Astrometric Reconnaissance of Exoplanetary Systems (ARES) - I. Methodology validation with HST point-source images of Proxima Centauri

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Volume 706 (February 2026)

A&A, 706 (2026) A112

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Table 2

Fitted astrometric parameters for Proxima.

Parameter	Prior	Best-fit value	Gaia DR3 value	Agreement in σ
α_2016.0 [deg]	𝒰(217.35, 217.41)	$217.392321386 (_{- 0.386}^{+ 0.422} mas)$ $217.392321386\left( {_{ - 0.386}^{ + 0.422}{\rm{mas}}} \right)$	$217.392321472 (_{- 0.024}^{+ 0.024} mas)$ ${\rm{217}}{\rm{.392321472}}\left( {_{ - 0.024}^{ + 0.024}{\rm{mas}}} \right)$	0.54
δ_2016.0 [deg]	𝒰(−62.69, −62.65)	$- 62.676075116 (\begin{array}{l} + 0.186 \\ - 0.187 \end{array} mas)$ $- 62.676075116\left( {\matrix{ { + 0.186} \hfill \cr { - 0.187} \hfill \cr } {\rm{mas}}} \right)$	$- 62.676075117 (_{- 0.034}^{+ 0.034} mas)$ $- 62.676075117\left( {_{ - 0.034}^{ + 0.034}{\rm{mas}}} \right)$	0.01
µ_α cos δ [mas yr⁻¹]	𝒰(−4000, −3500)	$- 3781.761 (\begin{matrix} + 0.045 \\ - 0.050 \end{matrix})$ $- 3781.761\left( {\matrix{ { + 0.045} \cr { - 0.050} \cr } } \right)$	$- 3781.741 (\begin{matrix} + 0.031 \\ - 0.031 \end{matrix})$ $- {\rm{3781}}{\rm{.741}}\left( {\matrix{ { + 0.031} \cr { - 0.031} \cr } } \right)$	0.28
µ_δ [mas yr⁻¹]	𝒰(700, 800)	$769.458 (\begin{matrix} + 0.048 \\ - 0.047 \end{matrix})$ ${\rm{769}}{\rm{.458}}\left( {\matrix{ { + 0.048} \cr { - 0.047} \cr } } \right)$	$769.465 (\begin{matrix} + 0.051 \\ - 0.051 \end{matrix})$ ${\rm{769}}{\rm{.465}}\left( {\matrix{ { + 0.051} \cr { - 0.051} \cr } } \right)$	0.08
ϖ [mas]	𝒰(700, 800)	$768.373 (\begin{matrix} + 0.194 \\ - 0.162 \end{matrix})$ ${\rm{768}}{\rm{.373}}\left( {\matrix{ { + 0.194} \cr { - 0.162} \cr } } \right)$	$768.067 (\begin{matrix} + 0.050 \\ - 0.050 \end{matrix})$ ${\rm{768}}{\rm{.067}}\left( {\matrix{ { + 0.050} \cr { - 0.050} \cr } } \right)$	1.19

Notes. The second column provides the prior used in the MCMC fit. The third column contains the best-fit parameters (and ±1σ uncertainty). The last two columns report the corresponding value in the Gaia DR3 catalog, and the agreements in σ with our HST-based measurement.

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