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1. CHEOPS observations confirm nodal precession in the WASP-33 system

Author

Smith, A. M. S., Csizmadia, Sz., Van Grootel, V., Lendl, M., Persson, C. M., Olofsson, G., Ehrenreich, D., Günther, M. N., Heitzmann, A., Barros, S. C. C., Bonfanti, A., Brandeker, A., Cabrera, J., Demangeon, O. D. S., Fossati, L., Harre, J. -V., Hooton, M. J., Hoyer, S., Kalman, Sz., Salmon, S., Sousa, S. G., Szabó, Gy. M., Wilson, T. G., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T., Barrado, D., Baumjohann, W., Benz, W., Billot, N., Borsato, L., Broeg, C., Cameron, A. Collier, Correia, A. C. M., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demory, B. -O., Derekas, A., Edwards, B., Egger, J. A., Erikson, A., Fortier, A., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Hasiba, J., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Merín, B., Mordasini, C., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Stalport, M., Sulis, S., Udry, S., Ulmer-Moll, S., Venturini, J., Villaver, E., Viotto, V., Walter, I., Walton, N. A., and Wolf, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $\delta$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods., Comment: 18 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics

Published
2024

2. TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit

Author

Alqasim, A., Grieves, N., Rosário, N. M., Gandolfi, D., Livingston, J. H., Sousa, S., Collins, K. A., Teske, J. K., Fridlund, M., Egger, J. A., Cabrera, J., Hellier, C., Lanza, A. F., Van Eylen, V., Bouchy, F., Oelkers, R. J., Srdoc, G., Shectman, S., Günther, M., Goffo, E., Wilson, T., Serrano, L. M., Brandeker, A., Wang, S. X., Heitzmann, A., Bonfanti, A., Fossati, L., Alibert, Y., Delrez, L., Sefako, R., Barros, S., Collins, K. I., Demangeon, O. D. S., Albrecht, S. H., Alonso, R., Asquier, J., Barczy, T., Barrado, D., Baumjohann, W., Beck, T., Benz, W., Billot, N., Borsato, L., Broeg, C., Bryant, E. M., Butler, R. P., Cochran, W. D., Cameron, A. Collier, Correia, A. C. M., Crane, J. D., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Daylan, T., Deleuil, M., Deline, A., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Essack, Z., Fortier, A., Gazeas, K., Gillon, M., Gudel, M., Hasiba, J., Hatzes, A. P., Helling, Ch., Hirano, T., Howell, S. B., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kanodia, S., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lund, M. B., Luque, R., Mann, A. W., Magrin, D., Maxted, P. F. L., Mordasini, C., Narita, N., Nascimbeni, V., Nowak, G., Olofsson, G., Osborn, H. P., Osborne, H. L. M., Osip, D., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Redfield, S., Ribas, I., Rice, M., Ricker, G. R., Rieder, M., Salmon, S., Santos, N. C., Scandariato, G., Seager, S., Segransan, D., Shporer, A., Simon, A. E., Smith, A. M. S., Stalport, M., Szabo, Gy. M., Thompson, I., Twicken, J. D., Udry, S., Vanderspek, R., Van Grootel, V., Venturini, J., Villaver, E., Villaseñor, J., Viotto, V., Walter, I., Walton, N. A., Winn, J. N., and Yee, S. W.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day orbit transiting a bright star ($V = 9.7$ mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of $R_{\mathrm{p}} = 2.5 \pm 0.1 R_{\oplus}$ and a mass of $M_{\mathrm{p}} = 10.5^{+2.2}_{-2.1} M_{\oplus}$, implying a bulk density of $\rho_{\text{p}} = 3.6 \pm 0.8$ g cm$^{-3}$. Our internal composition modeling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with $e$ = 0.39$^{+0.08}_{-0.07}$, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b's formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star-star interactions during the earlier epoch of the Galactic disk formation, given the low metallicity and older age of TOI-757., Comment: Accepted for publication in MNRAS; 26 pages, 14 figures, 6 tables

Published
2024

3. Characterisation of the TOI-421 planetary system using CHEOPS, TESS, and archival radial velocity data

Author

Krenn, A. F., Kubyshkina, D., Fossati, L., Egger, J. A., Bonfanti, A., Deline, A., Ehrenreich, D., Beck, M., Benz, W., Cabrera, J., Wilson, T. G., Leleu, A., Sousa, S. G., Adibekyan, V., Correira, A. C. M., Alibert, Y., Delrez, L., Lendl, M., Patel, J. A., Venturini, J., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fortier, A., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Hasiba, J., Heitzmann, A., Helling, C., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Rieder, M., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Stalport, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Villaver, E., Viotto, V., Walton, N. A., and Zingales, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TOI-421 planetary system contains two sub-Neptune-type planets and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital separation cannot be explained by current formation models without previous orbital migration. We jointly analysed photometric data of three TESS sectors and six CHEOPS visits as well as 156 radial velocity data points to retrieve improved planetary parameters. We also searched for TTVs and modelled the interior structure of the planets. Finally, we simulated the evolution of the primordial H-He atmospheres of the planets using two different modelling frameworks. We determine the planetary radii and masses of TOI-421 b and c to be $R_{\rm b} = 2.64 \pm 0.08 \, R_{\oplus}$, $M_{\rm b} = 6.7 \pm 0.6 \, M_{\oplus}$, $R_{\rm c} = 5.09 \pm 0.07 \, R_{\oplus}$, and $M_{\rm c} = 14.1 \pm 1.4 \, M_{\oplus}$. We do not detect any statistically significant TTV signals. Assuming the presence of a hydrogen-dominated atmosphere, the interior structure modelling results in both planets having extensive envelopes. While the modelling of the atmospheric evolution predicts for TOI-421 b to have lost any primordial atmosphere that it could have accreted at its current orbital position, TOI-421 c could have started out with an initial atmospheric mass fraction somewhere between 10 and 35%. We conclude that the low observed mean density of TOI-421 b can only be explained by either a bias in the measured planetary parameters (e.g. driven by high-altitude clouds) and/or in the context of orbital migration. We also find that the results of atmospheric evolution models are strongly dependent on the employed planetary structure model., Comment: 21 pages, 12 figures, accepted for publication in A&A

Published
2024

4. Refining the properties of the TOI-178 system with CHEOPS and TESS

Author

Delrez, L., Leleu, A., Brandeker, A., Gillon, M., Hooton, M. J., Cameron, A. Collier, Deline, A., Fortier, A., Queloz, D., Bonfanti, A., Van Grootel, V., Wilson, T. G., Egger, J. A., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Güdel, M., Hasiba, J., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Luque, R., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Santos, N. C., Scandariato, G., Seager, S., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Vanderspek, R., Venturini, J., Viotto, V., Walton, N. A., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. Mass estimates derived from a preliminary radial velocity (RV) dataset suggest that the planetary densities do not decrease in a monotonic way with the orbital distance to the star, contrary to what one would expect based on simple formation and evolution models. To improve the characterisation of this key system and prepare for future studies (in particular with JWST), we perform a detailed photometric study based on 40 new CHEOPS visits, one new TESS sector, as well as previously published CHEOPS, TESS, and NGTS data. First we perform a global analysis of the 100 transits contained in our data to refine the transit parameters of the six planets and study their transit timing variations (TTVs). We then use our extensive dataset to place constraints on the radii and orbital periods of potential additional transiting planets in the system. Our analysis significantly refines the transit parameters of the six planets, most notably their radii, for which we now obtain relative precisions $\lesssim$3%, with the exception of the smallest planet $b$ for which the precision is 5.1%. Combined with the RV mass estimates, the measured TTVs allow us to constrain the eccentricities of planets $c$ to $g$, which are found to be all below 0.02, as expected from stability requirements. Taken alone, the TTVs also suggest a higher mass for planet $d$ than the one estimated from the RVs, which had been found to yield a surprisingly low density for this planet. However, the masses derived from the current TTV dataset are very prior-dependent and further observations, over a longer temporal baseline, are needed to deepen our understanding of this iconic planetary system., Comment: 20 pages, 5 figures, 9 tables. Accepted for publication in A&A

Published
2023
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5. TOI-5678 b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS

Author

Ulmer-Moll, S., Osborn, H. P., Tuson, A., Egger, J. A., Lendl, M., Maxted, P., Bekkelien, A., Simon, A. E., Olofsson, G., Adibekyan, V., Alibert, Y., Bonfanti, A., Bouchy, F., Brandeker, A., Fridlund, M., Gandolfi, D., Mordasini, C., Persson, C. M., Salmon, S., Serrano, L. M., Sousa, S. G., Wilson, T. G., Rieder, M., Hasiba, J., Asquier, J., Sicilia, D., Walter, I., Alonso, R., Anglada, G., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bárczy, T., Cabrera, J., Charnoz, S., Cointepas, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dumusque, X., Ehrenreich, D., Eisner, N. L., Erikson, A., Fortier, A., Fossati, L., Gillon, M., Grieves, N., Güdel, M., Hagelberg, J., Helled, R., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Nascimbeni, V., Otegi, J., Ottensammer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Psaridi, A., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Smith, A. M. S., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

A large sample of long-period giant planets has been discovered thanks to long-term radial velocity surveys, but only a few dozen of these planets have a precise radius measurement. Transiting gas giants are crucial targets for the study of atmospheric composition across a wide range of equilibrium temperatures and for shedding light on the formation and evolution of planetary systems. Indeed, compared to hot Jupiters, the atmospheric properties and orbital parameters of cooler gas giants are unaltered by intense stellar irradiation and tidal effects. We identify long-period planets in the Transiting Exoplanet Survey Satellite (TESS) data as duo-transit events. To solve the orbital periods of TESS duo-transit candidates, we use the CHaracterising ExOPlanet Satellite (CHEOPS) to observe the highest-probability period aliases in order to discard or confirm a transit event at a given period. We also collect spectroscopic observations with CORALIE and HARPS in order to confirm the planetary nature and measure the mass of the candidates. We report the discovery of a warm transiting Neptune-mass planet orbiting TOI-5678. After four non-detections corresponding to possible periods, CHEOPS detected a transit event matching a unique period alias. Joint modeling reveals that TOI-5678 hosts a 47.73 day period planet. TOI-5678 b has a mass of 20 (+-4) Me and a radius of 4.91 (+-0.08 Re) . Using interior structure modeling, we find that TOI-5678 b is composed of a low-mass core surrounded by a large H/He layer with a mass of 3.2 (+1.7, -1.3) Me. TOI-5678 b is part of a growing sample of well-characterized transiting gas giants receiving moderate amounts of stellar insolation (11 Se). Precise density measurement gives us insight into their interior composition, and the objects orbiting bright stars are suitable targets to study the atmospheric composition of cooler gas giants., Comment: 17 pages, 10 figures, accepted to A&A

Published
2023
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6. The phase curve and the geometric albedo of WASP-43b measured with CHEOPS, TESS and HST WFC3/UVIS

Author

Scandariato, G., Singh, V., Kitzmann, D., Lendl, M., Brandeker, A., Bruno, G., Bekkelien, A., Benz, W., Gutermann, P., Maxted, P. F. L., Bonfanti, A., Charnoz, S., Fridlund, M., Heng, K., Hoyer, S., Pagano, I., Persson, C. M., Salmon, S., Van Grootel, V., Wilson, T. G., Asquier, J., Bergomi, M., Gambicorti, L., Hasiba, J., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Billot, N., Bonfils, X., Broeg, C., Cabrera, J., Cameron, A. Collier, Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O., Demory, B. -O., Erikson, A., Fortier, A., Fossati, L., Gandolfi, D., Gillon, M., Güdel, M., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pallé, E., Parviainen, H., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Ségransan, D., Serrano, L. M., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., and Walton, N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Observations of the phase curves and secondary eclipses of extrasolar planets provide a window on 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. 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 $\sim$1400~K. To this purpose, we analyze the secondary eclipse light curves collected by CHEOPS, together with TESS observations of the system and the publicly available photometry obtained with HST WFC3/UVIS. We also analyze 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 correct the optical eclipses for thermal emission and derive the optical $A_g$. The fit of the optical data leads to a marginal detection of the phase curve signal, characterized by an amplitude of $160\pm60$~ppm and 80$^{+60}_{-50}$~ppm in the CHEOPS and TESS passband respectively, with an eastward phase shift of $\sim50^\circ$ (1.5$\sigma$ detection). The analysis of the infrared data suggests a non-inverted thermal profile and solar-like metallicity. The combination of optical and infrared analysis allows us to derive an upper limit for the optical albedo of $A_g<0.087$ with a confidence of 99.9\%. 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.

