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4,018 results on '"BECK, M."'

2. A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067

Author

Luque, R., Osborn, H. P., Leleu, A., Pallé, E., Bonfanti, A., Barragán, O., Wilson, T. G., Broeg, C., Cameron, A. Collier, Lendl, M., Maxted, P. F. L., Alibert, Y., Gandolfi, D., Delisle, J.-B., Hooton, M. J., Egger, J. A., Nowak, G., Lafarga, M., Rapetti, D., Twicken, J. D., Morales, J. C., Carleo, I., Orell-Miquel, J., Adibekyan, V., Alonso, R., Alqasim, A., Amado, P. J., Anderson, D. R., Anglada-Escudé, G., Bandy, T., Bárczy, T., Barrado Navascues, D., Barros, S. C. C., Baumjohann, W., Bayliss, D., Bean, J. L., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Boyle, A. W., Brandeker, A., Bryant, E. M., Cabrera, J., Carrazco-Gaxiola, S., Charbonneau, D., Charnoz, S., Ciardi, D. R., Cochran, W. D., Collins, K. A., Crossfield, I. J. M., Csizmadia, Sz., Cubillos, P. E., Dai, F., Davies, M. B., Deeg, H. J., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B.-O., Ehrenreich, D., Erikson, A., Esparza-Borges, E., Falk, B., Fortier, A., Fossati, L., Fridlund, M., Fukui, A., Garcia-Mejia, J., Gill, S., Gillon, M., Goffo, E., Gómez Maqueo Chew, Y., Güdel, M., Guenther, E. W., Günther, M. N., Hatzes, A. P., Helling, Ch., Hesse, K. M., Howell, S. B., Hoyer, S., Ikuta, K., Isaak, K. G., Jenkins, J. M., Kagetani, T., Kiss, L. L., Kodama, T., Korth, J., Lam, K. W. F., Laskar, J., Latham, D. W., Lecavelier des Etangs, A., Leon, J. P. D., Livingston, J. H., Magrin, D., Matson, R. A., Matthews, E. C., Mordasini, C., Mori, M., Moyano, M., Munari, M., Murgas, F., Narita, N., Nascimbeni, V., Olofsson, G., Osborne, H. L. M., Ottensamer, R., Pagano, I., Parviainen, H., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Quinn, S. N., Quirrenbach, A., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Redfield, S., Ribas, I., Ricker, G. R., Rudat, A., Sabin, L., Salmon, S., Santos, N. C., Scandariato, G., Schanche, N., Schlieder, J. E., Seager, S., Ségransan, D., Shporer, A., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Szabó, Gy. M., Thomas, N., Tuson, A., Udry, S., Vanderburg, A. M., Van Eylen, V., Van Grootel, V., Venturini, J., Walter, I., Walton, N. A., Watanabe, N., Winn, J. N., and Zingales, T.

Published
2023
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4. Suture versus open mesh repair for small umbilical hernia: Results of a propensity-matched cohort study

Author

Antor, M., Beck, M., Barrat, C., Berney, C., Binot, D., Bousquet, J., Blazquez, D., Bonan, A., Cas, O., Champault-Fezais, A., Chastan, P., Chollet, J.-M., Cossa, J.-P., Dabrowski, A., Delaunay, T., Démaret, S., Drissi, F., Demian, H., Dubuisson, V., Dugue, T., Fromont, G., Gillion, J.-F., Jacquin, C., Jurczak, F., Khalil, H., Launay-Savary, M., Lepère, M., Lépront, D., Longeville, J.H., Le Toux, N., Loriau, J., Magne, E., Ngo, P., Oberlin, O., Passot, G., Pavis d’Escurac, X., Putinier, J.B., Renard, Y., Romain, B., Soler, M., Roos, S., Thillois, J.-M., Tiry, P., Vu, P., Verhaeghe, R., Warlaumont, M., Zaranis, C., Frey, Samuel, Beauvais, Adrien, Soler, Marc, Beck, Mathieu, Dugué, Timothée, Pavis d’Escurac, Xavier, Dabrowski, André, Jurczak, Florent, and Gillion, Jean-François

Published
2023
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6. F18-FDG PET/CT imaging early predicts pathologic complete response to induction chemoimmunotherapy of locally advanced head and neck cancer: preliminary single-center analysis of the checkrad-cd8 trial

Author

Beck, M., Hartwich, J., Eckstein, M., Schmidt, D., Gostian, A. O., Müller, S., Rutzner, S., Gaipl, U. S., von der Grün, J., Illmer, T., Hautmann, M. G., Klautke, G., Döscher, J., Brunner, T., Tamaskovics, B., Hartmann, A., Iro, H., Kuwert, T., Fietkau, R., Hecht, M., and Semrau, S.

Published
2022
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9. CHEOPS in-flight performance: A comprehensive look at the first 3.5 yr of operations.

Author

Fortier, A., Simon, A. E., Broeg, C., Olofsson, G., Deline, A., Wilson, T. G., Maxted, P. F. L., Brandeker, A., Collier Cameron, A., Beck, M., Bekkelien, A., Billot, N., Bonfanti, A., Bruno, G., Cabrera, J., Delrez, L., Demory, B.-O., Futyan, D., Florén, H.-G., and Günther, M. N.

