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1. Architecture of TOI-561 planetary system

Author

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

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561's orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be $77.14399\pm0.00025$ days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ($R_p = 2.517 \pm 0.045 R_{\oplus}$ from 5$\%$ to 2$\%$ precision) and mass ($M_p = 12.4 \pm 1.4 M_{\oplus}$) estimates, implying a density of $\rho_p = 0.778 \pm 0.097 \rho_{\oplus}$. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f., Comment: 13 pages, 10 Figures. Accepted on MNRAS. Updated the author list

Published
2024

2. The CHEOPS view on the climate of WASP-3 b

Author

Scandariato, G., Carone, L., Cubillos, P. E., Maxted, P. F. L., Zingales, T., Günther, M. N., Heitzmann, A., Lendl, M., Wilson, T. G., Bonfanti, A., Bruno, G., Krenn, A., Valdes, E. Meier, Singh, V., Swayne, M. I., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Benz, W., Billot, N., Borsato, L., Brandeker, A., Broeg, C., Buder, M., Busch, M. -D., Cameron, A. Collier, Correia, A. C. M., Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Merín, B., Mordasini, C., Nascimbeni, V., Olofsson, G., 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., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere makes them the most amenable targets for the atmospheric characterization. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92+-21 ppm in the CHEOPS passband, 83+-27 ppm for TESS and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands we propose a set of likely emission spectra which constrain the emission contribution in the \cheops and TESS passbands to approximately a few dozens of parts per million. This allowed us to measure a geometric albedo of 0.21+-0.07 in the CHEOPS passband, while the TESS data lead to a 95\% upper limit of $\sim$0.2. WASP-3 b belongs to the group of ultra-hot Jupiters which are characterized by low Bond albedo (<0.3+-0.1), as predicted by different atmospheric models. On the other hand, it unexpectedly seems to efficiently recirculate the absorbed stellar energy, unlike similar highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms may be at play other than advection (for example, dissociation and recombination of H_2). Another possibility is that the observations in different bandpasses probe different atmospheric layers, making the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date.

Published
2024
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3. Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS

Author

Egger, J. A., Osborn, H. P., Kubyshkina, D., Mordasini, C., Alibert, Y., Günther, M. N., Lendl, M., Brandeker, A., Heitzmann, A., Leleu, A., Damasso, M., Bonfanti, A., Wilson, T. G., Sousa, S. G., Haldemann, J., Delrez, L., Hooton, M. J., Zingales, T., Luque, R., Alonso, R., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Benz, W., Billot, N., Borsato, L., Broeg, C., Buder, M., Castro-González, A., Cameron, A. Collier, Correia, A. C. M., Cortes, D., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Lavie, B., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., Maxted, P. F. L., Merín, B., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Rodrigues, J., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and a sub-Neptune. We observe HIP 29442 with CHEOPS for a total of 9.6 days, which we model jointly with 2 sectors of TESS data to derive planetary radii of $3.410\pm0.046$, $1.551\pm0.045$ and $1.538\pm0.049$ R$_\oplus$ for planets b, c and d, which orbit HIP 29442 with periods of 13.6, 3.5 and 6.4 days. For planet d, this value deviates by more than 3 sigma from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit S/N and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduce the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then apply hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identify planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with both a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope as well as a scenario with water-rich sub-Neptunes., Comment: 30 pages, 17 figures, accepted for publication in A&A

Published
2024
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4. The tidal deformation and atmosphere of WASP-12b from its phase curve

Author

Akinsanmi, B., Barros, S. C. C., Lendl, M., Carone, L., Cubillos, P. E., Bekkelien, A., Fortier, A., Florén, H. -G., Cameron, A. Collier, Boué, G., Bruno, G., Demory, B. -O., Brandeker, A., Sousa, S. G., Wilson, T. G., Deline, A., Bonfanti, A., Scandariato, G., Hooton, M. J., Correia, A. C. M., Demangeon, O. D. S., Smith, A. M. S., Singh, V., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T., Navascues, D. Barrado, Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, Ch., Buder, M., Charnoz, S., Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Ehrenreich, D., Erikson, A., Farinato, J., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mecina, M., Mordasini, Ch., Nascimbeni, V., Olofsson, G., 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., Ségransan, D., Simon, A. E., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets at extreme conditions. WASP-12b stands out as an archetype of this class of exoplanets. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data to measure the planet's tidal deformation, atmospheric properties, and orbital decay rate. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number, $h_2$, which quantifies its radial deformation and provides insight into the interior structure. We measured the tidal deformation of WASP-12b and estimated a Love number of $h_2=1.55_{-0.49}^{+0.45}$ (at 3.2$\sigma$) from its phase curve. We measured occultation depths of $333\pm24$ppm and $493\pm29$ppm in the CHEOPS and TESS bands, respectively, while the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of 2900K. We also estimated low geometric albedos of $0.086\pm0.017$ and $0.01\pm0.023$ in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the dayside of the WASP-12b. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet. Finally, we refine the orbital decay rate by 12% to a value of -30.23$\pm$0.82 ms/yr. WASP-12b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured (at 3$sigma$) from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring $h_2$ with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared., Comment: accepted for publication in A&A

Published
2024

5. 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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6. Refined parameters of the HD 22946 planetary system and the true orbital period of planet d