Published
2022
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7. The EBLM project -- IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves

Author

Sebastian, D., Swayne, M. I., Maxted, P. F. L., Triaud, A. H. M. J., Sousa, S. G., Olofsson, G., Beck, M., Billot, N., Hoyer, S., Gill, S., Heidari, N., Martin, D. V., Persson, C. M., Standing, M. R., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Barrado, D., Barros, S. C. C., Battley, M. P., Baumjohann, W., Beck, T., Benz, W., Bergomi, M., Boisse, I., Bonfils, X., Brandeker, A., Broeg, C., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dransfield, G., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Hasiba, J., Hébrard, G., Heng, K., Isaak, K. G., Kiss, L. L., Kopp, E., Kunovac, V., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Magrin, D., McCormac, J., Miller, N. J., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Pepe, F. A., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Lalitha, S., Santerne, A., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Grootel, V., and Walton, N. A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Eclipsing binaries are important benchmark objects to test and calibrate stellar structure and evolution models. This is especially true for binaries with a fully convective M-dwarf component for which direct measurements of these stars' masses and radii are difficult using other techniques. Within the potential of M-dwarfs to be exoplanet host stars, the accuracy of theoretical predictions of their radius and effective temperature as a function of their mass is an active topic of discussion. Not only the parameters of transiting exoplanets but also the success of future atmospheric characterisation rely on accurate theoretical predictions. We present the analysis of five eclipsing binaries with low-mass stellar companions out of a sub-sample of 23, for which we obtained ultra high-precision light curves using the CHEOPS satellite. The observation of their primary and secondary eclipses are combined with spectroscopic measurements to precisely model the primary parameters and derive the M-dwarfs mass, radius, surface gravity, and effective temperature estimates using the PYCHEOPS data analysis software. Combining these results to the same set of parameters derived from TESS light curves, we find very good agreement (better than 1\% for radius and better than 0.2% for surface gravity). We also analyse the importance of precise orbits from radial velocity measurements and find them to be crucial to derive M-dwarf radii in a regime below 5% accuracy. These results add five valuable data points to the mass-radius diagram of fully-convective M-dwarfs., Comment: 19 pages, 12 figures, accepted for publication in MNRAS

Published
2022
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8. The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

Author

Deline, A., Hooton, M. J., Lendl, M., Morris, B., Salmon, S., Olofsson, G., Broeg, C., Ehrenreich, D., Beck, M., Brandeker, A., Hoyer, S., Sulis, S., Van Grootel, V., Bourrier, V., Demangeon, O., Demory, B. -O., Heng, K., Parviainen, H., Serrano, L. M., Singh, V., Bonfanti, A., Fossati, L., Kitzmann, D., Sousa, S. G., Wilson, T. G., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Bekkelien, A., Benz, W., Billot, N., Bonfils, X., Cabrera, J., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., de Roche, T., Erikson, A., Fortier, A., Fridlund, M., Futyan, D., Gandolfi, D., Gillon, M., Güdel, M., Gutermann, P., Hasiba, J., Isaak, K. G., Kiss, L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Munari, M., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Walter, I., and Walton, N.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Gas giants orbiting close to hot and massive early-type stars can reach dayside temperatures that are comparable to those of the coldest stars. These "ultra-hot Jupiters" have atmospheres made of ions and atomic species from molecular dissociation and feature strong day-to-night temperature gradients. Photometric observations at different orbital phases provide insights on the planet atmospheric properties. We analyse the photometric observations of WASP-189 acquired with the instrument CHEOPS to derive constraints on the system architecture and the planetary atmosphere. We implement a light curve model suited for asymmetric transit shape caused by the gravity-darkened photosphere of the fast-rotating host star. We also model the reflective and thermal components of the planetary flux, the effect of stellar oblateness and light-travel time on transit-eclipse timings, the stellar activity and CHEOPS systematics. From the asymmetric transit, we measure the size of the ultra-hot Jupiter WASP-189 b, $R_p=1.600^{+0.017}_{-0.016}\,R_J$, with a precision of 1%, and the true orbital obliquity of the planetary system $\Psi_p=89.6\pm1.2\deg$ (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth $\delta_\text{ecl}=96.5^{+4.5}_{-5.0}\,\text{ppm}$, from which we derive an upper limit on the geometric albedo: $A_g<0.48$. We also find that the eclipse depth can only be explained by thermal emission alone in the case of extremely inefficient energy redistribution. Finally, we attribute the photometric variability to the stellar rotation, either through superficial inhomogeneities or resonance couplings between the convective core and the radiative envelope., Comment: 25 pages, 16 figures, 5 tables (including the appendix); published in A&A

Published
2022
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9. CHEOPS observations of the HD 108236 planetary system: A fifth planet, improved ephemerides, and planetary radii

Author

Bonfanti, A., Delrez, L., Hooton, M. J., Wilson, T. G., Fossati, L., Alibert, Y., Hoyer, S., Mustill, A. J., Osborn, H. P., Adibekyan, V., Gandolfi, D., Salmon, S., Sousa, S. G., Tuson, A., Van Grootel, V., Cabrera, J., Nascimbeni, V., Maxted, P. F. L., Barros, S. C. C., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Fridlund, M., Lacedelli, G., Lendl, M., Persson, C., Santos, N. C., Scandariato, G., Szabó, Gy. M., Cameron, A. Collier, Udry, S., Benz, W., Beck, M., Ehrenreich, D., Fortier, A., Isaak, K. G., Queloz, D., Alonso, R., Asquier, J., Bandy, T., Bárczy, T., Barrado, D., Barragán, O., Baumjohann, W., Beck, T., Bekkelien, A., Bergomi, M., Busch, M-D., Brandeker, A., Cessa, V., Charnoz, S., Chazelas, B., Van Damme, C. Corral, Demory, B. -O., Erikson, A., Farinato, J., Futyan, D., Muñoz, A. Garcia, Gillon, M., Guedel, M., Guterman, P., Hasiba, J., Heng, K., Hernandez, E., Kiss, L., Kuntzer, T., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Salatti, M., Ségransan, D., Simon, A. E., Smith, A. M. S., Sordet, M., Steller, M., Thomas, N., Tschentscher, M., Van Eylen, V., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The detection of a super-Earth and three mini-Neptunes transiting the bright ($V$ = 9.2 mag) star HD 108236 (also known as TOI-1233) was recently reported on the basis of TESS and ground-based light curves. We perform a first characterisation of the HD 108236 planetary system through high-precision CHEOPS photometry and improve the transit ephemerides and system parameters. We characterise the host star through spectroscopic analysis and derive the radius with the infrared flux method. We constrain the stellar mass and age by combining the results obtained from two sets of stellar evolutionary tracks. We analyse the available TESS light curves and one CHEOPS transit light curve for each known planet in the system. We find that HD 108236 is a Sun-like star with $R_{\star}=0.877\pm0.008 R_{\odot}$, $M_{\star}=0.869^{+0.050}_{-0.048} M_{\odot}$, and an age of $6.7_{-5.1}^{+4.0}$ Gyr. We report the serendipitous detection of an additional planet, HD 108236 f, in one of the CHEOPS light curves. For this planet, the combined analysis of the TESS and CHEOPS light curves leads to a tentative orbital period of about 29.5 days. From the light curve analysis, we obtain radii of $1.615\pm0.051$, $2.071\pm0.052$, $2.539_{-0.065}^{+0.062}$, $3.083\pm0.052$, and $2.017_{-0.057}^{+0.052}$ $R_{\oplus}$ for planets HD 108236 b to HD 108236 f, respectively. These values are in agreement with previous TESS-based estimates, but with an improved precision of about a factor of two. We perform a stability analysis of the system, concluding that the planetary orbits most likely have eccentricities smaller than 0.1. We also employ a planetary atmospheric evolution framework to constrain the masses of the five planets, concluding that HD 108236 b and HD 108236 c should have an Earth-like density, while the outer planets should host a low mean molecular weight envelope., Comment: 20 pages, 14 figures, accepted for publication by A&A

Published
2021
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10. The hot dayside and asymmetric transit of WASP-189b seen by CHEOPS

Author

Lendl, M., Csizmadia, Sz., Deline, A., Fossati, L., Kitzmann, D., Heng, K., Hoyer, S., Salmon, S., Benz, W., Broeg, C., Ehrenreich, D., Fortier, A., Queloz, D., Bonfanti, A., Brandeker, A., Cameron, A. Collier, Delrez, L., Muñoz, A. Garcia, Hooton, M. J., Maxted, P. F. L., Morris, B. M., Van Grootel, V., Wilson, T. G., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T. Bandy T., Barrado, D., Barros, S. C. C, Baumjohann, W., Beck, M., Beck, T., Bekkelien, A., Bergomi, M., Billot, N., Biondi, F., Bonfils, X., Bourrier, V., Busch, M-D., Cabrera, J., Cessa, V., Charnoz, S., Chazelas, B., Van Damme, C. Corral, Davies, M. B., Deleuil, M., Demangeon, O. D. S, Demory, B. -O., Erikson, A., Farinato, J., Fridlund, M., Futyan, D., Gandolfi, D., Gillon, M., Guterman, P., Hasiba, J., Hernandez, E., Isaak, K. G., Kiss, L., Kuntzer, T., Etangs, A. Lecavelier des, Lüftinger, T., Laskar, J., Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Nascimbeni, V., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ratti, F., Rauer, H., Ragazzoni, R., Rando, N., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Singh, V., Smith, A. M. S., Sordet, M., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Tschentscher, M., Udry, S., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189b, a $M_P \approx 2 M_J$ planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of $dF = 87.9 \pm 4.3$ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of $3435 \pm 27$K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a $\sim25\%$ deeper transit compared to the discovery paper and updating the radius of WASP-189b to $1.619\pm0.021 R_J$. We further measured the projected orbital obliquity to be $\lambda = 86.4^{+2.9}_{-4.4}$deg, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of $\Psi = 85.4\pm4.3$deg. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the V=6.6 mag star, and using a one-hour binning, we obtain a residual RMS between 10 and 17ppm on the individual light curves, and 5.7ppm when combining the four visits., Comment: In press at Astronomy and Astrophysics

Published
2020
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11. The CHEOPS mission

Author

Benz, W., Broeg, C., Fortier, A., Rando, N., Beck, T., Beck, M., Queloz, D., Ehrenreich, D., Maxted, P. F. L., Isaak, K. G., Billot, N., Alibert, Y., Alonso, R., António, C., Asquier, J., Bandy, T., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Bekkelien, A., Bergomi, M., Biondi, F., Bonfils, X., Borsato, L., Brandeker, A., Busch, M.-D., Cabrera, J., Cessa, V., Charnoz, S., Chazelas, B., Collier Cameron, A., Corral Van Damme, C., Cortes, D., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O., Demory, B. O., Erikson, A., Farinato, J., Fossati, L., Fridlund, M., Futyan, D., Gandolfi, D., Garcia Munoz, A., Gillon, M., Guterman, P., Gutierrez, A., Hasiba, J., Heng, K., Hernandez, E., Hoyer, S., Kiss, L. L., Kovacs, Z., Kuntzer, T., Laskar, J., Lecavelier des Etangs, A., Lendl, M., López, A., Lora, I., Lovis, C., Lüftinger, T., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., de Miguel, D., Modrego, D., Munari, M., Nascimbeni, V., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Palacios, R., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pizarro, A., Pollaco, D., Ragazzoni, R., Ratti, F., Rauer, H., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Salatti, M., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sordet, M., Sousa, S. G., Steller, M., Szabó, G. M., Szoke, J., Thomas, N., Tschentscher, M., Udry, S., Van Grootel, V., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Published
2021
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12. Refining the properties of the TOI-178 system with CHEOPS and TESS

