  Several fluctuation studies on the near-infrared extragalactic background
light (EBL) find an excess power at tens of arcminute scales ($\ell\sim10^3$).
Emission from the intra-halo light (IHL) has been proposed as a possible
explanation for the excess signal. In this work, we investigate the emission
from the integrated galaxy light (IGL) and IHL in the power spectrum of EBL
fluctuations using the simulated galaxy catalog MICECAT. We find that at
$\ell\sim10^3$, the one-halo clustering from satellite galaxies has comparable
power to the two-halo term in the IGL power spectrum. In some previous EBL
analyses, the IGL model assumed a small one-halo clustering signal, which may
result in overestimating the IHL contribution to the EBL. We also investigate
the dependence of the IGL$+$IHL power spectrum on the IHL distribution as a
function of redshift and halo mass, and the spatial profile within the halo.
Our forecast suggests that the upcoming SPHEREx deep field survey can
distinguish different IHL models considered in this work with high
significance. Finally, we quantify the bias in the power spectrum from the
correlation of the mask and the signal, which has not been accounted for in
previous analyses.
