2013A&A...556A..89Y

In the deeply embedded stage of star formation, protostars start to heat and disperse their surrounding cloud cores. The evolution of these sources has traditionally been traced through dust continuum spectral energy distributions (SEDs), but the use of CO excitation as an evolutionary probe has not yet been explored due to the lack of high-J CO observations. The aim is to constrain the physical characteristics (excitation, kinematics, column density) of the warm gas in low-mass protostellar envelopes using spectrally resolved Herschel data of CO and compare those with the colder gas traced by lower excitation lines. Herschel-HIFI observations of high-J lines of ¹²CO, ¹³CO, and C¹⁸O (up to J_u=10, E_u up to 300K) are presented toward 26 deeply embedded low-mass Class 0 and Class I young stellar objects, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. This is the first large spectrally resolved high-J CO survey conducted for these types of sources. Complementary lower J CO maps were observed using ground-based telescopes, such as the JCMT and APEX and convolved to matching beam sizes. The ¹²CO 10-9 line is detected for all objects and can generally be decomposed into a narrow and a broad component owing to the quiescent envelope and entrained outflow material, respectively. The ¹²CO excitation temperature increases with velocity from ∼60K up to ∼130K. The median excitation temperatures for ¹²CO, ¹³CO, and C¹⁸O derived from single-temperature fits to the J_ u_=2-10 integrated intensities are ∼70K, 48K and 37K, respectively, with no significant difference between Class 0 and Class I sources and no trend with M_env or L_ bol_. Thus, in contrast to the continuum SEDs, the spectral line energy distributions (SLEDs) do not show any evolution during the embedded stage. In contrast, the integrated line intensities of all CO isotopologs show a clear decrease with evolutionary stage as the envelope is dispersed. Models of the collapse and evolution of protostellar envelopes reproduce the C¹⁸O results well, but underproduce the ¹³CO and ¹²CO excitation temperatures, due to lack of UV heating and outflow components in those models. The H₂O 1₁₀-1₀₁/CO 10-9 intensity ratio does not change significantly with velocity, in contrast to the H₂O/CO 3-2 ratio, indicating that CO 10-9 is the lowest transition for which the line wings probe the same warm shocked gas as H₂O. Modeling of the full suite of C¹⁸O lines indicates an abundance profile for Class 0 sources that is consistent with a freeze-out zone below 25K and evaporation at higher temperatures, but with some fraction of the CO transformed into other species in the cold phase. In contrast, the observations for two Class I sources in Ophiuchus are consistent with a constant high CO abundance profile. The velocity resolved line profiles trace the evolution from the Class 0 to the Class I phase through decreasing line intensities, less prominent outflow wings, and increasing average CO abundances. However, the CO excitation temperature stays nearly constant. The multiple components found here indicate that the analysis of spectrally unresolved data, such as provided by SPIRE and PACS, must be done with caution.