Abstract
We report new results on outflow and infall in the star forming cores W3-SE SMA-1 and SMA-2 based on analysis of $\sim2.5\arcsec$ resolution observations of the molecular lines HCN(3-2), HCO$^+$(3-2), N$_2$H$^+$(3-2) and CH$_3$OH(5$_{2,3}-4_{1,3}$) with the Submillimeter Array. A high-velocity bipolar outflow originating from the proto-stellar core SMA-1 was observed in the HCN(3-2) line, with a projected outflow axis in position angle 48$\arcdeg$. The detection of the outflow is confirmed from other molecular lines. An inverse P-Cygni profile in the HCN(3-2) line toward SMA-1 suggests that at least one of the double cores accretes matters from the molecular core. A filamentary structure in the molecular gas surrounds SMA-1 and SMA-2. Based on the SMA observations, our analysis suggests that the double pre-stellar cores SMA-1 and SMA-2 result from fragmentation in the collapsing massive molecular core W3-SE, and it is likely that they are forming intermediate to high-mass stars which will be new members of a star cluster in the W3-SE region.
Highlights
One of the key questions in the study of star formation is how protostars accrete material from their parent molecular clouds
The HCN(3–2) line components A-NE and A-SW are located 2 northeast and 4 southwest of the protostellar core Submillimeter Array (SMA)-1 while the component A-SE nearly coincides with SMA-2
A high-velocity bipolar outflow originating from SMA-1 is seen in HCN(3–2), with confirmation from other molecular lines, which shows a star formation activity in W3-SE
Summary
One of the key questions in the study of star formation is how protostars accrete material from their parent molecular clouds. Low-resolution observations of a bluedominated double-peaked spectral profile as expected from a model of self-absorption in infalling gas clumps (NGC 1333IRAS 2 as an example; see Ward-Thompson et al 1996; WardThompson & Buckley 2001; Jorgensen et al 2004a; Peretto et al 2006) do not unambiguously identify infall because massive cores usually contain bipolar outflows, disk rotation, and multiple sub-cores in addition to gas infall. Complex dynamical processes can produce characteristics similar to those expected from the self-absorption model of a molecular core with infall. It is crucial to carry out high angular and spectral resolution observations along with comprehensive modeling of the dynamical processes involved in a massive star-forming region
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