Integral field spectroscopy supports atmospheric optics to reveal the finite outer scale of the turbulence

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Volume 687 (July 2024)

A&A, 687 (2024) A40

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Table B.1

Atmospheric parameters derived from the measured image quality at different wavelengths from MUSE data cubes.

HD90177a			HD90177b			HD90177C			HD90177d			OGLEII
Star	$ϵ_{0}^{b}$ $\[\epsilon_0^b\]$	$ℒ_{0}^{b}$ $\[\mathcal{L}_0^b\]$	Star	$ϵ_{0}^{b}$ $\[\epsilon_0^b\]$	$ℒ_{0}^{b}$ $\[\mathcal{L}_0^b\]$	Star	$ϵ_{0}^{b}$ $\[\epsilon_0^b\]$	$ℒ_{0}^{b}$ $\[\mathcal{L}_0^b\]$	Star	$ϵ_{0}^{b}$ $\[\epsilon_0^b\]$	$ℒ_{0}^{b}$ $\[\mathcal{L}_0^b\]$	Star	$ϵ_{0}^{b}$ $\[\epsilon_0^b\]$	$ℒ_{0}^{b}$ $\[\mathcal{L}_0^b\]$
(1)	(2)	(3)	(1)	(2)	(3)	(1)	(2)	(3)	(1)	(2)	(3)	(1)	(2)	(3)
1	0.79	18.1±1.3	1	0.78	14.0±0.9	1	0.81	15.3±1.0	1	0.71	21.3±1.7	1	0.99	15.9±1.0
2	0.82	15.5±1.0	2	0.78	17.6±1.3	2	0.82	14.8±1.0	2	0.69	32.9±3.2	2	0.98	10.3±0.6
3	0.79	28.9±2.5	3	0.76	31.4±3.0	3	0.83	19.5±1.4	3	0.77	21.1±1.6	4	0.96	10.4±0.6
11	0.77	22.0±1.8	11	0.72	29.8±2.6	11	0.79	17.5±1.3	11	0.63	47.9±6.2	7	0.93	29.1±2.5

												9	0.87	21.4±1.6
												10	0.91	11.2±0.6
$(\bar{P})$ $\[(\bar{P})\]$	0.79	21.1		0.76	23.2		0.81	16.8		0.70	30.8		0.94	16.3
σ_P	0.02	5.8		0.03	8.7		0.02	2.2		0.06	12.7		0.05	7.6

Notes. Columns indicate the MUSE observed field, and each sub-column corresponds to (1) the number label of the star in the field (see Fig. B.2), and (2) and (3) the best combination of ε₀ and $ℒ_{0}$ $\[\mathcal{L}_0\]$ values minimizing residuals when comparing the predicted ε_LE using Eq. 5 with these values to the measured IQ at any wavelength, assuming a negligible dome turbulence contribution. The last two lines present the average ( $(\bar{P})$ $\[(\bar{P})\]$ ) and standard deviation (σ_P) of the estimated parameters. These values are derived by averaging the individual estimations from each star in the field.

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