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

After 30 Doradus, N11 is the second largest and brightest nebula in the LMC.This large nebula has several OB associations with bright nebulae at itssurroundings. N11 was previously mapped at the lowest rotational transitions of$^{12}$CO (J=1--0 and 2--1), and in some particular regions pointings of the$^{13}$CO J=1--0 and 2--1 lines were also performed. Using ASTE we mapped thewhole extension of the N11 nebula in the $^{12}$CO J=3--2 line, and threesub-regions in the $^{13}$CO J=3--2 line. The regions mapped in the $^{13}$COJ=3--2 were selected based on that they may be exposed to the radiation atdifferent ways: a region lying over the nebula related to the OB associationLH10 (N11B), another one that it is associated with the southern part of thenebula related to the OB association LH13 (N11D), and finally a farther area atthe southwest without any embedded OB association (N11I). We found that themorphology of the molecular clouds lying in each region shows some signaturesthat could be explained by the expansion of the nebulae and the action of theradiation. Fragmentation generated in a molecular shell due to the expansion ofthe N11 nebula is suggested. The integrated line ratios $^{12}$CO/$^{13}$COshow evidences of selective photodissociation of the $^{13}$CO, and probablyother mechanisms such as chemical fractionation. The CO contribution to thecontinuum at 870 $\mu$m was directly derived. The distribution of theintegrated line ratios $^{12}$CO J=3--2/2--1 show hints of stellar feedback inN11B and N11D. The ratio between the virial and LTE mass (M$_{\rm vir}$/M$_{\rmLTE}$) is higher than unity in all analyzed molecular clumps, which suggeststhat the clumps are not gravitationally bounded and may be supported byexternal pressure. A non-LTE analysis suggests that we are mapping gas withdensities about a few 10$^{3}$ cm$^{-3}$.

12CO and 13CO J=3-2 observations toward N11 in the Large Magellanic Cloud