A systematic bias in template-based radial velocity extraction algorithms

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Volume 700 (August 2025)

A&A, 700 (2025) A93

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Table E.1

Pearson ’s correlation coefficient - R - and 90% confidence interval of the RV residuals over time for Indi and HD40307 observations when applying a template constructed from the first night available to us.

Δ days	R of ϵ Indi	R of HD40307
0	$- {0.95}_{- 0.01}^{0.01}$ $-0.95^{0.01}_{-0.01}$	$- {0.98}_{- 0.00}^{0.00}$ $-0.98^{0.00}_{-0.00}$
1	$- {0.70}_{- 0.04}^{0.05}$ $-0.70^{0.05}_{-0.04}$	$- {0.97}_{- 0.01}^{0.01}$ $-0.97^{0.01}_{-0.01}$
2	${0.64}_{- 0.05}^{0.05}$ $0.64^{0.05}_{-0.05}$	$- {0.96}_{- 0.01}^{0.01}$ $-0.96^{0.01}_{-0.01}$
3	${0.33}_{- 0.08}^{0.08}$ $0.33^{0.08}_{-0.08}$	${0.86}_{- 0.04}^{0.03}$ $0.86^{0.03}_{-0.04}$
4	$- {0.09}_{- 0.09}^{0.09}$ $-0.09^{0.09}_{-0.09}$	${0.89}_{- 0.03}^{0.02}$ $0.89^{0.02}_{-0.03}$
5	$- {0.20}_{- 0.08}^{0.09}$ $-0.20^{0.09}_{-0.08}$	–

Notes. The correlation coefficient is shown as a function of the number of days between the night that was used to construct the stellar template and the night from which we extract the RVs (refer to Appendix E for details).

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