Author

Delrez, L., primary, Leleu, A., additional, Brandeker, A., additional, Gillon, M., additional, Hooton, M. J., additional, Collier Cameron, A., additional, Deline, A., additional, Fortier, A., additional, Queloz, D., additional, Bonfanti, A., additional, Van Grootel, V., additional, Wilson, T. G., additional, Egger, J. A., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Asquier, J., additional, Bárczy, T., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfıls, X., additional, Borsato, L., additional, Broeg, C., additional, Buder, M., additional, Cabrera, J., additional, Cessa, V., additional, Charnoz, S., additional, Csizmadia, Sz., additional, Cubillos, P. E., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Güdel, M., additional, Hasiba, J., additional, Hoyer, S., additional, Isaak, K. G., additional, Jenkins, J. M., additional, Kiss, L. L., additional, Laskar, J., additional, Latham, D. W., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lovis, C., additional, Luque, R., additional, Magrin, D., additional, Maxted, P. F. L., additional, Mordasini, C., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Ricker, G., additional, Santos, N. C., additional, Scandariato, G., additional, Seager, S., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Vanderspek, R., additional, Venturini, J., additional, Viotto, V., additional, Walton, N. A., additional, and Winn, J. N., additional

Published
2023
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13. TOI-5678b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS

Author

Ulmer-Moll, S., primary, Osborn, H. P., additional, Tuson, A., additional, Egger, J. A., additional, Lendl, M., additional, Maxted, P., additional, Bekkelien, A., additional, Simon, A. E., additional, Olofsson, G., additional, Adibekyan, V., additional, Alibert, Y., additional, Bonfanti, A., additional, Bouchy, F., additional, Brandeker, A., additional, Fridlund, M., additional, Gandolfi, D., additional, Mordasini, C., additional, Persson, C. M., additional, Salmon, S., additional, Serrano, L. M., additional, Sousa, S. G., additional, Wilson, T. G., additional, Rieder, M., additional, Hasiba, J., additional, Asquier, J., additional, Sicilia, D., additional, Walter, I., additional, Alonso, R., additional, Anglada, G., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Broeg, C., additional, Bárczy, T., additional, Cabrera, J., additional, Charnoz, S., additional, Cointepas, M., additional, Cameron, A. Collier, additional, Csizmadia, Sz., additional, Cubillos, P. E., additional, Davies, M. B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Dumusque, X., additional, Ehrenreich, D., additional, Eisner, N. L., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Gillon, M., additional, Grieves, N., additional, Güdel, M., additional, Hagelberg, J., additional, Helled, R., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Laskar, J., additional, des Etangs, A. Lecavelier, additional, Lovis, C., additional, Magrin, D., additional, Nascimbeni, V., additional, Otegi, J., additional, Ottensammer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Psaridi, A., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, G. M., additional, Ségransan, D., additional, Thomas, N., additional, Udry, S., additional, Van Grootel, V., additional, Venturini, J., additional, and Walton, N. A., additional

Published
2023
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14. TOI-5678b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS

Author

Ulmer-Moll, S; https://orcid.org/0000-0003-2417-7006, Osborn, H P; https://orcid.org/0000-0002-4047-4724, Tuson, A; https://orcid.org/0000-0002-2830-9064, Egger, J A; https://orcid.org/0000-0003-1628-4231, Lendl, M; https://orcid.org/0000-0001-9699-1459, Maxted, P; https://orcid.org/0000-0003-3794-1317, Bekkelien, A, Simon, A E; https://orcid.org/0000-0001-9773-2600, Olofsson, G; https://orcid.org/0000-0003-3747-7120, Adibekyan, V; https://orcid.org/0000-0002-0601-6199, Alibert, Y; https://orcid.org/0000-0002-4644-8818, Bonfanti, A; https://orcid.org/0000-0002-1916-5935, Bouchy, F, Brandeker, A; https://orcid.org/0000-0002-7201-7536, Fridlund, M; https://orcid.org/0000-0002-0855-8426, Gandolfi, D; https://orcid.org/0000-0001-8627-9628, Mordasini, C, Persson, C M; https://orcid.org/0000-0003-1257-5146, Salmon, S; https://orcid.org/0000-0002-1714-3513, Serrano, L M; https://orcid.org/0000-0001-9211-3691, Sousa, S G; https://orcid.org/0000-0001-9047-2965, Wilson, T G; https://orcid.org/0000-0001-8749-1962, Rieder, M, Hasiba, J, Asquier, J, Sicilia, D; https://orcid.org/0000-0001-7851-5168, Walter, I; https://orcid.org/0000-0002-5839-1521, Alonso, R; https://orcid.org/0000-0001-8462-8126, Anglada, G; https://orcid.org/0000-0002-3645-5977, Barrado y Navascues, D; https://orcid.org/0000-0002-5971-9242, et al, Ulmer-Moll, S; https://orcid.org/0000-0003-2417-7006, Osborn, H P; https://orcid.org/0000-0002-4047-4724, Tuson, A; https://orcid.org/0000-0002-2830-9064, Egger, J A; https://orcid.org/0000-0003-1628-4231, Lendl, M; https://orcid.org/0000-0001-9699-1459, Maxted, P; https://orcid.org/0000-0003-3794-1317, Bekkelien, A, Simon, A E; https://orcid.org/0000-0001-9773-2600, Olofsson, G; https://orcid.org/0000-0003-3747-7120, Adibekyan, V; https://orcid.org/0000-0002-0601-6199, Alibert, Y; https://orcid.org/0000-0002-4644-8818, Bonfanti, A; https://orcid.org/0000-0002-1916-5935, Bouchy, F, Brandeker, A; https://orcid.org/0000-0002-7201-7536, Fridlund, M; https://orcid.org/0000-0002-0855-8426, Gandolfi, D; https://orcid.org/0000-0001-8627-9628, Mordasini, C, Persson, C M; https://orcid.org/0000-0003-1257-5146, Salmon, S; https://orcid.org/0000-0002-1714-3513, Serrano, L M; https://orcid.org/0000-0001-9211-3691, Sousa, S G; https://orcid.org/0000-0001-9047-2965, Wilson, T G; https://orcid.org/0000-0001-8749-1962, Rieder, M, Hasiba, J, Asquier, J, Sicilia, D; https://orcid.org/0000-0001-7851-5168, Walter, I; https://orcid.org/0000-0002-5839-1521, Alonso, R; https://orcid.org/0000-0001-8462-8126, Anglada, G; https://orcid.org/0000-0002-3645-5977, Barrado y Navascues, D; https://orcid.org/0000-0002-5971-9242, and et al

Abstract

Context. A large sample of long-period giant planets has been discovered thanks to long-term radial velocity surveys, but only a few dozen of these planets have a precise radius measurement. Transiting gas giants are crucial targets for the study of atmospheric composition across a wide range of equilibrium temperatures and, more importantly, for shedding light on the formation and evolution of planetary systems. Indeed, compared to hot Jupiters, the atmospheric properties and orbital parameters of cooler gas giants are unaltered by intense stellar irradiation and tidal effects. Aims. We aim to identify long-period planets in the Transiting Exoplanet Survey Satellite (TESS) data as single or duo-transit events. Our goal is to solve the orbital periods of TESS duo-transit candidates with the use of additional space-based photometric observations and to collect follow-up spectroscopic observations in order to confirm the planetary nature and measure the mass of the candidates. Methods. We use the CHaracterising ExOPlanet Satellite (CHEOPS) to observe the highest-probability period aliases in order to discard or confirm a transit event at a given period. Once a period is confirmed, we jointly model the TESS and CHEOPS light curves along with the radial velocity datasets to measure the orbital parameters of the system and obtain precise mass and radius measurements. Results. We report the discovery of a long-period transiting Neptune-mass planet orbiting the G7-type star TOI-5678. Our spectroscopic analysis shows that TOI-5678 is a star with a solar metallicity. The TESS light curve of TOI-5678 presents two transit events separated by almost two years. In addition, CHEOPS observed the target as part of its Guaranteed Time Observation program. After four non-detections corresponding to possible periods, CHEOPS detected a transit event matching a unique period alias. Follow-up radial velocity observations were carried out with the ground-based high-resolution spectrograph

Published
2023

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

Author

Scandariato, G., primary, Singh, V., additional, Kitzmann, D., additional, Lendl, M., additional, Brandeker, A., additional, Bruno, G., additional, Bekkelien, A., additional, Benz, W., additional, Gutermann, P., additional, Maxted, P. F. L., additional, Bonfanti, A., additional, Charnoz, S., additional, Fridlund, M., additional, Heng, K., additional, Hoyer, S., additional, Pagano, I., additional, Persson, C. M., additional, Salmon, S., additional, Van Grootel, V., additional, Wilson, T. G., additional, Asquier, J., additional, Bergomi, M., additional, Gambicorti, L., additional, Hasiba, J., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Billot, N., additional, Bonfils, X., additional, Broeg, C., additional, Cabrera, J., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O., additional, Demory, B.-O., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Isaak, K. G., additional, Kiss, L. L., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lovis, C., additional, Magrin, D., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pallé, E., additional, Parviainen, H., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Santos, N. C., additional, Ségransan, D., additional, Serrano, L. M., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Ulmer, B., additional, and Walton, N., additional

Published
2022
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16. The Electron Drift Instrument for MMS

Author

Torbert, R. B., Vaith, H., Granoff, M., Widholm, M., Gaidos, J. A., Briggs, B. H., Dors, I. G., Chutter, M. W., Macri, J., Argall, M., Bodet, D., Needell, J., Steller, M. B., Baumjohann, W., Nakamura, R., Plaschke, F., Ottacher, H., Hasiba, J., Hofmann, K., Kletzing, C. A., Bounds, S. R., Dvorsky, R. T., Sigsbee, K., and Kooi, V.

