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Several publications highlight the importance of the observations of bowshocks to learn more about the surrounding interstellar medium and radiationfield. We revisit the most prominent dusty and gaseous bow shock source, X7,close to the supermassive black hole, Sgr~A*, using multiwavelength analysis.For the purpose of this study, we use SINFONI (H+K-band) and NACO ($L'$- and$M'$-band) data-sets between 2002 and 2018 with additional COMIC/ADONIS+RASOIR($L'$-band) data of 1999. By analyzing the line maps of SINFONI, we identify avelocity of $\sim 200$ km/s from the tip to the tail. Furthermore, acombination of the multiwavelength data of NACO and SINFONI in the $H$-, $K$-,$L'$-, and $M'$-band results in a two-component black-body fit that impliesthat X7 is a dust-enshrouded stellar object. The observed ongoing elongationand orientation of X7 in the Br$\gamma$ line maps and the NACO $L'$-bandcontinuum indicate a wind arising at the position of Sgr~A* or at the IRS16complex. Observations after 2010 show that the dust and the gas shell seems tobe decoupled in projection from its stellar source S50. The data also impliesthat the tail of X7 gets thermally heated up due to the presence of S50. Thegas emission at the tip is excited because of the related forward scattering(Mie-scattering), which will continue to influence the shape of X7 in the nearfuture. In addition, we find excited [FeIII] lines, which underline togetherwith the recently analyzed dusty sources and the Br$\gamma$-bar the uniquenessof this source.

First observed interaction of the circumstellar envelope of an S-star with the environment of Sgr A*