths $>5000\
\textrm{\AA}$ for the Sloan Digital Sky Survey quasar composite spectrum.
Second, the half-light radius of a given relatively long wavelength is
significantly larger than for an AGN disk without sBHs, which can be tested by
microlensing observations. With appropriate sBH distributions, the model can be
reconciled with quasar microlensing disk sizes. We propose that the half-light
radius-wavelength relation can be utilized to investigate the distributions of
embedded sBHs in AGN accretion disks.
