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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We report observations of dust continuum emission at 1.2 mm toward the starforming region NGC 6334 made with the SEST SIMBA bolometer array. Theobservations cover an area of $\sim 2$ square degrees with approximatelyuniform noise. We detected 181 clumps spanning almost three orders of magnitudein mass (3\Msun$-6\times10^3$ \Msun) and with sizes in the range 0.1--1.0 pc.We find that the clump mass function $dN/d\log M$ is well fit with a power lawof the mass with exponent -0.6 (or equivalently $dN/dM \propto M^{-1.6}$). Thederived exponent is similar to those obtained from molecular line emissionsurveys and is significantly different from that of the stellar initial massfunction. We investigated changes in the mass spectrum by changing theassumptions on the temperature distribution of the clumps and on thecontribution of free-free emission to the 1.2 mm emission, and found littlechanges on the exponent. The Cumulative Mass Distribution Function is alsoanalyzed giving consistent results in a mass range excluding the high-mass endwhere a power-law fit is no longer valid. The masses and sizes of the clumpsobserved in NGC 6334 indicate that they are not direct progenitors of stars andthat the process of fragmentation determines the distribution of masses lateron or occurs at smaller spatial scales. The spatial distribution of the clumpsin NGC 6334 reveals clustering which is strikingly similar to that exhibited byyoung stars in other star forming regions. A power law fit to the surfacedensity of companions gives $\Sigma\propto \theta^{-0.62}$.

Massive Clumps in the NGC 6334 Star Forming Region