  We use the Sternberg et al. (2014) theory for interstellar atomic to
molecular (HI-to-H$_2$) conversion to analyze HI-to-H$_2$ transitions in five
(low-mass) star-forming and dark regions in the Perseus molecular cloud, B1,
B1E, B5, IC348, and NGC1333. The observed HI mass surface densities of 6.3 to
9.2 M$_{\odot}$ pc$^{-2}$ are consistent with HI-to-H$_2$ transitions dominated
by HI-dust shielding in predominantly atomic envelopes. For each source, we
constrain the dimensionless parameter $\alpha G$, and the ratio $I_{\rm UV}/n$,
of the FUV intensity to hydrogen gas density. We find $\alpha G$ values from
5.0 to 26.1, implying characteristic atomic hydrogen densities 11.8 to 1.8
cm$^{-3}$, for $I_{\rm UV} \approx 1$ appropriate for Perseus. Our analysis
implies that the dusty HI shielding layers are probably multiphased, with
thermally unstable UNM gas in addition to cold CNM within the 21 cm kinematic
radius.
