The Bolocam Galactic Plane Survey. XIV. Physical Properties of Massive Starless and Star-forming Clumps

We sort 4683 molecular clouds between 10° < ℓ < 65° from the Bolocam Galactic Plane Survey based on observational diagnostics of star formation activity: compact 70 μm sources, mid-IR color-selected YSOs, H₂O and CH₃OH masers, and UCH II regions. We also present a combined NH₃-derived gas kinetic temperature and H₂O maser catalog for 1788 clumps from our own GBT 100 m observations and from the literature. We identify a subsample of 2223 (47.5%) starless clump candidates (SCCs), the largest and most robust sample identified from a blind survey to date. Distributions of flux density, flux concentration, solid angle, kinetic temperature, column density, radius, and mass show strong (>1 dex) progressions when sorted by star formation indicator. The median SCC is marginally subvirial (α ∼ 0.7) with >75% of clumps with known distance being gravitationally bound (α < 2). These samples show a statistically significant increase in the median clump mass of ΔM ∼ 170-370 M _⊙ from the starless candidates to clumps associated with protostars. This trend could be due to (I) mass growth of the clumps at \dot{M}∼ 200{--}440 M _⊙ Myr^-1 for an average freefall 0.8 Myr timescale, (II) a systematic factor of two increase in dust opacity from starless to protostellar phases, and/or (III) a variation in the ratio of starless to protostellar clump lifetime that scales as ∼M ^-0.4. By comparing to the observed number of CH₃OH maser containing clumps, we estimate the phase lifetime of massive (M > 10³ M _⊙) starless clumps to be 0.37 ± 0.08 Myr (M/10³ M _⊙)^-1 the majority (M < 450 M _⊙) have phase lifetimes longer than their average freefall time.