A new approach to spectroscopic phase curves - The emission spectrum of WASP-12b observed in quadrature with HST/WFC3

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Table 2

Measured black-body temperatures from HST compared to brightness temperatures in Spitzer, binned to the same phases, derived from Bell et al. (2019).

Instrument		Dayside T_p		Quadrature T_p	Observation
	Before	Mean	After	K	year
HST G141	3108 ± 520	3186 ± 677	3270 ± 557	2124 ± 417	2011
(this work)

Spitzer Ch1	2720 ± 49	2522 ± 44	2319 ± 74	2340 ± 75	2010
(3.6 μm)	2400 ± 70	2576 ± 43	2746 ± 51	2032 ± 87	2013
Spitzer Ch2	2759 ± 59	2721 ± 49	2684 ± 80	2904 ± 84	2010
(4.5 μm)	2689 ± 71	2612 ± 47	2534 ± 62	3024 ± 91	2013

Notes. Our method uses the slope of the emission spectrum to estimate the brightness temperature rather than the absolute emission, and does not marginalise over a given model, and therefore the uncertainities on the final temperatures are considerably larger.

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