Subjects
INNER planets, INSTRUMENT flying, SPACE telescopes, SPACE vehicles, LIGHT curves
Abstract

Context. Since the discovery of the first exoplanet almost three decades ago, the number of known exoplanets has increased dramatically. By beginning of the 2000s it was clear that dedicated facilities to advance our studies in this field were needed. The CHaracterising ExOPlanet Satellite (CHEOPS) is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, CHEOPS completed its nominal mission duration of 3.5 yr and remains in excellent operational conditions. As a testament to this, the mission has been extended until the end of 2026. Aims. Scientific and instrumental data have been collected throughout in-orbit commissioning and nominal operations, enabling a comprehensive analysis of the mission's performance. In this article, we present the results of this analysis with a twofold goal. First, we aim to inform the scientific community about the present status of the mission and what can be expected as the instrument ages. Secondly, we intend for this publication to serve as a legacy document for future missions, providing insights and lessons learned from the successful operation of CHEOPS. Methods. To evaluate the instrument performance in flight, we developed a comprehensive monitoring and characterisation (M&C) programme. It consists of dedicated observations that allow us to characterise the instrument's response and continuously monitor its behaviour. In addition to the standard collection of nominal science and housekeeping data, these observations provide valuable input for detecting, modelling, and correcting instrument systematics, discovering and addressing anomalies, and comparing the instrument's actual performance with expectations. Results. The precision of the CHEOPS measurements has enabled the mission objectives to be met and exceeded. The satellite's performance remains stable and reliable, ensuring accurate data collection throughout its operational life. Careful modelling of the instrumental systematics allows the data quality to be significantly improved during the light curve analysis phase, resulting in more precise scientific measurements. Conclusions. CHEOPS is compliant with the driving scientific requirements of the mission. Although visible, the ageing of the instrument has not affected the mission's performance. The satellite's capabilities remain robust, and we are confident that we will continue to acquire high-quality data during the mission extension. [ABSTRACT FROM AUTHOR]

Published
2024
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10. Open IPOMs for medium/large incisional ventral hernia repairs in the French Hernia Registry: factors associated with their use and mesh-related outcomes.

Author

Gillion, J.-F., Fromont, G., Verhaeghe, R., Tiry, P., Binot, D., Dugué, T., Dabrowski, A., Arnalsteen, L., Atger, J., Beck, M., Belhassen, A., Bensignor, T., Bernard, P., Bousquet, J., Blazquez, D., Bonan, A., Cahais, J., Cas, O., Champault-Fezais, A., and Chastan, P.

Subjects
VENTRAL hernia, HERNIA surgery, MINIMALLY invasive procedures, HERNIA, DATABASES
Abstract

Purpose: The use of open intra-peritoneal onlay mesh repairs (O-IPOMs) for treating medium/large incisional ventral hernias has come into question due to the development of minimally invasive and sublay procedures. This study aimed to identify factors that are associated with the use of O-IPOMs in France. Methods: We analysed prospectively collected data from the French Hernia Registry on incisional ventral hernia repairs (IVHR) for hernias ≥ 4 cm in width. Results: We obtained data for 2261 IVHR (from 11/09/2011 to 30/03/2020): 733 O-IPOMs and 1,528 other techniques. We found that the O-IPOMs were performed on patients with more patient-related risk factors compared with the other techniques. Specifically, there was a higher proportion of patients with ASA III/IV (40.47% vs. 28.02%; p < 0.00001) and at least one patient-related risk factor (66.17% vs. 58.51%; p = 0.0005). Of the 733 O-IPOMs, 195 used Ventrio ST™ (VST), the most commonly used mesh for such IPOMs in our database; the other 538 O-IPOMs used other meshes (OM). The VST subgroup had a higher proportion of patients with ASA III/IV (52.58% vs. 36.07%; p < 0.0001) and on anticoagulants (26.04% vs. 18.41%; p = 0.0229) compared with the OM subgroup; they also had a lower recurrence rate after 2 years (5.83% vs. 15.41%; p = 0.008). However, large (≥ 10 cm) or lateral defects were more common in the OM subgroup, and their mesh/defect area ratio was lower. Conclusion: O-IPOMs were performed on patients with more comorbidities and/or complex incisional hernias compared with other techniques. [ABSTRACT FROM AUTHOR]

Published
2024
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11. Functional outcomes in symptomatic versus asymptomatic patients undergoing incisional hernia repair: Replacing one problem with another? A prospective cohort study in 1312 patients

Author

Abet, E., Ain, J.-F., Arnalsteen, L., Baraket, O., Beck, M., Bellouard, A., Benizri, E., Berney, C., Bilem, D., Binot, D., Blanc, B., Blazquez, D., Bonan, A., Boukortt, T., Brehant, O., Cas, O., Champault-Fezais, A., Chau, A., Chollet, J.-M., Constantin, M., Cossa, J.-P., Dabrowski, A., David, A., Demaret, S., Dubuisson, V., Dugue, T., El Nakadi, I., Faure, J.-P., Frileux, P., Fromont, G., Gadiri, N., Gillion, J.-F., Glehen, O., Hennequin, S., Isambert, M., Jurczak, F., Khalil, H., Lamblin, A., Largenton, C., Lavy, M., Lepère, M., Le Toux, N., Magne, E., Manfredelli, S., Mariette, C., Marion, Y., Mercoli, H.-A., Mesli Smain, N., Moszkowicz, D., Najim, M., Oberlin, O., Odet, E., Ortega Deballon, P., Pavis d’Escurac, X., Pichot Delahaye, V., Putinier, J.B., Regimbeau, J.M., Renard, Y., Romain, B., Rouquie, D., Soler, M., Soufron, J., Roos, S., Thillois, J.-M., Tiry, P., Vauchaussade De Chaumont, A., Vinatier, E., Vu, P., Verhaeghe, R., Zaranis, C., Zeineb, M., de Smet, Gijs H.J., Sneiders, Dimitri, Yurtkap, Yagmur, Menon, Anand G., Jeekel, Johannes, Kleinrensink, Gert-Jan, Lange, Johan F., and Gillion, Jean-François

Published
2020
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12. Imaging-based target volume reduction in chemoradiotherapy for locally advanced non-small-cell lung cancer (PET-Plan): a multicentre, open-label, randomised, controlled trial