Author

Garai, Z., Osborn, H. P., Gandolfi, D., Brandeker, A., Sousa, S. G., Lendl, M., Bekkelien, A., Broeg, C., Cameron, A. Collier, Egger, J. A., Hooton, M. J., Alibert, Y., Delrez, L., Fossati, L., Salmon, S., Wilson, T. G., Bonfanti, A., Tuson, A., Ulmer-Moll, S., Serrano, L. M., Borsato, L., Alonso, R., Anglada, G., Asquier, J., Navascues, D. Barrado y, Barros, S. C. C., Bárczy, T., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Biondi, F., Bonfils, X., 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., Van Eylen, V., Fortier, A., Fridlund, M., Gillon, M., Van Grootel, V., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Kristiansen, M. H., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., 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., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., and Walton, N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Multi-planet systems are important sources of information regarding the evolution of planets. However, the long-period planets in these systems often escape detection. HD 22946 is a bright star around which 3 transiting planets were identified via TESS photometry, but the true orbital period of the outermost planet d was unknown until now. We aim to use CHEOPS to uncover the true orbital period of HD 22946d and to refine the orbital and planetary properties of the system, especially the radii of the planets. We used the available TESS photometry of HD 22946 and observed several transits of the planets b, c, and d using CHEOPS. We identified 2 transits of planet d in the TESS photometry, calculated the most probable period aliases based on these data, and then scheduled CHEOPS observations. The photometric data were supplemented with ESPRESSO radial velocity data. Finally, a combined model was fitted to the entire dataset. We successfully determined the true orbital period of the planet d to be 47.42489 $\pm$ 0.00011 d, and derived precise radii of the planets in the system, namely 1.362 $\pm$ 0.040 R$_\oplus$, 2.328 $\pm$ 0.039 R$_\oplus$, and 2.607 $\pm$ 0.060 R$_\oplus$ for planets b, c, and d, respectively. Due to the low number of radial velocities, we were only able to determine 3$\sigma$ upper limits for these respective planet masses, which are 13.71 M$_\oplus$, 9.72 M$_\oplus$, and 26.57 M$_\oplus$. We estimated that another 48 ESPRESSO radial velocities are needed to measure the predicted masses of all planets in HD 22946. Planet c appears to be a promising target for future atmospheric characterisation. We can also conclude that planet d, as a warm sub-Neptune, is very interesting because there are only a few similar confirmed exoplanets to date. Such objects are worth investigating in the near future, for example in terms of their composition and internal structure.

Published
2023
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7. Glancing through the debris disk: Photometric analysis of DE Boo with CHEOPS

Author

Boldog, Á., Szabó, Gy. M., Kriskovics, L., Brandeker, A., Kiefer, F., Bekkelien, A., Guterman, P., Olofsson, G., Simon, A. E., Gandolfi, D., Serrano, L. M., Wilson, T. G., Sousa, S. G., Etangs, A. Lecavelier des, Alibert, Y., Alonso, R., Anglada, G., Bandy, T., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Broeg, C., Buder, M., Cabrera, J., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Csizmadia, Sz., Davies, M. B., Deline, A., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Lendl, M., Lovis, C., Magrin, D., Maxted, P. F. L., Mecina, 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., Smith, A. M. S., Steller, M., Thomas, N., Udry, S., Van Grootel, V., and Walton, N. A.

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

DE Boo is a unique system, with an edge-on view through the debris disk around the star. The disk, which is analogous to the Kuiper belt in the Solar System, was reported to extend from 74 to 84 AU from the central star. The high photometric precision of the Characterising Exoplanet Satellite (CHEOPS) provided an exceptional opportunity to observe small variations in the light curve due to transiting material in the disk. This is a unique chance to investigate processes in the debris disk. Photometric observations of DE Boo of a total of four days were carried out with CHEOPS. Photometric variations due to spots on the stellar surface were subtracted from the light curves by applying a two-spot model and a fourth-order polynomial. The photometric observations were accompanied by spectroscopic measurements with the 1m RCC telescope at Piszk\'estet\H{o} and with the SOPHIE spectrograph in order to refine the astrophysical parameters of DE Boo. We present a detailed analysis of the photometric observation of DE Boo. We report the presence of nonperiodic transient features in the residual light curves with a transit duration of 0.3-0.8 days. We calculated the maximum distance of the material responsible for these variations to be 2.47 AU from the central star, much closer than most of the mass of the debris disk. Furthermore, we report the first observation of flaring events in this system. We interpreted the transient features as the result of scattering in an inner debris disk around DE Boo. The processes responsible for these variations were investigated in the context of interactions between planetesimals in the system., Comment: 10 pages, 4 figures, 5 tables; accepted by Astronomy and Astrophysics

Published
2023
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8. 55 Cancri e's occultation captured with CHEOPS

Author

Demory, B. -O., Sulis, S., Valdes, E. Meier, Delrez, L., Brandeker, A., Billot, N., Fortier, A., Hoyer, S., Sousa, S. G., Heng, K., Lendl, M., Krenn, A., Morris, B. M., Patel, J. A., Alibert, Y., Alonso, R., Anglada, G., Barczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Bonfils, X., Broeg, C., Buder, M., Cabrera, J., Charnoz, S., Cameron, A. Collier, Cottard, H., Csizmadia, Sz., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Gudel, M., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., Marafatto, L., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Segransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabo, Gy. M., Thomas, N., Udry, S., Van Grootel, V., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e's occultation with an average depth of $12\pm3$ ppm. We derive a corresponding 2-$\sigma$ upper limit on the geometric albedo of $A_g < 0.55$ once decontaminated from the thermal emission measured by Spitzer at 4.5$\mu$m. CHEOPS's photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth., Comment: In press. Accepted for publication in Astronomy and Astrophysics on 13 October 2022. 10 pages, 7 figures and 3 tables

