Studies of the diffuse X-ray emitting gas in galaxy clusters have provided powerful constraints on cosmological parameters and insights into plasma astrophysics. However, measurements of the faint cluster outskirts have become possible only over the last few years. I will review the recent Suzaku measurements of the thermodynamic properties of the ICM at large radii, and then focus on the latest results for the Perseus and Virgo clusters. In particular I will discuss the evidence for a clumpy distribution of the gas in the outskirts, which is important for understanding the physics of the ongoing growth of clusters from the surrounding cosmic web.