The Star-forming Core of Monoceros R2

The central region of the Monoceros R2 molecular cloud has been studied using molecular line maps, maps in continuum emission, and an M-band (4.7 μm) absorption spectrum toward Mon R2 IRS 3. Maps were made in the emission lines CO (3-2) H2CO (51,5-41,4), and HCN (4-3), all with a 14'' beam size. CO (2-1) and 13CO (3-2) spectra were obtained at a dozen positions. Maps of continuum emission were made at 1300 μm (25'' resolution), 1100 μm (20'' resolution), 800 μm (14'' resolution), and 450 μm (14'' resolution). The M-band spectrum of IRS 3 has a velocity resolution of 5.2 km s-1 and shows fundamental vibrational band absorption lines of CO and 13CO over a range of rotational states. The CO map has numerous intensity peaks which, if interpreted as clumps, have masses from 0.1 to 3 M☉. The large velocity dispersion of these structures implies that they cannot be gravitationally bound. The brightest CO-emitting gas shows no bipolar distribution with velocity. Diffuse CO-emitting gas with low velocities does have a generally bipolar distribution, but there are no collimated lobes pointing to a particular source. We conclude that the source (or sources) of the very extended Mon R2 outflow is (are) now inactive. The highest velocity gas is found toward the embedded young stellar object IRS 3, suggesting that IRS 3 is the source of a compact outflow, unresolved at our 14'' resolution. The presence of blueshifted CO in the absorption spectrum supports the interpretation of IRS 3 as an outflow source. The H2CO and HCN maps demonstrate that much of the dense gas is distributed within three structures having different velocities. The fundamental band absorption lines of 13CO show two gas temperatures in the line of sight to IRS 3. The colder (45 K) is identified as gas in the clump surrounding IRS 3, which is seen in emission lines of CO, H2CO, and HCN. The warmer (310 K) we interpret as gas very close to IRS 3. From the submillimeter continuum maps we identify 11 clumps whose masses lie in the range 3-10 M☉. A clump that is prominent in the continuum maps but not in the molecular line maps is attributed to heated dust inside the compact H II region, where molecules have been destroyed.

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