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Galactic magnetic field (GMF) and secondary cosmic rays (CRs) (e.g.$^{10}$beryllium, boron, antiproton) are important components to understand thepropagation of CRs in the Milky Way Galaxy. Realistic modeling of GMF is basedon the Faraday rotation measurements of various Galactic and extragalacticradio sources and synchrotron emission from CR leptons in the radio frequencyrange, thereby providing information of halo height. On the other hand,diffusion coefficient and halo height are also estimated from the$^{10}$Be/$^{9}$Be and B/C ratios. Moreover, density distribution of gaseouscomponents of interstellar medium (ISM) also plays an important role assecondary CRs are produced due to interaction of primary CRs with the gaseouscomponents of ISM. We consider mainly molecular, atomic, and ionized componentsof hydrogen gas for our study. Recent observations and hydrodynamicalsimulations provide new forms of density profiles of hydrogen gas in Milky WayGalaxy. In the \texttt{DRAGON} code, we have implemented our chosen densityprofiles, based on realistic observations in radio, X-ray and $\gamma$-raywavebands, and hydrodynamical simulations of interstellar hydrogen gas to studythe variation in the height of the halo required to fit the observed CRspectra. Our results show the halo height ($z_{t}$) varies in the range of 2 to6 kpc for the density profiles considered in our work.

Constraining the halo size from possible density profiles of hydrogen gas of Milky Way Galaxy