Published
2016
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17. The EBLM project – IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves

Author

Sebastian, D, primary, Swayne, M I, additional, Maxted, P F L, additional, Triaud, A H M J, additional, Sousa, S G, additional, Olofsson, G, additional, Beck, M, additional, Billot, N, additional, Hoyer, S, additional, Gill, S, additional, Heidari, N, additional, Martin, D V, additional, Persson, C M, additional, Standing, M R, additional, Alibert, Y, additional, Alonso, R, additional, Anglada, G, additional, Asquier, J, additional, Bárczy, T, additional, Barrado, D, additional, Barros, S C C, additional, Battley, M P, additional, Baumjohann, W, additional, Beck, T, additional, Benz, W, additional, Bergomi, M, additional, Boisse, I, additional, Bonfils, X, additional, Brandeker, A, additional, Broeg, C, additional, Cabrera, J, additional, Charnoz, S, additional, Collier Cameron, A, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Delrez, L, additional, Demangeon, O D S, additional, Demory, B-O, additional, Dransfield, G, additional, Ehrenreich, D, additional, Erikson, A, additional, Fortier, A, additional, Fossati, L, additional, Fridlund, M, additional, Gandolfi, D, additional, Gillon, M, additional, Güdel, M, additional, Hasiba, J, additional, Hébrard, G, additional, Heng, K, additional, Isaak, K G, additional, Kiss, L L, additional, Kopp, E, additional, Kunovac, V, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, McCormac, J, additional, Miller, N J, additional, Nascimbeni, V, additional, Ottensamer, R, additional, Pagano, I, additional, Pallé, E, additional, Pepe, F A, additional, Peter, G, additional, Piotto, G, additional, Pollacco, D, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Ribas, I, additional, Lalitha, S, additional, Santerne, A, additional, Santos, N C, additional, Scandariato, G, additional, Ségransan, D, additional, Simon, A E, additional, Smith, A M S, additional, Steller, M, additional, Szabó, Gy M, additional, Thomas, N, additional, Udry, S, additional, Van Grootel, V, additional, and Walton, N A, additional

Published
2022
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18. The Electron Drift Instrument for MMS

Author

Torbert, R. B., primary, Vaith, H., additional, Granoff, M., additional, Widholm, M., additional, Gaidos, J. A., additional, Briggs, B. H., additional, Dors, I. G., additional, Chutter, M. W., additional, Macri, J., additional, Argall, M., additional, Bodet, D., additional, Needell, J., additional, Steller, M. B., additional, Baumjohann, W., additional, Nakamura, R., additional, Plaschke, F., additional, Ottacher, H., additional, Hasiba, J., additional, Hofmann, K., additional, Kletzing, C. A., additional, Bounds, S. R., additional, Dvorsky, R. T., additional, Sigsbee, K., additional, and Kooi, V., additional

Published
2016
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19. The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

Author

Deline, A., primary, Hooton, M. J., additional, Lendl, M., additional, Morris, B., additional, Salmon, S., additional, Olofsson, G., additional, Broeg, C., additional, Ehrenreich, D., additional, Beck, M., additional, Brandeker, A., additional, Hoyer, S., additional, Sulis, S., additional, Van Grootel, V., additional, Bourrier, V., additional, Demangeon, O., additional, Demory, B.-O., additional, Heng, K., additional, Parviainen, H., additional, Serrano, L. M., additional, Singh, V., additional, Bonfanti, A., additional, Fossati, L., additional, Kitzmann, D., additional, Sousa, S. G., additional, Wilson, T. G., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, T., additional, Bekkelien, A., additional, Benz, W., additional, Billot, N., additional, Bonfils, X., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Corral van Damme, C., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deleuil, M., additional, Delrez, L., additional, de Roche, T., additional, Erikson, A., additional, Fortier, A., additional, Fridlund, M., additional, Futyan, D., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Gutermann, P., additional, Hasiba, J., additional, Isaak, K. G., additional, Kiss, L., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lovis, C., additional, Magrin, D., additional, Maxted, P. F. L., additional, Munari, M., additional, Nascimbeni, V., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Walter, I., additional, and Walton, N., additional

Published
2022
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20. CHEOPS observations of the HD 108236 planetary system: A fifth planet, improved ephemerides, and planetary radii

Author

Bonfanti, A, Delrez, L, Hooton, MJ, Wilson, TG, Fossati, L, Alibert, Y, Hoyer, S, Mustill, AJ, Osborn, HP, Adibekyan, V, Gandolfi, D, Salmon, S, Sousa, SG, Tuson, A, Van Grootel, V, Cabrera, J, Nascimbeni, V, Maxted, PFL, Barros, SCC, Billot, N, Bonfils, X, Borsato, L, Broeg, C, Davies, MB, Deleuil, M, Demangeon, ODS, Fridlund, M, Lacedelli, G, Lendl, M, Persson, C, Santos, NC, Scandariato, G, Szabó, GM, Collier Cameron, A, Udry, S, Benz, W, Beck, M, Ehrenreich, D, Fortier, A, Isaak, KG, Queloz, D, Alonso, R, Asquier, J, Bandy, T, Bárczy, T, Barrado, D, Barragán, O, Baumjohann, W, Beck, T, Bekkelien, A, Bergomi, M, Brandeker, A, Busch, MD, Cessa, V, Charnoz, S, Chazelas, B, Corral Van Damme, C, Demory, BO, Erikson, A, Farinato, J, Futyan, D, Garcia Muñoz, A, Gillon, M, Guedel, M, Guterman, P, Hasiba, J, Heng, K, Hernandez, E, Kiss, L, Kuntzer, T, Laskar, J, Lecavelier Des Etangs, A, Lovis, C, Magrin, D, Malvasio, L, Marafatto, L, Michaelis, H, Munari, M, Olofsson, G, Ottacher, H, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Rieder, M, Rohlfs, R, Safa, F, Salatti, M, Ségransan, D, Simon, AE, Smith, AMS, Sordet, M, Hooton, Matthew John [0000-0003-0030-332X], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, stars: fundamental parameters, ephemerides, planets and satellites: fundamental parameters
Abstract

The detection of a super-Earth and three mini-Neptunes transiting the bright ($V$ = 9.2 mag) star HD 108236 (also known as TOI-1233) was recently reported on the basis of TESS and ground-based light curves. We perform a first characterisation of the HD 108236 planetary system through high-precision CHEOPS photometry and improve the transit ephemerides and system parameters. We characterise the host star through spectroscopic analysis and derive the radius with the infrared flux method. We constrain the stellar mass and age by combining the results obtained from two sets of stellar evolutionary tracks. We analyse the available TESS light curves and one CHEOPS transit light curve for each known planet in the system. We find that HD 108236 is a Sun-like star with $R_{\star}=0.877\pm0.008 R_{\odot}$, $M_{\star}=0.869^{+0.050}_{-0.048} M_{\odot}$, and an age of $6.7_{-5.1}^{+4.0}$ Gyr. We report the serendipitous detection of an additional planet, HD 108236 f, in one of the CHEOPS light curves. For this planet, the combined analysis of the TESS and CHEOPS light curves leads to a tentative orbital period of about 29.5 days. From the light curve analysis, we obtain radii of $1.615\pm0.051$, $2.071\pm0.052$, $2.539_{-0.065}^{+0.062}$, $3.083\pm0.052$, and $2.017_{-0.057}^{+0.052}$ $R_{\oplus}$ for planets HD 108236 b to HD 108236 f, respectively. These values are in agreement with previous TESS-based estimates, but with an improved precision of about a factor of two. We perform a stability analysis of the system, concluding that the planetary orbits most likely have eccentricities smaller than 0.1. We also employ a planetary atmospheric evolution framework to constrain the masses of the five planets, concluding that HD 108236 b and HD 108236 c should have an Earth-like density, while the outer planets should host a low mean molecular weight envelope.

Published
2021
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21. The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS

Author

Lendl, M, Csizmadia, S, Deline, A, Fossati, L, Kitzmann, D, Heng, K, Hoyer, S, Salmon, S, Benz, W, Broeg, C, Ehrenreich, D, Fortier, A, Queloz, D, Bonfanti, A, Brandeker, A, Collier Cameron, A, Delrez, L, Garcia Muñoz, A, Hooton, MJ, Maxted, PFL, Morris, BM, Van Grootel, V, Wilson, TG, Alibert, Y, Alonso, R, Asquier, J, Bandy, T, Bárczy, T, Barrado, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Bekkelien, A, Bergomi, M, Billot, N, Biondi, F, Bonfils, X, Bourrier, V, Busch, MD, Cabrera, J, Cessa, V, Charnoz, S, Chazelas, B, Corral Van Damme, C, Davies, MB, Deleuil, M, Demangeon, ODS, Demory, BO, Erikson, A, Farinato, J, Fridlund, M, Futyan, D, Gandolfi, D, Gillon, M, Guterman, P, Hasiba, J, Hernandez, E, Isaak, KG, Kiss, L, Kuntzer, T, Lecavelier Des Etangs, A, Lüftinger, T, Laskar, J, Lovis, C, Magrin, D, Malvasio, L, Marafatto, L, Michaelis, H, Munari, M, Nascimbeni, V, Olofsson, G, Ottacher, H, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Ratti, F, Rauer, H, Ragazzoni, R, Rando, N, Ribas, I, Rieder, M, Rohlfs, R, Safa, F, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Singh, V, Smith, AMS, Sordet, M, Sousa, SG, Steller, M, Szabó, GM, Thomas, N, Tschentscher, M, Queloz, Didier [0000-0002-3012-0316], Hooton, Matthew John [0000-0003-0030-332X], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: atmospheres, techniques: photometric, planets and satellites: individual: WASP-189 b
Abstract

The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189b, a $M_P \approx 2 M_J$ planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of $dF = 87.9 \pm 4.3$ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of $3435 \pm 27$K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a $\sim25\%$ deeper transit compared to the discovery paper and updating the radius of WASP-189b to $1.619\pm0.021 R_J$. We further measured the projected orbital obliquity to be $\lambda = 86.4^{+2.9}_{-4.4}$deg, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of $\Psi = 85.4\pm4.3$deg. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the V=6.6 mag star, and using a one-hour binning, we obtain a residual RMS between 10 and 17ppm on the individual light curves, and 5.7ppm when combining the four visits.

Published
2021
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22. The CHEOPS mission

Author

Benz, W, Broeg, C, Fortier, A, Rando, N, Beck, T, Beck, M, Queloz, D, Ehrenreich, D, Maxted, PFL, Isaak, KG, Billot, N, Alibert, Y, Alonso, R, António, C, Asquier, J, Bandy, T, Bárczy, T, Barrado, D, Barros, SCC, Baumjohann, W, Bekkelien, A, Bergomi, M, Biondi, F, Bonfils, X, Borsato, L, Brandeker, A, Busch, MD, Cabrera, J, Cessa, V, Charnoz, S, Chazelas, B, Collier Cameron, A, Corral Van Damme, C, Cortes, D, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, O, Demory, BO, Erikson, A, Farinato, J, Fossati, L, Fridlund, M, Futyan, D, Gandolfi, D, Garcia Munoz, A, Gillon, M, Guterman, P, Gutierrez, A, Hasiba, J, Heng, K, Hernandez, E, Hoyer, S, Kiss, LL, Kovacs, Z, Kuntzer, T, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, López, A, Lora, I, Lovis, C, Lüftinger, T, Magrin, D, Malvasio, L, Marafatto, L, Michaelis, H, De Miguel, D, Modrego, D, Munari, M, Nascimbeni, V, Olofsson, G, Ottacher, H, Ottensamer, R, Pagano, I, Palacios, R, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pizarro, A, Pollaco, D, Ragazzoni, R, Ratti, F, Rauer, H, Ribas, I, Rieder, M, Rohlfs, R, Safa, F, Salatti, M, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Sordet, M, Sousa, SG, Steller, M, Szabó, GM, Benz, W [0000-0001-7896-6479], and Apollo - University of Cambridge Repository

Subjects
High-precision transit photometry, Exoplanets, Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, CHEOPS, Small mission, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The CHaracterising ExOPlanet Satellite (CHEOPS) was selected in 2012, as the first small mission in the ESA Science Programme and successfully launched in December 2019. CHEOPS is a partnership between ESA and Switzerland with important contributions by ten additional ESA Member States. CHEOPS is the first mission dedicated to search for transits of exoplanets using ultrahigh precision photometry on bright stars already known to host planets. As a follow-up mission, CHEOPS is mainly dedicated to improving, whenever possible, existing radii measurements or provide first accurate measurements for a subset of those planets for which the mass has already been estimated from ground-based spectroscopic surveys and to following phase curves. CHEOPS will provide prime targets for future spectroscopic atmospheric characterisation. Requirements on the photometric precision and stability have been derived for stars with magnitudes ranging from 6 to 12 in the V band. In particular, CHEOPS shall be able to detect Earth-size planets transiting G5 dwarf stars in the magnitude range between 6 and 9 by achieving a photometric precision of 20 ppm in 6 hours of integration. For K stars in the magnitude range between 9 and 12, CHEOPS shall be able to detect transiting Neptune-size planets achieving a photometric precision of 85 ppm in 3 hours of integration. This is achieved by using a single, frame-transfer, back-illuminated CCD detector at the focal plane assembly of a 33.5 cm diameter telescope. The 280 kg spacecraft has a pointing accuracy of about 1 arcsec rms and orbits on a sun-synchronous dusk-dawn orbit at 700 km altitude. The nominal mission lifetime is 3.5 years. During this period, 20% of the observing time is available to the community through a yearly call and a discretionary time programme managed by ESA.

