  We present NIR and MIR observations of eight embedded young stellar groups
around Herbig Ae/Be stars (HAEBEs) using archived Spitzer IRAC data and 2MASS
data. These young stellar groups are nearby ($\leq$ 1 kpc) and still embedded
within their molecular clouds. In order to identify the young stellar objects
in our sample, we use the color-color diagram of J - [3.6] vs. Ks - [4.5]. The
Spitzer images of our sample show that the groups around HAEBEs, spectral types
earlier than B8, are usually associated with bright infrared nebulosity. Within
this, there are normally 10 - 50 young stars distributed close to the HAEBEs
($<$ 1 pc). Not only are there young stars around the HAEBEs, there are also
young stellar populations throughout the whole cloud, some are distributed and
some are clumped. The groups around the HAEBEs are sub-structures of the large
young population within the molecular cloud. The sizes of groups are also
comparable with those sub-structures seen in massive clusters. Young stars in
groups around HAEBEs have generally larger SED slopes compared to those
outside, which suggests that the young stars in groups are probably younger
than the distributed systems. This might imply that there is usually a higher
and more continuous star forming rate in groups, that the formation of groups
initiates later, or that low mass stars in groups form slower than those
outside. Finally, there is no obvious trend between the SED slopes and the
distance to the HAEBEs for those young stars within the groups. This suggests
that the clustering of young stars dominates over the effect of massive stars
on the low-mass young stars at the scale of our study.
