2017ApJ...850....3K

We use Green Bank Ammonia Survey observations of NH₃ (1, 1) and (2, 2) emission with 32'' FWHM resolution from a ∼10 pc² portion of the Cepheus-L1251 molecular cloud to identify hierarchical dense gas structures. Our dendrogram analysis of the NH₃ data results in 22 top-level structures, which reside within 13 lower-level parent structures. The structures are compact (0.01 pc R_eff 0.1 pc) and are spatially correlated with the highest H₂ column density portions of the cloud. We also compare the ammonia data to a catalog of dense cores identified by higher-resolution (18.''2 FWHM) Herschel Space Observatory observations of dust continuum emission from Cepheus-L1251. Maps of kinetic gas temperature, velocity dispersion, and NH₃ column density, derived from detailed modeling of the NH₃ data, are used to investigate the stability and chemistry of the ammonia-identified and Herschel-identified structures. We show that the dust and dense gas in the structures have similar temperatures, with median T_dust and T_K measurements of 11.7 ± 1.1 K and 10.3 ± 2.0 K, respectively. Based on a virial analysis, we find that the ammonia-identified structures are gravitationally dominated, yet may be in or near a state of virial equilibrium. Meanwhile, the majority of the Herschel-identified dense cores appear to be not bound by their own gravity and instead confined by external pressure. CCS (2₀ - 1₀) and HC₅N (9-8) emission from the region reveal broader line widths and centroid velocity offsets when compared to the NH₃ (1, 1) emission in some cases, likely due to these carbon-based molecules tracing the turbulent outer layers of the dense cores.