Published
2021
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23. Exoplanet discoveries with the CoRoT space observatory

Author

Lammer, H., Dvorak, R., Deleuil, M., Barge, P., Deeg, H. J., Moutou, C., Erikson, A., Csizmadia, Sz., Tingley, B., Bruntt, H., Havel, M., Aigrain, S., Almenara, J. M., Alonso, R., Auvergne, M., Baglin, A., Barbieri, M., Benz, W., Bonomo, A. S., Bordé, P., Bouchy, F., Cabrera, J., Carone, L., Carpano, S., Ciardi, D., Ferraz-Mello, S., Fridlund, M., Gandolfi, D., Gazzano, J. -C., Gillon, M., Gondoin, P., Guenther, E., Guillot, T., den Hartog, R., Hasiba, J., Hatzes, A., Hidas, M., Hébrard, G., Jorda, L., Kabath, P., Léger, A., Lister, T., Llebaria, A., Lovis, C., Mayor, M., Mazeh, T., Mura, A., Ollivier, M., Ottacher, H., Pätzold, M., Pepe, F., Pont, F., Queloz, D., Rabus, M., Rauer, H., Rouan, D., Samuel, B., Schneider, J., Shporer, A., Stecklum, B., Steller, M., Street, R., Udry, S., Weingrill, J., and Wuchterl, G.

Published
2010
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24. enCHEOPS observations of the HD 108236 planetary system: a fifth planet, improved ephemerides, and planetary radii

Author

Bonfanti, A., Delrez, L., Hooton, M. J., Wilson, T. G., Fossati, L., Alibert, Y., Hoyer, S., Mustill, A. J., Osborn, H. P., Adibekyan, V., Gandolfi, D., Salmon, S., Sousa, S. G., Tuson, A., Van Grootel, V., Cabrera, J., Nascimbeni, V., Maxted, P. F. L., Barros, S. C. C., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Fridlund, M., Lacedelli, G., Lendl, M., Persson, C., Santos, N. C., Scandariato, G., Szabó, Gy. M., Collier Cameron, A., Udry, S., Benz, W., Beck, M., Ehrenreich, D., Fortier, A., Isaak, K. G., Queloz, D., Alonso, R., Asquier, J., Bandy, T., Bárczy, T., Barrado, D., Barragán, O., Baumjohann, W., Beck, T., Bekkelien, A., Bergomi, M., Brandeker, A., Busch, M.-D., Cessa, V., Charnoz, S., Chazelas, B., Corral Van Damme, C., Demory, B.-O., Erikson, A., Farinato, J., Futyan, D., Garcia Muñoz, A., Gillon, M., Guedel, M., Guterman, P., Hasiba, J., Heng, K., Hernandez, E., Kiss, L., Kuntzer, T., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Salatti, M., Ségransan, D., Simon, A. E., Smith, A. M. S., Sordet, M., Steller, M., Thomas, N., Tschentscher, M., Van Eylen, V., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Subjects
530 Physics, 520 Astronomy, 620 Engineering
Abstract

Context. The detection of a super-Earth and three mini-Neptunes transiting the bright (V = 9.2 mag) star HD 108236 (also known as TOI-1233) was recently reported on the basis of TESS and ground-based light curves. Aims. We perform a first characterisation of the HD 108236 planetary system through high-precision CHEOPS photometry and improve the transit ephemerides and system parameters. Methods. We characterise the host star through spectroscopic analysis and derive the radius with the infrared flux method. We constrain the stellar mass and age by combining the results obtained from two sets of stellar evolutionary tracks. We analyse the available TESS light curves and one CHEOPS transit light curve for each known planet in the system. Results. We find that HD 108236 is a Sun-like star with R⋆ = 0.877 ± 0.008 R⊙, M⋆ = 0.869−0.048+0.050 M⊙, and an age of 6.7−5.1+4.0 Gyr. We report the serendipitous detection of an additional planet, HD 108236 f, in one of the CHEOPS light curves. For this planet, the combined analysis of the TESS and CHEOPS light curves leads to a tentative orbital period of about 29.5 days. From the light curve analysis, we obtain radii of 1.615 ± 0.051, 2.071 ± 0.052, 2.539−0.065+0.062, 3.083 ± 0.052, and 2.017−0.057+0.052 R⊕ for planets HD 108236 b to HD 108236 f, respectively. These values are in agreement with previous TESS-based estimates, but with an improved precision of about a factor of two. We perform a stability analysis of the system, concluding that the planetary orbits most likely have eccentricities smaller than 0.1. We also employ a planetary atmospheric evolution framework to constrain the masses of the five planets, concluding that HD 108236 b and HD 108236 c should have an Earth-like density, while the outer planets should host a low mean molecular weight envelope. Conclusions. The detection of the fifth planet makes HD 108236 the third system brighter than V = 10 mag to host more than four transiting planets. The longer time span enables us to significantly improve the orbital ephemerides such that the uncertainty on the transit times will be of the order of minutes for the years to come. A comparison of the results obtained from the TESS and CHEOPS light curves indicates that for a V ~ 9 mag solar-like star and a transit signal of ~500 ppm, one CHEOPS transit light curve ensures the same level of photometric precision as eight TESS transits combined, although this conclusion depends on the length and position of the gaps in the light curve.

Published
2021
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25. Exploiting timing capabilities of the CHEOPS mission with warm-Jupiter planets

Author

Borsato, L, primary, Piotto, G, additional, Gandolfi, D, additional, Nascimbeni, V, additional, Lacedelli, G, additional, Marzari, F, additional, Billot, N, additional, Maxted, P F L, additional, Sousa, S, additional, Cameron, A C, additional, Bonfanti, A, additional, Wilson, T G, additional, Serrano, L M, additional, Garai, Z, additional, Alibert, Y, additional, Alonso, R, additional, Asquier, J, additional, Bárczy, T, additional, Bandy, T, additional, Barrado, D, additional, Barros, S C C, additional, Baumjohann, W, additional, Beck, M, additional, Beck, T, additional, Benz, W, additional, Bonfils, X, additional, Brandeker, A, additional, Broeg, C, additional, Cabrera, J, additional, Charnoz, S, additional, Csizmadia, S, additional, Davies, M B, additional, Deleuil, M, additional, Delrez, L, additional, Demangeon, O, additional, Demory, B-O, additional, des Etangs, A L, additional, Ehrenreich, D, additional, Erikson, A, additional, Escudé, G A, additional, Fortier, A, additional, Fossati, L, additional, Fridlund, M, additional, Gillon, M, additional, Guedel, M, additional, Hasiba, J, additional, Heng, K, additional, Hoyer, S, additional, Isaak, K G, additional, Kiss, L, additional, Kopp, E, additional, Laskar, J, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, Munari, M, additional, Olofsson, G, additional, Ottensamer, R, additional, Pagano, I, additional, Pallé, E, additional, Peter, G, additional, Pollacco, D, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Ribas, I, additional, Ségransan, D, additional, Santos, N C, additional, Scandariato, G, additional, Simon, A, additional, Smith, A M S, additional, Steller, M, additional, Szabó, G, additional, Thomas, N, additional, Udry, S, additional, Van Grootel, V, additional, and Walton, N, additional

Published
2021
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26. Exploiting timing capabilities of the CHEOPS mission with warm-Jupiter planets

Author

Borsato, L., Piotto, G., Gandolfi, D., Nascimbeni, V, Lacedelli, G., Marzari, F., Billot, N., Maxted, P. F. L., Sousa, S., Cameron, A. C., Bonfanti, A., Wilson, T. G., Serrano, L. M., Garai, Z., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T., Bandy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Bonfils, X., Brandeker, Alexis, Broeg, C., Cabrera, J., Charnoz, S., Csizmadia, S., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O., Demory, B-O, des Etangs, A. L., Ehrenreich, D., Erikson, A., Escudé, G. A., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Guedel, M., Hasiba, J., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L., Kopp, E., Laskar, J., Lendl, M., Lovis, C., Magrin, D., Munari, M., Olofsson, Göran, Ottensamer, R., Pagano, I, Pallé, E., Peter, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I, Ségransan, D., Santos, N. C., Scandariato, G., Simon, A., Smith, A. M. S., Steller, M., Szabó, G., Thomas, N., Udry, S., Van Grootel, V., Walton, N., Borsato, L., Piotto, G., Gandolfi, D., Nascimbeni, V, Lacedelli, G., Marzari, F., Billot, N., Maxted, P. F. L., Sousa, S., Cameron, A. C., Bonfanti, A., Wilson, T. G., Serrano, L. M., Garai, Z., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T., Bandy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Bonfils, X., Brandeker, Alexis, Broeg, C., Cabrera, J., Charnoz, S., Csizmadia, S., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O., Demory, B-O, des Etangs, A. L., Ehrenreich, D., Erikson, A., Escudé, G. A., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Guedel, M., Hasiba, J., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L., Kopp, E., Laskar, J., Lendl, M., Lovis, C., Magrin, D., Munari, M., Olofsson, Göran, Ottensamer, R., Pagano, I, Pallé, E., Peter, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I, Ségransan, D., Santos, N. C., Scandariato, G., Simon, A., Smith, A. M. S., Steller, M., Szabó, G., Thomas, N., Udry, S., Van Grootel, V., and Walton, N.

Abstract

We present 17 transit light curves of seven known warm-Jupiters observed with the CHaracterising ExOPlanet Satellite (CHEOPS). The light curves have been collected as part of the CHEOPS Guaranteed Time Observation (GTO) program that searches for transit-timing variation (TTV) of warm-Jupiters induced by a possible external perturber to shed light on the evolution path of such planetary systems. We describe the CHEOPS observation process, from the planning to the data analysis. In this work, we focused on the timing performance of CHEOPS, the impact of the sampling of the transit phases, and the improvement we can obtain by combining multiple transits together. We reached the highest precision on the transit time of about 13–16 s for the brightest target (WASP-38, G = 9.2) in our sample. From the combined analysis of multiple transits of fainter targets with G ≥ 11, we obtained a timing precision of ∼2 min. Additional observations with CHEOPS, covering a longer temporal baseline, will further improve the precision on the transit times and will allow us to detect possible TTV signals induced by an external perturber.

Published
2021
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27. Erratum to: The Electron Drift Instrument for MMS

Author

Torbert, R. B., Vaith, H., Granoff, M., Widholm, M., Gaidos, J. A., Briggs, B. H., Dors, I. G., Chutter, M. W., Macri, J., Argall, M., Bodet, D., Needell, J., Steller, M. B., Baumjohann, W., Nakamura, R., Plaschke, F., Ottacher, H., Hasiba, J., Hofmann, K., Kletzing, C. A., Bounds, S. R., Dvorsky, R. T., Sigsbee, K., and Kooi, V.

