Franeck, A., Walch, S., Seifried, D., Clarke, S. D., Ossenkopf-Okada, V., Glover, S. C. O., Klessen, R. S., Girichidis, P., Naab, T., Wuensch, R., Clark, P. C., Pellegrini, E. and Peters, T. (2018). Synthetic [C II] emission maps of a simulated molecular cloud in formation. Mon. Not. Roy. Astron. Soc., 481 (4). S. 4277 - 4300. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966
Full text not available from this repository.Abstract
The C+ ion is an important coolant of interstellar gas, and so the [CII] fine structure line is frequently observed in the interstellar medium. However, the physical and chemical properties of the [CII]-emitting gas are still unclear. We carry out non-LTE (local thermal equilibrium) radiative transfer simulations with RADMC-3D to study the [CII] line emission from a young, turbulent molecular cloud before the onset of star formation, using data from the SILCC-Zoom project. The [C II] emission is optically thick over 40 per cent of the observable area with I[C II] > 0.5 K km s(-1). To determine the physical properties of the [C II] emitting gas, we treat the [C II] emission as optically thin. We find that the [CII] emission originates primarily from cold, moderate density gas (40 less than or similar to T less than or similar to 65 K and 50 less than or similar to n less than or similar to 440 cm(-3)), composed mainly of atomic hydrogen and with an effective visual extinction between similar to 0.50 and similar to 0.91. Gas dominated by molecular hydrogen contributes only less than or similar to 20 per cent of the total [C II] line emission. Thus, [C II] is not a good tracer for CO-dark H-2 at this early phase in the cloud's lifetime. We also find that the total gas, H and C+ column densities are all correlated with the integrated [C II] line emission, with power law slopes ranging from 0.5 to 0.7. Further, the median ratio between the total column density and the [C II] line emission is Y-C II approximate to 1.1 x 10(21) cm(-2) (K km s(-1))(-1), and YCII scales with I-[C II](-0.3). We expect YCII to change in environments with a lower or higher radiation field than simulated here.
| Item Type: | Journal Article | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Creators: |
|
||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| URN: | urn:nbn:de:hbz:38-163006 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1093/mnras/sty2507 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Journal or Publication Title: | Mon. Not. Roy. Astron. Soc. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Volume: | 481 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Number: | 4 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Page Range: | S. 4277 - 4300 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Date: | 2018 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Publisher: | OXFORD UNIV PRESS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Place of Publication: | OXFORD | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ISSN: | 1365-2966 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Language: | English | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Faculty: | Unspecified | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Divisions: | Unspecified | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Subjects: | no entry | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Uncontrolled Keywords: |
|
||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Refereed: | Yes | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| URI: | http://kups.ub.uni-koeln.de/id/eprint/16300 |
Downloads
Downloads per month over past year
Altmetric
Export
Actions (login required)
 |
View Item |