CHEOPS precision phase curve of the Super-Earth 55 Cancri e

Morris, Brett M.; Delrez, Laetitia; Brandeker, Alexis; Cameron, A. Collier; Simon, A. E.; Futyan, D.; Olofsson, G.; Hoyer, S.; Fortier, A.; Demory, Brice-Olivier; Lendl, M.; Wilson, T. G.; Oshagh, M.; Heng, Kevin; Ehrenreich, D.; Sulis, S.; Alibert, Yann; Alonso, R.; Anglada-Escudé, G.; Barrado, D.; Barros, S. C. C.; Baumjohann, W.; Beck, M.; Beck, T.; Bekkelien, A.; Benz, W.; Bergomi, Maria; Billot, N.; Bonfils, X.; Bourrier, V.; Broeg, C.; Bárczy, T.; Cabrera, J.; Charnoz, S.; Davies, Melvyn B.; Ferreras, D. De Miguel; Deleuil, M.; Deline, A.; Demangeon, O.; Erikson, A.; Florén, Hans-Gustav; Fossati, L.; Fridlund, M.; Gandolfi, D.; Muñoz, A. García; Gillon, M.; Guêdel, M.; Guterman, P.; Isaak, K. G.; Kiss, L. L.; Laskar, Jacques; Étangs, A. Lecavelier des; Lieder, Matthias; Lovis, C.; Magrin, Demetrio; Maxted, P. F. L.; Nascimbeni, V.; Ottensamer, R.; Pagano, I.; Pallé, E.; Peter, G.; Piotto, G.; Rubio, A. Pizarro; Pollacco, D.; Pozuelos, F. J.; Queloz, D.; Ragazzoni, Roberto; Rando, N.; Rauer, H.; Ribas, I.; Santos, N. C.; Scandariato, G.; Smith, A. M. S.; Sousa, S. G.; Steller, M.; Szabó, Gy. M.; Ségransan, D.; Thomas, N.; Udry, S.; Ulmer, B.; Grootel, V. Van; Walton, N. A.

doi:10.1051/0004-6361/202140892

Cited by 43 publications

(22 citation statements)

References 65 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…CHEOPS photometry is known to suffer from at least two types of systematic error arising from thermal effects which are found to be correlated with the output of temperature sensors in the telescope structure (Morris et al 2021). It has been established that when the sunlight illumination pattern on the spacecraft changes, thermal flexure of the telescope structure causes subtle changes in the shape of the PSF.…”

Section: Psfmentioning

confidence: 99%

“…The first scientific results from CHEOPS show the range of science that can be achieved with such a high-precision instrument (Lendl et al 2020;Borsato et al 2021;Delrez et al 2021;Leleu et al 2021;Morris et al 2021;Szabó et al 2021;Van Grootel et al 2021;Maxted et al accepted). One such study reports on the improvement in precision of exoplanet sizes in the HD 108236 system (Bonfanti et al 2021), that highlights a key scientific goal of the CHEOPS mission: the refinement of exoplanet radii to decrease bulk density uncertainties, and thereby allowing internal structure and atmospheric evolution modelling.…”

Section: Cheopsmentioning

confidence: 99%

See 1 more Smart Citation

A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Wilson,

Goffo,

Alibert

et al. 2022

Preprint

View full text Add to dashboard Cite

We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine 𝑇 eff,★ = 4734 ± 67 K, 𝑅 ★ = 0.726 ± 0.007 𝑅 , and 𝑀 ★ = 0.748 ± 0.032 𝑀 . We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of 𝑃 b = 6.44387 ± 0.00003 d, a radius of 𝑅 b = 2.59 ± 0.04 𝑅 ⊕ , and a mass of 𝑀 b = 13.5 +1.7 −1.8 𝑀 ⊕ , whilst TOI-1064 c has an orbital period of 𝑃 c = 12.22657 +0.00005 −0.00004 d, a radius of 𝑅 c = 2.65 ± 0.04 𝑅 ⊕ , and a 3𝜎 upper mass limit of 8.5 M ⊕ . From the high-precision photometry we obtain radius uncertainties of ∼1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b is important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets.

