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1. Large wood debris that clogged bridges followed by a sudden release. The 2019 flash flood in Catalonia.

Author

J.P. Martín-Vide, A. Bateman, M. Berenguer, C. Ferrer-Boix, A. Amengual, M. Campillo, C. Corral, M.C. Llasat, M. Llasat-Botija, S. Gómez-Dueñas, B. Marín-Esteve, F. Núñez-González, A. Prats-Puntí, R. Ruiz-Carulla, and R. Sosa-Pérez

Subjects
Flash flood, Large wood debris, Bridge hydraulics, Open-channel surge, Torrential flow, Physical geography, GB3-5030, Geology, QE1-996.5
Abstract

Study region: Francolí River (Catalonia, Iberian Peninsula). Study focus: The aim is the reconstruction of the October 2019 flash flood, that was documented through extensive field work: rainfall (300 mm in just a few hours), flood marks, times of flood passage and witnesses' snapshots and reports, channel changes, log drift (20,000 trees) and woody debris at bridges, as well as large damage and six fatalities. The methods are: hydrological model built for the rainfall-runoff in the basin and the flood routing in the river, use of hydraulic principles such as flow at waterfalls, flow against obstacles (trees), etc. and finally 1D/2D free surface numerical models. New hydrological insights: The uppermost 100 km2 produced discharges of 700 m3/s (up to 50 m3/s/km2, locally). Three bridges failed, but their cascading failure (when one failure triggers the next one downstream) was not proved. The main channel widened more than 10 times, dragging away soil and vegetation like a bulldozer. The resulting large wood debris that clogged two bridges worsened the inundation. An anomalous flow downstream, probably a surge of around 1090 m3/s, due to the failure of a woody jam at a narrow bridge, took two lives. Water Authority is now warning flood planners that vegetated, torrential basins may cause catastrophic floods in the valley towns, if their narrow bridges are sensitive to woody debris.

Published
2023
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2. HIP 41378 observed by CHEOPS: Where is planet d?

Author

Sulis, S., Borsato, L., Grouffal, S., Osborn, H. P., Santerne, A., Brandeker, A., Günther, M. N., Heitzmann, A., Lendl, M., Fridlund, M., Gandolfi, D., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C., Baumjohann, W., Beck, T., Benz, W., Bergomi, M., Billot, N., Bonfanti, A., Broeg, C., Cameron, A. Collier, van Damme, C. Corral, Correia, A. C. M., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., 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., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Steinberger, M., Szabó, M. Gy., Tuson, A., Udry, S., Ulmer-Moll, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., Wilson, T. G., Wolter, D., and Zingales, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, $P_\mathrm{d} = 278.36$ d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on $P_\mathrm{d}= 278.36$ d, but the observations show no transit. We find that large ($>22.4$ hours) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If $P_\mathrm{d} \neq 278.36$ d, the periods that minimize the eccentricity would be $101.22$ d and $371.14$ d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs., Comment: Accepted for publication in Astronomy and Astrophysics

Published
2024
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3. No random transits in CHEOPS observations of HD 139139

Author

Alonso, R., Hoyer, S., Deleuil, M., Simon, A. E., Beck, M., Benz, W., Florén, H. -G., Guterman, P., Borsato, L., Brandeker, A., Gandolfi, D., Wilson, T. G., Zingales, T., Alibert, Y., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, Ch., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Sz., Csizmadia, Cubillos, P. E., Davies, M. B., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D, Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Maxted, P. F. L., Mordasini, Ch., 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., Sousa, S. G., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van grootel, V., Venturini, J., Verrecchia, F., and Walton, N. A.

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

HD 139139 (a.k.a. 'The Random Transiter') is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events ($\sim$200 ppm -- equivalent to transiting objects with radii of $\sim$1.5 R$_\oplus$ in front of a Sun-like star), and their non-periodicity, constitutes a challenge for the photometric follow-up of this star. The goal of this study is to confirm with independent measurements the presence of shallow, non-periodic transit-like features on this object. We performed observations with CHEOPS, for a total accumulated time of 12.75 d, distributed in visits of roughly 20 h in two observing campaigns in years 2021 and 2022. The precision of the data is sufficient to detect 150 ppm features with durations longer than 1.5 h. We use the duration and times of the events seen in the K2 curve to estimate how many should have been detected in our campaigns, under the assumption that their behaviour during the CHEOPS observations would be the same as in the K2 data of 2017. We do not detect events with depths larger than 150 ppm in our data set. If the frequency, depth, and duration of the events were the same as in the K2 campaign, we estimate the probability of having missed all events due to our limited observing window would be 4.8 %. We suggest three different scenarios to explain our results: 1) Our observing window was not long enough, and the events were missed with the estimated 4.8 % probability. 2) The events recorded in the K2 observations were time critical, and the mechanism producing them was either not active in the 2021 and 2022 campaigns or created shallower events under our detectability level. 3) The enigmatic events in the K2 data are the result of an unidentified and infrequent instrumental noise in the original data set or its data treatment., Comment: 7 pages, 3 figures, accepted for publication in A&A. Language-corrected version

Published
2023
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4. Constraining the reflective properties of WASP-178b using Cheops photometry

Author

Pagano, I., Scandariato, G., Singh, V., Lendl, M., Queloz, D., Simon, A. E., Sousa, S. G., Brandeker, A., Cameron, A. Collier, Sulis, S., Van Grootel, V., Wilson, T. G., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bruno, G., Carone, L., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Reimers, C., Ribas, I., Rieder, M., Santos, N. C., Ségransan, D., Smith, A. M. S., Stalport, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Multiwavelength photometry of the secondary eclipses of extrasolar planets is able to disentangle the reflected and thermally emitted light radiated from the planetary dayside. This leads to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere, and the recirculation efficiency $\epsilon$, which quantifies the energy transport within the atmosphere. In this work we aim to measure $A_g$ and $\epsilon$ for the planet WASP-178 b, a highly irradiated giant planet with an estimated equilibrium temperature of 2450 K.} We analyzed archival spectra and the light curves collected by Cheops and Tess to characterize the host WASP-178, refine the ephemeris of the system and measure the eclipse depth in the passbands of the two respective telescopes. We measured a marginally significant eclipse depth of 70$\pm$40 ppm in the Tess passband and statistically significant depth of 70$\pm$20 ppm in the Cheops passband. Combining the eclipse depth measurement in the Cheops (lambda_eff=6300 AA) and Tess (lambda_eff=8000 AA) passbands we constrained the dayside brightness temperature of WASP-178 b in the 2250-2800 K interval. The geometric albedo 0.1<$\rm A_g$<0.35 is in general agreement with the picture of poorly reflective giant planets, while the recirculation efficiency $\epsilon>$0.7 makes WASP-178 b an interesting laboratory to test the current heat recirculation models., Comment: Accepted by Astronomy and Astrophysics on 31/08/2023

Published
2023

5. TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS

Author

Bonfanti, A., Gandolfi, D., Egger, J. A., Fossati, L., Cabrera, J., Krenn, A., Alibert, Y., Benz, W., Billot, N., Florén, H. -G., Lendl, M., Adibekyan, V., Salmon, S., Santos, N. C., Sousa, S. G., Wilson, T. G., Barragán, O., Cameron, A. Collier, Delrez, L., Esposito, M., Goffo, E., Osborne, H., Osborn, H. P., Serrano, L. M., Van Eylen, V., Alarcon, J., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Bedell, M., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Charnoz, S., Van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fridlund, M., Gillon, M., Güdel, M., Hoyer, S., Isaak, K. G., Kerschbaum, F., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lorenzo-Oliveira, D., Lovis, C., Magrin, D., Marafatto, L., Maxted, P. F. L., Meléndez, J., 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., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by $\sim$ 2$\sigma$. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope. We fit a skew normal (SN) function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo (MCMC) scheme to simultaneously detrend the light curves and the RV time series. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of $M_b=20.4_{-2.5}^{+2.6} M_{\oplus}$ ($\sim$12%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of $R_b=3.490_{-0.064}^{+0.070} R_{\oplus}$ ($\sim$1.9%). Our mass and radius measurements imply a mean density of $\rho_b=2.65_{-0.35}^{+0.37}$ g cm$^{-3}$ ($\sim$14%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of $0.41^{+0.34}_{-0.20}$ M$_\oplus$ and a thickness of $1.05^{+0.30}_{-0.29}$ R$_\oplus$., Comment: 13 pages, 6 figures, 5 tables. Accepted for publication in A&A

Published
2023
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6. 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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7. A full transit of $\nu^2$ Lupi d and the search for an exomoon in its Hill sphere with CHEOPS