Author

Grosu, A L, Weber, W, Meyer, P, Hoffmanns, H, Nestle, U, Aurisch, R, Schäfer, W, Hehr, T, Eschmann, S M, Dornoff, W, Siekmeyer, B, Trampert, L, Gademann, G, Brunner, T, Amthauer, A, Ricke, J, Pech, M, Rübe, C, Kirsch, C M, Ezzidin, S, Schmidberger, H, Schreckenberger, M, Bamberg, M, Zips, D, Bares, R, La Fougere, C, Budach, V, Brenner, W, Beck, M, Freiherr von Gumppenberg, R, Aebersold, D, Krause, T, Feldmann, H J, Hertel, A, Stüben, G, Sciuk, J, Annweiler, H, Holl, G, Oehler, W, Schlöcker, I, Baum, R, Kimmig, B, Dunst, J, Henze, E, Lützen, U, Schwaiger, M, Strehle, K, Alberti, W, Piroth, M, Tosch, M, Pötter, R, Widder, J, Herold, C, Freund, U, Momm, F, Sautter-Bihl, M L, Tatsch, K, Hildebrandt, G, Krause, B, Nestle, Ursula, Schimek-Jasch, Tanja, Kremp, Stephanie, Schaefer-Schuler, Andrea, Mix, Michael, Küsters, Andreas, Tosch, Marco, Hehr, Thomas, Eschmann, Susanne Martina, Bultel, Yves-Pierre, Hass, Peter, Fleckenstein, Jochen, Thieme, Alexander, Stockinger, Marcus, Dieckmann, Karin, Miederer, Matthias, Holl, Gabriele, Rischke, H Christian, Gkika, Eleni, Adebahr, Sonja, König, Jochem, and Grosu, Anca-Ligia

Published
2020
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13. The CHEOPS mission

Author

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

Published
2021
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15. Muon-induced background in the KATRIN main spectrometer

Author

Altenmüller, K., Arenz, M., Baek, W.-J., Beck, M., Beglarian, A., Behrens, J., Bergmann, T., Berlev, A., Besserer, U., Blaum, K., Bobien, S., Bode, T., Bornschein, B., Bornschein, L., Brunst, T., Buzinsky, N., Chilingaryan, S., Choi, W.Q., Deffert, M., Doe, P.J., Dragoun, O., Drexlin, G., Dyba, S., Edzards, F., Eitel, K., Ellinger, E., Engel, R., Enomoto, S., Erhard, M., Eversheim, D., Fedkevych, M., Formaggio, J.A., Fränkle, F.M., Franklin, G.B., Friedel, F., Fulst, A., Gil, W., Glück, F., Gonzalez Ureña, A., Grohmann, S., Grössle, R., Gumbsheimer, R., Hackenjos, M., Hannen, V., Harms, F., Haußmann, N., Heizmann, F., Helbing, K., Herz, W., Hickford, S., Hilk, D., Hillesheimer, D., Howe, M.A., Huber, A., Jansen, A., Kellerer, J., Kernert, N., Kippenbrock, L., Kleesiek, M., Klein, M., Kopmann, A., Korzeczek, M., Kovalík, A., Krasch, B., Kraus, M., Kuckert, L., Lasserre, T., Lebeda, O., Leiber, B., Letnev, J., Linek, J., Lokhov, A., Machatschek, M., Marsteller, A., Martin, E.L., Mertens, S., Mirz, S., Monreal, B., Neumann, H., Niemes, S., Off, A., Osipowicz, A., Otten, E., Parno, D.S., Pollithy, A., Poon, A.W.P., Priester, F., Ranitzsch, P.C.-O., Rest, O., Rink, R., Robertson, R.G.H., Roccati, F., Rodenbeck, C., Röllig, M., Röttele, C., Rovedo, P., Ryšavý, M., Sack, R., Saenz, A., Schimpf, L., Schlösser, K., Schlösser, M., Schönung, K., Schrank, M., Seitz-Moskaliuk, H., Sentkerestiová, J., Sibille, V., Slezák, M., Steidl, M., Steinbrink, N., Sturm, M., Suchopar, M., Suesser, M., Telle, H.H., Thorne, L.A., Thümmler, T., Titov, N., Tkachev, I., Trost, N., Valerius, K., Vénos, D., Vianden, R., Vizcaya Hernández, A.P., Wandkowsky, N., Weber, M., Weinheimer, C., Weiss, C., Welte, S., Wendel, J., Wilkerson, J.F., Wolf, J., Wüstling, S., Zadoroghny, S., and Zeller, G.

Published
2019
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17. Cardio- Renal Outcomes With Long- Term Agalsidase Alfa Enzyme Replacement Therapy: A 10- Year Fabry Outcome Survey (FOS) Analysis

Author

Ramaswami U, Beck M, Hughes D, Kampmann C, Botha J, Pintos-Morell G, West ML, Niu DM, Nicholls K, and Giugliani R

Subjects
Agalsidase alfa, Enzyme replacement therapy, Fabry disease, Cardio-renal outcomes, Therapeutics. Pharmacology, RM1-950
Abstract

