Left: Percentage of dust mass carried by Fe as a function ol the gas-to-dust mass ratio Rg/d (from Frisch and Slavin, 2003). The interstellar column densities for these stars span three orders of magnitude, with the smallest values of Rg/d corresponding to the lowest percentages of Fe in the grain mass. Right: Abundances relative to Asplund et al. (2005) solar abundances vs. condensation temperature. Results from models of the ionization for the ϵ CMa line of sight including radiative transfer (Model 26 in Slavin and Frisch (2008)). The symbol shape indicates the assumed HI column density for the model, while the color indicates the assumed temperature for the hot gas of the Local Bubble. The abundances are fixed so as to match the observed ion column densities. An overabundance of carbon in the gas phase is required to match the observed carbon abundances, suggesting that carbonaceous dust grains have been destroyed in the LIC. The carbon abundance in these models has been reconstructed from the cloud ionization and the 1335.7 Å carbon fine-struture line (see Slavin and Frisch, 2008 for additional information).