Multi-band infrared imaging reveals dusty spiral arcs around the binary B[e] star 3 Puppis

Open Access

Table B.2

Statistic figures obtained with MYTHRA applied on the resulting PYRA grid of 3360 images reconstructed from 3 Puppis data.

Spectral band	L-curve inflection point ( $μ^{+} \| χ_{+}^{2}$ $\mu^+\|\,\chi_+^2$ )	$χ_{M i R A}^{2}$ $\chi^2_\mathrm{MiRA}$ criterion	Selected subset	Images kept for the mean	Averaged image characteristics
Spectral band		$χ_{M i R A}^{2}$ $\chi^2_\mathrm{MiRA}$ criterion	Selected subset	Images kept for the mean	Pixel size (mas · pixel⁻¹)	$χ_{g l o b a l}^{2}$ $\chi^2_\mathrm{global}$	$χ_{v i s}^{2}$ $\chi^2_\mathrm{vis}$	$χ_{c l o s}^{2}$ $\chi^2_\mathrm{clos}$
L-band	2.95 · 10⁴ \| 2.1	[0.5 - 3.0]	224	181	0.397	7.6	8.4	6.4
M-band	2.41 · 10⁴ \| 6.5	[0.5 - 10]	226	80	0.594	5.3	6.8	2.9
N-band	1.57 · 10⁴ \| 2.2	[0.5 - 5.0]	253	253	1.056	2.2	3.3	0.6

Notes. The $χ_{M i R A}^{2}$ $\chi^2_\mathrm{MiRA}$ interval corresponds to the reduced chi-squared value returned by MiRA in output for the reconstructed image. Whereas $χ_{g l o b a l}^{2}$ $\chi^2_\mathrm{global}$ corresponds to the weighted sum of the $χ_{v i s}^{2}$ $\chi^2_\mathrm{vis}$ from the squared visibility fit and of the $χ_{c l o s}^{2}$ $\chi^2_\mathrm{clos}$ from the closure phase fit. Both fits result from the comparison between the simulated data (computed from the MYTHRA averaged images) and the VLTI/MATISSE data.

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