Author

Ehrenreich, D., Delrez, L., Akinsanmi, B., Wilson, T. G., Bonfanti, A., Beck, M., Benz, W., Hoyer, S., Queloz, D., Alibert, Y., Charnoz, S., Cameron, A. Collier, Deline, A., Hooton, M., Lendl, M., Olofsson, G., Sousa, S. G., Adibekyan, V., Alonso, R., Anglada, G., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, T., Bekkelien, A., Bergomi, M., Billot, N., Bonfils, X., Brandeker, A., Broeg, C., Bárczy, T., Berta-Thompson, Z. K., Cabrera, J., Van Damme, C. Corral, Csizmadia, S., Davies, M. B., Deleuil, M., Demangeon, O., Demory, B. -O., Doty, J. P., Erikson, A., Fausnaugh, M. M., Florén, H. G., Fortier, A., Fossati, L., Fridlund, M., Futyan, D., Gandolfi, D., Gillon, M., Guterman, P., Güdel, M., Heng, K., Isaak, K. G., Jäckel, A., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Etangs, A. Lecavelier des, Levine, A. M., Lovis, C., Magrin, D., Maxted, P. F. L., Morgan, E. H., Nascimbeni, V., Osborn, H. P., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G. R., Salmon, S., Santos, N. C., Scandariato, G., Simon, A. E., Smith, A. M. S., Steinberger, M., Steller, M., Szabó, G. M., Ségransan, D., Shporer, A., Thomas, N., Tschentscher, M., Udry, S., Vanderspek, R., Van Grootel, V., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The planetary system around the naked-eye star $\nu^2$ Lupi (HD 136352; TOI-2011) is composed of three exoplanets with masses of 4.7, 11.2, and 8.6 Earth masses. The TESS and CHEOPS missions revealed that all three planets are transiting and have radii straddling the radius gap separating volatile-rich and volatile-poor super-earths. Only a partial transit of planet d had been covered so we re-observed an inferior conjunction of the long-period 8.6 Earth-mass exoplanet $\nu^2$ Lup d with the CHEOPS space telescope. We confirmed its transiting nature by covering its whole 9.1 h transit for the first time. We refined the planet transit ephemeris to P = 107.1361 (+0.0019/-0.0022) days and Tc = 2,459,009.7759 (+0.0101/-0.0096) BJD_TDB, improving by ~40 times on the previously reported transit timing uncertainty. This refined ephemeris will enable further follow-up of this outstanding long-period transiting planet to search for atmospheric signatures or explore the planet's Hill sphere in search for an exomoon. In fact, the CHEOPS observations also cover the transit of a large fraction of the planet's Hill sphere, which is as large as the Earth's, opening the tantalising possibility of catching transiting exomoons. We conducted a search for exomoon signals in this single-epoch light curve but found no conclusive photometric signature of additional transiting bodies larger than Mars. Yet, only a sustained follow-up of $\nu^2$ Lup d transits will warrant a comprehensive search for a moon around this outstanding exoplanet., Comment: 16 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics

Published
2023
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8. The geometric albedo of the hot Jupiter HD 189733b measured with CHEOPS

Author

Krenn, A. F., Lendl, M., Patel, J. A., Carone, L., Deleuil, M., Sulis, S., Cameron, A. Collier, Deline, A., Guterman, P., Queloz, D., Fossati, L., Brandeker, A., Heng, K., Akinsanmi, B., Adibekyan, V., Bonfanti, A., Demangeon, O. D. S., Kitzmann, D., Salmon, S., Sousa, S. G., Wilson, T. G., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Blecha, L., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Delrez, L., Demory, B. -O., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., 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., 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., Ulmer, B., Van Grootel, V., Venturini, J., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Measurements of the occultation of an exoplanet at visible wavelengths allow us to determine the reflective properties of a planetary atmosphere. The observed occultation depth can be translated into a geometric albedo. This in turn aids in characterising the structure and composition of an atmosphere by providing additional information on the wavelength-dependent reflective qualities of the aerosols in the atmosphere. Aims. Our aim is to provide a precise measurement of the geometric albedo of the gas giant HD 189733b by measuring the occultation depth in the broad optical bandpass of CHEOPS (350 - 1100 nm). Methods. We analysed 13 observations of the occultation of HD 189733b performed by CHEOPS utilising the Python package PyCHEOPS. The resulting occultation depth is then used to infer the geometric albedo accounting for the contribution of thermal emission from the planet. We also aid the analysis by refining the transit parameters combining observations made by the TESS and CHEOPS space telescopes. Results. We report the detection of an $24.7 \pm 4.5$ ppm occultation in the CHEOPS observations. This occultation depth corresponds to a geometric albedo of $0.076 \pm 0.016$. Our measurement is consistent with models assuming the atmosphere of the planet to be cloud-free at the scattering level and absorption in the CHEOPS band to be dominated by the resonant Na doublet. Taking into account previous optical-light occultation observations obtained with the Hubble Space Telescope, both measurements combined are consistent with a super-stellar Na elemental abundance in the dayside atmosphere of HD 189733b. We further constrain the planetary Bond albedo to between 0.013 and 0.42 at 3$\sigma$ confidence., Comment: 17 pages, 10 figures, accepted for publication in A&A

Published
2023
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9. Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

Author

Sulis, S., Lendl, M., Cegla, H., Diaz, L. F. Rodriguez, Bigot, L., Van Grootel, V., Bekkelien, A., Cameron, A. Collier, Maxted, P. F. L., Simon, A. E., Lovis, C., Scandariato, G., Bruno, G., Nardiello, D., Bonfanti, A., Fridlund, M., Persson, C. M., Salmon, S., Sousa, S. G., Wilson, T. G., Krenn, A., Hoyer, S., Santerne, A., Ehrenreich, D., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Cabrera, J., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fortier, A., Fossati, L., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, 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., Rieder, M., Santos, N. C., Ségransan, D., Smith, A. M. S., Steinberger, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Walton, N. A., and Wolter, D.

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

Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. In this study, we aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. For the first time, we observed two bright stars (Teff = 5833 K and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise dependent variations. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process., Comment: Accepted to A&A, 30 pages, 21 figures, 10 tables (one online)

Published
2022
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10. CHEOPS finds KELT-1b darker than expected in visible light: Discrepancy between the CHEOPS and TESS eclipse depths

Author

Parviainen, H., Wilson, T. G., Lendl, M., Kitzmann, D., Pallé, E., Serrano, L. M., Valdes, E. Meier, Benz, W., Deline, A., Ehrenreich, D., Guterman, P., Heng, K., Demangeon, O. D. S., Bonfanti, A., Salmon, S., Singh, V., Santos, N. C., Sousa, S. G., 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., Brandeker, A., Broeg, C., Cabrera, J., Charnoz, S., Cameron, A. Collier, Van Damme, C. Corral, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demory, B. -O., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Mecina, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoi, R., Rando, N., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., VanGrootel, V., and Walton, N. A.

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

Recent TESS-based studies have suggested that the dayside of KELT-1b, a strongly-irradiated brown dwarf, is significantly brighter in visible light than what would be expected based on Spitzer observations in infrared. We observe eight eclipses of KELT-1b with CHEOPS (CHaracterising ExOPlanet Satellite) to measure its dayside brightness temperature in the bluest passband observed so far, and model the CHEOPS photometry jointly with the existing optical and NIR photometry from TESS, LBT, CFHT, and Spitzer. Our modelling leads to a self-consistent dayside spectrum for KELT-1b covering the CHEOPS, TESS, H , Ks, and Spitzer IRAC 3.6 and 4.5 ${\mu}$m bands, where our TESS, H , Ks, and Spitzer band estimates largely agree with the previous studies, but we discover a strong discrepancy between the CHEOPS and TESS bands. The CHEOPS observations yield a higher photometric precision than the TESS observations, but do not show a significant eclipse signal, while a deep eclipse is detected in the TESS band. The derived TESS geometric albedo of $0.36^{+0.12}_{-0.13}$ is difficult to reconcile with a CHEOPS geometric albedo that is consistent with zero because the two passbands have considerable overlap. Variability in cloud cover caused by the transport of transient nightside clouds to the dayside could provide an explanation for reconciling the TESS and CHEOPS geometric albedos, but this hypothesis needs to be tested by future observations., Comment: Accepted to A&A

Published
2022
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11. 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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12. CHEOPS geometric albedo of the hot Jupiter HD 209458b