Published
2022
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9. A CHEOPS-enhanced view of the HD3167 system

Author

Bourrier, V., Deline, A., Krenn, A., Egger, J. A., Petit, A. C., Malavolta, L., Cretignier, M., Billot, N., Broeg, C., Florén, H. -G., Queloz, D., Alibert, Y., Bonfanti, A., Bonomo, A. S., Delisle, J. -B., Demangeon, O. D. S., Demory, B. -O., Dumusque, X., Ehrenreich, D., Haywood, R. D., Howell, S. B, Lendl, M., Mortier, A., Nigro, G., Salmon, S., Sousa, S. G., Wilson, T. G., Adibekyan, V., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Benz, W., Biondi, F., Bonfils, X., Brandeker, A., Cabrera, J., Charnoz, S., Csizmadia, Sz., Cameron, A. Collier, Damasso, M., Davies, M. B., Deleuil, M., Delrez, L., Di Fabrizio, L., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lorenzi, V., Lovis, C., Magrin, D., Massa, A., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, 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., Van Grootel, V., Verrecchia, F., Walton, N., Beck, T., Buder, M., Ratti, F., Ulmer, B., and Viotto, V.

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

Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD\,3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD3167 system, which remains a target of choice for follow-up observations and simulations., Comment: 22 pages, 23 pages, accepted for publication in A&A (18 August 2022). Updated author list in new version

Published
2022
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10. Fundamental effective temperature measurements for eclipsing binary stars -- III. SPIRou near-infrared spectroscopy and CHEOPS photometry of the benchmark G0V star EBLM J0113+31

Author

Maxted, P. F. L., Miller, N. J., Hoyer, S., Adibekyan, V., Sousa, S. G., Billot, N., Fortier, A., Simon, A. E., Cameron, A. Collier, Sawyne, M. I., Gutermann, P., Triaud, A. H. M. J., Southworth, J., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Bonfils, X., Brandeker, A., Broeg, C., Buder, M., Cabrera, J., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O., Demory, B. -O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Leon, J. E. Hernández, Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Magrin, D., Munari, M., 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., Santos, N. C., Scandariato, G., Ségransan, D., Smith, A. M. S., Steinberger, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Grootel, V., and Walton, N.

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

EBLM J0113+31 is moderately bright (V=10.1), metal-poor ([Fe/H]$\approx-0.3$) G0V star with a much fainter M dwarf companion on a wide, eccentric orbit (=14.3 d). We have used near-infrared spectroscopy obtained with the SPIRou spectrograph to measure the semi-amplitude of the M dwarf's spectroscopic orbit, and high-precision photometry of the eclipse and transit from the CHEOPS and TESS space missions to measure the geometry of this binary system. From the combined analysis of these data together with previously published observations we obtain the following model-independent masses and radii: $M_1 = 1.029 \pm 0.025 M_{\odot}$, $M_2 = 0.197 \pm 0.003 M_{\odot}$, $R_1 = 1.417 \pm 0.014 R_{\odot}$, $R_2 = 0.215 \pm 0.002 R_{\odot}$. Using $R_1$ and the parallax from Gaia EDR3 we find that this star's angular diameter is $\theta = 0.0745 \pm 0.0007$ mas. The apparent bolometric flux of the G0V star corrected for both extinction and the contribution from the M dwarf ($<0.2$ per cent) is ${\mathcal F}_{\oplus,0} = (2.62\pm 0.05)\times10^{-9}$ erg.cm$^{-2}$.s$^{-1}$. Hence, this G0V star has an effective temperature $T_{\rm eff,1} = 6124{\rm\,K} \pm 40{\rm \,K\,(rnd.)} \pm 10 {\rm \,K\,(sys.)}$. EBLM J0113+31 is an ideal benchmark star that can be used for "end-to-end" tests of the stellar parameters measured by large-scale spectroscopic surveys, or stellar parameters derived from asteroseismology with PLATO. The techniques developed here can be applied to many other eclipsing binaries in order to create a network of such benchmark stars., Comment: Accepted for publication in MNRAS. 15 pages, 9 figures

Published
2022
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11. Six transiting planets and a chain of Laplace resonances in TOI-178

