The GAPS Programme at TNG - LXIX. The dayside of WASP-76 b revealed by GIANO-B, HARPS-N, and ESPRESSO: Evidence of 3D atmospheric effects

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Volume 701 (September 2025)

A&A, 701 (2025) A261

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Table 3

Cross-correlation results.

	V_rest [km s⁻¹]		Kp [km s⁻¹]		S/N
	gaussian fit	max(S/N)-1	gaussian fit	max(S/N)-1	S/N
CO (GIANO-B)	2.71 ± 0.51	${3.00}_{- 6.00}^{+ 3.00}$ $3.00_{-6.00}^{+3.00}$	195.00 ± 0.34	${195.00}_{- 5.00}^{+ 5.00}$ $195.00_{-5.00}^{+5.00}$	10.4
Fe I (GIANO-B)_∗	14.5 ±0.5	/	205.9 ± 0.7	/	4.0
Fe I (HARPS-N)	0.55 ± 0.71	${0.00}_{- 4.50}^{+ 4.50}$ $0.00_{-4.50}^{+4.50}$	193.59 ± 0.59	${196.00}_{- 9.00}^{+ 5.00}$ $196.00_{-9.00}^{+5.00}$	3.5
Fe I (ESPRESSO)	−0.36 ± 0.40	${0.00}_{- 3.00}^{+ 3.00}$ $0.00_{-3.00}^{+3.00}$	189.10 ± 0.49	${189.00}_{- 5.00}^{+ 5.00}$ $189.00_{-5.00}^{+5.00}$	6.2

Notes. For each investigated molecule, the planet’s orbital velocity (Kp), the velocity in the planet’s rest frame (V_rest), and the S/N of the detection are reported. Two types of values (with associated uncertainties) are provided for each measurement: one obtained by fitting a Gaussian to the 1D CC function at the peak position, and one estimated directly from the position of the peak of S/N in the map. In the latter case, the uncertainty is estimated by identifying where the S/N value decreases by 1 unit. Consequently, the number of decimal digits in the table differs according to the method employed to derive the corresponding value. ^∗Marginal detection obtained from only one observing night (namely N2). The K_p and V_rest values are computed by using a 2D Gaussian, including a rotation angle to account for the inclined feature of the detection blob (see Sect. 4.1).

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