English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The Carina region is an excellent astrophysical laboratory for studying thefeedback mechanisms of newly born, very massive stars within their natal giantmolecular clouds (GMCs) at only 2.35 kpc distance. We use a clumpy PDR model toanalyse the observed intensities of atomic carbon and CO and to derive theexcitation conditions of the gas. The NANTEN2-4m submillimeter telescope wasused to map the [CI] 3P1-3P0, 3P2-3P1 and CO 4-3, 7-6 lines in two 4'x4'regions of Carina where molecular material interfaces with radiation from themassive star clusters. One region is the northern molecular cloud near thecompact OB cluster Tr14, and the second region is in the molecular cloud southof etaCar and Tr16. These data were combined with 13CO SEST spectra, HIRES/IRAS60um and 100um maps of the FIR continuum, and maps of 8um IRAC/Spitzer and MSXemission. We used the HIRES far-infrared dust data to create a map of the FUVfield heating the gas. The northern region shows an FUV field of a few 1000 inDraine units while the field of the southern region is about a factor 10weaker. We constructed models consisting of an ensemble of small sphericallysymmetric PDR clumps within the 38" beam (0.43pc), which follow canonicalpower-law mass and mass-size distributions. We find that an average local clumpdensity of 2x10**5 cm-3 is needed to reproduce the observed line emission attwo selected interface positions. Stationary, clumpy PDR models reproduce theobserved cooling lines of atomic carbon and CO at two positions in the CarinaNebula.

Clumpy photon-dominated regions in Carina. I. [CI] and mid-J CO lines in two 4'x4' fields