Uma Ramaswami,1 Michael Beck,2 Derralynn Hughes,1 Christoph Kampmann,2 Jaco Botha,3 Guillem Pintos-Morell,4 Michael L West,5 Dau-Ming Niu,6 Kathy Nicholls,7,8 Roberto Giugliani9 On behalf of the FOS Study Group 1Royal Free London NHS Foundation Trust, Lysosomal Disorders Unit, Institute of Immunity and Transplantation, London, UK; 2Centre for Paediatric and Adolescent Medicine, University Medical Centre, University of Mainz, Mainz, Germany; 3Department of Biostatistics and Programming, Takeda, Zug, Switzerland; 4Centre for Rare Diseases, University Hospital Vall d’Hebron, Barcelona, CIBERER-GCV08_IGTP Research Institute and Teaching Unit Germans Trias i Pujol, Universitat Autònoma de Barcelona, Badalona, Spain; 5Department of Medicine, Dalhousie University, Halifax, Nova Scotia, Canada; 6Department of Paediatrics, Taipei Veterans General Hospital, Taipei, Taiwan; 7Department of Nephrology, Royal Melbourne Hospital, University of Melbourne, Parkville, VIC, Australia; 8Department of Medicine, Royal Melbourne Hospital, University of Melbourne, Parkville, VIC, Australia; 9Medical Genetics Service HCPA, Department of Genetics, UFRGS, and INAGEMP, Porto Alegre, BrazilCorrespondence: Uma RamaswamiLysosomal Disorders Unit, Institute of Immunity and Transplantation, 2nd Floor, Royal Free Hospital, Pond Street, London NW3 2QG, UKTel +44 207 794 0500 Ext 22492Fax +44 207 317 7665Email uma.ramaswami@nhs.netPurpose: Following the publication of 5-year agalsidase alfa enzyme replacement therapy (ERT) outcomes data from the Fabry Outcome Survey (FOS), 10-year data were analyzed.Patients and methods: FOS (ClinicalTrials.gov identifier: NCT03289065) data (April 2001 to August 2018) were retrospectively analyzed. Estimated glomerular filtration rate (eGFR) and left ventricular mass indexed to height (LVMI) were analyzed after treatment start (baseline) for patients with ≥3 measurements, including baseline and year 10.Results: Median (range) age (years) of the evaluable treated renal cohort at treatment start was 48.8 (17.9–67.3) for females (n=62), 34.4 (18.0–66.8) for males (n=90). With eGFR ≥60 mL/min/1.73 m2 at baseline, mean (95% CI) rate of eGFR change (eGFR/year) over 10 years was relatively stable in females (n=52; −0.55 [−1.12, +0.01]) and slightly declined in males (n=79; −1.99 [−2.45, −1.54]). With impaired kidney function (eGFR 48 g/m2.7 in females, >50 g/m2.7 in males) at baseline, mean (95% CI) LVMI/year slightly increased over 10 years in females (n=18; +1.51 [+0.91, +2.12]) and males (n=14; +0.87 (+0.19, +1.55). Without LVH at baseline, mean (95% CI) LVMI/year was stable in females (n=16; +0.52 [−0.13, +1.17]) and males (n=21; +0.57 [+0.02, +1.13]) over 10 years.Conclusion: Agalsidase alfa-treated patients with 10-year FOS data and preserved kidney function and/or normal LVMI at baseline remained largely stable; those with decreased kidney function or LVH at baseline experienced modest declines in renal function and/or increases in LVMI.Keywords: agalsidase alfa, enzyme replacement therapy, Fabry disease, cardio-renal outcomes

Published
2019

20. Model risk : illuminating the black box

Author

Black, R., Tsanakas, A., Smith, A. D., Beck, M. B., Maclugash, I. D., Grewal, J., Witts, L., Morjaria, N., Green, R. J., and Lim, Z.

Published
2018

21. External Validation of the European Hernia Society Classification for Postoperative Complications after Incisional Hernia Repair: A Cohort Study of 2,191 Patients

Author

Ain, J.-F., Beck, M., Barrat, C., Berney, C., Berrod, J.-L., Binot, D., Boudet, M.-J., Bousquet, J., Blazquez, D., Bonan, A., Cas, O., Champault-Fezais, A., Chastan, P., Cardin, J.-L., Chollet, J.-M., Cossa, J.-P., Dabrowski, A., Démaret, S., Drissi, F., Durou, J., Dugue, T., Faure, J.-P., Framery, D., Fromont, G., Gainant, A., Gauduchon, L., Genser, L., Gillion, J.-F., Guillaud, A., Jacquin, C., Jurczak, F., Khalil, H., Lacroix, A., Ledaguenel, P., Lepère, M., Lépront, D., Letoux, N., Loriau, J., Magne, E., Ngo, P., Oberlin, O., Paterne, D., Pavis d'Escurac, X., Potiron, L., Renard, Y., Soler, M., Rignier, P., Roos, S., Thillois, J.-M., Tiry, P., Verhaeghe, R., Vu, P., Zaranis, C., Kroese, Leonard F., Kleinrensink, Gert-Jan, Lange, Johan F., and Gillion, Jean-Francois

Published
2018
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24. Constraining the reflective properties of WASP-178 b 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., and Beck, M.

Subjects
GAS giants, PHOTOMETRY, EXTRASOLAR planets, BRIGHTNESS temperature, LIGHT curves
Abstract

Context. Multiwavelength photometry of the secondary eclipses of extrasolar planets is able to disentangle the reflected and thermally emitted light radiated from the planetary dayside. Based on this, we can measure the planetary geometric albedo Ag, which is an indicator of the presence of clouds in the atmosphere, and the recirculation efficiency ϵ, which quantifies the energy transport within the atmosphere. Aims. We measure Ag and ϵ for the planet WASP-178 b, a highly irradiated giant planet with an estimated equilibrium temperature of 2450 K. Methods. 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 telescopes. Results. We measured a marginally significant eclipse depth of 70 ± 40 ppm in the TESS passband, and a statistically significant depth of 70 ± 20 ppm in the CHEOPS passband. Conclusions. Combining the eclipse-depth measurement in the CHEOPS (λeff = 6300 Å) and TESS (λeff = 8000 Å) passbands, we constrained the dayside brightness temperature of WASP-178 b in the 2250–2800 K interval. The geometric albedo 0.1< Ag<0.35 generally supports the picture that giant planets are poorly reflective, while the recirculation efficiency ϵ >0.7 makes WASP-178 b an interesting laboratory for testing the current heat-recirculation models. [ABSTRACT FROM AUTHOR]

Published
2024
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25. TESS and CHEOPS discover two warm sub-Neptunes transiting the bright K-dwarf HD 15906

