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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We performed a multi-wavelength study toward the filamentary cloudG47.06+0.26 to investigate the gas kinematics and star formation. We presentthe 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) observations of G47.06+0.26obtained with the Purple Mountain Observation (PMO) 13.7 m radio telescope toinvestigate the detailed kinematics of the filament. The 12CO (J=1-0) and 13CO(J=1-0) emission of G47.06+0.26 appear to show a filamentary structure. Thefilament extends about 45 arcmin (58.1 pc) along the east-west direction. Themean width is about 6.8 pc, as traced by the 13CO (J=1-0) emission. G47.06+0.26has a linear mass density of about 361.5 Msun/pc. The external pressure (due toneighboring bubbles and H II regions) may help preventing the filament fromdispersing under the effects of turbulence. From the velocity-field map, wediscern a velocity gradient perpendicular to G47.06+0.26. From the BolocamGalactic Plane Survey (BGPS) catalog, we found nine BGPS sources inG47.06+0.26, that appear to these sources have sufficient mass to form massivestars. We obtained that the clump formation efficiency (CFE) is about 18% inthe filament. Four infrared bubbles were found to be located in, and adjacentto, G47.06+0.26. Particularly, infrared bubble N98 shows a cometary structure.CO molecular gas adjacent to N98 also shows a very intense emission. H IIregions associated with infrared bubbles can inject the energy to surroundinggas. We calculated the kinetic energy, ionization energy, and thermal energy oftwo H II regions in G47.06+0.26. From the GLIMPSE I catalog, we selected someClass I sources with an age of about 1 yr, which are clustered along thefilament. The feedback from the H II regions may cause the formation of a newgeneration of stars in filament G47.06+0.26.

Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26