Context : We trace several dusty infrared sources on their orbits around Sgr A* with SINFONI and NACO mounted at the VLT/Chile .
These sources show near-infrared excess and Doppler-shifted line emission .
We investigate these sources in order to clarify their nature and compare their relationship to other observed NIR objects close to Sgr A* .

Aims : By using SINFONI , we are able to determine the spectroscopic properties of the investigated dusty infrared sources .
Furthermore , we extract spatial and velocity information of these objects .
We are able to identify X7 , X7.1 , X8 , G1 , DSO/G2 , D2 , D23 , D3 , D3.1 , D5 , and D9 in the Doppler-shifted line maps of the SINFONI H+K data .
From our K- and L ^ { \prime } -band NACO data , we derive the related magnitudes of the brightest sources located west of Sgr A* .

Methods : For determining the line of sight velocity information and to investigate single emission lines , we use the near-infrared integral field spectrograph SINFONI data-sets between 2005 and 2015 .
For the kinematic analysis , we use NACO data-sets between 2002 and 2018 .
This study is done in the H , K _ { s } , and L ^ { \prime } band .
From the 3D SINFONI data-cubes , we extract line-maps in order to derive positional information of the sources .
In the NACO images , we identify the dusty counterpart of the objects .
If possible , we determine Keplerian orbits and apply a photometric analysis .

Results : The spectrum of the investigated objects show a Doppler-shifted Br \gamma and HeI line emission .
For some objects west of Sgr A* , we find additionally [ Fe III ] line emission that can be clearly distinguished from the background .
A one-component blackbody model fits the extracted near-infrared flux for the majority of the investigated objects , with the characteristic dust temperature of 500 { K } .
The photometric derived H - and K _ { S } -band magnitudes are between mag _ { H } > 22.5 and mag _ { K } = 18.1 ^ { +0.3 } _ { -0.8 } for the dusty sources .
For the H -band magnitudes we can provide an upper limit .
For the bright dusty sources D2 , D23 , and D3 , the Keplerian orbits are elliptical with a semi-major axis of a _ { D 2 } = ( 749 \pm 13 ) mas , a _ { D 23 } = ( 879 \pm 13 ) , and a _ { D 3 } = ( 880 \pm 13 ) mas .
For the DSO/G2 , a single-temperature and a two-component blackbody model is fitted to the H- , K- , L ^ { \prime } - , and M-band data , while the two-component model that consists of a star and an envelope fits its SED better than an originally proposed single-temperature dusty cloud .

Conclusions : The spectroscopic analysis indicates , that the investigated objects could be dust embedded pre-main-sequence stars .
The Doppler-shifted [ Fe III ] line can be spectroscopically identified in several sources that are located between 17:45:40.05 and 17:45:42.00 in DEC .
However , the sources with a DEC less than 17:45:40.05 show no [ Fe III ] emission .
Therefore , these two groups show different spectroscopic features that could be explained by the interaction with a non-spherical outflow that originates at the position of Sgr A* .
Followed by this , the hot bubble around Sgr A* consists out of isolated sources with [ Fe III ] line emission that can partially account for the previously detected [ Fe III ] distribution on larger scales .