We present centimeter and millimeter observations of gas and dust around IRAS 21391+5802 , an intermediate-mass source embedded in the core of IC 1396N .
Continuum observations from 3.6 cm to 1.2 mm are used to study the embedded objects and overall distribution of the dust , while molecular line observations of CO , CS , and CH _ { 3 } OH are used to probe the structure and chemistry of the outflows in the region .
The continuum emission at centimeter and millimeter wavelengths has been resolved into three sources separated \sim 15 \arcsec from each other , and with one of them , BIMA 2 , associated with IRAS 21391+5802 .
The dust emission around this source shows a very extended envelope , which accounts for most of the circumstellar mass of 5.1 ~ { } M _ { \sun } .
This source is powering a strong molecular outflow , elongated in the E–W direction , which presents a complex structure and kinematics .
While at high outflow velocities the outflow is clearly bipolar , at low outflow velocities the blueshifted and redshifted emission are highly overlapping , and the strongest emission shows a V-shaped morphology .
The outflow as traced by CS and CH _ { 3 } OH exhibits two well differentiated and clumpy lobes , with two prominent northern blueshifted and redshifted clumps .
The curved shape of the clumps and the spectral shape at these positions are consistent with shocked material .
In addition , CS and CH _ { 3 } OH are strongly enhanced toward these positions with respect to typical quiescent material abundances in other star-forming regions .
These kinematical and chemical evidences suggest that the clumps are tracing gas entrained within the surface of interaction between the molecular outflow and the dense ambient quiescent core , and that the morphology of the molecular outflow is a result of this interaction .
The circumstellar mass together with the power-law index of the dust emissivity measured , \beta = 1.1 \pm 0.3 , and the fact that the source is driving a molecular outflow are consistent with the source BIMA 2 being an embedded intermediate-mass protostar .
In addition , the source fits very well correlations between source and outflow properties found for low-mass Class 0 objects .
The other two sources in the region , BIMA 1 and BIMA 3 have a mass of 0.07 ~ { } M _ { \sun } , and their dust emissivity index , \beta < 0.3 and \beta = 0.1 \pm 0.3 , respectively , is consistent with more evolved objects .
BIMA 1 is also driving a very collimated and small bipolar outflow elongated in the N–S direction .