Same as in Figure 3, but for sightlines toward Monoceros R2 (l = 215.°2, b = −12.°9), Gemini OB1 (l = 193.°4, b = 0.°3), Rosette (l = 206.°0, b = −2.°7), and Maddalena (l = 216.°9, b = −2.°4). These panels highlight the limitations of our simple line-of-sight dust model. In comparison to the rest of our clouds (whose systematic uncertainty we estimate to be 5%), these four clouds display a “ramp” in foreground extinction leading up to the cloud. This behavior is not captured by our simple model, which assumes a flat, well-behaved foreground cloud. These modeling mismatches cause us to systematically underestimate the distances to these sightlines and suggests higher systematic uncertainties (see Section 5.2).