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Table D.1

For GJ 436b models, with different metallicities, and the ULAS J1335+11 model, maximum variations of abundances (in %) for each species for which the reduced scheme is designed.

Species GJ 436b GJ 436b, Z = 100⊙ ULAS J1335+11
H2O 7 × 10−2 (@6 × 102) 1 (@6 × 10−1) 1 × 10−1(@6 × 103)
CH4 2 × 10−1 (@6 × 102) 3 (@3 × 102) 2 × 10−1 (@1 × 101)
CO 1 × 101 (@1 × 10−1) 2 (@1 × 10−1) 1 × 101 (@6 × 103)
CO2 1 × 101 (@1 × 10−1) 1 (@1 × 10−1) 1 × 101(@5 × 103)
NH3 2 × 10−2 (@8 × 102) 2 × 10−1 (@9 × 102) 3 × 10−3 (@5 × 104)
HCN 1 × 101 (@1 × 10−1) 3 (@1 × 10−1) 7 (@7 × 103)
C2H2 4 × 10−1 (@6 × 10−1) 8 (@1) 5 × 10−1 (@1 × 103)

Notes. The pressure level (@level in mbar) at which the maximum variation is reached is indicated within parentheses.These values are calculated within the regions probed by infrared observations: i.e., [0.1–1000] mbar and [10–104 ] mbar for the warm Neptune and the T Dwarf, respectively.

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