Table 3: Ice column densities. The errors are at 3$\sigma $ level and are dominated by systematics.

Source		 $\tau$(H2O $_{{\rm ice}}$) $N_{{\rm ice}}$(H2O) $T_{{\rm ice}}$(H2O) $N_{{\rm ice}}$(OCN-)a $N_{{\rm ice}}$(CH3OH)b
      (1018 cm-2) (K) (1016 cm-2) (1017 cm-2)

LLN 8		 IRAS 08211-4158 0.55 $\pm$ 0.10 0.80 $\pm$ 0.15 10-40 <1.5 <1.0
LLN 8b IRAS 08211-4158b 1.2 $\pm$ 0.3 1.7 $\pm$ 0.4 10-40 ... ...
LLN 13 IRAS 08375-4109 1.4 $\pm$ 0.3 2.2 $\pm$ 0.4 10-40 <0.5 <1.0
LLN 13b IRAS 08375-4109b 1.1 $\pm$ 0.3 1.7 $\pm$ 0.4 10-40 ... ...
LLN 17 IRAS 08448-4343 2.46 $\pm$ 0.50 3.61 $\pm$ 0.70 10-40 4.3 $\pm$ 0.5 2.5 $\pm$ 1.0
LLN 17b IRAS 08448-4343b 1.4 $\pm$ 0.3 2.2 $\pm$ 0.2 10-40 <1.5 ...
LLN 19 IRAS 08470-4321 0.72 $\pm$ 0.10 1.05 $\pm$ 0.2 10-40 <0.5 <1.0
LLN 41 IRAS 09017-4716 1.26 $\pm$ 0.20 1.85 $\pm$ 0.4 10-40 <1.5 <1.0
LLN 41b IRAS 09017-4716b 0.8 $\pm$ 0.3 1.2 $\pm$ 0.4 10-40 <1.5 ...
Notes:
a The 3$\sigma $ upper limits are derived assuming $\Delta \nu=25$ cm-1 and $A=1.0 \times 10^{-16}$ cm-1 molec-1. Upper limits derived from low resolution spectra are higher than that from medium resolution because of the possible contamination by CO gas phase lines. b The 3$\sigma $ upper limits are derived assuming $\Delta \nu=14$ cm-1 and $A =2.8 \times 10^{-18}$ cm-1 molec-1. No upper limits are given for the companion objects because the signal-to-noise ratios are too low to provide scientifically meaningful upper limits.

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