Author

Brandeker, A., Heng, K., Lendl, M., Patel, J. A., Morris, B. M., Broeg, C., Guterman, P., Beck, M., Maxted, P. F. L., Demangeon, O., Delrez, L., Demory, B. -O., Kitzmann, D., Santos, N. C., Singh, V., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Bruno, G., Cabrera, J., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Hoyer, S., Isaak, K. G., Kiss, L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., 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., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Grootel, V., Walton, N., and Wolter, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the detection of the secondary eclipse of the hot Jupiter HD 209458b in optical/visible light using the CHEOPS space telescope. Our measurement of 20.4 +/- 3.3 ppm translates into a geometric albedo of A_g = 0.096 +/- 0.016. The previously estimated dayside temperature of about 1500 K implies that our geometric albedo measurement consists predominantly of reflected starlight and is largely uncontaminated by thermal emission. This makes the present result one of the most robust measurements of A_g for any exoplanet. Our calculations of the bandpass-integrated geometric albedo demonstrate that the measured value of A_g is consistent with a cloud-free atmosphere, where starlight is reflected via Rayleigh scattering by hydrogen molecules, and the water and sodium abundances are consistent with stellar metallicity. We predict that the bandpass-integrated TESS geometric albedo is too faint to detect and that a phase curve of HD 209458b observed by CHEOPS would have a distinct shape associated with Rayleigh scattering if the atmosphere is indeed cloud free., Comment: 9 pages, accepted by A&A Letters

Published
2022
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13. 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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14. Analysis of Early Science observations with the CHaracterising ExOPlanets Satellite (CHEOPS) using pycheops

Author

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

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

CHEOPS(CHaracterising ExOPlanet Satellite) is an ESA S-class mission that observes bright stars at high cadence from low-Earth orbit. The main aim of the mission is to characterize exoplanets that transit nearby stars using ultrahigh precision photometry. Here we report the analysis of transits observed by CHEOPS during its Early Science observing programme for four well-known exoplanets: GJ436b, HD106315b, HD97658b and GJ1132b. The analysis is done using pycheops, an open-source software package we have developed to easily and efficiently analyse CHEOPS light curve data using state-of-the-art techniques that are fully described herein. We show that the precision of the transit parameters measured using CHEOPS is comparable to that from larger space telescopes such as Spitzer Space Telescope and Kepler. We use the updated planet parameters from our analysis to derive new constraints on the internal structure of these four exoplanets., Comment: This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review

Published
2021
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15. The changing face of AU Mic b: stellar spots, spin-orbit commensurability, and Transit Timing Variations as seen by CHEOPS and TESS

Author

Szabó, Gy. M., Gandolfi, D., Brandeker, A., Csizmadia, Sz., Garai, Z., Billot, N., Broeg, C., Ehrenreich, D., Fortier, A., Fossati, L., Hoyer, S., Kiss, L., Etangs, A. Lecavelier des, Maxted, P. F. L., Ribas, I., Alibert, Y., Alonso, R., Escudé, G. Anglada, Bárczy, T., Barros, S. C. C., Barrado, D., Baumjohann, W., Beck, M., Beck, T., Bekkelien, A., Bonfils, X., Benz, W., Borsato, L., Busch, M-D., Cabrera, J., Charnoz, S., Cameron, A. Collier, Van Damme, C. Corral, Davies, M. B., Delrez, L., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fridlund, M., Futyan, D., Muñoz, A. García, Gillon, M., Guedel, M., Guterman, P., Heng, K., Isaak, K. G., Lacedelli, G., Laskar, J., Lend, M., Lovis, C., Luntzer, A., Magrin, D., Nascimbeni, V., Olofsson, G., Osborn, H. P., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Santos, N. C., Scandariato, G., Ségransan, D., Serrano, L. M., Sicilia, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Thomas, N., Udry, S., Van Grootel, V., Walton, N. A., and Wilson, T. G.

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

AU Mic is a young planetary system with a resolved debris disc showing signs of planet formation and two transiting warm Neptunes near mean-motion resonances. Here we analyse three transits of AU Mic b observed with the CHaracterising ExOPlanet Satellite (CHEOPS), supplemented with sector 1 and 27 Transiting Exoplanet Survey Satellite (TESS) photometry, and the All-Sky Automated Survey (ASAS) from the ground. The refined orbital period of AU Mic b is 8.462995 \pm 0.000003 d, whereas the stellar rotational period is P_{rot}=4.8367 \pm 0.0006 d. The two periods indicate a 7:4 spin--orbit commensurability at a precision of 0.1%. Therefore, all transits are observed in front of one of the four possible stellar central longitudes. This is strongly supported by the observation that the same complex star-spot pattern is seen in the second and third CHEOPS visits that were separated by four orbits (and seven stellar rotations). Using a bootstrap analysis we find that flares and star spots reduce the accuracy of transit parameters by up to 10% in the planet-to-star radius ratio and the accuracy on transit time by 3-4 minutes. Nevertheless, occulted stellar spot features independently confirm the presence of transit timing variations (TTVs) with an amplitude of at least 4 minutes. We find that the outer companion, AU Mic c may cause the observed TTVs., Comment: 16 pages, 11 figures, 7 tables; accepted by Astronomy and Astrophysics

Published
2021
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17. 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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18. 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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19. 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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21. The Large Observatory For x-ray Timing

Author

Feroci, M., Herder, J. W. den, Bozzo, E., Barret, D., Brandt, S., Hernanz, M., van der Klis, M., Pohl, M., Santangelo, A., Stella, L., Watts, A., Wilms, J., Zane, S., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J. -L., Azzarello, P., Bakala, P., Baldazzi, G., Balman, S., Barbera, M., van Baren, C., Bhattacharyya, S., Baykal, A., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bodin, P., Bombaci, I., Bidaud, J. -M. Bonnet, Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz-Jørgensen, C., Cackett, E., Cadoux, F. R., Cais, P., Caliandro, G. A., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro-Tirado, A. J., Cavazzuti, E., Cerda-Duran, P., Chakrabarty, D., Château, F., Chenevez, J., Coker, J., Cole, R., Collura, A., Cornelisse, R., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Aì, A., D'Elia, V., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Diebold, S., Di Salvo, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Erkut, M. H., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Finger, M. H., Fraser, G. W., Frericks, M., Fuschino, F., Gabler, M., Galloway, D. K., Sanchez, J. L. Galvez, Garcia-Berro, E., Gendre, B., Gezari, S., Giles, A. B., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Gschwender, M., Gualtieri, L., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hansen, F., Hartmann, D. H., Haswell, C. A., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., Zand, J. J. M. in't, Israel, G., Iwasawa, K., Izzo, L., Jacobs, H. M., Jetter, F., Johannsen, T., Jonker, P., Josè, J., Kaaret, P., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Kokkotas, K., Korpela, S., Kouveliotou, C., Kreykenbohm, I., Kuiper, L. M., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F. K., Laubert, P. P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T. J., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Mandel, I., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., McHardy, I. M., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M. C., Miller, J. M., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz-Darias, T., Negueruela, I., Neilsen, J., Norton, A. J., Nowak, M., O'Brien, P., Olsen, P. E. H., Orienti, M., Orio, M., Orlandini, M., Orleanski, P., Osborne, J. P., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J. M., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A. V., Perez, M. A., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Poutanen, J., Prakash, M., Provost, P. Le, Psaltis, D., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rachevski, A., Rashevskaya, I., Ray, P. S., Rea, N., Reddy, S., Reig, P., Aranda, M. Reina, Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Gil, P. Rodríguez, Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E. M. R., Rozanska, A., Rousseau, A., Ryde, F., Sabau-Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Sandberg, J., Scaringi, S., Schanne, S., Schee, J., Schmid, C., Shore, S., Schneider, R., Schwenk, A., Schwope, A. D., Seyler, J. -Y., Shearer, A., Smith, A., Smith, D. M., Smith, P. J., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A. W., Stergioulas, N., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J. M., Torres, D. F., Tramacere, A., Trois, A., Turolla, R., Turriziani, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vrba, V., Walton, D., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson-Hodge, C. A., Winter, B., Wood, K., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zhang, B., Zwart, F., Ayre, M., Boenke, T., van Damme, C. Corral, Kuulkers, E., and Lumb, D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study., Comment: Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T

Published
2014
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22. Eupatilin Improves Cilia Defects in Human CEP290 Ciliopathy Models

Author

Julio C. Corral-Serrano, Paul E. Sladen, Daniele Ottaviani, Olivia F. Rezek, Dimitra Athanasiou, Katarina Jovanovic, Jacqueline van der Spuy, Brian C. Mansfield, and Michael E. Cheetham

Subjects
CEP290, Leber congenital amaurosis (LCA), retina, ciliopathy, photoreceptor, cilium, Cytology, QH573-671
Abstract

The photoreceptor outer segment is a highly specialized primary cilium that is essential for phototransduction and vision. Biallelic pathogenic variants in the cilia-associated gene CEP290 cause non-syndromic Leber congenital amaurosis 10 (LCA10) and syndromic diseases, where the retina is also affected. While RNA antisense oligonucleotides and gene editing are potential treatment options for the common deep intronic variant c.2991+1655A>G in CEP290, there is a need for variant-independent approaches that could be applied to a broader spectrum of ciliopathies. Here, we generated several distinct human models of CEP290-related retinal disease and investigated the effects of the flavonoid eupatilin as a potential treatment. Eupatilin improved cilium formation and length in CEP290 LCA10 patient-derived fibroblasts, in gene-edited CEP290 knockout (CEP290 KO) RPE1 cells, and in both CEP290 LCA10 and CEP290 KO iPSCs-derived retinal organoids. Furthermore, eupatilin reduced rhodopsin retention in the outer nuclear layer of CEP290 LCA10 retinal organoids. Eupatilin altered gene transcription in retinal organoids by modulating the expression of rhodopsin and by targeting cilia and synaptic plasticity pathways. This work sheds light on the mechanism of action of eupatilin and supports its potential as a variant-independent approach for CEP290-associated ciliopathies.

