The W 3 core: masses, densities, sizes and kinematics.

Details The W 3 core: masses, densities, sizes and kinematics. The W 3 core: masses, densities, sizes and kinematics.

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...303..901t&link_type=abstract

Astronomy and Astrophysics, v.303, p.901

Astronomy and Astrophysics

Astrophysics

26

Ism: Clouds, Ism: Molecules, Radio Lines: Ism, Ism: Magnetic Fields, Ism: W 3

Scientific paper

The core of the W 3 molecular cloud has been mapped in a 3'x2' region in the J=2-1 transition of C^18^O and the J=3-2 and J=5-4 transitions of C^34^S with angular resolutions of 11", 17" and 10", respectively, using the IRAM 30-m telescope. The W 3 core consists of two regions separated by 75" (=0.85pc at 2.3kpc). The region associated with W 3 IRS 5 has an average v_lsr_=~-39km/s and a mass of 800Msun_. The other, more extended region associated with W 3 IRS 4 has an average v_lsr_=~-43km/s and a mass of 1500Msun_. The IRS 4 region is resolved into four smaller clumps. One of these is close to, but not coincident with, the submillimeter continuum peak SMS 3; another is very close to IRS 4 and SMS 2. The IRS 5 region is barely resolved into four clumps. There is a clump centered on IRS 5. From the C^18^O data, the H_2_ column densities of the clumps have been determined. From a Large Velocity Gradient analysis of the C^34^S 3-2/5-4 ratios the H_2_ densities and masses were estimated; these are compared with general results from the virial theorem. Dynamics are investigated using velocity channel maps. Over a 70" region in Declination, the v_lsr_ of the IRS 4 region changes from -42km/s in the southern part to -46km/s in the northern part. For the northern part of IRS 4, over 70" in Right Ascension, there is a change from -41km/s in the western part to -47km/s in the eastern part. This velocity change is opposite to the sense of galactic rotation; the gradient is 9km/s/pc. For the IRS 5 region, there is a similar change in v_lsr_ with Dec., but only a small change with R.A. Considering the presence of a magnetic field of 100μG towards IRS 4 and the striking change in radial velocity, we speculate that "magnetic braking" dominates the dynamics in the IRS 4 region. Our C^18^O and C^34^S results are compared with the abundances of other molecular species and show that the IRS 4 and IRS 5 regions have distinctly different chemistry.

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