Figure 9 from A Spitzer Transmission Spectrum for the Exoplanet GJ 436b, Evidence for Stellar Variability, and Constraints on Dayside Flux Variations

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A Spitzer Transmission Spectrum for the Exoplanet GJ 436b, Evidence for Stellar Variability, and Constraints on Dayside Flux Variations

Authors: Heather A. Knutson, Nikku Madhusudhan, Nicolas B. Cowan, Jessie L. Christiansen, Eric Agol, Drake Deming, Jean-Michel Désert, David Charbonneau, Gregory W. Henry, Derek Homeier, Jonathan Langton, Gregory Laughlin, and Sara Seager

Knutson et al. 2011 The Astrophysical Journal 735 27.

Provider: AAS Journals

Caption: Figure 9.

Observed minus calculated secondary eclipse times using the best-fit period from the transit fits and allowing the phase of the secondary eclipse to vary freely. Filled circles are eclipse times reported in this paper, and filled stars are additional 3.6 and 4.5 μm eclipse times from Stevenson et al. (2010). The solid line indicates the best-fit phase, with ±1σ uncertainties plotted as dashed lines.

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