Published
2023
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24. Síndromes motores

Author

J. Roa Escobar, A. García Leal, C. Corral Quereda, C. Estebas Armas, E. Mariño Trillo, R. García Yu, R. González Sarmiento, and M. Hernández Barral

Subjects
General Medicine
Published
2023
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28. Building a Synthetic Task Environment to Support Artificial Social Intelligence Research

Author

Nancy J. Cooke, Keerthi Shrikar Tatapudi, Christopher C. Corral, Lixiao Huang, and Verica Buchanan

Subjects
Medical Terminology, Social intelligence, Human–computer interaction, Psychology, Medical Assisting and Transcription, Task (project management)
Abstract

To support research on artificial social intelligence for successful teams (ASIST), an urban search and rescue task (USAR) was simulated within Minecraft to serve as a Synthetic Task Environment (STE). The goal for the development of the present STE was to create an environment that provides ample opportunities to allow ASI agents to demonstrate the theory of mind by making inferences and predictions of humans’ states and actions in the USAR task environment, and in the future to intervene to improve teamwork in real-time. This paper describes the STE design background, design potentials and considerations, rich data collection opportunities, and potential usage for more broad research.

Published
2021
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29. Remote research methods for Human–AI–Robot Teaming

Author

Nancy J. Cooke, Craig J. Johnson, Jimin Kim, Anagha Mudigonda, Glenn J. Lematta, Eric Holder, Akuadasuo Ezenyilimba, Margaret E. Wong, Verica Buchanan, Christopher C. Corral, Erin K. Chiou, Manuel Baeriswyl, and Federico Scholcover

Subjects
Coronavirus disease 2019 (COVID-19), Computer science, media_common.quotation_subject, Severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2), Human Factors and Ergonomics, Onboarding, Industrial and Manufacturing Engineering, Task (project management), Human–computer interaction, Pandemic, Robot, Confidentiality, Function (engineering), media_common
Abstract

This study focuses on methodological adaptations and considerations for remote research on Human-AI-Robot Teaming (HART) amidst the COVID-19 pandemic. Themes and effective remote research methods were explored. Central issues in remote research were identified, such as challenges in attending to participants' experiences, coordinating experimenter teams remotely, and protecting privacy and confidentiality. Instances of experimental design overcoming these challenges were identified in methods for recruitment and onboarding, training, team task scenarios, and measurement. Three case studies are presented in which interactive in-person testbeds for HART were rapidly redesigned to function remotely. Although COVID-19 may have temporarily constrained experimental design, future HART studies may adopt remote research methods to expand the research toolkit.

Published
2021
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31. A look into retinal organoids: methods, analytical techniques, and applications

Author

Ronald Roepman, Julio C. Corral-Serrano, Alejandro Garanto, Rob W.J. Collin, Michael E. Cheetham, and Tess A. V. Afanasyeva

Subjects
Organoid, Inherited, Cell type, Induced Pluripotent Stem Cells, Omics, Review, Biology, Retinal ganglion, Retina, Sensory disorders Donders Center for Medical Neuroscience [Radboudumc 12], 03 medical and health sciences, Cellular and Molecular Neuroscience, chemistry.chemical_compound, 0302 clinical medicine, Retinal Diseases, Retinal Rod Photoreceptor Cells, medicine, Animals, Humans, Induced pluripotent stem cell, Molecular Biology, 030304 developmental biology, Pharmacology, 0303 health sciences, Retinal, Cell Differentiation, Metabolic Disorders Radboud Institute for Molecular Life Sciences [Radboudumc 6], Cell Biology, 3. Good health, Organoids, medicine.anatomical_structure, Renal disorders Radboud Institute for Molecular Life Sciences [Radboudumc 11], chemistry, Degeneration, Molecular Medicine, Therapy, sense organs, Cellular model, Neuroscience, Muller glia, Neuroglia, 030217 neurology & neurosurgery
Abstract

Contains fulltext : 243899.pdf (Publisher’s version ) (Open Access) Inherited retinal diseases (IRDs) cause progressive loss of light-sensitive photoreceptors in the eye and can lead to blindness. Gene-based therapies for IRDs have shown remarkable progress in the past decade, but the vast majority of forms remain untreatable. In the era of personalised medicine, induced pluripotent stem cells (iPSCs) emerge as a valuable system for cell replacement and to model IRD because they retain the specific patient genome and can differentiate into any adult cell type. Three-dimensional (3D) iPSCs-derived retina-like tissue called retinal organoid contains all major retina-specific cell types: amacrine, bipolar, horizontal, retinal ganglion cells, Müller glia, as well as rod and cone photoreceptors. Here, we describe the main applications of retinal organoids and provide a comprehensive overview of the state-of-art analysis methods that apply to this model system. Finally, we will discuss the outlook for improvements that would bring the cellular model a step closer to become an established system in research and treatment development of IRDs.

Published
2021

32. 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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34. PCARE and WASF3 regulate ciliary F-actin assembly that is required for the initiation of photoreceptor outer segment disk formation

Author

Max D van Essen, Rossano Butcher, Marius Ueffing, Adem Yildirim, Rob W.J. Collin, Qin Liu, Lonneke Duijkers, Krzysztof Palczewski, Anita D M. Hoogendoorn, Nikoleta Argyrou, Sylvia E. C. van Beersum, Alejandro Garanto, Uwe Wolfrum, Julio C. Corral-Serrano, Karsten Boldt, Ronald Roepman, Renate A A Ruigrok, Ideke J.C. Lamers, Stef J.F. Letteboer, Jeroen van Reeuwijk, Sanae Sakami, and Michael E. Cheetham

Subjects
cilium, macromolecular substances, Sensory disorders Donders Center for Medical Neuroscience [Radboudumc 12], Actin-Related Protein 2-3 Complex, chemistry.chemical_compound, Mice, All institutes and research themes of the Radboud University Medical Center, retinitis pigmentosa, Retinitis pigmentosa, medicine, Genetics, Animals, Humans, Cilia, RNA, Small Interfering, Ciliary tip, Eye Proteins, Ciliary membrane, Actin, Mice, Knockout, Multidisciplinary, Cilium, outer segments, Retinal, Biological Sciences, medicine.disease, Rod Cell Outer Segment, Photoreceptor outer segment, photoreceptor, Actins, Cell biology, Wiskott-Aldrich Syndrome Protein Family, Disease Models, Animal, Renal disorders Radboud Institute for Molecular Life Sciences [Radboudumc 11], chemistry, PNAS Plus, Gene Expression Regulation, Retinal Cone Photoreceptor Cells, sense organs, actin, Cone-Rod Dystrophies, Visual phototransduction
Abstract

Significance The photoreceptor outer segments are primary cilia, modified for phototransduction by incorporation of stacked opsin-loaded membrane disks that are continuously regenerated. This process is disrupted in several types of inherited retinal dystrophy, but the driving force remained unclear. We show that C2orf71/PCARE (photoreceptor cilium actin regulator), associated with inherited retinal dystrophy subtype RP54, efficiently recruits the Arp2/3 complex activator WASF3 to the cilium. This activates an actin dynamics-driven expansion of the ciliary tip, resembling membrane evagination in lamellipodia formation. Colocalization of this actin dynamics module to the base of the outer segments, and absence thereof in Pcare−/− mice, suggests PCARE-regulated actin dynamics as a critical process in outer segment disk formation., The outer segments (OS) of rod and cone photoreceptor cells are specialized sensory cilia that contain hundreds of opsin-loaded stacked membrane disks that enable phototransduction. The biogenesis of these disks is initiated at the OS base, but the driving force has been debated. Here, we studied the function of the protein encoded by the photoreceptor-specific gene C2orf71, which is mutated in inherited retinal dystrophy (RP54). We demonstrate that C2orf71/PCARE (photoreceptor cilium actin regulator) can interact with the Arp2/3 complex activator WASF3, and efficiently recruits it to the primary cilium. Ectopic coexpression of PCARE and WASF3 in ciliated cells results in the remarkable expansion of the ciliary tip. This process was disrupted by small interfering RNA (siRNA)-based down-regulation of an actin regulator, by pharmacological inhibition of actin polymerization, and by the expression of PCARE harboring a retinal dystrophy-associated missense mutation. Using human retinal organoids and mouse retina, we observed that a similar actin dynamics-driven process is operational at the base of the photoreceptor OS where the PCARE module and actin colocalize, but which is abrogated in Pcare−/− mice. The observation that several proteins involved in retinal ciliopathies are translocated to these expansions renders it a potential common denominator in the pathomechanisms of these hereditary disorders. Together, our work suggests that PCARE is an actin-associated protein that interacts with WASF3 to regulate the actin-driven expansion of the ciliary membrane at the initiation of new outer segment disk formation.

