The Secondary Eclipse of the Inflated Super-Neptune WASP-107b

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Abstract The inflated transiting super-Neptune WASP-107b is believed to be generating measurable internal heat, possibly by tidal dissipation of energy in a slightly eccentric orbit. Small orbital eccentricities can be difficult to measure using radial velocity data alone. Fortunately, the orbital phase of the secondary eclipse is very sensitive to eccentricity. Wu et al. recently claimed a possible secondary eclipse using JWST NIRSpec archival data. We here demonstrate that photometry from four Spitzer eclipses confirms Wu et al.’s eclipse phase, and we measure e cos ( ω ) = 0.0143 ± 0.0014 . This establishes a lower limit to the orbital eccentricity, and we also measure the eclipse depth and day side brightness temperature in the sum of Spitzer’s 3.6 and 4.5 μ m bands. We obtain T b = 820 ± 26 K, consistent within the errors with the temperature at the evening limb inferred from JWST transit spectroscopy.

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