Author

Tuson, A, Queloz, D, Osborn, H P, Wilson, T G, Hooton, M J, Beck, M, Lendl, M, Olofsson, G, Fortier, A, Bonfanti, A, Brandeker, A, Buchhave, L A, Collier Cameron, A, Ciardi, D R, Collins, K A, Gandolfi, D, Garai, Z, Giacalone, S, Gomes da Silva, J, Howell, S B, Patel, J A, Persson, C M, Serrano, L M, Sousa, S G, Ulmer-Moll, S, Vanderburg, A, Ziegler, C, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado Navascues, D, Barros, S C C, Baumjohann, W, Beck, T, Benz, W, Billot, N, Bonfils, X, Borsato, L, Broeg, C, Cabrera, J, Charnoz, S, Conti, D M, Csizmadia, Sz, Cubillos, P E, Davies, M B, Deleuil, M, Delrez, L, Demangeon, O D S, Demory, B-O, Dragomir, D, Dressing, C D, Ehrenreich, D, Erikson, A, Essack, Z, Farinato, J, Fossati, L, Fridlund, M, Furlan, E, Gill, H, Gillon, M, Gnilka, C L, Gonzales, E, Güdel, M, Günther, M N, Hoyer, S, Isaak, K G, Jenkins, J M, Kiss, L L, Laskar, J, Latham, D W, Law, N, Lecavelier des Etangs, A, Curto, G Lo, Lovis, C, Luque, R, Magrin, D, Mann, A W, Maxted, P F L, Mayor, M, McDermott, S, Mecina, M, Mordasini, C, Mortier, A, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Pritchard, T, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Ricker, G R, Rieder, M, Santos, N C, Savel, A B, Scandariato, G, Schwarz, R P, Seager, S, Ségransan, D, Shporer, A, Simon, A E, Smith, A M S, Steller, M, Stockdale, C, Szabó, Gy M, Thomas, N, Torres, G, Tronsgaard, R, Udry, S, Ulmer, B, Van Grootel, V, Vanderspek, R, Venturini, J, Walton, N A, Winn, J N, Wohler, B, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCP, DAS
Abstract

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by ∼ 734 d, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS, and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 ± 0.08 R⊕ and a period of 10.924709 ± 0.000032 d, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R⊕ and a period of 21.583298$^{+0.000052}_{-0.000055}$ d. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 ± 13 K and 532 ± 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm (≲ 700 K) sub-Neptune sized planets transiting a bright star (G ≤ 10 mag). It is an excellent target for detailed characterization studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution. Publisher PDF

Published
2023

26. Structure of nascent 5S RNPs at the crossroad between ribosome assembly and MDM2-p53 pathways

Author

Castillo Duque de Estrada, N., Thoms, M., Flemming, D., Hammaren, H., Buschauer, R., Ameismeier, M., Baßler, J., Beck, M., https://orcid.org/0000-0002-7397-1321, Beckmann, R., and Hurt, E.

Abstract

The 5S ribonucleoprotein (RNP) is assembled from its three components (5S rRNA, Rpl5/uL18 and Rpl11/uL5) before being incorporated into the pre-60S subunit. However, when ribosome synthesis is disturbed, a free 5S RNP can enter the MDM2–p53 pathway to regulate cell cycle and apoptotic signaling. Here we reconstitute and determine the cryo-electron microscopy structure of the conserved hexameric 5S RNP with fungal or human factors. This reveals how the nascent 5S rRNA associates with the initial nuclear import complex Syo1–uL18–uL5 and, upon further recruitment of the nucleolar factors Rpf2 and Rrs1, develops into the 5S RNP precursor that can assemble into the pre-ribosome. In addition, we elucidate the structure of another 5S RNP intermediate, carrying the human ubiquitin ligase Mdm2, which unravels how this enzyme can be sequestered from its target substrate p53. Our data provide molecular insight into how the 5S RNP can mediate between ribosome biogenesis and cell proliferation.

Published
2023

27. TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906

Author

Tuson, A., Queloz, D., Osborn, H. P., Wilson, T. G., Hooton, M. J., Beck, M., Lendl, M., Olofsson, G., Fortier, A., Bonfanti, A., Brandeker, A., Buchhave, L. A., Collier Cameron, A., Ciardi, D. R., Collins, K. A., Gandolfi, D., Garai, Z., Giacalone, S., Gomes da Silva, J., Howell, S. B., Patel, J. A., Persson, C. M., Serrano, L. M., Sousa, S. G., Ulmer-Moll, S., Vanderburg, A., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Bàrczy, T., Barrado Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Conti, D. M., Csizmadia, Szilard, Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dragomir, D., Dressing, C. D., Ehrenreich, D., Erikson, A., Essack, Z., Farinato, J., Fossati, L., Fridlund, M., Furlan, E., Gill, H., Gillon, M., Gnilka, C. L., Gonzales, E.J., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Law, N., Lecavelier des Etangs, A., Curto, G. Lo, Lovis, C., Luque, R., Magrin, D., Mann, A. W., Maxted, P. F. L., Mayor, M., McDermott, S., Mecina, M., Mordasini, C., Mortier, A., Nascimbeni, V., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Pritchard, T., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H, Ribas, I., Ricker, G. R., Rieder, M., Santos, N. C., Savel, A. B., Scandariato, G., Schwarz, R. P., Seager, S., Ségransan, D., Shporer, A., Simon, A. E., Smith, A. M. S., Steller, M., Stockdale, C., Szabó, Gy. M., Thomas, N., Torres, G., Tronsgaard, R., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Venturini, J., Walton, N. A., Winn, J. N., Wohler, B., 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, fundamental parameters [Planets and satellites], photometric [Techniques], TIC 4646810), individual: HD 15906 (TOI 461, TIC 4646810) [Stars], FOS: Physical sciences, fundamental parameters [Stars], detection [Planets and satellites], techniques: photometric, [SDU]Sciences of the Universe [physics], stars: fundamental parameters, stars: individual: HD 15906 (TOI 461, planets and satellites: fundamental parameters, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution., 30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS

Published
2023

34. Measurement of sub-Poissonian shot noise in a quantum cascade detector.

Author

Heckelmann, I., Bertrand, M., Forrer, A., Shahmohammadi, M., Beck, M., and Faist, J.

