In our Galaxy, the Milky Way, the space between the stars is permeated with magnetic field, relativistic cosmic rays and interstellar matter consisting of gas in ionized, atomic, and molecular states, and of dust. It is interesting to observe how different gas phases interact with each other and how magnetic field shapes diffuse interstellar gas. Therefore, in this work we study the radiation of neutral hydrogen and cosmic dust, and determine orientations of linear structures which will then be compared with each other and with the orientation of the magnetic field. Study was conducted using magneto-hydrodynamic simulations of colliding super-shells, based on which was simulated synchrotron emission of our Galaxy and determined emission of neutral hydrogen and dust. The linear structures obtained from the synthetic observations surprisingly resemble the filamentary structures and depolarization canals found in the real data. An analysis of synchrotron radiation is performed by RM synthesis, which untangles the radiation by Faraday depths, since the magneto-ionic medium causes Faraday rotation. To identify and quantify the orientation of straight depolarization canals, the Rolling Hough Transform algorithm is applied. Furthermore, hydrogen emission is determined from MHD simulation. In an image of the temperature brightness the orientation of the observed filamentary HI structures is determined by RHT analysis. The polarized dust emission is also analysed since it measures the orientation of the magnetic field. Comparing orientations of linear structures shows that hydrogen filaments and depolarization canals follow orientation of the magnetic field in the plane of the sky, as found in the real observations.