[논문]CHEMICAL DIAGNOSTICS OF THE MASSIVE STAR CLUSTER-FORMING CLOUD G33.92+0.11. IV. HIERARCHICAL STRUCTURE

Minh, Young Chol; Liu, Hauyu Baobab; Chen, Huei-Ru Vivien

doi:10.5303/jkas.2020.53.3.77

[국내논문] CHEMICAL DIAGNOSTICS OF THE MASSIVE STAR CLUSTER-FORMING CLOUD G33.92+0.11. IV. HIERARCHICAL STRUCTURE 원문보기

Journal of the Korean astronomical society = 천문학회지, v.53 no.3, 2020년, pp.77 - 85

Minh, Young Chol (Korea Astronomy and Space Science Institute) , Liu, Hauyu Baobab (Academia Sinica Institute of Astronomy and Astrophysics) , Chen, Huei-Ru Vivien (Institute of Astronomy and Department of Physics, National Tsing Hua University)

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In the molecular cloud G33.92+0.11A, massive stars are forming sequentially in dense cores, probably due to interaction with accreted gas. Cold dense gas, which is likely the pristine gas of the cloud, is traced by DCN line and dust continuum emission. Clear chemical differences were observed in different source locations and for different velocity components in the same line of sight. Several distinct gas components coexist in the cloud: the pristine cold gas, the accreted dense gas, and warm turbulent gas, in addition to the star-forming dense clumps. Filaments of accreted gas occur in the northern part of the A1 and A5 clumps, and the velocity gradient along these features suggests that the gas is falling toward the cloud and may have triggered the most recent star formation. The large concentration of turbulent gas in the A2 clump seems to have formed mainly through disturbances from the outside.

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표/그림 (7)

그림 Figure 1. Integrated intensity map for the emission from the ¹³CS 5 − 4 transition.
그림 Figure 2. Continuum map at 1.3 mm taken from Liu et al. (2015) with ¹³CS contours (black; levels are 1, 2, 3, 4 × 0.06 Jy beam⁻¹ kms⁻¹).
그림 Figure 3. Spectra taken toward the positions marked by circles in Figure 1.
표 Table 1 Line parameters of the observed spectra in Figure 3 and total column densities.
그림 Figure 4. Position-velocity diagrams obtained along the cut lines shown in Figure 1.
그림 Figure 5. Integrated intensity maps for the DCN 3 − 2 (left) and H₂S 2_2,0 − 2_1,1 (right) transitions.
그림 Figure 6. Difference maps for the integrated intensities between H₂S 2_2,0 − 2_1,1 and DCN 3 − 2 (left), and between H₂S 2_2,0 − 2_1,1 and ¹³CS 5 − 4 (right).

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When comparing the spectral data, we spatially smoothed our present 13CS data with a beam size of 0.6'' to match the angular resolutions of our previous DCN and H2S data.

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