IRAS 09581-5607 , the SIMBAD biblio

We present the second dust continuum data release in the Census of High- and Medium-mass Protostars (CHaMP), expanding the methodology trialed in Pitts et al. to the entire CHaMP survey area (280° < l < 300°, - 4° < b < + 2°). This release includes maps of dust temperature (T_d), H₂ column density (N_H2_), gas-phase CO abundance, and temperature-density plots for every prestellar clump with Herschel coverage, showing no evidence of internal heating for most clumps in our sample. We show that CO abundance is a strong function of T_d and can be fit with a second-order polynomial in log-space, with a typical dispersion of a factor of 2-3. The CO abundance peaks at 20.0_–1.0^+0.4 K with a value of 7.4_–0.3^+0.2×10^–5 per H₂; the low T_d at which this maximal abundance occurs relative to laboratory results is likely due to interstellar UV bombardment in the largest survey fields. Finally, we show that, as predicted by theoretical literature and hinted at in previous studies of individual clouds, the conversion factor from integrated ¹²CO line intensity (I_^12CO) to N_H2_, the X_CO factor, varies as a broken power law in I_^12CO with a transition zone between 70 and 90 K km s^–1. The X_CO function we propose has N_H2_∝I_^12CO0.51 for I_^12CO≲70 K km s^–1 and N_H2_∝I_^12CO2.3 for I_^12CO≳90 K km s^–1. The high-I_^12CO side should be generalizable with known adjustments for metallicity, but the influence of interstellar UV fields on the low-I_^12CO side may be sample specific. We discuss how these results expand on previous works in the CHaMP series and help tie together observational, theoretical, and laboratory studies on CO over the past decade.