Author

Leleu, A., Alibert, Y., Hara, N. C., Hooton, M. J., Wilson, T. G., Robutel, P., Delisle, J. -B., Laskar, J., Hoyer, S., Lovis, C., Bryant, E. M., Ducrot, E., Cabrera, J., Delrez, L., Acton, J. S., Adibekyan, V., Allart, R., Prieto, C. Allende, Alonso, R., Alves, D., Anderson, D. R., Angerhausen, D., Escudé, G. Anglada, Asquier, J., Barrado, D., Barros, S. C. C., Baumjohann, W., Bayliss, D., Beck, M., Beck, T., Bekkelien, A., Benz, W., Billot, N., Bonfanti, A., Bonfils, X., Bouchy, F., Bourrier, V., Boué, G., Brandeker, A., Broeg, C., Buder, M., Burdanov, A., Burleigh, M. R., Bárczy, T., Cameron, A. C., Chamberlain, S., Charnoz, S., Cooke, B. F., Van Damme, C. Corral, Correia, A. C. M., Cristiani, S., Damasso, M., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Di Marcantonio, P., Di Persio, G., Dumusque, X., Ehrenreich, D., Erikson, A., Figueira, P., Fortier, A., Fossati, L., Fridlund, M., Futyan, D., Gandolfi, D., Muñoz, A. García, Garcia, L. J., Gill, S., Gillen, E., Gillon, M., Goad, M. R., Hernández, J. I. González, Guedel, M., Günther, M. N., Haldemann, J., Henderson, B., Heng, K., Hogan, A. E., Isaak, K., Jehin, E., Jenkins, J. S., Jordán, A., Kiss, L., Kristiansen, M. H., Lam, K., Lavie, B., Etangs, A. Lecavelier des, Lendl, M., Lillo-Box, J., Curto, G. Lo, Magrin, D., Martins, C. J. A. P., Maxted, P. F. L., McCormac, J., Mehner, A., Micela, G., Molaro, P., Moyano, M., Murray, C. A., Nascimbeni, V., Nunes, N. J., Olofsson, G., Osborn, H. P., Oshagh, M., Ottensamer, R., Pagano, I., Pallé, E., Pedersen, P. P., Pepe, F. A., Persson, C. M., Peter, G., Piotto, G., Polenta, G., Pollacco, D., Poretti, E., Pozuelos, F. J., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Raynard, L., Rebolo, R., Reimers, C., Ribas, I., Santos, N. C., Scandariato, G., Schneider, J., Sebastian, D., Sestovic, M., Simon, A. E., Smith, A. M. S., Sousa, S. G., Sozzetti, A., Steller, M., Mascareño, A. Suárez, Szabó, Gy. M., Ségransan, D., Thomas, N., Thompson, S., Tilbrook, R. H., Triaud, A., Turner, O., Udry, S., Van Grootel, V., Venus, H., Verrecchia, F., Vines, J. I., Walton, N. A., West, R. G., Wheatley, P. J., Wolter, D., and Osorio, M. R. Zapatero

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at a 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152(-0.070/+0.073) to 2.87(-0.13/+0.14) Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02(+0.28/-0.23) to 0.177(+0.055/-0.061) times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.

Published
2021
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12. The tidal deformation and atmosphere of WASP-12\,b from its phase curve

Author

Akinsanmi, B., primary, Barros, S.C., additional, Lendl, M., additional, Carone, L., additional, Cubillos, P.E., additional, Bekkelien, A., additional, Fortier, A., additional, Florén, H.-G., additional, Collier Cameron, A., additional, Boué, G., additional, Bruno, G., additional, Demory, B.-O., additional, Brandeker, A., additional, Sousa, S.G., additional, Wilson, T.G., additional, Deline, A., additional, Bonfanti, A., additional, Scandariato, G., additional, Hooton, M.J., additional, Correia, A.C.M., additional, Demangeon, O.D.S., additional, Smith, A.M.S., additional, Singh, V., additional, Alibert, Y., additional, Alonso, R., additional, Asquier, J., additional, Bárczy, T., additional, Barrado Navascues, D., 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, Buder, M., additional, Charnoz, S., additional, Csizmadia, Sz., additional, Davies, M.B., additional, Deleuil, M., additional, Delrez, L., additional, Ehrenreich, D., additional, Erikson, A., additional, Farinato, J., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Günther, M.N., additional, Heitzmann, A., additional, Helling, Ch., additional, Hoyer, S., additional, Isaak, K.G., additional, Kiss, L., additional, Lam, K.W.F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Magrin, D., additional, Maxted, P.F.L., additional, Mecina, M., additional, Mordasini, C., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piazza, D., 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, Simon, A.E., additional, Stalport, M., additional, Szabó, M. Gy., additional, Thomas, N., additional, Udry, S., additional, Van Grootel, V., additional, Venturini, J., additional, Villaver, E., additional, and Walton, N.A., additional

Published
2024
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13. 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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14. Refined parameters of the HD 22946 planetary system and the true orbital period of planet d

Author

Garai, Z., primary, Osborn, H. P., additional, Gandolfi, D., additional, Brandeker, A., additional, Sousa, S. G., additional, Lendl, M., additional, Bekkelien, A., additional, Broeg, C., additional, Cameron, A. Collier, additional, Egger, J. A., additional, Hooton, M. J., additional, Alibert, Y., additional, Delrez, L., additional, Fossati, L., additional, Salmon, S., additional, Wilson, T. G., additional, Bonfanti, A., additional, Tuson, A., additional, Ulmer-Moll, S., additional, Serrano, L. M., additional, Borsato, L., additional, Alonso, R., additional, Anglada, G., additional, Asquier, J., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Bárczy, T., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Biondi, F., additional, Bonfils, X., 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, Van Eylen, V., additional, Fortier, A., additional, Fridlund, M., additional, Gillon, M., additional, Van Grootel, V., additional, Güdel, M., additional, Günther, M. N., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Kristiansen, M. H., additional, Laskar, J., additional, des Etangs, A. Lecavelier, additional, Lovis, C., additional, Luntzer, A., 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, 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, Venturini, J., additional, and Walton, N., additional

Published
2023
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15. Glancing through the debris disk: Photometric analysis of DE Boo with CHEOPS

Author

Boldog, Á., primary, Szabó, Gy. M., additional, Kriskovics, L., additional, Brandeker, A., additional, Kiefer, F., additional, Bekkelien, A., additional, Guterman, P., additional, Olofsson, G., additional, Simon, A. E., additional, Gandolfi, D., additional, Serrano, L. M., additional, Wilson, T. G., additional, Sousa, S. G., additional, Lecavelier des Etangs, A., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Bandy, T., additional, Bárczy, T., additional, Barrado, 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, Broeg, C., additional, Buder, M., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Corral van Damme, C., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deline, A., additional, Deleuil, M., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Farinato, J., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Gillon, M., additional, Güdel, M., additional, Heng, K., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Laskar, J., additional, Lendl, M., additional, Lovis, C., additional, Magrin, D., additional, Maxted, P. F. L., additional, Mecina, 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, Smith, A. M. S., additional, Steller, M., additional, Thomas, N., additional, Udry, S., additional, Van Grootel, V., additional, and Walton, N. A., additional

