Fig. 3: Density distribution.
From: Asymmetric eROSITA bubbles as the evidence of a circumgalactic medium wind
Panel a shows the initial density distribution of the hot halo (Y = 0), and the grey line denotes the Galactic disk. Panel b shows the density and velocity (arrows) at t = 360 Myr, with black contours representing the boundary of the initial halo medium. Due to the shielding of the Galactic disk, density and metal abundance in northern and southern halos are quite different. In the northern halo, the materials at Z ≳ 3 kpc are incoming CGM wind. In the southern halo, the region of ∣Z∣ ≲ 4 kpc is almost unaffected, and the initial halo medium even stretches to Z ≃ −20 kpc in the leeward region.
