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

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Table C.1

Analysis of the bias and uncertainty arising from the chosen extent of the simulation domain.

Spectral line	New/old ratio	Smallest and largest ratio
Helium	${0.91}_{- 0.14}^{+ 0.16}$ $\[0.91_{-0.14}^{+0.16}\]$	0.70 and 1.2
Calcium	${1.1}_{- 0.3}^{+ 0.3}$ $\[1.1_{-0.3}^{+0.3}\]$	0.69 and 1.5
Magnesium	${1.2}_{- 0.1}^{+ 0.2}$ $\[1.2_{-0.1}^{+0.2}\]$	0.95 and 1.9
Iron	${0.95}_{- 0.09}^{+ 0.13}$ $\[0.95_{-0.09}^{+0.13}\]$	0.82 and 1.1
Carbon	${1.4}_{- 0.3}^{+ 0.9}$ $\[1.4_{-0.3}^{+0.9}\]$	0.98 and 8.7
Oxygen	${0.92}_{- 0.08}^{+ 0.15}$ $\[0.92_{-0.08}^{+0.15}\]$	0.80 and 1.1
Silicon	${1.1}_{- 0.1}^{+ 0.2}$ $\[1.1_{-0.1}^{+0.2}\]$	0.86 and 1.7

Notes. In the main work, we fixed the upper boundary at 8R_p. In Appendix C, we run 27 new models extending to the stellar radius. This table presents how the newly found 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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