Dark skies of the slightly eccentric WASP-18 b from its optical-to-infrared dayside emission

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Table 7

Retrieved thermal flux in the CHEOPS and TESS passbands.

Retrieval model	Passband	Thermal flux (ppm)	Flux diff. (ppm)	n_σ	A _g
JWST	CHEOPS	${204.1}_{- 10.5}^{+ 10.7}$ $204.1_{-10.5}^{+10.7}$	+7.8 ± 13.1	+0.6	< 0.061
	TESS	${375.6}_{- 12.0}^{+ 12.3}$ $375.6_{-12.0}^{+12.3}$	−35.2 ± 13.9	−2.5	< 0.009
JWST+Spitzer	CHEOPS	${222.1}_{- 7.8}^{+ 7.0}$ $222.1_{-7.8}^{+7.0}$	−10.2 ± 10.9	−0.9	< 0.029
JWST+Spitzer	TESS	${391.6}_{- 10.3}^{+ 9.5}$ $391.6_{-10.3}^{+9.5}$	−51.2 ± 12.5	−4.1	<< 0^†
JWST+Spitzer+TESS	CHEOPS	${190.7}_{- 3.5}^{+ 3.3}$ $190.7_{-3.5}^{+3.3}$	+21.2 ± 8.2	+2.6	0.027 ± 0.011
JWST+Spitzer+TESS	TESS	351.5 ± 4.3	−11.1 ± 8.2	−1.4	< 0.017
JWST+Spitzer+CHEOPS+TESS	CHEOPS	${196.1}_{- 3.4}^{+ 3.0}$ $196.1_{-3.4}^{+3.0}$	+15.8 ± 8.1	+2.0	0.020 ± 0.010
JWST+Spitzer+CHEOPS+TESS	TESS	${358.2}_{- 4.3}^{+ 4.0}$ $358.2_{-4.3}^{+4.0}$	−17.8 ± 8.2	−2.2	< 0.009

Notes. The thermal flux is derived by integrating the retrieval model values in the corresponding passband (CHEOPS or TESS) following Eq. (13). The flux difference is computed with respect to the measured dayside fluxes listed in Table 3. The n_σ column reports the significance of the flux difference in number of σ. The A _g column shows the geometric albedo values corresponding to the flux difference assuming this difference is attributed to reflected light. When the significance on A _g is < 2 σ, we report the 3-σ upper limit. ^(†)The 3-σ upper limit is −0.017.

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