Properties of the Magellanic Stream produced in our simulations. Panels (a) and (b) show the observed and simulated Stream respectively in zenithal equal-area coordinates with line-of-sight velocity indicated by the color scale and the relative gas column density indicated by the brightness. The H I data in Panel (a) are from the GASS survey (McClure-Griffiths et al. 2009) with the points showing sight lines with UV-absorption-line observations from the Hubble Space Telescope (Fox et al. 2014) colored by their line-of-sight velocity. Panel (c) shows the column density of the total gas in the Stream (including the ionized Magellanic Corona and neutral Magellanic disk components) in Magellanic Coordinates (l _MS and b _MS). Panel (d) only shows the neutral gas originating in the disks of the LMC and SMC compared to the observed data from Nidever et al. (2010) shown in contours (black, gray, and white correspond to 10²¹, 10²⁰, and 10¹⁹ cm⁻²). The centroids of the LMC and SMC stellar disks are marked by white circles. Panel (e) shows the local standard of rest (LSR) velocity gradient along the Stream with data shown as contours (Nidever et al. 2010). Panel (f) shows the line-of-sight distance to the gas in the Stream along its length with the centroids of the Clouds marked with circles. Note that the bulk of the simulated Stream is significantly closer to us than the Magellanic Clouds are (∼20 kpc vs. ∼60 kpc).