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Where is the Atomic Carbon in Ophiuchus

Where is the Atomic Carbon in Ophiuchus. Di Li Paul Goldsmith Gary Melnick and SWAS team. JCMT 850 Micron. Telescopes. FCRAO 44” resolution at 2.6mm Beam sampling. SWAS 4.2’ resolution at 0.6mm Nyquist Sampling. Mapping Parameters. CO Raw Data. Temperature Structure.

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Where is the Atomic Carbon in Ophiuchus

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  1. Where is the Atomic Carbon in Ophiuchus Di Li Paul Goldsmith Gary Melnick and SWAS team

  2. JCMT 850 Micron

  3. Telescopes

  4. FCRAO 44” resolution at 2.6mm Beam sampling SWAS 4.2’ resolution at 0.6mm Nyquist Sampling Mapping Parameters

  5. CO Raw Data

  6. Temperature Structure

  7. Dust Radiative Transfer

  8. UV, Opacity, and Temperature Schematic Model of Orion

  9. Optically Thin Tracer CI and C18O 1-0 Modest Optical Depth 13CO Column Density Tx and LTE will give the correction factor, Z.

  10. Opacity Effects

  11. The “Norm” of CI and CO in Ophiuchus

  12. 13CO Column Density

  13. Cloud Structures: the Rho Oph Clouds

  14. Turbulence

  15. Opacity Correction

  16. Clump and Inter-Clump Structure

  17. offset 3D Model Fit Model; Vmic=0.2 km/s; f_b = 0.35 r = 0.5 pc

  18. Fit to the Center Position

  19. Fitting Results to the Center Position

  20. The Fit to the Offset Position

  21. CI and HI in Dark Clouds From Cloud to Cloud Across One Cloud

  22. Summary • Ophiuchus Clouds are low mass star forming clouds in enhanced UV fields. • The distribution and abundance of CI cannot be explained by UV field alone. • The statistics of CO, CI, and HINSA turbulence suggest different origin of atomic CI and cold atomic hydrogen in molecular clouds. • Clump-Interclump structure is a straightforward model to provide good fit to both CO and CI spectra through 3d radiative transfer. • GALFA, combined with large scale millimeter surveys, would provide a unprecedented opportunity to study the distribution, kinematics, and correlation between atomic hydrogen and molecules in nearby star forming clouds. Particularly, whether UV is import in regulating HINSA abundance.

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