Subjects
QUANTUM noise, SUBMILLIMETER waves, DETECTORS, INFRARED absorption, LIGHT absorption, POWER density, INFRARED radiation
Abstract

In a Quantum Cascade Detector, photocurrent is generated by the absorption of infrared and terahertz radiation in the quantum-well-based modules arranged in series. Consequently, the current responsivity is by construction inversely proportional to the number of cascading modules. Upon absorption of a photon, the electron travels through only a single period of the detector, with a mean free path corresponding to the period length. Therefore, the shot noise power density is expected to decrease by the same factor under sufficiently high illumination, reflecting the same inverse relationship with the number of cascading modules. This phenomenon leads to sub-Poissonian noise characteristics. We experimentally observe this effect in a 90-period Quantum Cascade Detector operating at 4.5 μm, confirming a reduction in the shot noise contribution by the anticipated Fano factor of 1/90. This measurement underscores the suitability of these detectors for coherent detection scenarios, particularly where shot noise dominates. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
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35. Gamma-induced background in the KATRIN main spectrometer

Author

Altenmüller, K., Arenz, M., Baek, W.-J., Beck, M., Beglarian, A., Behrens, J., Berlev, A., Besserer, U., Blaum, K., Block, F., Bobien, S., Bode, T., Bornschein, B., Bornschein, L., Bouquet, H., Brunst, T., Buzinsky, N., Chilingaryan, S., Choi, W. Q., Deffert, M., Doe, P. J., Dragoun, O., Drexlin, G., Dyba, S., Eitel, K., Ellinger, E., Engel, R., Enomoto, S., Erhard, M., Eversheim, D., Fedkevych, M., Formaggio, J. A., Fränkle, F. M., Franklin, G. B., Friedel, F., Fulst, A., Gil, W., Glück, F., Ureña, A. Gonzalez, Grössle, R., Gumbsheimer, R., Hackenjos, M., Hannen, V., Harms, F., Haußmann, N., Heizmann, F., Helbing, K., Herz, W., Hickford, S., Hilk, D., Hillesheimer, D., Howe, M. A., Huber, A., Jansen, A., Karl, C., Kellerer, J., Kernert, N., Kippenbrock, L., Klein, M., Kopmann, A., Korzeczek, M., Kovalík, A., Krasch, B., Kraus, A., Kraus, M., Lasserre, T., Lebeda, O., Lehnert, B., Letnev, J., Lokhov, A., Machatschek, M., Marsteller, A., Martin, E. L., Mertens, S., Mirz, S., Monreal, B., Neumann, H., Niemes, S., Osipowicz, A., Otten, E., Parno, D. S., Pollithy, A., Poon, A. W. P., Priester, F., Ranitzsch, P. C.-O., Rest, O., Robertson, R. G. H., Rodenbeck, C., Röllig, M., Röttele, C., Ryšavý, M., Sack, R., Saenz, A., Schimpf, L., Schlösser, K., Schlösser, M., Schlüter, L., Schrank, M., Seitz-Moskaliuk, H., Sibille, V., Slezák, M., Steidl, M., Steinbrink, N., Sturm, M., Suchopar, M., Tcherniakhovski, D., Telle, H. H., Thorne, L. A., Thümmler, T., Titov, N., Tkachev, I., Trost, N., Valerius, K., Vénos, D., Vianden, R., Hernández, A. P. Vizcaya, Weber, M., Weinheimer, C., Weiss, C., Welte, S., Wendel, J., Wilkerson, J. F., Wolf, J., Wüstling, S., Zadoroghny, S., and Zeller, G.

Published
2019
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39. Space-charge effects in Penning ion traps

Author

Porobić, T., Beck, M., Breitenfeldt, M., Couratin, C., Finlay, P., Knecht, A., Fabian, X., Friedag, P., Fléchard, X., Liénard, E., Ban, G., Zákoucký, D., Soti, G., Van Gorp, S., Weinheimer, Ch., Wursten, E., and Severijns, N.

Published
2015
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41. Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

Author

Sulis, S., Lendl, M., Cegla, H. M., Rodriguez Diaz, L. F., Bigot, L., Van Grootel, V., Bekkelien, A., Collier Cameron, A., 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 Escudé, G., Bàrczy, T., Barrado y Navascués, D., 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., Corral Van Damme, C., 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., Lecavelier des Etangs, A., Magrin, D., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Rieder, M., Santos, N. C., Segransan, D., Smith, A. M. S., Steinberger, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Walton, N. A., Wolter, D., 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), 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, University of St Andrews. School of Economics and Finance, and University of St Andrews. University of St Andrews

Subjects
radial velocities and photometric [Techniques], FOS: Physical sciences, Sun: granulation, techniques: photometric, stars: atmospheres, techniques: radial velocities, QB Astronomy, atmospheres [Stars], data analysis [Methods], QC, Solar and Stellar Astrophysics (astro-ph.SR), QB, MCC, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], photometric [Techniques], 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, DAS, Astronomy and Astrophysics, methods: data analysis, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], granulation [Sun], Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. Characterizing granulation is key for understanding stellar atmospheres and detecting planets. Aims. We aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for mainsequence stars, and test predictions from 3D hydrodynamic models. Methods. For the first time, we observed two bright stars (Teff = 5833 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 dataset. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating and filtering the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. Results. 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 versus radial velocities, RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to S/N dependent variations. Conclusions. 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., Astronomy & Astrophysics, 670, ISSN:0004-6361, ISSN:1432-0746