Published
2023
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16. 55 Cancri e’s occultation captured with CHEOPS,

Author

Demory, B.-O., primary, Sulis, S., additional, Meier Valdés, E., additional, Delrez, L., additional, Brandeker, A., additional, Billot, N., additional, Fortier, A., additional, Hoyer, S., additional, Sousa, S. G., additional, Heng, K., additional, Lendl, M., additional, Krenn, A., additional, Morris, B. M., additional, Patel, J. A., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, 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, Broeg, C., additional, Buder, M., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Cottard, H., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Ehrenreich, D., additional, Erikson, A., additional, Fossati, L., additional, Fridlund, M., 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, Luntzer, A., additional, Magrin, D., additional, Marafatto, L., additional, Maxted, P. F. L., 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, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., 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, Van Grootel, V., additional, and Walton, N. A., additional

Published
2023
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17. A CHEOPS-enhanced view of the HD 3167 system,

Author

Bourrier, V., primary, Deline, A., additional, Krenn, A., additional, Egger, J. A., additional, Petit, A. C., additional, Malavolta, L., additional, Cretignier, M., additional, Billot, N., additional, Broeg, C., additional, Florén, H.-G., additional, Queloz, D., additional, Alibert, Y., additional, Bonfanti, A., additional, Bonomo, A. S., additional, Delisle, J.-B., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Dumusque, X., additional, Ehrenreich, D., additional, Haywood, R. D., additional, Howell, S. B., additional, Lendl, M., additional, Mortier, A., additional, Nigro, G., additional, Salmon, S., additional, Sousa, S. G., additional, Wilson, T. G., additional, Adibekyan, V., 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, Benz, W., additional, Biondi, F., additional, Bonfils, X., additional, Brandeker, A., additional, Cabrera, J., additional, Charnoz, S., additional, Csizmadia, Sz., additional, Collier Cameron, A., additional, Damasso, M., additional, Davies, M. B., additional, Deleuil, M., additional, Delrez, L., additional, Di Fabrizio, L., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Heng, K., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lorenzi, V., additional, Lovis, C., additional, Magrin, D., additional, Massa, A., additional, Maxted, P. F. L., 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, 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, Verrecchia, F., additional, Walton, N., additional, Beck, T., additional, Buder, M., additional, Ratti, F., additional, Ulmer, B., additional, and Viotto, V., additional

Published
2022
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18. A CHEOPS-enhanced view of the HD 3167 system

Author

Bourrier, V., Deline, A., Krenn, A., Egger, J. A., Petit, A. C., Malavolta, L., Cretignier, M., Billot, N., Broeg, C., Florén, H.-G., Queloz, D., Alibert, Y., Bonfanti, A., Bonomo, A. S., Delisle, J.-B., Demangeon, O. D. S., Demory, B.-O., Dumusque, X., Ehrenreich, D., Haywood, R. D., Howell, S. B., Lendl, M., Mortier, A., Nigro, G., Salmon, S., Sousa, S. G., Wilson, T. G., Adibekyan, V., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Benz, W., Biondi, F., Bonfils, X., Brandeker, A., Cabrera, J., Charnoz, S., Csizmadia, Sz., Cameron, A. Collier, Damasso, M., Davies, M. B., Deleuil, M., Delrez, L., Di Fabrizio, L., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., des Etangs, A. Lecavelier, Lorenzi, V., Lovis, C., Magrin, D., Massa, A., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, 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., Van Grootel, V., Verrecchia, F., Walton, N., Beck, T., Buder, M., Ratti, F., Ulmer, B., Viotto, V., Bourrier, V., Deline, A., Krenn, A., Egger, J. A., Petit, A. C., Malavolta, L., Cretignier, M., Billot, N., Broeg, C., Florén, H.-G., Queloz, D., Alibert, Y., Bonfanti, A., Bonomo, A. S., Delisle, J.-B., Demangeon, O. D. S., Demory, B.-O., Dumusque, X., Ehrenreich, D., Haywood, R. D., Howell, S. B., Lendl, M., Mortier, A., Nigro, G., Salmon, S., Sousa, S. G., Wilson, T. G., Adibekyan, V., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Benz, W., Biondi, F., Bonfils, X., Brandeker, A., Cabrera, J., Charnoz, S., Csizmadia, Sz., Cameron, A. Collier, Damasso, M., Davies, M. B., Deleuil, M., Delrez, L., Di Fabrizio, L., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., des Etangs, A. Lecavelier, Lorenzi, V., Lovis, C., Magrin, D., Massa, A., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, 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., Van Grootel, V., Verrecchia, F., Walton, N., Beck, T., Buder, M., Ratti, F., Ulmer, B., and Viotto, V.

Abstract

Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD 3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD 3167 system, which remains a target of choice for follow-up observations and simulations.

