Molecular Line Observation Toward Polaris Flare

Details Molecular Line Observation Toward Polaris Flare Molecular Line Observation Toward Polaris Flare

Mar 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jkas...39....9c&link_type=abstract

Journal of the Korean Astronomical Society, vol. 39, no. 1, pp. 9-17

Astronomy and Astrophysics

Astronomy

3

Stars: Formation, Ism: Cloud, Ism: Molecules, Ism: Kinematics And Dynamics

Scientific paper

In an attempt to investigate star formation activity and statistical properties of clumps of high Galactic latitude clouds (HLCs), we mapped the Polaris Flare region, PF121.3+25.5, in 12CO and 13CO J=1-0 using SRAO 6-m telescope and also observed its 12 13CO peak positions in CS J=2-1 with TRAO 14-m telescope. 13CO integrated intensity map shows clearly its clumpy structure and the locations of clumps well agree with 12CO morphology. CS line is not detected toward the 12 13CO peak positions, so we can conclude there are no dense (˜ 104 cm-3) in this region. We decomposed 105 clumps from 13CO map using GAUSSCLUMPS algorithm. The mass of clumps ranges from 7.8 M&sun; to 7.4×10-2 M&sun; with a total mass of 66.4 M&sun;. The mass spectrum follows a power law, dN/dM ∝ M-α with a power index of α =1.91± 0.13. The virial masses of clumps are in the range of 10 ˜ 100 MLTE and so these clumps are considered to be gravitationally unbound.

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