sunset: A database of synthetic atmospheric-escape transmission spectra for nearly every transiting planet

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Table C.2

Analysis of the bias and uncertainty arising from the chosen atmospheric temperature.

Parameter	New/old ratio	Smallest and largest ratio	Notes
T₀	${0.81}_{- 0.11}^{+ 0.11}$ $\[0.81_{-0.11}^{+0.11}\]$	0.56 and 1.0	Strong dependence on ϕ, with largest difference at both low and high ϕ. No clear trend with other parameters.
Helium depth	${1.5}_{- 0.3}^{+ 2.0}$ $\[1.5_{-0.3}^{+2.0}\]$	0.98 and 7.2	Depends mainly on the change in T₀, which in turn depends on ϕ.
Calcium depth	${3.0}_{- 1.3}^{+ 19.1}$ $\[3.0_{-1.3}^{+19.1}\]$	0.97 and 79	Five planets with low F_XUV show very strong changes above a factor 20. Other planets are below a factor 10.
Magnesium depth	${1.3}_{- 0.2}^{+ 1.5}$ $\[1.3_{-0.2}^{+1.5}\]$	0.99 and 4.8	Only planets with low to medium F_XUV show a significant change.
Iron depth	${1.5}_{- 0.2}^{+ 1.3}$ $\[1.5_{-0.2}^{+1.3}\]$	0.97 and 8.3	Depends mainly on the change in T₀, which in turn depends on ϕ.
Carbon depth	${1.1}_{- 0.2}^{+ 0.7}$ $\[1.1_{-0.2}^{+0.7}\]$	0.46 and 8.9	Only planets with low F_XUV show a change above a factor 2.
Oxygen depth	${1.5}_{- 0.3}^{+ 1.2}$ $\[1.5_{-0.3}^{+1.2}\]$	0.97 and 7.0	Depends mainly on the change in T₀, which in turn depends on ϕ.
Silicon depth	${1.5}_{- 0.3}^{+ 1.6}$ $\[1.5_{-0.3}^{+1.6}\]$	0.99 and 6.5	Depends mainly on the change in T₀, which in turn depends on ϕ.

Notes. In the main work, we used a self-consistent temperature $\hat{T}$ $\[\hat{T}\]$ that is equal to the maximum of the nonisothermal profile. In Appendix C, we run 27 new models using a self-consistent temperature that is equal to the mean of the nonisothermal profile between 1 and 3 R_p. This table presents how the newly found temperatures and resulting spectral line strengths compare to the results of the main work. We report the 0th, 16th, 50th, 84th, and 100th percentile of the ratio between new and old value.

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