Published
2020

35. Structural Variants Create New Topological-Associated Domains and Ectopic Retinal Enhancer-Gene Contact in Dominant Retinitis Pigmentosa

Author

Michel Michaelides, Michael E. Cheetham, Marco Aben, Alison J. Hardcastle, Hannie Kremer, Daniele Ottaviani, Stefan Mundlos, Graeme C.M. Black, Susan M Downes, Robert K. Koenekoop, Julio C. Corral-Serrano, Jordi Corominas, Gavin Arno, Andrew R. Webster, Claire E. L. Smith, Uirá Souto Melo, Carlo Rivolta, Suzanne E. de Bruijn, Chris F. Inglehearn, Raj Ramesar, L. Ingeborgh van den Born, Susanne Roosing, Christian Gilissen, Nikolas Pontikos, Musa M. Mhlanga, Jacquie Greenberg, F. Lucy Raymond, Frans P.M. Cremers, Alessia Fiorentino, Timo W. F. Mulders, Stephanie Fanucchi, Silvia Albert, Simon Mead, Lisa Roberts, Michalis Georgiou, George Rebello, Carel B. Hoyng, and Repositório da Universidade de Lisboa

Subjects
Male, Gene Expression, Enhancer RNAs, Stem cells, Sensory disorders Donders Center for Medical Neuroscience [Radboudumc 12], Cohort Studies, chemistry.chemical_compound, Hi-C, Induced pluripotent stem cell, Child, Genetics (clinical), Genes, Dominant, 0303 health sciences, Genome, 030305 genetics & heredity, Chromosome Mapping, Nuclear Proteins, Cell Differentiation, Metabolic Disorders Radboud Institute for Molecular Life Sciences [Radboudumc 6], Cellular Reprogramming, Cell biology, Organoids, Enhancer Elements, Genetic, Ectopic expression, Retinal Cone Photoreceptor Cells, Photoreceptor precursors cells, Female, Dominant retinitis pigmentosa, Topologically associated domains, Retinitis Pigmentosa, Human, dominant retinitis pigmentosa, ectopic expression, GDPD, photoreceptor precursors cells, retinal organoids, RP17, stem cells, structural variants, topologically associated domains, whole-genome sequencing, Adult, Amino Acid Sequence, Chromosomes, Human, Pair 17, Fibroblasts, Genome, Human, Humans, Induced Pluripotent Stem Cells, Phosphoric Diester Hydrolases, Polymorphism, Genetic, Primary Cell Culture, Transcription Factors, Whole Genome Sequencing, Enhancer Elements, Biology, Chromosomes, Article, 03 medical and health sciences, Genetic, Retinitis pigmentosa, Genetics, medicine, Dominant, Polymorphism, Enhancer, Gene, Transcription factor, 030304 developmental biology, Whole-genome sequencing, Pair 17, Retinal organoids, Retinal, Cell Biology, medicine.disease, chemistry, Genes, Structural variants
Abstract

© 2020 The Authors. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/), The cause of autosomal-dominant retinitis pigmentosa (adRP), which leads to loss of vision and blindness, was investigated in families lacking a molecular diagnosis. A refined locus for adRP on Chr17q22 (RP17) was delineated through genotyping and genome sequencing, leading to the identification of structural variants (SVs) that segregate with disease. Eight different complex SVs were characterized in 22 adRP-affected families with >300 affected individuals. All RP17 SVs had breakpoints within a genomic region spanning YPEL2 to LINC01476. To investigate the mechanism of disease, we reprogrammed fibroblasts from affected individuals and controls into induced pluripotent stem cells (iPSCs) and differentiated them into photoreceptor precursor cells (PPCs) or retinal organoids (ROs). Hi-C was performed on ROs, and differential expression of regional genes and a retinal enhancer RNA at this locus was assessed by qPCR. The epigenetic landscape of the region, and Hi-C RO data, showed that YPEL2 sits within its own topologically associating domain (TAD), rich in enhancers with binding sites for retinal transcription factors. The Hi-C map of RP17 ROs revealed creation of a neo-TAD with ectopic contacts between GDPD1 and retinal enhancers, and modeling of all RP17 SVs was consistent with neo-TADs leading to ectopic retinal-specific enhancer-GDPD1 accessibility. qPCR confirmed increased expression of GDPD1 and increased expression of the retinal enhancer that enters the neo-TAD. Altered TAD structure resulting in increased retinal expression of GDPD1 is the likely convergent mechanism of disease, consistent with a dominant gain of function. Our study highlights the importance of SVs as a genomic mechanism in unsolved Mendelian diseases.

Published
2020

37. Leptin protects against the development and expression of cocaine addiction-like behavior in heterogenous stock rats

Author

G. de Guglielmo, Kokila Shankar, Sierra Simpson, Lisa Maturin, C. Ortez, Abraham A. Palmer, Brent Boomhower, C. Crook, Olivier George, Leah Solberg-Woods, Lieselot L. G. Carrette, Molly Brennan, and C. Corral

Subjects
medicine.medical_specialty, Protracted abstinence, business.industry, Addiction, media_common.quotation_subject, Leptin, Causal effect, Protective factor, Small sample, Endocrinology, Internal medicine, Cohort, Medicine, business, Hormone, media_common
Abstract

In addition to its pleasurable effects, weight control is a significant contributor to initiation, maintenance and relapse of cocaine use. This suggests that individual differences in bodyweight control and feeding hormones, such as leptin may contribute to the vulnerability to cocaine use disorder. While pre-clinical studies have shown a mutually inhibitory relationship between leptin and cocaine, they have used small sample sizes and did not investigate individual differences in a large heterogeneous population. Here, we tested if individual differences in bodyweight and blood leptin level is associated with high or low vulnerability to addiction-like behaviors using data from 500 heterogenous stock rats and 160 blood samples from the Cocaine Biobank, using a model of extended access to intravenous self-administration of cocaine. Finally, we tested a separate cohort to evaluate the causal effect of exogenous leptin administration on cocaine seeking. Bodyweight, while changing due to cocaine self-administration in males, was not related to the vulnerability to addiction-like behavior. Blood leptin levels after ~6 weeks of cocaine self-administration did not correlate with addiction-like behaviors, however, baseline blood leptin levels before any access to cocaine negatively predicted addiction-like behavior. Finally, administration of leptin reduced cocaine intake after acute withdrawal and cocaine seeking after 6 weeks of protracted abstinence. These results demonstrate that high blood leptin level before access to cocaine may be a protective factor against the development of cocaine addiction-like behavior, that exogenous leptin reduces the motivation to take and seek cocaine, but that blood leptin level and bodyweight changes in current users are not good biomarkers for addiction-like behaviors.

Published
2021
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38. The changing face of AU Mic b: stellar spots, spin-orbit commensurability, and transit timing variations as seen by CHEOPS and TESS

Author

Szabó, Gy. M., primary, Gandolfi, D., additional, Brandeker, A., additional, Csizmadia, Sz., additional, Garai, Z., additional, Billot, N., additional, Broeg, C., additional, Ehrenreich, D., additional, Fortier, A., additional, Fossati, L., additional, Hoyer, S., additional, Kiss, L., additional, des Etangs, A. Lecavelier, additional, Maxted, P. F. L., additional, Ribas, I., additional, Alibert, Y., additional, Alonso, R., additional, Anglada Escudé, G., additional, Bárczy, T., additional, Barros, S. C. C., additional, Barrado, D., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Bekkelien, A., additional, Bonfils, X., additional, Benz, W., additional, Borsato, L., additional, Busch, M-D., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Van Damme, C. Corral, additional, Davies, M. B., additional, Delrez, L., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Erikson, A., additional, Fridlund, M., additional, Futyan, D., additional, García Muñoz, A., additional, Gillon, M., additional, Guedel, M., additional, Guterman, P., additional, Heng, K., additional, Isaak, K. G., additional, Lacedelli, G., additional, Laskar, J., additional, Lendl, M., additional, Lovis, C., additional, Luntzer, A., additional, Magrin, D., additional, Nascimbeni, V., additional, Olofsson, G., additional, Osborn, H. P., 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, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Serrano, L. M., additional, Sicilia, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Steller, M., additional, Thomas, N., additional, Udry, S., additional, Van Grootel, V., additional, Walton, N. A., additional, and Wilson, T. G., additional

Published
2021
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39. Adult Colloid Milium