Published
2016
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28. CHEOPS observations of the HD 108236 planetary system: a fifth planet, improved ephemerides, and planetary radii

Author

Bonfanti, A., primary, Delrez, L., additional, Hooton, M. J., additional, Wilson, T. G., additional, Fossati, L., additional, Alibert, Y., additional, Hoyer, S., additional, Mustill, A. J., additional, Osborn, H. P., additional, Adibekyan, V., additional, Gandolfi, D., additional, Salmon, S., additional, Sousa, S. G., additional, Tuson, A., additional, Van Grootel, V., additional, Cabrera, J., additional, Nascimbeni, V., additional, Maxted, P. F. L., additional, Barros, S. C. C., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Broeg, C., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Fridlund, M., additional, Lacedelli, G., additional, Lendl, M., additional, Persson, C., additional, Santos, N. C., additional, Scandariato, G., additional, Szabó, Gy. M., additional, Collier Cameron, A., additional, Udry, S., additional, Benz, W., additional, Beck, M., additional, Ehrenreich, D., additional, Fortier, A., additional, Isaak, K. G., additional, Queloz, D., additional, Alonso, R., additional, Asquier, J., additional, Bandy, T., additional, Bárczy, T., additional, Barrado, D., additional, Barragán, O., additional, Baumjohann, W., additional, Beck, T., additional, Bekkelien, A., additional, Bergomi, M., additional, Brandeker, A., additional, Busch, M.-D., additional, Cessa, V., additional, Charnoz, S., additional, Chazelas, B., additional, Corral Van Damme, C., additional, Demory, B.-O., additional, Erikson, A., additional, Farinato, J., additional, Futyan, D., additional, Garcia Muñoz, A., additional, Gillon, M., additional, Guedel, M., additional, Guterman, P., additional, Hasiba, J., additional, Heng, K., additional, Hernandez, E., additional, Kiss, L., additional, Kuntzer, T., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lovis, C., additional, Magrin, D., additional, Malvasio, L., additional, Marafatto, L., additional, Michaelis, H., additional, Munari, M., additional, Olofsson, G., additional, Ottacher, H., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piazza, D., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Ribas, I., additional, Rieder, M., additional, Rohlfs, R., additional, Safa, F., additional, Salatti, M., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sordet, M., additional, Steller, M., additional, Thomas, N., additional, Tschentscher, M., additional, Van Eylen, V., additional, Viotto, V., additional, Walter, I., additional, Walton, N. A., additional, Wildi, F., additional, and Wolter, D., additional

Published
2021
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29. The CHEOPS mission

Author

Benz, W., primary, Broeg, C., additional, Fortier, A., additional, Rando, N., additional, Beck, T., additional, Beck, M., additional, Queloz, D., additional, Ehrenreich, D., additional, Maxted, P. F. L., additional, Isaak, K. G., additional, Billot, N., additional, Alibert, Y., additional, Alonso, R., additional, António, C., additional, Asquier, J., additional, Bandy, T., additional, Bárczy, T., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Bekkelien, A., additional, Bergomi, M., additional, Biondi, F., additional, Bonfils, X., additional, Borsato, L., additional, Brandeker, A., additional, Busch, M.-D., additional, Cabrera, J., additional, Cessa, V., additional, Charnoz, S., additional, Chazelas, B., additional, Collier Cameron, A., additional, Corral Van Damme, C., additional, Cortes, D., additional, Davies, M. B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O., additional, Demory, B. O., additional, Erikson, A., additional, Farinato, J., additional, Fossati, L., additional, Fridlund, M., additional, Futyan, D., additional, Gandolfi, D., additional, Garcia Munoz, A., additional, Gillon, M., additional, Guterman, P., additional, Gutierrez, A., additional, Hasiba, J., additional, Heng, K., additional, Hernandez, E., additional, Hoyer, S., additional, Kiss, L. L., additional, Kovacs, Z., additional, Kuntzer, T., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, López, A., additional, Lora, I., additional, Lovis, C., additional, Lüftinger, T., additional, Magrin, D., additional, Malvasio, L., additional, Marafatto, L., additional, Michaelis, H., additional, de Miguel, D., additional, Modrego, D., additional, Munari, M., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottacher, H., additional, Ottensamer, R., additional, Pagano, I., additional, Palacios, R., additional, Pallé, E., additional, Peter, G., additional, Piazza, D., additional, Piotto, G., additional, Pizarro, A., additional, Pollaco, D., additional, Ragazzoni, R., additional, Ratti, F., additional, Rauer, H., additional, Ribas, I., additional, Rieder, M., additional, Rohlfs, R., additional, Safa, F., additional, Salatti, M., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sordet, M., additional, Sousa, S. G., additional, Steller, M., additional, Szabó, G. M., additional, Szoke, J., additional, Thomas, N., additional, Tschentscher, M., additional, Udry, S., additional, Van Grootel, V., additional, Viotto, V., additional, Walter, I., additional, Walton, N. A., additional, Wildi, F., additional, and Wolter, D., additional

Published
2020
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30. The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS

Author

Lendl, M., primary, Csizmadia, Sz., additional, Deline, A., additional, Fossati, L., additional, Kitzmann, D., additional, Heng, K., additional, Hoyer, S., additional, Salmon, S., additional, Benz, W., additional, Broeg, C., additional, Ehrenreich, D., additional, Fortier, A., additional, Queloz, D., additional, Bonfanti, A., additional, Brandeker, A., additional, Collier Cameron, A., additional, Delrez, L., additional, Garcia Muñoz, A., additional, Hooton, M. J., additional, Maxted, P. F. L., additional, Morris, B. M., additional, Van Grootel, V., additional, Wilson, T. G., additional, Alibert, Y., additional, Alonso, R., additional, Asquier, J., additional, Bandy, T., additional, Bárczy, T., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Bekkelien, A., additional, Bergomi, M., additional, Billot, N., additional, Biondi, F., additional, Bonfils, X., additional, Bourrier, V., additional, Busch, M.-D., additional, Cabrera, J., additional, Cessa, V., additional, Charnoz, S., additional, Chazelas, B., additional, Corral Van Damme, C., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Erikson, A., additional, Farinato, J., additional, Fridlund, M., additional, Futyan, D., additional, Gandolfi, D., additional, Gillon, M., additional, Guterman, P., additional, Hasiba, J., additional, Hernandez, E., additional, Isaak, K. G., additional, Kiss, L., additional, Kuntzer, T., additional, Lecavelier des Etangs, A., additional, Lüftinger, T., additional, Laskar, J., additional, Lovis, C., additional, Magrin, D., additional, Malvasio, L., additional, Marafatto, L., additional, Michaelis, H., additional, Munari, M., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottacher, H., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piazza, D., additional, Piotto, G., additional, Pollacco, D., additional, Ratti, F., additional, Rauer, H., additional, Ragazzoni, R., additional, Rando, N., additional, Ribas, I., additional, Rieder, M., additional, Rohlfs, R., additional, Safa, F., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Simon, A. E., additional, Singh, V., additional, Smith, A. M. S., additional, Sordet, M., additional, Sousa, S. G., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Tschentscher, M., additional, Udry, S., additional, Viotto, V., additional, Walter, I., additional, Walton, N. A., additional, Wildi, F., additional, and Wolter, D., additional

Published
2020
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31. Erratum to: “Exoplanet discoveries with the CoRoT space observatory”

Author

Lammer, H., Dvorak, R., Deleuil, M., Barge, P., Deeg, H. J., Moutou, C., Erikson, A., Csizmadia, Sz., Tingley, B., Bruntt, H., Havel, M., Aigrain, S., Almenara, J. M., Alonso, R., Auvergne, M., Baglin, A., Barbieri, M., Benz, W., Bonomo, A. S., Bordé, P., Bouchy, F., Cabrera, J., Carone, L., Carpano, S., Ciardi, D., Ferraz-Mello, S., Fridlund, M., Gandolfi, D., Gazzano, J. -C., Gillon, M., Gondoin, P., Guenther, E., Guillot, T., den Hartog, R., Hasiba, J., Hatzes, A., Hidas, M., Hébrard, G., Jorda, L., Kabath, P., Léger, A., Lister, T., Llebaria, A., Lovis, C., Mayor, M., Mazeh, T., Mura, A., Ollivier, M., Ottacher, H., Pätzold, M., Pepe, F., Pont, F., Queloz, D., Rabus, M., Rauer, H., Rouan, D., Samuel, B., Schneider, J., Shporer, A., Stecklum, B., Steller, M., Street, R., Udry, S., Weingrill, J., and Wuchterl, G.

Published
2011
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32. The Electron Drift Instrument for MMS

Author

Torbert, R. B., primary, Vaith, H., additional, Granoff, M., additional, Widholm, M., additional, Gaidos, J. A., additional, Briggs, B. H., additional, Dors, I. G., additional, Chutter, M. W., additional, Macri, J., additional, Argall, M., additional, Bodet, D., additional, Needell, J., additional, Steller, M. B., additional, Baumjohann, W., additional, Nakamura, R., additional, Plaschke, F., additional, Ottacher, H., additional, Hasiba, J., additional, Hofmann, K., additional, Kletzing, C. A., additional, Bounds, S. R., additional, Dvorsky, R. T., additional, Sigsbee, K., additional, and Kooi, V., additional

Published
2015
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33. Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first super-Earth with measured radius

Author

Leger, A., Rouan, D., Jodi Schneider, Barge, P., Fridlund, M., Samuel, B., Ollivier, M., Guenther, E., Deleuil, M., Deeg Hj, Auvergne, M., Alonso, R., Aigrain, S., Alapini, A., Almenara Jm, Baglin, A., Barbieri, M., Bruntt, H., Pascal Bordé, Bouchy, F., Cabrera, J., Catala, C., Carone, L., Carpano, S., Csizmadia, S., Dvorak, R., Erikson, A., Ferraz-Mello, S., Foing, B., Grasset, O., Fressin, F., Gandolfi, D., Gillon, M., Gondoin, P., Guillot, T., Hatzes, A., Hebrard, G., Jorda, L., Lammer, H., Llebaria, A., Loeillet, B., Mayor, M., Mazeh, T., Moutou, C., Patzold, M., Pont, F., Queloz, D., Rauer, H., Renner, S., Samadi, R., Shporer, A., Sotin, C., Tingley, B., Wuchterl, G., Adda, M., Agogu, P., Appourchaux, T., Ballans, H., Baron, P., Beaufort, T., Bellenger, R., Berlin, R., Bernardi, P., Blouin, D., Baudin, F., Bodin, P., Boisnard, L., Boit, L., Bonneau, F., Borzeix, S., Briet, R., Buey Jt, Butler, B., Cailleau, D., Cautain, R., Chabaud Py, Chaintreuil, S., Chiavassa, F., Costes V, Parrho Vc, Fialho Fd, Decaudin, M., Defise Jm, Djalal, S., Epstein, G., Exil Ge, Faure, C., Fenouillet, T., Gaboriaud, A., Gallic, A., Gamet, P., Gavalda, P., Grolleau, E., Gruneisen, R., Gueguen, L., Guis, V., V. Guivarc'H, Guterman, P., Hallouard, D., Hasiba, J., Heuripeau, F., Huntzinger, G., Hustaix, H., Imad, C., Imbert, C., Johlander, B., Jouret, M., Journoud, P., Karioty, F., Kerjean, L., Lafaille, V., Lafond, L., Lam-Trong, T., Landiech, P., Lapeyrere, V., Larque, T., Laudet, P., Lautier, N., Lecann, H., Lefevre, L., Leruyet, B., Levacher, P., Magnan, A., Mazy, E., Mertens, F., Mesnager Jm, Meunier Jc, Michel Jp, Monjoin, W., Naudet, D., Nguyen-Kim, K., Orcesi Jl, Ottacher, H., Perez, R., Peter, G., Plasson, P., Plesseria Jy, Pontet, B., Pradines, A., Céline Quentin, Reynaud Jl, Rolland, G., Rollenhagen, F., Romagnan, R., Russ, N., Schmidt, R., Schwartz, N., Sebbag, I., Sedes, G., Smit, H., Steller Mb, Sunter, W., Surace, C., Tello, M., Tiphene, D., Toulouse, P., Ulmer, B., Vandermarcq, O., Vergnault, E., Vuillemin, A., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA)

Subjects
[SDU.STU]Sciences of the Universe [physics]/Earth Sciences, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

