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A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c



Three Earth-sized exoplanets were recently discovered close to the habitable zone1,2 of the nearby ultracool dwarf star TRAPPIST-1 (ref. 3). The nature of these planets has yet to be determined, as their masses remain unmeasured and no observational constraint is available for the planetary population surrounding ultracool dwarfs, of which the TRAPPIST-1 planets are the first transiting example. Theoretical predictions span the entire atmospheric range, from depleted to extended hydrogen-dominated atmospheres4,5,6,7,8. Here we report observations of the combined transmission spectrum of the two inner planets during their simultaneous transits on 4 May 2016. The lack of features in the combined spectrum rules out cloud-free hydrogen-dominated atmospheres for each planet at ≥10σ levels; TRAPPIST-1 b and c are therefore unlikely to have an extended gas envelope as they occupy a region of parameter space in which high-altitude cloud/haze formation is not expected to be significant for hydrogen-dominated atmospheres9. Many denser atmospheres remain consistent with the featureless transmission spectrum—from a cloud-free water-vapour atmosphere to a Venus-like one.

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Figure 1: Hubble/WFC3 white-light curve for the TRAPPIST-1b and TRAPPIST-1c double transit of 4 May 2016.
Figure 2: Hubble/WFC3 spectrophotometry of the TRAPPIST-1b and TRAPPIST-1c double transit of 4 May 2016.
Figure 3: Transmission spectra of TRAPPIST-1b and TRAPPIST-1c compared with models.


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This work is based on observations made with the NASA/ESA Hubble Space Telescope that were obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. These observations are associated with program HST-GO-14500 (principal investigator J.d.W.), support for which was provided by NASA through a grant from the Space Telescope Science Institute. The research leading to our results was funded in part by the European Research Council (ERC) under the FP/2007-2013 ERC grant 336480, and through an Action de Recherche Concertée (ARC) grant financed by the Wallonia-Brussels Federation. H.R.W. acknowledges support through an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by the Universities Space Research Association through a contract with NASA. M.G. is Research Associate at the Belgian Fonds (National) de la Recherche Scientifique (FRS–FNRS). L.D. acknowledges support of the Fund for Research Training in Industry and Agriculture of the FRS–FNRS. We thank D. Taylor, S. Deustua, P. McCullough, and N. Reid for their assistance in planning and executing our observations. We are also grateful for discussions with Z. Berta-Thompson and Pierre Magain about this study and manuscript. We thank the ATLAS and PHOENIX teams for providing stellar models.

Author information

Authors and Affiliations



J.d.W. and H.R.W. led the data reduction and analysis, with the support of M.G., N.K.L. and B.-O.D. J.d.W., H.R.W., and N.K.L. led the data interpretation, with the support of M.G. and J.A.V. J.A.V. provided the limb-darkening coefficients and further insights into TRAPPIST-1’s properties and emission together with A.J.B. Every author contributed to writing both the manuscript and the HST proposal behind these observations.

Corresponding author

Correspondence to Julien de Wit.

Additional information

Reviewer Information Nature thanks D. Ehrenreich and the other anonymous reviewer(s) for their contribution to the peer review of this work.

Extended data figures and tables

Extended Data Figure 1 Marginal effects of instrumental systematics on transit depth estimates.

a, Evidence-based weight, Wq, for each systematic model12 applied to the white-light curve. b, Combined transit depth estimate (ΔFb+c) obtained by correcting the data, using each systematic model. c, d, Individual transit depth estimates for TRAPPIST-1b and TRAPPIST-1c, ΔFb and ΔFc. The horizontal lines indicate the final marginalized measurements and associated uncertainties. The scale of the values here indicates that all of the systematic models fit equally well to the data.

Extended Data Figure 2 TRAPPIST-1’s limb darkening.

Stellar limb-darkening relationships for TRAPPIST-1 (black curves) and four stellar models (coloured curves) that bracket the effective temperature and surface gravity of TRAPPIST-1 (shown in coloured and black numbers in a; temperature is in K and surface gravity is expressed in log(g). The circles are theoretical15 specific intensities (I) relative to disc centre (Ic) as a function of μ′ (the cosine of the angle between an outward radial vector and the direction towards the observer). We fitted I/Ic averaged over the indicated wavelength intervals to determine the quadratic (dashed curves) and four-parameter (solid curves) limb-darkening coefficients. a, Stellar limb-darkening relationship integrated over WFC3’s spectral band. bl, Stellar limb-darkening relationship over the 11 spectral channels used here.

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de Wit, J., Wakeford, H., Gillon, M. et al. A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c. Nature 537, 69–72 (2016).

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