Author

M, Macedo-Pérez, A V, Delgado-Gaytán, P, Fernández-Rueda, and J C, Corral-Chávez

Published
2021

40. Síndromes topográficos del cerebro, cerebelo y troncoencéfalo

Author

Castro, J. García, Leal, A. García, Bravo, A. Mena, Quereda, C. Corral, Armas, C. Estebas, López, J. Granja, Serrano, M. Aledo, Yu, R. García, and Montes, Á. Martín

Abstract

La concepción clásica de la semiología neurológica ha relacionado cada región cerebral con una función determinada, permitiendo un diagnóstico topográfico basado en la anamnesis y la exploración. Las más recientes técnicas de neuroimagen funcional han demostrado mecanismos algo más complejos, otorgando un papel predominante a las redes neuronales establecidas entre diversas regiones cerebrales como las principales generadoras de las diferentes funciones. A pesar de ello, el conocimiento de los síndromes topográficos del cerebro, cerebelo y troncoencéfalo sigue siendo fundamental en la aproximación inicial al diagnóstico topográfico y etiológico de los pacientes con síntomas neurológicos. Así, la afectación de la primera motoneurona debe hacer sospechar una lesión en el lóbulo frontal contralateral, la afectación sensitiva debe orientar a una afectación parietal contralateral, la afasia motora a una lesión en el lóbulo frontal dominante, la sensitiva a una en el temporal dominante o los síndromes cruzados a una afectación troncoencefálica.

Published
2023
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41. Síndromes motores

Author

Escobar, J. Roa, Leal, A. García, Quereda, C. Corral, Armas, C. Estebas, Trillo, E. Mariño, Yu, R. García, Sarmiento, R. González, and Barral, M. Hernández

Abstract

El sistema motor tiene su origen en las motoneuronas (primera motoneurona) de la circunvolución precentral del lóbulo frontal (corteza motora primaria, área 4 de Brodmann) y en áreas corticales adyacentes. Los axones de estas células constituyen la vía piramidal que desciende por la corona radiada, cápsula interna y pedúnculos cerebrales. En el tronco del encéfalo, parte de estas fibras motoras sinaptan con los núcleos motores troncoencefálicos. El resto continúan descendiendo por el tronco del encéfalo, se decusan a nivel de las pirámides bulbares y bajan por la médula espinal hasta el asta anterior donde hacen sinapsis con la segunda motoneurona. Los axones de las segundas motoneuronas pasan por las raíces anteriores, plexos nerviosos y nervios periféricos hasta llegar al músculo esquelético. Los impulsos se transmiten a las células musculares a través de las placas terminales motoras de la unión neuromuscular. Las lesiones de la primera motoneurona producen paresia espástica e hiperreflexia; las lesiones de la segunda motoneurona producen paresia flácida e hiporreflexia y las lesiones del nervio periférico producen paresia flácida asociando frecuentemente alteración sensitiva. La fatigabilidad es característica de alteraciones de la unión neuromuscular y las miopatías generan debilidad muscular, atrofia y mialgias.

Published
2023
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42. Six transiting planets and a chain of Laplace resonances in TOI-178

Author

A. Leleu, Nathan Hara, Rosanna H. Tilbrook, Matthew J. Hooton, Jack S. Acton, Giuseppina Micela, Heike Rauer, Francisco J. Pozuelos, Xavier Dumusque, Michael R. Goad, T. Bárczy, Andrew Collier Cameron, Francesco Pepe, G. Lo Curto, Rafael Rebolo, Juan Cabrera, Pedro Figueira, M. Buder, Willy Benz, Romain Allart, Oliver Turner, Enric Palle, Alexis M. S. Smith, Ignasi Ribas, F. Ratti, M. Steller, Richard G. West, James McCormac, A. Lecavelier des Etangs, Alexandre C. M. Correia, Daniel Sebastian, S. G. Sousa, Emmanuel Jehin, Mathias Beck, J. Schneider, François Bouchy, Baptiste Lavie, J.-B. Delisle, Liam Raynard, Roberto Ragazzoni, K. Lam, H. Venus, Kate Gudrun Isaak, Roi Alonso, C. Murray, Laetitia Delrez, Martti H. Kristiansen, Mario Damasso, A. Bonfanti, David Ehrenreich, Stéphane Udry, Samuel Gill, Sergio Hoyer, Lionel Garcia, V. Adibekyan, Carina M. Persson, Maximiliano Moyano, Beth A. Henderson, Giampaolo Piotto, Andrés Jordán, Samantha Thompson, Alexis Brandeker, Elsa Ducrot, Daniel Angerhausen, Nuno C. Santos, David Barrado, Xavier Bonfils, Vincent Bourrier, F. Verrecchia, Monika Lendl, Andrea Mehner, C. Broeg, M. R. Zapatero Osorio, Matthew R. Burleigh, D. Futyan, Damien Ségransan, Amaury H. M. J. Triaud, Mahmoudreza Oshagh, C. Allende Prieto, J. Asquier, B. O. Demory, Philippe Robutel, C. Corral Van Damme, Nicola Rando, Malcolm Fridlund, Gisbert Peter, Roland Ottensamer, Alessandro Sozzetti, Paolo Molaro, James S. Jenkins, Melvyn B. Davies, Jorge Lillo-Box, S. Chamberlain, Thomas Beck, P. Di Marcantonio, Carlos Martins, Maximilian N. Günther, Daniel Bayliss, Jacques Laskar, Peter J. Wheatley, P. P. Pedersen, Nicolas Thomas, Nicholas A. Walton, Göran Olofsson, Marko Sestovic, David R. Anderson, Artem Burdanov, Kevin Heng, Manuel Guedel, Jose I. Vines, A. García Muñoz, Edward Gillen, Valérie Van Grootel, T. G. Wilson, Michaël Gillon, Olivier Demangeon, D. Wolter, Demetrio Magrin, G. Polenta, G. Anglada Escudé, Stefano Cristiani, J. Haldemann, László L. Kiss, H. P. Osborn, Valerio Nascimbeni, Aleisha Hogan, Ennio Poretti, Pierre F. L. Maxted, S. C. C. Barros, G. Boué, Sébastien Charnoz, Benjamin F. Cooke, Nicolas Billot, C. Reimers, Don Pollacco, Gaetano Scandariato, Luca Fossati, Douglas R. Alves, J. I. González Hernández, Edward M. Bryant, Anders Erikson, Nelson J. Nunes, Wolfgang Baumjohann, Yann Alibert, A. Suárez Mascareño, Antoine Simon, Gy. M. Szabó, C. Lovis, Magali Deleuil, Andrea Fortier, Isabella Pagano, A. Bekkelien, G. Di Persio, Didier Queloz, Davide Gandolfi, Centre Hospitalier Régional Universitaire [Lille] (CHRU Lille), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, ITA, USA, GBR, FRA, DEU, AUT, BEL, CHL, DNK, NLD, PRT, SWE, CHE, HUN, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Genève (UNIGE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Swiss National Science Foundation, Agence Nationale de la Recherche (France), Science and Technology Facilities Council (UK), Belgian Science Policy Office, Université de Liège, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Fundação para a Ciência e a Tecnologia (Portugal), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Alvarez, M. [0000-0002-6786-2620], Carrasco Martínez, J. M. [0000-0002-3029-5853], Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Brightness, planets and satellites: detection, Laplace resonance, 010504 meteorology & atmospheric sciences, spectroscopic techniques, planets and satellites: dynamical evolution and stability, Astrophysics, 01 natural sciences, Transits, spectroscopic [Techniques], techniques: photometric, Planet, QB460, QB Astronomy, 010303 astronomy & astrophysics, planets and satellites dynamical evolution and stability, QC, Institut für Optische Sensorsysteme, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Laplace transform, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, photmetric [Techniques], 3rd-DAS, dynamical evolution and stability [Planets and satellites], planets and satellites detection, Astrophysics::Earth and Planetary Astrophysics, Extrasolare Planeten und Atmosphären, Techniques: photmetric, FOS: Physical sciences, Context (language use), SPECULOOS, Earth radius, Mean-motion resonance, 0103 physical sciences, Celestial mechanics, CHEOPS, QB600, 0105 earth and related environmental sciences, photometric techniques, TESS, Scattering, Leitungsbereich PF, photometric [Techniques], Astronomy and Astrophysics, celestial mechanics, 620 Engineering, detection [Planets and satellites], QC Physics, 13. Climate action, Space and Planetary Science, NGTS, Planetare Sensorsysteme, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Event (particle physics), techniques: spectroscopic, QB799, Planets and satellites: Detection, Planets and satellites: Dynamical evolution and stability, Techniques: Photometric, Techniques: Spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract

Leleu, A., et al., 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 the possible presence of a near 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 1.152to 2.87Earth 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 1.02to 0.177times 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 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) 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., The authors acknowledge support from the Swiss NCCR PlanetS and the Swiss National Science Foundation. Y.A. and M.J.H. acknowledge the support of the Swiss National Fund under grant 200020_172746. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/M001296/1. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. SH acknowledges CNES funding through the grant 837319. Based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) project ST/M001962/1. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. V.A. acknowledges the support from FCT through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. ABr was supported by the SNSA. A.C. acknowledges support by CFisUC projects (UIDB/04564/2020 and UIDP/04564/2020), GRAVITY (PTDC/FIS-AST/7002/2020), ENGAGE SKA (POCI-01-0145-FEDER-022217), and PHOBOS (POCI-01-0145-FEDER-029932), funded by COMPETE 2020 and FCT, Portugal. This work was supported by FCT - Fundaçãopara a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa OperacionalCompetitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER- 032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). M.F. and C.M.P. gratefully acknowledgethe support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a WintonExoplanet Fellowship. M.G. is an F.R.S.-FNRS Senior Research Associate. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal programme RYC-2013-14875. J.I.G.H., A.S.M., R.R., and C.A.P. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. MNG ackowledges support from the MIT Kavli Institute as a Juan Carlos Torres Fellow. J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. KGI is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme.She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection forthe programme. J.S.J. acknowledges support by FONDECYT grant 1201371, and partial support from CONICYT project Basal AFB-170002. A.J. acknowledges support from ANID - Millennium Science Initiative - ICN12_009 and from FONDECYT project 1171208. P.M. acknowledges support from STFC research grant number ST/M001040/1. N.J.N is supported by the contract and exploratory project IF/00852/2015, and projects UID/FIS/04434/2019, PTDC/FIS-OUT/29048/2017, COMPETE2020: POCI-01-0145-FEDER-028987 & FCT: PTDC/FIS-AST/28987/2017. N.J.N is supported by the contract and exploratory project IF/00852/2015, and project PTDC/FIS-OUT/29048/2017. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). Acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This project has been supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grants GINOP-2.3.2-15-2016-00003, K-119517, K-125015, and the City of Szombathely under Agreement No. 67.177-21/2016. This research received funding from the MERAC foundation, from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no 803193/ BEBOP, and from the Science and Technology Facilites Council (STFC, grant no ST/S00193X/1). V.V.G. is an F.R.S-FNRS Research Associate. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. M. R. Z. O. acknowledges financial support from projects AYA2016-79425-C3-2-P and PID2019-109522GB-C51 from the Spanish Ministry of Science, Innovation and Universities.

Published
2021
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44. Life cycle analysis (LCA) of the production of wood waste briquettes from Pinus spp.: Case study San Francisco Pichátaro, México

Author

J C Corral-Huacuz, L B López-Sosa, M Morales-Máximo, E Medina-Ríos, and A Aguilera-Mandujano

Subjects
%22">Pinus , Wood waste, Briquette, Production (economics), Environmental science, Pulp and paper industry
Abstract

This study shows a life cycle analysis (LCA) of the production of briquettes from wood residues of Pinus spp. in an indigenous community in Mexico. The analysis was carried out considering one Mega Joule (1MJ) of heat as a functional unit, including mainly environmental sustainability indicators, through the Life Cycle Analysis (LCA), and generating environmental impact scenarios for the functional unit by: a) comparing the carbon footprint using solar drying and firewood drying in the production of briquettes and (b) comparing the carbon footprint of the heat obtained by the briquettes from both previous systems with heat obtained from liquefied petroleum gas (LP gas) and firewood. The results show that solar-dried briquettes have the lowest carbon footprint, and more than 80% of the emissions are biogenic, making it an excellent choice as a clean and renewable energy source. In addition, the methane emissions from LP gas is much higher than emissions from briquettes, but the carbon monoxide (CO) and particulate matter (PM2.5) emissions are lower. This methodology applied to the production process will help decision-making in the creation of a micro-enterprise for the generation of solid biofuels in rural communities in Mexico.

Published
2021
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45. Assessment of the energy potential as a solid biofuel of Sargassum spp. considering sustainability indicator

Author

L B López-Sosa, J C Corral-Huacuz, R E Rodríguez-Martínez, C A Ávalos-Betancourt, A Aguilera-Mandujano, and M Morales-Máximo

Subjects
biology, Environmental protection, Biofuel, Sargassum, Sustainability, Environmental science, biology.organism_classification
Abstract

The present study evaluates the potential use of pelagic Sargassum spp. as a solid biofuel. Massive landings of these brown algae across the Atlantic have produced ecologic and economic problems since 2011. Sargassum biomass valorization could compensate for economic losses and reduce environmental impacts. The production of biofuels could be one of its applications. This research consists of two stages: (a) the physical-energy characterization: morphology, humidity, ash, volatiles, and calorific value, and (b) an estimate of the energy potential of these algae, considering their removal from 600 kilometers of coastline along the Mexican Caribbean coast. An analysis of sustainability indicators considering socioeconomic aspects shows the benefits of using this resource in comparison with other types of low-cost biofuels that produce low environmental impact. The results show the pertinence of using Sargassum spp. as an alternative energy resource with low cost, low environmental impact, high accessibility, and added value for localities along the Mexican Caribbean.

Published
2021
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46. PO-1132: Magnetic resonance imaging (mri) based image-guided adaptive brachytherapy in cervical cancer

Author

Y. Ríos Kavadoy, B. Baños Perez, J. Quirós Rivero, V. Vera Barragán, J. Cabrera Rodriguez, P. Simón Silva, J.L. Munoz Garcia, M.F. Ropero Carmona, C. Corral Fernandez, and B. Ortiz Sierra

Subjects
Cervical cancer, Oncology, medicine.diagnostic_test, business.industry, medicine.medical_treatment, Brachytherapy, medicine, Radiology, Nuclear Medicine and imaging, Magnetic resonance imaging, Hematology, medicine.disease, business, Nuclear medicine
Published
2020
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47. PO-1170: Long-Term testosterone levels and its influence in treatment outcomes in prostate cancer patients

Author

P. Simón Silva, F. Ropero Carmona, J. Quirós Rivero, Y. Ríos Kavadoy, C. Corral Fernandez, B. Ortiz Sierra, J. Cabrera Rodriguez, B. Baños Perez, and J.L. Munoz Garcia

Subjects
Oncology, medicine.medical_specialty, business.industry, Treatment outcome, Testosterone (patch), Hematology, medicine.disease, Term (time), Prostate cancer, Internal medicine, Medicine, Radiology, Nuclear Medicine and imaging, business
Published
2020
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48. The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS

Author

H. Ottacher, T. Kuntzer, M. Steller, Xavier Bonfils, A. García Muñoz, Don Pollacco, Ingo Walter, Gaetano Scandariato, A. Deline, Ignasi Ribas, J. Hasiba, T. Bandy, Bruno Chazelas, Yann Alibert, Luca Marafatto, Maria Bergomi, E. Hernandez, Michaël Gillon, Anders Erikson, O. Demangeon, Valerio Nascimbeni, Heike Rauer, N. Thomas, Virginie Cessa, G. Olofsson, F. Safa, R. Rohlfs, N. A. Walton, C. Broeg, Didier Queloz, C. Corral Van Damme, D. Futyan, Nicola Rando, Malcolm Fridlund, Federico Biondi, Roi Alonso, David Ehrenreich, T. Lüftinger, Stéphane Udry, László L. Kiss, K. G. Isaak, Wolfgang Baumjohann, Alexis M. S. Smith, Monika Lendl, D. Wolter, A. E. Simon, Thomas Beck, L. Malvasio, Nuno C. Santos, David Barrado, Demetrio Magrin, J. Asquier, V. Singh, Enric Palle, Damien Ségransan, Pierre F. L. Maxted, Roland Ottensamer, Gisbert Peter, M.-D. Busch, S. C. C. Barros, D. Kitzmann, Willy Benz, S. Hoyer, B. M. Morris, C. Lovis, Kevin Heng, Isabella Pagano, S. Salmon, Davide Gandolfi, Jacopo Farinato, Gy. M. Szabó, Sébastien Charnoz, Giampaolo Piotto, A. Bekkelien, Andrea Fortier, M. Sordet, A. Bonfanti, Nicolas Billot, Luca Fossati, Jacques Laskar, Francois Wildi, Szilard Csizmadia, Martin Rieder, M. Tschentscher, Valérie Van Grootel, Valentina Viotto, Vincent Bourrier, Roberto Ragazzoni, M. Beck, M. J. Hooton, F. Ratti, T. G. Wilson, T. Bárczy, L. Delrez, Daniele Piazza, A. Collier Cameron, Melvyn B. Davies, S. G. Sousa, B. O. Demory, Juan Cabrera, Alexis Brandeker, P. Guterman, M. Deleuil, A. Lecavelier des Etangs, Harald Michaelis, Matteo Munari, Swiss Space Office, University of Bern, Swiss National Science Foundation, Austrian Research Promotion Agency, German Research Foundation, European Commission, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), Generalitat de Catalunya, Fundação para a Ciência e a Tecnologia (Portugal), Fédération Wallonie-Bruxelles, Hungarian Scientific Research Fund, Agenzia Spaziale Italiana, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Wilson, T. G. [0000-0001-8749-1962], Cameron, A. [0000-0002-8863-7828], Fridlund, M. [0000-0002-0855-8426], Cabrera, J. [0000-0001-6653-5487], Barros, S. [0000-0003-2434-3625], Santos, N. [0000-0003-4422-2919], Piotto, G. [0000-0002-9937-6387], Austrian Research Promotion Agency (FFG), Deutsche Forschungsgemeinschaft (DFG), European Research Council (ERC), Swiss National Science Foundation (SNSF), Agencia Estatal de Investigación (AEI), Fundação para a Ciência e a Tecnologia (FCT), National Research Development and Innovation Office, Hungarian (NKFIH), Agenzia Spaziale Italiana (ASI), European Space Agency (ESA), Fundacao para a Ciencia e a Tecnologia (FCT), Belgian Federal Science Policy Office (BELSPO), Istituto Nazionale di Astrofisica (INAF), University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Physikalisches Institut [Bern], Universität Bern [Bern], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), European Research Council (ERC) under European Union, European Commission (EU), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, European Space Agency, FEDER through COMPETE2020 Programa Operacional Competitividade e Internacionalizacao, Hungarian National Research, and Centre National D'etudes Spatiales

