Observations of the Clumpy Shell of the L1551 Bipolar Outflow

Details Observations of the Clumpy Shell of the L1551 Bipolar Outflow Observations of the Clumpy Shell of the L1551 Bipolar Outflow

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...446..234p&link_type=abstract

Astrophysical Journal v.446, p.234

Astronomy and Astrophysics

Astronomy

12

Ism: Individual Alphanumeric: L1551 Irs 5, Ism: Jets And Outflows, Ism: Kinematics And Dynamics, Shock Waves

Scientific paper

We have studied two regions along the edges of the L1551 IRS 5 bipolar outflow where unusually bright "high-velocity" CS emission is seen. These regions are 4' west and 2' east of IRS 5; a line drawn through them passes directly through IRS 5, along the axis of the highly collimated ionized jets from the star.
We mapped the J = 2-1 CS emission from these two spots with 7" angular resolution, and obtained single- dish spectra of 12 molecular transitions toward both regions. The maps show that the high-velocity gas is an integral part of a clumpy shell of molecular gas along the periphery of the bipolar lobes. Typical clumps have CS brightness temperatures of 5-7 K, line widths of ˜0.8 km s-1, and diameters down to our resolution limit of ˜1000 AU. One of the CS clumps in the L1551-2E field is coincident with IRAS source L1551NE. The clumps are estimated to have kinetic temperatures of 20-30 K and densities of ˜4 × 105 cm-3. The total mass of high velocity gas toward each region is roughly 0.02 Msun; individual clumps have masses as small as 0.001 Msun. The chemical abundances of SO, CS, and NH3 may be unusually large in these regions.
The data suggest that low velocity (V < 15 km s1) shocks propagate into the swept-up molecular shell at these locations. Apparently the collimated high velocity jets from IRS 5 are degraded into a broader, lower velocity wind before impacting these regions.

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