34. Determining the mass loss limit for close-in exoplanets: what can we learn from transit observations?

Author

Lammer, H., primary, Odert, P., additional, Leitzinger, M., additional, Khodachenko, M. L., additional, Panchenko, M., additional, Kulikov, Yu. N., additional, Zhang, T. L., additional, Lichtenegger, H. I. M., additional, Erkaev, N. V., additional, Wuchterl, G., additional, Micela, G., additional, Penz, T., additional, Biernat, H. K., additional, Weingrill, J., additional, Steller, M., additional, Ottacher, H., additional, Hasiba, J., additional, and Hanslmeier, A., additional

Published
2009
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35. The CoRoT satellite in flight: description and performance

Author

Auvergne, M., primary, Bodin, P., additional, Boisnard, L., additional, Buey, J.-T., additional, Chaintreuil, S., additional, Epstein, G., additional, Jouret, M., additional, Lam-Trong, T., additional, Levacher, P., additional, Magnan, A., additional, Perez, R., additional, Plasson, P., additional, Plesseria, J., additional, Peter, G., additional, Steller, M., additional, Tiphène, D., additional, Baglin, A., additional, Agogué, P., additional, Appourchaux, T., additional, Barbet, D., additional, Beaufort, T., additional, Bellenger, R., additional, Berlin, R., additional, Bernardi, P., additional, Blouin, D., additional, Boumier, P., additional, Bonneau, F., additional, Briet, R., additional, Butler, B., additional, Cautain, R., additional, Chiavassa, F., additional, Costes, V., additional, Cuvilho, J., additional, Cunha-Parro, V., additional, De Oliveira Fialho, F., additional, Decaudin, M., additional, Defise, J.-M., additional, Djalal, S., additional, Docclo, A., additional, Drummond, R., additional, Dupuis, O., additional, Exil, G., additional, Fauré, C., additional, Gaboriaud, A., additional, Gamet, P., additional, Gavalda, P., additional, Grolleau, E., additional, Gueguen, L., additional, Guivarc'h, V., additional, Guterman, P., additional, Hasiba, J., additional, Huntzinger, G., additional, Hustaix, H., additional, Imbert, C., additional, Jeanville, G., additional, Johlander, B., additional, Jorda, L., additional, Journoud, P., additional, Karioty, F., additional, Kerjean, L., additional, Lafond, L., additional, Lapeyrere, V., additional, Landiech, P., additional, Larqué, T., additional, Laudet, P., additional, Le Merrer, J., additional, Leporati, L., additional, Leruyet, B., additional, Levieuge, B., additional, Llebaria, A., additional, Martin, L., additional, Mazy, E., additional, Mesnager, J.-M., additional, Michel, J.-P., additional, Moalic, J.-P., additional, Monjoin, W., additional, Naudet, D., additional, Neukirchner, S., additional, Nguyen-Kim, K., additional, Ollivier, M., additional, Orcesi, J.-L., additional, Ottacher, H., additional, Oulali, A., additional, Parisot, J., additional, Perruchot, S., additional, Piacentino, A., additional, Pinheiro da Silva, L., additional, Platzer, J., additional, Pontet, B., additional, Pradines, A., additional, Quentin, C., additional, Rohbeck, U., additional, Rolland, G., additional, Rollenhagen, F., additional, Romagnan, R., additional, Russ, N., additional, Samadi, R., additional, Schmidt, R., additional, Schwartz, N., additional, Sebbag, I., additional, Smit, H., additional, Sunter, W., additional, Tello, M., additional, Toulouse, P., additional, Ulmer, B., additional, Vandermarcq, O., additional, Vergnault, E., additional, Wallner, R., additional, Waultier, G., additional, and Zanatta, P., additional

Published
2009
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36. The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS

Author

Lendl, M., Csizmadia, Sz., Deline, A., Fossati, L., Kitzmann, D., Heng, K., Hoyer, S., Salmon, S., Benz, W., Broeg, C., Ehrenreich, D., Fortier, A., Queloz, D., Bonfanti, A., Brandeker, A., Collier Cameron, A., Delrez, L., Garcia Muñoz, A., Hooton, M. J., Maxted, P. F. L., Morris, B. M., Van Grootel, V., Wilson, T. G., Alibert, Y., Alonso, R., Asquier, J., Bandy, T., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Bekkelien, A., Bergomi, M., Billot, N., Biondi, F., Bonfils, X., Bourrier, V., Busch, M.-D., Cabrera, J., Cessa, V., Charnoz, S., Chazelas, B., Corral Van Damme, C., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B.-O., Erikson, A., Farinato, J., Fridlund, M., Futyan, D., Gandolfi, D., Gillon, M., Guterman, P., Hasiba, J., Hernández, E., Isaak, K. G., Kiss, L., Kuntzer, T., Lecavelier des Etangs, A., Lüftinger, T., Laskar, J., Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Nascimbeni, V., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ratti, F., Rauer, H., Ragazzoni, R., Rando, N., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Singh, V., Smith, A. M. S., Sordet, M., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Tschentscher, M., Udry, S., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Subjects
13. Climate action, 530 Physics, 520 Astronomy, 500 Science, 620 Engineering, 7. Clean energy
Abstract

The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189 b, a MP ≈ 2MJ planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of dF = 87.9 ± 4.3 ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of 3435 ± 27 K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189 b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a ~25% deeper transit compared to the discovery paper and updating the radius of WASP-189 b to 1.619 ± 0.021RJ. We further measured the projected orbital obliquity to be λ = 86.4−4.4+2.9°, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of Ψ = 85.4 ± 4.3°. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the V = 6.6 mag star, and using a 1-h binning, we obtain a residual RMS between 10 and 17 ppm on the individual light curves, and 5.7 ppm when combining the four visits.

37. The CHEOPS mission

Author

Benz, W., Broeg, C., Fortier, A., Rando, N., Beck, T., Beck, M., Queloz, D., Ehrenreich, D., Maxted, P. F. L., Isaak, K. G., Billot, N., Alibert, Y., Alonso, R., António, C., Asquier, J., Bandy, T., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Bekkelien, A., Bergomi, M., Biondi, F., Bonfils, X., Borsato, L., Brandeker, A., Busch, M.-D., Cabrera, J., Cessa, V., Charnoz, S., Chazelas, B., Collier Cameron, A., Corral Van Damme, C., Cortes, D., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O., Demory, B. O., Erikson, A., Farinato, J., Fossati, L., Fridlund, M., Futyan, D., Gandolfi, D., Garcia Munoz, A., Gillon, M., Guterman, P., Gutierrez, A., Hasiba, J., Heng, K., Hernandez, E., Hoyer, S., Kiss, L. L., Kovacs, Z., Kuntzer, T., Laskar, J., Lecavelier Des Etangs, A., Lendl, M., López, A., Lora, I., Lovis, C., Lüftinger, T., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., De Miguel, D., Modrego, D., Munari, M., Nascimbeni, V., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Palacios, R., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pizarro, A., Pollaco, D., Ragazzoni, R., Ratti, F., Rauer, H., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Salatti, M., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sordet, M., Sousa, S. G., Steller, M., Szabó, G. M., Szoke, J., Thomas, N., Tschentscher, M., Udry, S., Van Grootel, V., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Subjects
High-precision transit photometry, Exoplanets, CHEOPS, Original Article, Small mission, 7. Clean energy
Abstract

Funder: University of Bern, The CHaracterising ExOPlanet Satellite (CHEOPS) was selected on October 19, 2012, as the first small mission (S-mission) in the ESA Science Programme and successfully launched on December 18, 2019, as a secondary passenger on a Soyuz-Fregat rocket from Kourou, French Guiana. CHEOPS is a partnership between ESA and Switzerland with important contributions by ten additional ESA Member States. CHEOPS is the first mission dedicated to search for transits of exoplanets using ultrahigh precision photometry on bright stars already known to host planets. As a follow-up mission, CHEOPS is mainly dedicated to improving, whenever possible, existing radii measurements or provide first accurate measurements for a subset of those planets for which the mass has already been estimated from ground-based spectroscopic surveys. The expected photometric precision will also allow CHEOPS to go beyond measuring only transits and to follow phase curves or to search for exo-moons, for example. Finally, by unveiling transiting exoplanets with high potential for in-depth characterisation, CHEOPS will also provide prime targets for future instruments suited to the spectroscopic characterisation of exoplanetary atmospheres. To reach its science objectives, requirements on the photometric precision and stability have been derived for stars with magnitudes ranging from 6 to 12 in the V band. In particular, CHEOPS shall be able to detect Earth-size planets transiting G5 dwarf stars (stellar radius of 0.9R⊙) in the magnitude range 6 ≤ V ≤ 9 by achieving a photometric precision of 20 ppm in 6 hours of integration time. In the case of K-type stars (stellar radius of 0.7R⊙) of magnitude in the range 9 ≤ V ≤ 12, CHEOPS shall be able to detect transiting Neptune-size planets achieving a photometric precision of 85 ppm in 3 hours of integration time. This precision has to be maintained over continuous periods of observation for up to 48 hours. This precision and stability will be achieved by using a single, frame-transfer, back-illuminated CCD detector at the focal plane assembly of a 33.5 cm diameter, on-axis Ritchey-Chrétien telescope. The nearly 275 kg spacecraft is nadir-locked, with a pointing accuracy of about 1 arcsec rms, and will allow for at least 1 Gbit/day downlink. The sun-synchronous dusk-dawn orbit at 700 km altitude enables having the Sun permanently on the backside of the spacecraft thus minimising Earth stray light. A mission duration of 3.5 years in orbit is foreseen to enable the execution of the science programme. During this period, 20% of the observing time is available to the wider community through yearly ESA call for proposals, as well as through discretionary time approved by ESA’s Director of Science. At the time of this writing, CHEOPS commissioning has been completed and CHEOPS has been shown to fulfill all its requirements. The mission has now started the execution of its science programme.

38. CHEOPS observations of the HD 108236 planetary system: a fifth planet, improved ephemerides, and planetary radii

Author

Bonfanti, A., Delrez, L., Hooton, M. J., Wilson, T. G., Fossati, L., Alibert, Y., Hoyer, S., Mustill, A. J., Osborn, H. P., Adibekyan, V., Gandolfi, D., Salmon, S., Sousa, S. G., Tuson, A., Van Grootel, V., Cabrera, J., Nascimbeni, V., Maxted, P. F. L., Barros, S. C. C., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Fridlund, M., Lacedelli, G., Lendl, M., Persson, C., Santos, N. C., Scandariato, G., Szabó, Gy. M., Collier Cameron, A., Udry, S., Benz, W., Beck, M., Ehrenreich, D., Fortier, A., Isaak, K. G., Queloz, D., Alonso, R., Asquier, J., Bandy, T., Bárczy, T., Barrado, D., Barragán, O., Baumjohann, W., Beck, T., Bekkelien, A., Bergomi, M., Brandeker, A., Busch, M.-D., Cessa, V., Charnoz, S., Chazelas, B., Corral Van Damme, C., Demory, B.-O., Erikson, A., Farinato, J., Futyan, D., Garcia Muñoz, A., Gillon, M., Guedel, M., Guterman, P., Hasiba, J., Heng, K., Hernandez, E., Kiss, L., Kuntzer, T., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Salatti, M., Ségransan, D., Simon, A. E., Smith, A. M. S., Sordet, M., Steller, M., Thomas, N., Tschentscher, M., Van Eylen, V., Viotto, V., Walter, I., Walton, N. A., Wildi, F., and Wolter, D.