Subjects
010504 meteorology & atmospheric sciences, Astrophysics, atmospheres -planets and satellites, 01 natural sciences, 7. Clean energy, Occultation, Planet, Planets and satellites: atmospheres, QB Astronomy, photometric -planets and satellites, individual, 010303 astronomy & astrophysics, QC, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 16. Peace & justice, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, individual: WASP- 189 b [Planets and satellites], atmospheres [Planets and satellites], Astrophysics - Instrumentation and Methods for Astrophysics, Extrasolare Planeten und Atmosphären, Weltrauminstrumente, FOS: Physical sciences, WASP-189 b, Photometry (optics), 0103 physical sciences, Hot Jupiter, individual: WASP-189 b [Planets and satellites], Planets and satellites: individual: WASP-189 b, Techniques: photometric, Gravity darkening, planetary systems, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, abundance pattern, photometric [Techniques], Astronomy and Astrophysics, DAS, Light curve, Stars, QC Physics, Space and Planetary Science, exoplanet occultation, Planetare Sensorsysteme, techniques, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics, QB799
Abstract

Full author list: 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.a,g,l, Garcia Muñoz, A.m, Hooton, M.J.f, Maxted, P.F.L.i, Morris, B.M., Van Grootel, V., Wilson, T.G., Alibert, Y., Alonso, R., Asquier, J., Bandy, T.f, Bárczy, T.q, Barrado, D.r, Barros, S.C.C.s,t, Baumjohann, W.b, 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.l, Guterman, P., Hasiba, J., Hernandez, E., Isaak, K., 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, G.M., Thomas, N., Tschentscher, M., Udry, S., Viotto, V., Walter, I., Walton, N.A., Wildi, F., Wolter, D., 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., with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The Swiss participation to CHEOPS has been supported by the Swiss Space Office (SSO) in the framework of the Prodex Programme and the Activités Nationales Complémentaires (ANC), the Universities of Bern and Geneva as well as well as of the NCCR PlanetS and the Swiss National Science Foundation. M.L.E. acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859724 “GRAPPA”. Sz. Cs. thanks DFG Research Unit 2440: ‘Matter Under Planetary Interior Conditions: High Pressure, Planetary, and Plasma Physics’ for support. Sz. Cs. acknowledges support by DFG grants RA 714/14-1 within the DFG Schwerpunkt SPP 1992: “Exploring the Diversity of Extrasolar Planets”. A.D.E. and D.E.H. acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement no. 724427). M.J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. The Spanish scientific participation in CHEOPS has been supported by the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87676-C5-1-R, PGC2018-098153-B-C31, PGC2018-098153-B-C33, and MDM-2017-0737 Unidad de Excelencia María de Maeztu–Centro de Astrobiología (INTA-CSIC), as well as by the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liege through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. M.G. is F.R.S.-FNRS Senior Research Associate. S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). Gy.S. acknowledges funding from the Hungarian National Research, Development and Innovation Office (NKFIH) grant GINOP-2.3.2-15-2016-00003 and K-119517. For Italy, CHEOPS activities have been supported by the Italian Space Agency, under the programs: ASI-INAF n. 2013-016-R.0 and ASI-INAF n. 2019-29-HH.0. The team at LAM acknowledges CNES funding for the development of the CHEOPS DRP, including grants 124378 for O.D. and 837319 for S.H. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as an ESA-appointed CHEOPS science team members.

Published
2020
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49. CHEOPS: the characterizing exoplanets satellite ready for launch

Author

F. Ratti, D. Cortes, R. Southworth, K. G. Isaak, F. Safa, C. Corral Van Damme, Nicola Rando, A. Borges, Willy Benz, M. Gehler, Joel Asquier, R. Palacios, Thomas Beck, and Christopher Broeg

Subjects
Spacecraft, business.industry, Payload, Sun-synchronous orbit, Exoplanet, Space exploration, law.invention, Telescope, law, Environmental science, Satellite, Aerospace engineering, business, Transit (satellite)
Abstract

CHEOPS (Characterizing Exoplanets Satellite) is devoted to the characterization of known exoplanets orbiting bright stars, achieved through the precise measurement of exoplanet radii using the technique of transit photometry. CHEOPS was selected in October 2012 as the first Small-class mission (S1) within the Agency’s Scientific Programme, with the following programmatic requirements: science driven mission selected through an open Call; an implementation cycle, from the Call to launch, drastically shorter than for Medium-class (M) and Large-class (L) missions; a strict cost-cap to ESA, with possibly higher Member States involvement than for M or L missions. Following a phase A/B1 study, CHEOPS was adopted for implementation in February 2014 as a partnership between the ESA Science Programme and Switzerland, with a number of other Member States delivering significant contributions to the instrument development and to operations. The CHEOPS payload is a high precision photometer, with an optical Ritchey-Chretien telescope with 300 mm effective aperture and a large external baffle to minimize straylight. The CHEOPS spacecraft (280 kg mass, 1.5 m size) is based on a flight-proven platform and will orbit the Earth in a dawn-dusk Sun Synchronous Orbit at 700 km altitude. CHEOPS completed the Preliminary Design Review at the end of September 2014, and passed the Critical Design Review in May 2016. In 2017, flight platform and payload have been separately integrated and tested, while satellite activities were completed by end 2018, allowing to reach flight readiness. CHEOPS is scheduled for launch on a shared Soyuz flight by the end of 2019.

Published
2019
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50. Cell lines authentication and mycoplasma detection as minimun quality control of cell lines in biobanking

Author

B. Miranda, G. Lucena-Aguilar, R. Aguilar-Quesada, P. Catalina, G. Ligero, C. Corral-Vázquez, and J. A. Carrillo-Ávila

Subjects
Biobanking, DNA, Bacterial, Quality Control, 0301 basic medicine, Cell Culture Techniques, Biomedical Engineering, Computational biology, Biology, medicine.disease_cause, Polymerase Chain Reaction, Article, Cell line authentication, Cell Line, Biomaterials, 03 medical and health sciences, Mycoplasma, 0302 clinical medicine, Transplant surgery, medicine, Humans, Mycoplasma Infections, Biological Specimen Banks, Genetics, Transplantation, Authentication, Cell Biology, Tumor tissue, Biobank, PCR, STRs, 030104 developmental biology, Cell culture, 030220 oncology & carcinogenesis
Abstract

Establishment of continuous cell lines from human normal and tumor tissues is an extended and useful methodology for molecular characterization of cancer pathophysiology and drug development in research laboratories. The exchange of these cell lines between different labs is a common practice that can compromise assays reliability due to contamination with microorganism such as mycoplasma or cells from different flasks that compromise experiment reproducibility and reliability. Great proportions of cell lines are contaminated with mycoplasma and/or are replaced by cells derived for a different origin during processing or distribution process. The scientific community has underestimated this problem and thousand of research experiment has been done with cell lines that are incorrectly identified and wrong scientific conclusions have been published. Regular contamination and authentication tests are necessary in order to avoid negative consequences of widespread misidentified and contaminated cell lines. Cell banks generate, store and distribute cell lines for research, being mandatory a consistent and continuous quality program. Methods implementation for guaranteeing both, the absence of mycoplasma and authentication in the supplied cell lines, has been performed in the Andalusian Health System Biobank. Specifically, precise results were obtained using real time PCR detection for mycoplasma and 10 STRs identification by capillary electrophoresis for cell line authentication. Advantages and disadvantages of these protocols are discussed.

Published
2017
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