The dust emissivity spectral index , \textbeta , is a critical parameter for deriving the mass and temperature of star-forming structures , and consequently their gravitational stability .
The \textbeta value is dependent on various dust grain properties , such as size , porosity , and surface composition , and is expected to vary as dust grains evolve .
Here we present \textbeta , dust temperature , and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting SEDs to combined Herschel and JCMT observations in the 160 \textmu m , 250 \textmu m , 350 \textmu m , 500 \textmu m , and 850 \textmu m bands .
Most of the derived \textbeta , and dust temperature values fall within the ranges of 1.0 - 2.7 and 8 - 20 K , respectively .
In Perseus , we find the \textbeta distribution differs significantly from clump to clump , indicative of grain growth .
Furthermore , we also see significant , localized \textbeta variations within individual clumps and find low \textbeta regions correlate with local temperature peaks , hinting at the possible origins of low \textbeta grains .
Throughout Perseus , we also see indications of heating from B stars and embedded protostars , as well evidence of outflows shaping the local landscape .