  Blue Luminescence (BL) was first discovered in a proto-planetary nebula, the
Red Rectangle (RR) surrounding the post-AGB star HD 44179. BL has been
attributed to fluorescence by small, 3-4 ringed neutral polycyclic aromatic
hydrocarbon (PAH) molecules, and was thought to be unique to the RR environment
where such small molecules are actively being produced and shielded from the
harsh interstellar radiation by a dense circumstellar disk. In this paper we
present the BL spectrum detected in several ordinary reflection nebulae
illuminated by stars having temperatures between 10,000 -- 23,000 K. All these
nebulae are known to also exhibit the infrared emission features called
aromatic emission features (AEFs) attributed to large PAHs. We present the
spatial distribution of the BL in these nebulae. In the case of Ced~112, the BL
is spatially correlated with mid-IR emission structures attributed to AEFs.
These observations provide evidence for grain processing and possibly for
in-situ formation of small grains and large molecules from larger aggregates.
Most importantly, the detection of BL in these ordinary reflection nebulae
suggests that the BL carrier is an ubiquitous component of the ISM and is not
restricted to the particular environment of the RR.
