We present Submillimeter Array ( SMA ) 1.35 mm subarcsecond angular resolution observations 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 different outflows detected in the region .
The most evolved objects are located at the southeastern edge of the dust filamentary structure and the youngest ones at the northeastern edge .
The circumstellar structures around VLA 1 , VLA 3 , and MM 1 have radii between \sim 200 and \sim 375 au and masses in the \sim 0.08–0.3 M _ { \sun } range .
The 1.35 mm emission of VLA 2 arises from an unresolved ( r \la 135 au ) circumstellar disk with a mass of \sim 0.02 M _ { \sun } .
This source is powering a compact ( \sim 4000 au ) , low radial velocity ( \sim 7 km s ^ { -1 } ) SiO bipolar outflow , close to the plane of the sky .
We conclude that this outflow is the “ large-scale ” counterpart of the short-lived , episodic , bipolar outflow observed through H _ { 2 } O masers at much smaller scales ( \sim 180 au ) , and that has been created by the accumulation of the ejection of several episodic collimated events of material .
The circumstellar gas around VLA 2 and VLA 3 is hot ( \sim 130 K ) and exhibits velocity gradients that could trace rotation .
There is a bridge of warm and dense molecular gas connecting VLA 2 and VLA 3 .
We discuss the possibility that this bridge could trace a stream of gas between VLA 3 and VLA 2 , increasing the accretion rate onto VLA 2 to explain why this source has

an important outflow activity .