Combined JWST/MIRI eclipses at 12.8 and 15 µm give depths of 452±86 and 775±90 ppm, leaving an airless ultramafic surface and a hazy CO2 atmosphere as equally viable explanations.
The Mega-MUSCLES Spectral Energy Distribution Of TRAPPIST-1
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abstract
We present a 5A-100um Spectral Energy Distribution (SED) of the ultracool dwarf star TRAPPIST-1, obtained as part of the Mega-MUSCLES Treasury Survey. The SED combines ultraviolet and blue-optical spectroscopy obtained with the Hubble Space Telescope, X-ray spectroscopy obtained with XMM-Newton, and models of the stellar photosphere, chromosphere, transition region and corona. A new Differential Emission Measure model of the unobserved extreme-ultraviolet spectrum is provided, improving on the Lyman alpha to EUV relations often used to estimate the 100-911A flux from low-mass stars. We describe the observations and models used, as well as the recipe for combining them into an SED. We also provide a semi-empirical, noise-free model of the stellar ultraviolet spectrum based on our observations for use in atmospheric modelling of the TRAPPIST-1 planets.
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Combined analysis of the 12.8 and 15 $\mu m$ JWST/MIRI eclipse observations of TRAPPIST-1 b
Combined JWST/MIRI eclipses at 12.8 and 15 µm give depths of 452±86 and 775±90 ppm, leaving an airless ultramafic surface and a hazy CO2 atmosphere as equally viable explanations.