Subjects
13. Climate action, 530 Physics, 520 Astronomy, 620 Engineering
Abstract

Context. The detection of a super-Earth and three mini-Neptunes transiting the bright (V = 9.2 mag) star HD 108236 (also known as TOI-1233) was recently reported on the basis of TESS and ground-based light curves. Aims. We perform a first characterisation of the HD 108236 planetary system through high-precision CHEOPS photometry and improve the transit ephemerides and system parameters. Methods. We characterise the host star through spectroscopic analysis and derive the radius with the infrared flux method. We constrain the stellar mass and age by combining the results obtained from two sets of stellar evolutionary tracks. We analyse the available TESS light curves and one CHEOPS transit light curve for each known planet in the system. Results. We find that HD 108236 is a Sun-like star with R⋆ = 0.877 ± 0.008 R⊙, M⋆ = 0.869−0.048+0.050 M⊙, and an age of 6.7−5.1+4.0 Gyr. We report the serendipitous detection of an additional planet, HD 108236 f, in one of the CHEOPS light curves. For this planet, the combined analysis of the TESS and CHEOPS light curves leads to a tentative orbital period of about 29.5 days. From the light curve analysis, we obtain radii of 1.615 ± 0.051, 2.071 ± 0.052, 2.539−0.065+0.062, 3.083 ± 0.052, and 2.017−0.057+0.052 R⊕ for planets HD 108236 b to HD 108236 f, respectively. These values are in agreement with previous TESS-based estimates, but with an improved precision of about a factor of two. We perform a stability analysis of the system, concluding that the planetary orbits most likely have eccentricities smaller than 0.1. We also employ a planetary atmospheric evolution framework to constrain the masses of the five planets, concluding that HD 108236 b and HD 108236 c should have an Earth-like density, while the outer planets should host a low mean molecular weight envelope. Conclusions. The detection of the fifth planet makes HD 108236 the third system brighter than V = 10 mag to host more than four transiting planets. The longer time span enables us to significantly improve the orbital ephemerides such that the uncertainty on the transit times will be of the order of minutes for the years to come. A comparison of the results obtained from the TESS and CHEOPS light curves indicates that for a V ~ 9 mag solar-like star and a transit signal of ~500 ppm, one CHEOPS transit light curve ensures the same level of photometric precision as eight TESS transits combined, although this conclusion depends on the length and position of the gaps in the light curve.

39. The Soft X-ray Imager (SXI) on the SMILE Mission

Author

Sembay, S., Alme, A.L., Agnolon, D., Arnold, T., Beardmore, A., Belén Balado Margeli, A., Bicknell, C., Bouldin, C., Branduardi-Raymont, G., Breuer, J.P., Buggey, T., Butcher, G., Canchal, R., Carter, J.A., Crawford, T., Cheney, A., Collado-Vega, Y., Connor, H., Eaton, N., Feldman, C., Forsyth, C., Frantzen, T., Galgóczi, G., Garcia, J., Genov, G.Y., Gordillo, C., Gröbelbauer, H-P., Guedel, M., Guo, Y., Hailey, M., Hall, D., Hampson, R., Hasiba, J., Hetherington, O., Holland, A., Hsieh, S-Y, Hubbard, M., Jeszenszky, H., Jones, M., Kennedy, T., Koch-Mehrin, K., Kögl, S., Krucker, S., Kuntz, K.D., Lakin1, C., Laky, G., Lylund, O., Martindale, A., Miguel Mas Hesse, J., Nakamura, R., Oksavik, K., Østgaard, N., Ottacher, H., Ottensamer, R., Pagani, C., Parsons, S., Patel, P., Pearson, J., Peikert, G., Porter, F.S., Pouliantis, T., Randall, G., Qureshi, B.H, Raab, W., Read, A.M., Roque, N.M.M., Rostad, M.E., Runciman, C., Sachdev, S., Samsonov, A., Soman, M., Sibeck, D., Smit, S., Søndergaard, J., Speight, R., Stavland, S., Steller, M., Sun, TianRan, Thornhill, J., Thomas, W., Ullaland, K., Walsh, B., Walton, D., Wang, C., Yang, S., Sembay, S., Alme, A.L., Agnolon, D., Arnold, T., Beardmore, A., Belén Balado Margeli, A., Bicknell, C., Bouldin, C., Branduardi-Raymont, G., Breuer, J.P., Buggey, T., Butcher, G., Canchal, R., Carter, J.A., Crawford, T., Cheney, A., Collado-Vega, Y., Connor, H., Eaton, N., Feldman, C., Forsyth, C., Frantzen, T., Galgóczi, G., Garcia, J., Genov, G.Y., Gordillo, C., Gröbelbauer, H-P., Guedel, M., Guo, Y., Hailey, M., Hall, D., Hampson, R., Hasiba, J., Hetherington, O., Holland, A., Hsieh, S-Y, Hubbard, M., Jeszenszky, H., Jones, M., Kennedy, T., Koch-Mehrin, K., Kögl, S., Krucker, S., Kuntz, K.D., Lakin1, C., Laky, G., Lylund, O., Martindale, A., Miguel Mas Hesse, J., Nakamura, R., Oksavik, K., Østgaard, N., Ottacher, H., Ottensamer, R., Pagani, C., Parsons, S., Patel, P., Pearson, J., Peikert, G., Porter, F.S., Pouliantis, T., Randall, G., Qureshi, B.H, Raab, W., Read, A.M., Roque, N.M.M., Rostad, M.E., Runciman, C., Sachdev, S., Samsonov, A., Soman, M., Sibeck, D., Smit, S., Søndergaard, J., Speight, R., Stavland, S., Steller, M., Sun, TianRan, Thornhill, J., Thomas, W., Ullaland, K., Walsh, B., Walton, D., Wang, C., and Yang, S.

Abstract

The Soft X-ray Imager (SXI) is part of the scientific payload of the Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) mission. SMILE is a joint science mission between the European Space Agency (ESA) and the Chinese Academy of Sciences (CAS) and is due for launch in 2025. SXI is a compact X-ray telescope with a wide field-of-view (FOV) capable of encompassing large portions of Earth’s magnetosphere from the vantage point of the SMILE orbit. SXI is sensitive to the soft X-rays produced by the Solar Wind Charge eXchange (SWCX) process produced when heavy ions of solar wind origin interact with neutral particles in Earth’s exosphere. SWCX provides a mechanism for boundary detection within the magnetosphere, such as the position of Earth’s magnetopause, because the solar wind heavy ions have a very low density in regions of closed magnetic field lines. The sensitivity of the SXI is such that it can potentially track movements of the magnetopause on timescales of a few minutes and the orbit of SMILE will enable such movements to be tracked for segments lasting many hours. SXI is led by the University of Leicester in the United Kingdom (UK) with collaborating organisations on hardware, software and science support within the UK, Europe, China and the United States.

40. The Comet Interceptor Mission.

Author

Jones GH, Snodgrass C, Tubiana C, Küppers M, Kawakita H, Lara LM, Agarwal J, André N, Attree N, Auster U, Bagnulo S, Bannister M, Beth A, Bowles N, Coates A, Colangeli L, Corral van Damme C, Da Deppo V, De Keyser J, Della Corte V, Edberg N, El-Maarry MR, Faggi S, Fulle M, Funase R, Galand M, Goetz C, Groussin O, Guilbert-Lepoutre A, Henri P, Kasahara S, Kereszturi A, Kidger M, Knight M, Kokotanekova R, Kolmasova I, Kossacki K, Kührt E, Kwon Y, La Forgia F, Levasseur-Regourd AC, Lippi M, Longobardo A, Marschall R, Morawski M, Muñoz O, Näsilä A, Nilsson H, Opitom C, Pajusalu M, Pommerol A, Prech L, Rando N, Ratti F, Rothkaehl H, Rotundi A, Rubin M, Sakatani N, Sánchez JP, Simon Wedlund C, Stankov A, Thomas N, Toth I, Villanueva G, Vincent JB, Volwerk M, Wurz P, Wielders A, Yoshioka K, Aleksiejuk K, Alvarez F, Amoros C, Aslam S, Atamaniuk B, Baran J, Barciński T, Beck T, Behnke T, Berglund M, Bertini I, Bieda M, Binczyk P, Busch MD, Cacovean A, Capria MT, Carr C, Castro Marín JM, Ceriotti M, Chioetto P, Chuchra-Konrad A, Cocola L, Colin F, Crews C, Cripps V, Cupido E, Dassatti A, Davidsson BJR, De Roche T, Deca J, Del Togno S, Dhooghe F, Donaldson Hanna K, Eriksson A, Fedorov A, Fernández-Valenzuela E, Ferretti S, Floriot J, Frassetto F, Fredriksson J, Garnier P, Gaweł D, Génot V, Gerber T, Glassmeier KH, Granvik M, Grison B, Gunell H, Hachemi T, Hagen C, Hajra R, Harada Y, Hasiba J, Haslebacher N, Herranz De La Revilla ML, Hestroffer D, Hewagama T, Holt C, Hviid S, Iakubivskyi I, Inno L, Irwin P, Ivanovski S, Jansky J, Jernej I, Jeszenszky H, Jimenéz J, Jorda L, Kama M, Kameda S, Kelley MSP, Klepacki K, Kohout T, Kojima H, Kowalski T, Kuwabara M, Ladno M, Laky G, Lammer H, Lan R, Lavraud B, Lazzarin M, Le Duff O, Lee QM, Lesniak C, Lewis Z, Lin ZY, Lister T, Lowry S, Magnes W, Markkanen J, Martinez Navajas I, Martins Z, Matsuoka A, Matyjasiak B, Mazelle C, Mazzotta Epifani E, Meier M, Michaelis H, Micheli M, Migliorini A, Millet AL, Moreno F, Mottola S, Moutounaick B, Muinonen K, Müller DR, Murakami G, Murata N, Myszka K, Nakajima S, Nemeth Z, Nikolajev A, Nordera S, Ohlsson D, Olesk A, Ottacher H, Ozaki N, Oziol C, Patel M, Savio Paul A, Penttilä A, Pernechele C, Peterson J, Petraglio E, Piccirillo AM, Plaschke F, Polak S, Postberg F, Proosa H, Protopapa S, Puccio W, Ranvier S, Raymond S, Richter I, Rieder M, Rigamonti R, Ruiz Rodriguez I, Santolik O, Sasaki T, Schrödter R, Shirley K, Slavinskis A, Sodor B, Soucek J, Stephenson P, Stöckli L, Szewczyk P, Troznai G, Uhlir L, Usami N, Valavanoglou A, Vaverka J, Wang W, Wang XD, Wattieaux G, Wieser M, Wolf S, Yano H, Yoshikawa I, Zakharov V, Zawistowski T, Zuppella P, Rinaldi G, and Ji H

Abstract

Here we describe the novel, multi-point Comet Interceptor mission. It is dedicated to the exploration of a little-processed long-period comet, possibly entering the inner Solar System for the first time, or to encounter an interstellar object originating at another star. The objectives of the mission are to address the following questions: What are the surface composition, shape, morphology, and structure of the target object? What is the composition of the gas and dust in the coma, its connection to the nucleus, and the nature of its interaction with the solar wind? The mission was proposed to the European Space Agency in 2018, and formally adopted by the agency in June 2022, for launch in 2029 together with the Ariel mission. Comet Interceptor will take advantage of the opportunity presented by ESA's F-Class call for fast, flexible, low-cost missions to which it was proposed. The call required a launch to a halo orbit around the Sun-Earth L2 point. The mission can take advantage of this placement to wait for the discovery of a suitable comet reachable with its minimum Δ V capability of 600  ms - 1 . Comet Interceptor will be unique in encountering and studying, at a nominal closest approach distance of 1000 km, a comet that represents a near-pristine sample of material from the formation of the Solar System. It will also add a capability that no previous cometary mission has had, which is to deploy two sub-probes - B1, provided by the Japanese space agency, JAXA, and B2 - that will follow different trajectories through the coma. While the main probe passes at a nominal 1000 km distance, probes B1 and B2 will follow different chords through the coma at distances of 850 km and 400 km, respectively. The result will be unique, simultaneous, spatially resolved information of the 3-dimensional properties of the target comet and its interaction with the space environment. We present the mission's science background leading to these objectives, as well as an overview of the scientific instruments, mission design, and schedule., Competing Interests: Competing InterestsThe authors declare no competing interests., (© The Author(s) 2024.)

Published
2024
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