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

Star-forming regions are usually studied in the context of Galactic surveys,but dedicated observations are sometimes needed when the study reaches beyondthe survey area. Here, we studied the G345.5+1.5 region, which is locatedslightly above the Galactic plane, to understand its star formation properties.We combined the LABOCA and $^{12}$CO(4$-$3) transition line observationscomplemented with the Hi-GAL and $\it{Spitzer}$-GLIMPSE surveys to study thestar formation toward this region. We used the Clumpfind algorithm to extractthe clumps from the 870$\mu$m and $^{12}$CO(4$-$3) data. Radio emission at 36cmwas used to estimate the number of HII regions and to remove the contaminationfrom the free-free emission at 870$\mu$m. We employed color-color diagrams andspectral energy distribution slopes to distinguish between prestellar andprotostellar clumps. We studied the boundedness of the clumps through thevirial parameter. Finally, we estimated the star formation efficiency and starformation rate of the region and used the Schmidt-Kennicutt diagram to compareits ability to form stars. Of the 13 radio sources that we found using theMGPS-2 catalog, 7 are found to be associated with HII regions corresponding tolate-B or early-O stars. We found 45 870$\mu$m clumps, and 107 $^{12}$COclumps. More than 50\% of the clumps are protostellar and bounded and are ableto host star formation. High SFR and SFR density values are associated with theregion, with an SFE of a few percent. With submillimeter, CO transition, andshort-wavelength infrared observations, our study reveals a population ofmassive stars, protostellar and bound starless clumps, toward G345.5+1.5. Thisregion is therefore actively forming stars, and its location in the starburstquadrant of the Schmidt-Kennicutt diagram is comparable to other star-formingregions found within the Galactic plane.

Multiwavelength study of the G345.5+1.5 region