Published
2022

19. Fundamental effective temperature measurements for eclipsing binary stars – III. SPIRou near-infrared spectroscopy and CHEOPS photometry of the benchmark G0V star EBLM J0113+31

Author

Maxted, P F L, primary, Miller, N J, additional, Hoyer, S, additional, Adibekyan, V, additional, Sousa, S G, additional, Billot, N, additional, Fortier, A, additional, Simon, A E, additional, Cameron, A Collier, additional, Swayne, M I, additional, Gutermann, P, additional, Triaud, A H M J, additional, Southworth, J, additional, Alibert, Y, additional, Alonso, R, additional, Anglada, G, additional, Bárczy, T, additional, Navascues, D Barrado y, 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, Buder, M, additional, Cabrera, J, additional, Charnoz, S, additional, van Damme, C Corral, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Delrez, L, additional, Demangeon, O, additional, Demory, B-O, additional, Ehrenreich, D, additional, Erikson, A, additional, Fossati, L, additional, Fridlund, M, additional, Gandolfi, D, additional, Gillon, M, additional, Güdel, M, additional, Heng, K, additional, Leon, J E Hernández, additional, Isaak, K G, additional, Kiss, L L, additional, Laskar, J, additional, Etangs, A Lecavelier des, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, Munari, M, 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, 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, Smith, A M S, additional, Steinberger, M, additional, Steller, M, additional, Szabó, Gy M, additional, Thomas, N, additional, Udry, S, additional, Van Grootel, V, additional, and Walton, N, additional

Published
2022
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20. Six transiting planets and a chain of Laplace resonances in TOI-178

Author

Leleu, A, Alibert, Y, Hara, NC, Hooton, MJ, Wilson, TG, Robutel, P, Delisle, JB, Laskar, J, Hoyer, S, Lovis, C, Bryant, EM, Ducrot, E, Cabrera, J, Delrez, L, Acton, JS, Adibekyan, V, Allart, R, Allende Prieto, C, Alonso, R, Alves, D, Anderson, DR, Angerhausen, D, Anglada Escude´, G, Asquier, J, Barrado, D, Barros, SCC, Baumjohann, W, Bayliss, D, Beck, M, Beck, T, Bekkelien, A, Benz, W, Billot, N, Bonfanti, A, Bonfils, X, Bouchy, F, Bourrier, V, Boueundefined, G, Brandeker, A, Broeg, C, Buder, M, Burdanov, A, Burleigh, MR, Baundefinedrczy, T, Cameron, AC, Chamberlain, S, Charnoz, S, Cooke, BF, Corral Van Damme, C, Correia, ACM, Cristiani, S, Damasso, M, Davies, MB, Deleuil, M, Demangeon, ODS, Demory, BO, Di Marcantonio, P, Di Persio, G, Dumusque, X, Ehrenreich, D, Erikson, A, Figueira, P, Fortier, A, Fossati, L, Fridlund, M, Futyan, D, Gandolfi, D, Garciaundefined Munoundefinedz, A, Garcia, LJ, Gill, S, Gillen, E, Gillon, M, Goad, MR, Gonzaundefinedlez Hernaundefinedndez, JI, Guedel, M, Guundefinednther, MN, Haldemann, J, Henderson, B, Heng, K, Hogan, AE, Isaak, K, Jehin, E, Jenkins, JS, Jordaundefinedn, A, Kiss, L, Kristiansen, MH, Lam, K, Lavie, B, Lecavelier Des Etangs, A, Lendl, M, Lillo-Box, J, Lo Curto, G, Magrin, D, Martins, CJAP, Maxted, PFL, McCormac, J, Mehner, A, Micela, G, Molaro, P, Moyano, M, Hooton, Matthew John [0000-0003-0030-332X], and Apollo - University of Cambridge Repository

Subjects
techniques: photometric, planets and satellites: detection, planets and satellites: dynamical evolution and stability, Astrophysics::Earth and Planetary Astrophysics, celestial mechanics, techniques: spectroscopic
Abstract

Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at a 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152(-0.070/+0.073) to 2.87(-0.13/+0.14) Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02(+0.28/-0.23) to 0.177(+0.055/-0.061) times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.

Published
2021
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21. Six transiting planets and a chain of Laplace resonances in TOI-178

Author

Leleu, A., primary, Alibert, Y., additional, Hara, N. C., additional, Hooton, M. J., additional, Wilson, T. G., additional, Robutel, P., additional, Delisle, J.-B., additional, Laskar, J., additional, Hoyer, S., additional, Lovis, C., additional, Bryant, E. M., additional, Ducrot, E., additional, Cabrera, J., additional, Delrez, L., additional, Acton, J. S., additional, Adibekyan, V., additional, Allart, R., additional, Allende Prieto, C., additional, Alonso, R., additional, Alves, D., additional, Anderson, D. R., additional, Angerhausen, D., additional, Anglada Escudé, G., additional, Asquier, J., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Bayliss, D., additional, Beck, M., additional, Beck, T., additional, Bekkelien, A., additional, Benz, W., additional, Billot, N., additional, Bonfanti, A., additional, Bonfils, X., additional, Bouchy, F., additional, Bourrier, V., additional, Boué, G., additional, Brandeker, A., additional, Broeg, C., additional, Buder, M., additional, Burdanov, A., additional, Burleigh, M. R., additional, Bárczy, T., additional, Cameron, A. C., additional, Chamberlain, S., additional, Charnoz, S., additional, Cooke, B. F., additional, Corral Van Damme, C., additional, Correia, A. C. M., additional, Cristiani, S., additional, Damasso, M., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Di Marcantonio, P., additional, Di Persio, G., additional, Dumusque, X., additional, Ehrenreich, D., additional, Erikson, A., additional, Figueira, P., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Futyan, D., additional, Gandolfi, D., additional, García Muñoz, A., additional, Garcia, L. J., additional, Gill, S., additional, Gillen, E., additional, Gillon, M., additional, Goad, M. R., additional, González Hernández, J. I., additional, Guedel, M., additional, Günther, M. N., additional, Haldemann, J., additional, Henderson, B., additional, Heng, K., additional, Hogan, A. E., additional, Isaak, K., additional, Jehin, E., additional, Jenkins, J. S., additional, Jordán, A., additional, Kiss, L., additional, Kristiansen, M. H., additional, Lam, K., additional, Lavie, B., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lillo-Box, J., additional, Lo Curto, G., additional, Magrin, D., additional, Martins, C. J. A. P., additional, Maxted, P. F. L., additional, McCormac, J., additional, Mehner, A., additional, Micela, G., additional, Molaro, P., additional, Moyano, M., additional, Murray, C. A., additional, Nascimbeni, V., additional, Nunes, N. J., additional, Olofsson, G., additional, Osborn, H. P., additional, Oshagh, M., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Pedersen, P. P., additional, Pepe, F. A., additional, Persson, C. M., additional, Peter, G., additional, Piotto, G., additional, Polenta, G., additional, Pollacco, D., additional, Poretti, E., additional, Pozuelos, F. J., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Raynard, L., additional, Rebolo, R., additional, Reimers, C., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Schneider, J., additional, Sebastian, D., additional, Sestovic, M., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Sozzetti, A., additional, Steller, M., additional, Suárez Mascareño, A., additional, Szabó, Gy. M., additional, Ségransan, D., additional, Thomas, N., additional, Thompson, S., additional, Tilbrook, R. H., additional, Triaud, A., additional, Turner, O., additional, Udry, S., additional, Van Grootel, V., additional, Venus, H., additional, Verrecchia, F., additional, Vines, J. I., additional, Walton, N. A., additional, West, R. G., additional, Wheatley, P. J., additional, Wolter, D., additional, and Zapatero Osorio, M. R., additional

