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

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Table I.3

Values of the systematic parameters for Spitzer.

	σ_w [ppm]	f ₀	c ₁ [day⁻¹]
Visit 01	${- 949}_{- 89}^{+ 102}$ ${-949}_{-{89}}^{+{102}}$	0.997018 ± 0.000076	–
Visit 02	$1690_{- 160}^{+ 156}$ ${1690}_{-{160}}^{+{156}}$	${0.996087}_{- 0.000156}^{+ 0.000159}$ ${0.996087}_{-{0.000156}}^{+{0.000159}}$	–
Visit 03	$900_{- 300}^{+ 220}$ ${900}_{-{300}}^{+{220}}$	${0.996271}_{- 0.000076}^{+ 0.000078}$ ${0.996271}_{-{0.000076}}^{+{0.000078}}$	−0.00356 ± 0.00150
Visit 04	$1351_{- 158}^{+ 151}$ ${1351}_{-{158}}^{+{151}}$	${0.995746}_{- 0.000133}^{+ 0.000135}$ ${0.995746}_{-{0.000133}}^{+{0.000135}}$	–
Visit 05	${- 321}_{- 27}^{+ 35}$ ${-321}_{-{27}}^{+{35}}$	0.996462 ± 0.000038	–
Visit 06	$216_{- 49}^{+ 44}$ ${216}_{-{49}}^{+{44}}$	${0.996468}_{- 0.000035}^{+ 0.000036}$ ${0.996468}_{-{0.000035}}^{+{0.000036}}$	–
Visit 07	${- 176}_{- 44}^{+ 89}$ ${-176}_{-{44}}^{+{89}}$	0.996450 ± 0.000034	−0.00142 ± 0.00038
Visit 08	${- 514}_{- 15}^{+ 19}$ ${-514}_{-{15}}^{+{19}}$	0.996469 ± 0.000039	−0.00118 ± 0.00046
Visit 09	$172_{- 79}^{+ 55}$ ${172}_{-{79}}^{+{55}}$	${0.996468}_{- 0.000035}^{+ 0.000036}$ ${0.996468}_{-{0.000035}}^{+{0.000036}}$	−0.00097 ± 0.00040
Visit 10	$173_{- 63}^{+ 49}$ ${173}_{-{63}}^{+{49}}$	0.996471 ± 0.000034	${- 0.00123}_{- 0.00038}^{+ 0.00037}$ ${-0.00123}_{-{0.00038}}^{+{0.00037}}$
Visit 11	$166_{- 84}^{+ 57}$ ${166}_{-{84}}^{+{57}}$	0.996446 ± 0.000035	–
Visit 12	$138_{- 93}^{+ 58}$ ${138}_{-{93}}^{+{58}}$	0.996452 ± 0.000033	–
Visit 13	${- 425}_{- 10}^{+ 15}$ ${-425}_{-{10}}^{+{15}}$	${0.996427}_{- 0.000038}^{+ 0.000041}$ ${0.996427}_{-{0.000038}}^{+{0.000041}}$	–
Visit 14	${- 447}_{- 15}^{+ 19}$ ${-447}_{-{15}}^{+{19}}$	${0.996439}_{- 0.000037}^{+ 0.000038}$ ${0.996439}_{-{0.000037}}^{+{0.000038}}$	–

Notes. The parameters σ_w, f₀ and c ₁ are the additive noise jitter term, the flux normalisation factor and the flux linear slope, respectively. σ_w is expressed in parts-per-million (ppm) and is added to all error bars quadratically. A negative value of σ_w means that the error bars are shrunk. Each f ₀ value is fitted after the corresponding data set has been normalised by its median value (i.e. all flux values are close to 1 and without units). The linear slope c ₁ is expressed in normalised flux units per day.

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