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 present Submillimeter Array (SMA) 1.35 mm subarcsecond angular resolutionobservations toward the LkH{\alpha} 234 intermediate-mass star-forming region.The dust emission arises from a filamentary structure of $\sim$5 arcsec($\sim$4500 au) enclosing VLA 1-3 and MM 1, perpendicular to the differentoutflows detected in the region. The most evolved objects are located at thesoutheastern edge of the dust filamentary structure and the youngest ones atthe northeastern edge. The circumstellar structures around VLA 1, VLA 3, and MM1 have radii between $\sim$200 and $\sim$375 au and masses in the$\sim$0.08-0.3 M$_{\odot}$ range. The 1.35 mm emission of VLA 2 arises from anunresolved (r$< 135$ au) circumstellar disk with a mass of $\sim$0.02M$_{\odot}$. This source is powering a compact ($\sim$4000 au), low radialvelocity ($\sim$7 km s$^{-1}$) SiO bipolar outflow, close to the plane of thesky. We conclude that this outflow is the "large-scale" counterpart of theshort-lived, episodic, bipolar outflow observed through H$_2$O masers at muchsmaller scales ($\sim $180 au), and that has been created by the accumulationof the ejection of several episodic collimated events of material. Thecircumstellar gas around VLA 2 and VLA 3 is hot ($\sim$130 K) and exhibitsvelocity gradients that could trace rotation. There is a bridge of warm anddense molecular gas connecting VLA 2 and VLA 3. We discuss the possibility thatthis bridge could trace a stream of gas between VLA 3 and VLA 2, increasing theaccretion rate onto VLA 2 to explain why this source has an important outflowactivity.

SMA observations towards the compact, short-lived bipolar water maser outflow in the LkH{\alpha} 234 region