Published
2021
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22. CHEOPS: status summary of the instrument development

Author

Beck, T., Broeg, C., Fortier, A., Cessa, V., Malvasio, L., Piazza, D., Benz, W., Thomas, N., MAGRIN, DEMETRIO, VIOTTO, VALENTINA, BERGOMI, Maria, RAGAZZONI, Roberto, PAGANO, Isabella, Peter, G., Buder, M., Plesseria, J. Y., Steller, M., Ottensamer, R., Ehrenreich, D., Van Damme, C., Isaak, K., Ratti, F., Rando, N., Ngan, I., and ITA

Subjects
Physics, Time delay and integration, Cosmic Vision, 530 Physics, Payload, 520 Astronomy, 02 engineering and technology, 620 Engineering, 021001 nanoscience & nanotechnology, 01 natural sciences, Exoplanet, law.invention, 010309 optics, Telescope, Planet, law, 0103 physical sciences, Systems design, 0210 nano-technology, Transit (satellite), Remote sensing
Abstract

CHEOPS (CHaracterizing ExOPlanets Satellite) is the first ESA Small Mission as part of the ESA Cosmic Vision program 2015-2025. The mission was formally adopted in early February 2014 with a planned launch readiness end of 2017. The mission lead is performed in a partnership between Switzerland, led by the University of Bern, and the European Space Agency with important contributions from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The mission is dedicated to searching for exoplanetary transits by performing ultrahigh precision photometry on bright starts already known to host planets whose mass has been already estimated through ground based observations. The instrument is an optical Ritchey-Chretien telescope of 30 cm clear aperture using a single CCD detector. The optical system is designed to image a de-focused PSF onto the focal plane with very stringent stability and straylight rejection requirements providing a FoV of 0.32 degrees full cone. The system design is adapted to meet the top-level science requirements, which ask for a photometric precision of 20ppm, in 6 hours integration time, on transit measurements of G5 dwarf stars with V-band magnitudes in the range 6≤V≤9 mag. Additionally they ask for a photometric precision of 85 ppm in 3 hours integration time of Neptune-size planets transiting K-type dwarf stars with V-band magnitudes as faint as V=12 mag. Given the demanding schedule and cost constrains, the mission relies mostly on components with flight heritage for the platform as well as for the payload components. Nevertheless, several new developments are integrated into the design as for example the telescope structure and the very low noise, high stability CCD front end electronics. The instrument and mission have gone through critical design review in fall 2015 / spring 2016. This paper describes the current instrument and mission design with a focus on the instrument. It outlines the technical challenges and selected design implementation. Based on the current status, the instrument noise budget is presented including the current best estimate for instrument performance. The current instrument design meets the science requirements and mass and power margins are adequate for the current development status.

Published
2016

23. CHEOPS: status summary of the instrument development

Author

Beck, T., additional, Broeg, C., additional, Fortier, A., additional, Cessa, V., additional, Malvasio, L., additional, Piazza, D., additional, Benz, W., additional, Thomas, N., additional, Magrin, D., additional, Viotto, V., additional, Bergomi, M., additional, Ragazzoni, R., additional, Pagano, I., additional, Peter, G., additional, Buder, M., additional, Plesseria, J. Y., additional, Steller, M., additional, Ottensamer, R., additional, Ehrenreich, D., additional, Isaak, K., additional, Ratti, F., additional, Rando, N., additional, and Ngan, I., additional

Published
2016
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30. CHEOPS: status summary of the instrument development

Author

MacEwen, Howard A., Fazio, Giovanni G., Lystrup, Makenzie, Batalha, Natalie, Siegler, Nicholas, Tong, Edward C., Beck, T., Broeg, C., Fortier, A., Cessa, V., Malvasio, L., Piazza, D., Benz, W., Thomas, N., Magrin, D., Viotto, V., Bergomi, M., Ragazzoni, R., Pagano, I., Peter, G., Buder, M., Plesseria, J. Y., Steller, M., Ottensamer, R., Ehrenreich, D., Van Damme, C., Isaak, K., Ratti, F., Rando, N., and Ngan, I.

