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Appendix A: Snowline test

Water snowlines were inferred and compared with results from Min et al. (2011) in Fig. A.1 using the minimum mass solar nebula (MMSN) model (Σ ∝ r^-1.5). The comparison shows that our adopted method reproduces the water snowlines at high accretion rates. For low accretion rates Ṁ ≤ 10^-9M_⊙ yr^-1, our values are slightly lower, but still consistent with those reported in literature.

	Fig. A.1 Snowlines for the MMSN disk without an envelope: black circles show the radii calculated with our method and red squares are tabulated values from Min et al. (2011).
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Appendix B: H₂O, CO₂, and CO gas fraction

The H₂O, CO₂ and CO gas pressure dependent gas fraction abundances are shown in Fig. B.1. Figures B.2 and B.3 show the midplane CO₂ and CO snowlines as a function of luminosity and R_d similar to that of Fig. 9 for H₂O.

	Fig. B.1 Gas fraction (ngas/ngas + nice) for H2O (top), CO2 (middle) and CO (bottom) as a function of density and temperatures.
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	Fig. B.2 Midplane CO2 snowline as a function of stellar luminosity, accretion rate, and disk radius. The parameters are similar to that of Fig. 9.
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	Fig. B.3 Midplane CO snowline as a function of stellar luminosity, accretion rate, and disk radius. The parameters are similar to that of Fig. 9.
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© ESO, 2015