Published
2023

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

Author

Garai, Z., Osborn, H. P., Gandolfi, D., Brandeker, A., Sousa, S. G., Lendl, M., Bekkelien, A., Broeg, C., Cameron, A. Collier, Egger, J. A., Hooton, M. J., Alibert, Y., Delrez, L., Fossati, L., Salmon, S., Wilson, T. G., Bonfanti, A., Tuson, A., Ulmer-Moll, S., Serrano, L. M., Borsato, L., Alonso, R., Anglada, G., Asquier, J., Barrado y Navascués, D., Barros, S. C. C., Bàrczy, T., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Biondi, F., Bonfils, X., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Van Eylen, V., Fortier, A., Fridlund, M., Gillon, M., Van Grootel, V., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Kristiansen, M. H., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Luntzer, A., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Segransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., Walton, N. A., 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), techniques: photometric, [SDU]Sciences of the Universe [physics], FOS: Physical sciences, methods: observational, planets and satellites: fundamental parameters, Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; Context. Multi-planet systems are important sources of information regarding the evolution of planets. However, the long-period planets in these systems often escape detection. These objects in particular may retain more of their primordial characteristics compared to close-in counterparts because of their increased distance from the host star. HD 22946 is a bright (G = 8.13 mag) late F-type star around which three transiting planets were identified via Transiting Exoplanet Survey Satellite (TESS) photometry, but the true orbital period of the outermost planet d was unknown until now. Aims: We aim to use the Characterising Exoplanet Satellite (CHEOPS) space telescope to uncover the true orbital period of HD 22946d and to refine the orbital and planetary properties of the system, especially the radii of the planets. Methods: We used the available TESS photometry of HD 22946 and observed several transits of the planets b, c, and d using CHEOPS. We identified two transits of planet d in the TESS photometry, calculated the most probable period aliases based on these data, and then scheduled CHEOPS observations. The photometric data were supplemented with ESPRESSO (Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations) radial velocity data. Finally, a combined model was fitted to the entire dataset in order to obtain final planetary and system parameters. Results: Based on the combined TESS and CHEOPS observations, we successfully determined the true orbital period of the planet d to be 47.42489 ± 0.00011 days, and derived precise radii of the planets in the system, namely 1.362 ± 0.040 R⊕, 2.328 ± 0.039 R⊕, and 2.607 ± 0.060 R⊕ for planets b, c, and d, respectively. Due to the low number of radial velocities, we were only able to determine 3σ upper limits for these respective planet masses, which are 13.71 M⊕, 9.72 M⊕, and 26.57 M⊕. We estimated that another 48 ESPRESSO radial velocities are needed to measure the predicted masses of all planets in HD 22946. We also derived stellar parameters for the host star. Conclusions: Planet c around HD 22946 appears to be a promising target for future atmospheric characterisation via transmission spectroscopy. We can also conclude that planet d, as a warm sub-Neptune, is very interesting because there are only a few similar confirmed exoplanets to date. Such objects are worth investigating in the near future, for example in terms of their composition and internal structure. Photometry and radial velocity data of HD22946 are only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A44

Published
2023

43. TOI-5678b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS★

Author

Ulmer-Moll, S., Osborn, H. P., Tuson, A., Egger, J. A., Lendl, M., Maxted, P. F. L., Bekkelien, A., Simon, A. E., Olofsson, G., Adibekyan, V., Alibert, Y., Bonfanti, A., Bouchy, F., Brandeker, A., Fridlund, M., Gandolfi, D., Mordasini, C., Persson, C. M., Salmon, S., Serrano, L. M., Sousa, S. G., Wilson, T. G., Rieder, M., Hasiba, J., Asquier, J., Sicilia, D., Walter, I., Alonso, R., Anglada, G., Barrado y Navascués, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bàrczy, T., Cabrera, J., Charnoz, S., Cointepas, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dumusque, X., Ehrenreich, D., Eisner, N. L., Erikson, A., Fortier, A., Fossati, L., Gillon, M., Grieves, N., Güdel, M., Hagelberg, J., Helled, R., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Magrin, D., Nascimbeni, V., Otegi, J.F., Ottensammer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Psaridi, A., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Smith, A. M. S., Steller, M., Szabó, Gy. M., Ségransan, D., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., Walton, N. A., 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, [SDU]Sciences of the Universe [physics], FOS: Physical sciences, methods: data analysis, planets and satellites: individual: TOI-5678, planets and satellites: gaseous planets, Astrophysics - Earth and Planetary Astrophysics
Abstract

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

Published
2023

44. A full transit of v2 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., Collier Cameron, A., 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., Corral Van Damme, C., 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., Lecavelier des Etangs, A., 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., Tschentscher, M., Thomas, N., Udry, S., Vanderspek, R., Van Grootel, V., Walton, N. A., 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), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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
MCC, planets and satellites: detection, 530 Physics, 520 Astronomy, 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, DAS, 610 Medicine & health, Astronomy and Astrophysics, planets and satellites: general, 620 Engineering, general [Planets and satellites], detection [Planets and satellites], [SDU]Sciences of the Universe [physics], Space and Planetary Science, individual: HD 136352 [Planets and satellites], QB Astronomy, 570 Life sciences, biology, planets and satellites: individual: HD 136352, QB, 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

45. Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4b, and the transit-timing variations of HD 97658 b

Author

Harre, J.-V., Smith, A. M. S., Barros, S. C. C., Boué, G., Csizmadia, Sz., Ehrenreich, D., Florén, H.-G., Fortier, A., Maxted, P. F. L., Hooton, M. J., Akinsanmi, B., Serrano, L. M., Rosário, N. M., Demory, B.-O., Jones, K., Laskar, J., Adibekyan, V., Alibert, Y., Alonso, R., Anderson, D. R., Anglada, G., Asquier, J., Bárczy, T., Barrado y Navascues, D., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Biondi, F., Bonfanti, A., Bonfils, X., Brandeker, A., Broeg, C., Cabrera, J., Cessa, V., Charnoz, S., Collier Cameron, A., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Hellier, C., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Lecavelier des Etangs, A., Lendl, M., Lovis, C., Luntzer, A., Magrin, D., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Persson, C. M., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G. R., Salmon, S., Santos, N. C., Scandariato, G., Seager, S., Ségransan, D., Simon, A. E., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Walton, N. A., Wilson, T. G., Winn, J. N., Wohler, B., 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), 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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
Planet-star interactions, planets and satellites: dynamical evolution and stability, 530 Physics, FOS: Physical sciences, 610 Medicine & health, techniques: photometric, planet-star interactions, QB Astronomy, planets and satellites: dynamical evolution and stability / planet-star interactions / techniques: photometric, QB, MCC, Earth and Planetary Astrophysics (astro-ph.EP), 520 Astronomy, photometric [Techniques], dynamical evolution and stability, techniques: photometric [planets and satellites], 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, Astronomy and Astrophysics, 3rd-DAS, 620 Engineering, dynamical evolution and stability [Planets and satellites], Space and Planetary Science, [SDU]Sciences of the Universe [physics], 570 Life sciences, biology, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12 b. By examining this effect, information on the properties of the host star can be obtained using the so-called stellar modified tidal quality factor Q′∗, which describes the efficiency with which the kinetic energy of the planet is dissipated within the star. This can provide information about the interior of the star. Aims. In this study, we aim to improve constraints on the tidal decay of the KELT-9, KELT-16, and WASP-4 systems in order to find evidence for or against the presence of tidal orbital decay. With this, we want to constrain the Q′∗ value for each star. In addition, we aim to test the existence of the transit timing variations (TTVs) in the HD 97658 system, which previously favoured a quadratic trend with increasing orbital period. Methods. Making use of newly acquired photometric observations from CHEOPS (CHaracterising ExOplanet Satellite) and TESS (Transiting Exoplanet Survey Satellite), combined with archival transit and occultation data, we use Markov chain Monte Carlo (MCMC) algorithms to fit three models to the data, namely a constant-period model, an orbital-decay model, and an apsidal-precession model. Results. We find that the KELT-9 system is best described by an apsidal-precession model for now, with an orbital decay trend at over 2 σ being a possible solution as well. A Keplerian orbit model with a constant orbital period provides the best fit to the transit timings of KELT-16 b because of the scatter and scale of their error bars. The WASP-4 system is best represented by an orbital decay model at a 5 σ significance, although apsidal precession cannot be ruled out with the present data. For HD 97658 b, using recently acquired transit observations, we find no conclusive evidence for a previously suspected strong quadratic trend in the data., Astronomy & Astrophysics, 669, ISSN:0004-6361, ISSN:1432-0746

