Left: $F_{{\text{C}}_2{\text{H}}_2}/F_{{\text{H}}_2\text{O}}$ as a function of the strength of the 10 µm silicate feature (stronger silicate features have higher values). The four VLMSs for which we adopt a feature strength of one are denoted by open points. The two outliers at a 10 µm band strength of 3 and 3.8 are the transitional disks LkCa 15 and PDS 70, which were removed for clarity. Middle: relation between $F_{{\text{C}}_2{\text{H}}_2}/F_{{\text{H}}_2\text{O}}$ and Ṁ. Right: relation between $F_{{\text{C}}_2{\text{H}}_2}/F_{{\text{H}}_2\text{O}}$ and M_dust. The PCCs and p-values can be found for each panel. All of the relations are statistically significant (p-value<0.05); however the correlations are not as strong as the $F_{{\text{C}}_2{\text{H}}_2}/F_{{\text{H}}_2\text{O}}$ vs. stellar luminosity relation. Rotated triangular markers for the VLMS sample indicate lower limits on $F_{{\text{C}}_2{\text{H}}_2}/F_{{\text{H}}_2\text{O}}$ and upper limits on M_dust. The error bars are smaller than the points for most targets.