Published
2016
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32. On the opioid receptor subtype inhibiting the evoked release of 3H-noradrenaline from guinea-pig atria in vitro

Author

Fuder, H., Buder, M., Riers, H. -D., and Rothacher, G.

Abstract

1.Guinea-pig isolated atria were incubated and loaded with 3H-(-)-noradrenaline. The intrinsic nerves were stimulated with trains of 5 or 35 field pulses (4 Hz), and the evoked efflux of 3H-noradrenaline and of total tritium was determined in the presence of atropine, corticosterone, desipramine, and phentolamine by liquid scintillation spectrometry.2.Ethylketocyclazocine (1.4 nmol/l, IC50), MR 2033 (9.1 nmol/l), dynorphin A (1–13) (25 nmol/l, peptidase inhibitors present), etorphine (71 nmol/l), and [d-Ala2, d-Leu5]-enkephalin (>10 µmol/l, peptidase inhibitors present) inhibited the stimulation-evoked efflux of 3H-noradrenaline in a concentration-dependent manner, but not morphine up to 10 µmol/l.3.The inhibition by ethylketocyclazocine, MR 2033, and etorphine was antagonized by naloxone 1 µmol/l. Similarly, the MR 2033 effect was antagonized by SKF 10047 1 µmol/l. All antagonists investigated failed to affect the evoked 3H-noradrenaline efflux when present in the absence of exogenous agonists.4.Arunlakshana-Schild plots were calculated for the antagonism between ethylketocyclazocine and a pair of stereoisomers, (-)-MR 2266 (20 nmol/l–5 µmol/l) and (+)-MR 2267 (0.3–10 µmol/l) at the presynaptic opioid receptor, and pA2 values were estimated. The isomeric affinity ratio was 60, with pA2 values of (-)-MR 2266, 9.06, and (+)-MR 2267, 7.28, respectively.5.The results show that the 3H-noradrenaline release can be inhibited via activation of presynaptic opioid receptors. Under the conditions presently investigated endogenous opioids do not modulate the evoked transmitter release. The results favour the idea that a single population (presumably of the K-subtype) of opioid receptors is present at guinea-pig atrial noradrenergic nerves.

Published
1986
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33. Gasification at Navy Bases.

Author

BECHTEL NATIONAL INC SAN FRANCISCO CA, McCone,A I, Ruby,J D, Mackewicz,W V, Miller,T D, Buder,M K, BECHTEL NATIONAL INC SAN FRANCISCO CA, McCone,A I, Ruby,J D, Mackewicz,W V, Miller,T D, and Buder,M K

Abstract

The work described in this report was performed under Contract N68305-77-C-0021 with the Civil Engineering Laboratory (CEL) at the Naval Construction Battalion Center at Port Hueneme, CA. The title of the contract was 'Coal Gasification Feasibility Study.' Coal gasification is recognized as a way to produce a clean burning boiler fuel from coal within acceptable environmental limits. The study was to assist the Navy in determining how coal might best be utilized, by comparing gasification with central direct coal-fired boiler systems at each of five bases. Bechtel showed in a previous study for CEL that gasification plants could be economically attractive at Navy bases. Gas from a plant producing 250 x 1,000,000 Btu/hr with a load factor of 90 percent was shown to have a lower life cycle cost than continued use of fuel oil. This second study examined plants as they would actually be operated. A conceptual design study comparing coal gasification with central direct coal-fired boilers at five bases was performed.

Published
1978

37. Gait asymmetry in glucocerebrosidase mutation carriers with Parkinson's disease.

Author

Gera A, O'Keefe JA, Ouyang B, Liu Y, Ruehl S, Buder M, Joyce J, Purcell N, and Pal G

Subjects
Case-Control Studies, Cognitive Dysfunction diagnosis, Cognitive Dysfunction etiology, Female, Heterozygote, Humans, Male, Middle Aged, Movement Disorders diagnosis, Parkinson Disease genetics, Range of Motion, Articular, Arm physiopathology, Gait physiology, Glucosylceramidase genetics, Movement Disorders etiology, Mutation, Parkinson Disease complications
Abstract

Background: GBA mutation carriers with PD (PD-GBA) are at higher risk of cognitive decline, but there is limited data regarding whether there are differences in gait dysfunction between GBA mutation and non-mutation carriers with PD., Objectives/methods: The primary aim of this study was to use quantitative inertial sensor-based gait analysis to compare gait asymmetry in 17 PD-GBA subjects, 17 non-mutation carriers with PD, and 15 healthy control subjects using parameters that had gait laterality and were markers of bradykinesia, in particular arm swing velocity and arm swing range of motion and stride length., Results: Arm swing velocity was more symmetric in PD-GBA subjects vs. non-mutation carriers in the OFF state (12.5 +/- 8.3 vs. 22.9 +/- 11.8%, respectively, p = 0.018). In the ON-medication state, non-mutation carriers with PD, but not PD-GBA subjects, exhibited arm swing velocity (16.8 +/- 8.6 vs. 22.9 +/- 11.8%, p = 0.006) and arm range of motion (26.7 +/- 16.3 vs. 33.4 +/- 18.6%, p = 0.02) that was more asymmetric compared with the OFF-medication state., Conclusions: In the OFF medication state, arm swing velocity asymmetry may be a useful parameter in helping to distinguish GBA mutation carriers with PD from non-mutation carriers., Competing Interests: The authors have declared that no competing interests exist.

Published
2020
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