We analyse and report in detail new near-infrared ( 1.45 - 2.45 microns ) observations of the Dusty S-cluster Object ( DSO/G2 ) during its approach to the black hole at the center of the Galaxy that were carried out with ESO VLT/SINFONI between February and September 2014 .
Before May 2014 we detect spatially compact Br \gamma and Pa \alpha line emission from the DSO at about 40mas east of SgrA* .
The velocity of the source , measured from the red-shifted emission , is 2700 \pm 60 km/s .
No blue-shifted emission above the noise level is detected at the position of SgrA* or upstream the presumed orbit .
After May we find spatially compact Br \gamma blue-shifted line emission from the DSO at about 30mas west of SgrA* at a velocity of - 3320 \pm 60 km/s and no indication for significant red-shifted emission .
We do not detect any significant extension of velocity gradient across the source .
We find a Br \gamma -line full width at half maximum of 50 \pm 10 Å before and 15 \pm 10 Å after the peribothron transit , i.e .
no significant line broadening with respect to last year is observed .
Br \gamma line maps show that the bulk of the line emission originates from a region of less than 20 mas diameter .
This is consistent with a very compact source on an elliptical orbit with a peribothron time passage in 2014.39 \pm 0.14 .
For the moment , the flaring activity of the black hole in the near-infrared regime has not shown any statistically significant increment .
Increased accretion activity of SgrA* may still be upcoming .
We discuss details of a source model according to which the DSO is rather a young accreting star than a coreless gas and dust cloud .