We report H _ { 2 } O maser line observations of the bright-rimmed globule IC 1396 N using a ground-space interferometer with the 10-m RadioAstron radio telescope as the space-based element .
The source was not detected on projected baselines > 2.3 Earth diameters , which indicates a lower limit on the maser size of L > 0.03 AU and an upper limit on the brightness temperature of 6.25 \times 10 ^ { 12 } K. Positions and flux densities of maser spots were determined by fringe rate mapping .
Multiple low-velocity features from - 4.5 km/s to + 0.7 km/s are seen , and two high-velocity features of V _ { LSR } = - 9.4 km/s and V _ { LSR } = + 4.4 km/s are found at projected distances of 157 AU and 70 AU , respectively , from the strongest low-velocity feature at V _ { LSR } = \sim 0.3 km/s .
Maser components from the central part of the spectrum fall into four velocity groups but into three spatial groups .
Three spatial groups of low-velocity features detected in the 2014 observations are arranged in a linear structure about \sim 200 AU in length .
Two of these groups were not detected in 1996 and possibly are jets which formed between 1996 and 2014 .
The putative jet seems to have changed direction in 18 years , which we explain by the precession of the jet under the influence of the gravity of material surrounding the globule .
The jet collimation can be provided by a circumstellar protoplanetary disk .
There is a straight line orientation in the V _ { LSR } -Right Ascension diagram between the jet and the maser group at V _ { LSR } = \sim 0.3 km/s .
However , the central group with the same position but at the velocity V _ { LSR } \sim - 3.4 km/s falls on a straight line between two high-velocity components detected in 2014 .
Comparison of the low-velocity positions from 2014 and 1996 , based on the same diagram , shows that the majority of the masers maintain their positions near the central velocity V _ { LSR } = \sim 0.3 km/s during the 18 year period .