When combining the eclipse from CHEOPS with the measurements from TESS and Spitzer, our global climate models indicate that LTT 9779 b likely has a super metal-rich atmosphere, with a lower limit of 400× solar being found, and the presence of silicate clouds. This value is similar to that of Venus in our own Solar System. This surprisingly large depth provides a geometric albedo for the planet of 0.80 −0.17 +0.10, consistent with estimates of radiative-convective models. Each of our analysis methods yielded statistically similar results, providing a robust detection of the eclipse of LTT 9779 b with a depth of 115☒4 ppm. We carefully analyzed and detrended the light curves using three independent methods to perform the final astrophysical detrending and eclipse model fitting of the individual and combined light curves. We observed ten secondary eclipses of the planet with CHEOPS. We aim to detect and characterize the optical secondary eclipse of the planet LTT 9779 b using the CHaracterising ExOPlanet Satellite (CHEOPS) to measure the planetary albedo and search for the signature of atmospheric condensates. If such signals can be detected and modeled, however, they can provide planetary albedos, thermal characteristics, and information on absorbers in the upper atmosphere.Īims. Optical secondary eclipse measurements of small planets can provide a wealth of information about the reflective properties of these worlds, but the measurements are particularly challenging to attain because of their relatively shallow depth. Observatoire Astronomique de l’Université de Genève,ĭepartamento de Astronomía, Universidad de Chile,Ĭontext. Jet Propulsion Laboratory, California Institute of Technology, Las Campanas Observatory, Carnegie Institution of Washington, Colina El Pino,ĭepartment of Physics and Astronomy, University of Kansas,ĭepartment of Physics and Astronomy, The University of New Mexico, INAF, Osservatorio Astrofisico di Catania,Ĭentre for Exoplanet Science, SUPA School of Physics and Astronomy, University of St Andrews, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Vinés 12Į-mail: de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales,Ĭentro de Astrofísica y Tecnologías Afines (CATA), Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes In fact, you may even want to increase the Whites or the Highlights to create more contrast between the blue sky and the white clouds. If there is sufficient detail in the clouds, you don’t need to recover the bright areas further. That’s why we started by darkening the blue tones.īy the way, after darkening the blues, take a careful look at your photo. If you crank down the highlights, yes, you will add detail to the clouds – but you will push the tones of the blues and whites together so that there won’t be the strong contrast you want. The truth is that part of what makes a sky look great is deep, rich, blue tones combined with bright white clouds. Why didn’t we start by toning down the highlights? After all, that would handle a lot of the washed-out areas of the sky. Adjusting the blues too heavily can cause banding (i.e., separation of the colors into stripes) and other forms of image degradation. Note: As mentioned above, be careful not to go too far.
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