show abstract

Section: Psfmentioning

confidence: 99%

Section: Cheopsmentioning

confidence: 99%

A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Wilson,

Goffo,

Alibert

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…With the upcoming launch of JWST (Bean et al 2018) and the Ariel mission (Tinetti et al 2016), precise spectral data across the infrared wavelength regime will become available for the community to analyze. Kepler (Howell et al 2014), TESS (Ricker et al 2014), and CHEOPS (Broeg et al 2013) have provided optical-band photometric data of exoplanet phase curves, allowing examination of their albedo and thermal properties (e.g., Demory et al 2013;Wong et al 2020;Morris et al 2021). The unique 3D nature of each exoplanet atmosphere manifests itself in the observational properties of that specific object.…”

Section: Introductionmentioning

confidence: 99%

3D Radiative Transfer for Exoplanet Atmospheres. gCMCRT: A GPU-accelerated MCRT Code

Lee

Wardenier

Prinoth

et al. 2022

ApJ

View full text Add to dashboard Cite

Radiative transfer (RT) is a key component for investigating atmospheres of planetary bodies. With the 3D nature of exoplanet atmospheres being important in giving rise to their observable properties, accurate and fast 3D methods are required to be developed to meet future multidimensional and temporal data sets. We develop an open-source GPU RT code, gCMCRT, a Monte Carlo RT forward model for general use in planetary atmosphere RT problems. We aim to automate the post-processing pipeline, starting from direct global circulation model (GCM) output to synthetic spectra. We develop albedo, emission, and transmission spectra modes for 3D and 1D input structures. We include capability to use correlated-k and high-resolution opacity tables, the latter of which can be Doppler-shifted inside the model. We post-process results from several GCM groups, including ExoRad, SPARC/MITgcm THOR, UK Met Office UM, Exo-FMS, and the Rauscher model. Users can therefore take advantage of desktop and HPC GPU computing solutions. gCMCRT is well suited for post-processing large GCM model grids produced by members of the community and for high-resolution 3D investigations.

show abstract

“…One of the main themes of its science program is the characterization of exoplanet atmospheres (Benz et al 2021). This consists of observations of secondary eclipses of hot Jupiters (e.g., Lendl et al 2020;Hooton et al 2022) across a wide range of temperatures and planetary surface gravities, full or partial phase curves of the most compelling targets (e.g., Deline et al 2022), and detailed observations of ultra-hot super-Earths (e.g., Morris et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Phase curve and geometric albedo of WASP-43b measured with CHEOPS, TESS, and HST WFC3/UVIS

Scandariato

Singh

Kitzmann

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. Observations of the phase curves and secondary eclipses of extrasolar planets provide a window onto the composition and thermal structure of the planetary atmospheres. For example, the photometric observations of secondary eclipses lead to the measurement of the planetary geometric albedo, A g , which is an indicator of the presence of clouds in the atmosphere. Aims. In this work, we aim to measure the A g in the optical domain of WASP-43b, a moderately irradiated giant planet with an equilibrium temperature of ∼1400 K. Methods. For this purpose, we analyzed the secondary eclipse light curves collected by CHEOPS together with TESS along with observations of the system and the publicly available photometry obtained with HST WFC3/UVIS. We also analyzed the archival infrared observations of the eclipses and retrieve the thermal emission spectrum of the planet. By extrapolating the thermal spectrum to the optical bands, we corrected for the optical eclipses for thermal emission and derived the optical A g . Results. The fit of the optical data leads to a marginal detection of the phase-curve signal, characterized by an amplitude of 160 ± 60 ppm and 80 +60 −50 ppm in the CHEOPS and TESS passbands, respectively, with an eastward phase shift of ∼ 50 • (1.5σ detection). The analysis of the infrared data suggests a non-inverted thermal profile and solar-like metallicity. The combination of the optical and infrared analyses allows us to derive an upper limit for the optical albedo of A g < 0.087, with a confidence of 99.9%. Conclusions. Our analysis of the atmosphere of WASP-43b places this planet in the sample of irradiated hot Jupiters, with monotonic temperature-pressure profile and no indication of condensation of reflective clouds on the planetary dayside.

show abstract

CHEOPS precision phase curve of the Super-Earth 55 Cancri e

Cited by 43 publications

References 65 publications

A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

3D Radiative Transfer for Exoplanet Atmospheres. gCMCRT: A GPU-accelerated MCRT Code

Phase curve and geometric albedo of WASP-43b measured with CHEOPS, TESS, and HST WFC3/UVIS

Contact Info

Product

Resources

About