Published
2023

46. 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., Gandolfi, D., Serrano, L. M., Wilson, T. G., Sousa, S. G., Lecavelier des Etangs, A., 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., Collier Cameron, A., Corral van Damme, C., 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., Walton, N. A., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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), 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
530 Physics, FOS: Physical sciences, photometric, Methods: data analysis, Stars: flare, Starspots, Circumstellar matter [Techniques], 610 Medicine & health, circumstellar matter, techniques: photometric, QB Astronomy, data analysis [Methods], Solar and Stellar Astrophysics (astro-ph.SR), QB, MCC, Earth and Planetary Astrophysics (astro-ph.EP), 520 Astronomy, photometric [Techniques], 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, Astronomy and Astrophysics, Circumstellar matter, 3rd-DAS, flare [Stars], 620 Engineering, methods: data analysis, starspots, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 570 Life sciences, biology, stars: flare, Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. 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. Methods. 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 Piszkésteto and with the SOPHIE spectrograph in order to refine the astrophysical parameters of DE Boo. Results. 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. Conclusions. 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., Astronomy & Astrophysics, 671, ISSN:0004-6361, ISSN:1432-0746

Published
2023

47. Hint of an exocomet transit in the CHEOPS light curve of HD 172555

Author

Kiefer, F., Van Grootel, V., Lecavelier des Etangs, A., Szabo, Gy. M., Brandeker, A., Broeg, C., Collier Cameron, A., Deline, A., Olofsson, G., Wilson, T. G., Sousa, S. G., Gandolfi, D., Hebrard, G., Alibert, Y., Alonso, R., Anglada Escudé, G., Bàrczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Cabrera, J., Charnoz, S., Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., 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., Munari, M., Nascimbeni, V., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Reimers, C., Ribas, I., Santos, N. C., Scandariato, G., Segransan, D., Simon, A. E., Smith, Alexis M S, Steller, M., Thomas, N., Udry, S., Walter, I., Walton, N. A., Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, University of St Andrews. University of St Andrews, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), and 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)

Subjects
stars: variables: δ Scuti, 530 Physics, stars: variables: \ensuremathδ Scuti, FOS: Physical sciences, 610 Medicine & health, 000 Computer science, knowledge & systems, circumstellar matter, techniques: photometric, Earth and Planetary Astrophysics (astro-ph.EP), 520 Astronomy, comets: general, photometric [Techniques], 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, general [Comets], variables: δ Scuti [Stars], stars: individual: HD 172555, Astronomy and Astrophysics, Circumstellar matter, 3rd-DAS, 620 Engineering, [SDU]Sciences of the Universe [physics], Space and Planetary Science, MCP, 570 Life sciences, biology, individual: HD 172555 [Stars], Astrophysics - Earth and Planetary Astrophysics
Abstract

HD$\,$172555 is a young ($\sim$20$\,$Myr) A7V star surrounded by a 10$\,$au wide debris disk suspected to be replenished partly by collisions between large planetesimals. Small evaporating transiting bodies, exocomets, have also been detected in this system by spectroscopy. After $\beta\,$Pictoris, this is another example of a system possibly witnessing a phase of heavy bombardment of planetesimals. In such system, small bodies trace dynamical evolution processes. We aim at constraining their dust content by using transit photometry. We performed a 2-day-long photometric monitoring of HD$\,$172555 with the CHEOPS space telescope in order to detect shallow transits of exocomets with a typical expected duration of a few hours. The large oscillations in the lightcurve indicate that HD$\,$172555 is a $\delta\,$Scuti pulsating star. Once removing those dominating oscillations, we find a hint for a transient absorption. If fitted with an exocomet transit model, it corresponds to an evaporating body passing near the star at a distance of $6.8\pm1.4\,$R$_\star$ (or $0.05\pm 0.01\,$au) with a radius of 2.5 km. These properties are comparable to those of the exocomets already found in this system using spectroscopy, as well as those found in the $\beta\,$Pic system. The nuclei of solar system's Jupiter family comets, with radii of 2-6$\,$km, are also comparable in size. This is the first evidence for an exocomet photometric transit detection in the young system of HD$\,$172555., Comment: 12 pages, 10 figures, 5 tables, accepted for publication in A&A

Published
2023

48. 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., Collier Cameron, A., 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., Barrado Navascues, D., 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., Corral van Damme, C., 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., Lecavelier des Etangs, A., 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., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Walton, N. A., 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), 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, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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
530 Physics, FOS: Physical sciences, 610 Medicine & health, 000 Computer science, knowledge & systems, planets and satellites: individual: HD 189733b, techniques: photometric, SDG 3 - Good Health and Well-being, QB Astronomy, QB, MCC, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, individual: HD 189733b [Planets and satellites], 520 Astronomy, photometric [Techniques], 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, DAS, Astronomy and Astrophysics, 620 Engineering, Space and Planetary Science, [SDU]Sciences of the Universe [physics], atmospheres [Planets and satellites], 570 Life sciences, biology, 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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