214 results on '"A. Collier Cameron"'
Search Results
2. Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops
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Osborn, H P, primary, Nowak, G, additional, Hébrard, G, additional, Masseron, T, additional, Lillo-Box, J, additional, Pallé, E, additional, Bekkelien, A, additional, Florén, H-G, additional, Guterman, P, additional, Simon, A E, additional, Adibekyan, V, additional, Bieryla, A, additional, Borsato, L, additional, Brandeker, A, additional, Ciardi, D R, additional, Collier Cameron, A, additional, Collins, K A, additional, Egger, J A, additional, Gandolfi, D, additional, Hooton, M J, additional, Latham, D W, additional, Lendl, M, additional, Matthews, E C, additional, Tuson, A, additional, Ulmer-Moll, S, additional, Vanderburg, A, additional, Wilson, T G, additional, Ziegler, C, additional, Alibert, Y, additional, Alonso, R, additional, Anglada, G, additional, Arnold, L, additional, Asquier, J, additional, Barrado y Navascues, D, additional, Baumjohann, W, additional, Beck, T, additional, Belinski, A A, additional, Benz, W, additional, Biondi, F, additional, Boisse, I, additional, Bonfils, X, additional, Broeg, C, additional, Buchhave, L A, additional, Bárczy, T, additional, Barros, S C C, additional, Cabrera, J, additional, Cardona Guillen, C, additional, Carleo, I, additional, Castro-González, A, additional, Charnoz, S, additional, Christiansen, J, additional, Cortes-Zuleta, P, additional, Csizmadia, S, additional, Dalal, S, additional, Davies, M B, additional, Deleuil, M, additional, Delfosse, X, additional, Delrez, L, additional, Demory, B-O, additional, Dunlavey, A B, additional, Ehrenreich, D, additional, Erikson, A, additional, Fernandes, R B, additional, Fortier, A, additional, Forveille, T, additional, Fossati, L, additional, Fridlund, M, additional, Gillon, M, additional, Goeke, R F, additional, Goliguzova, M V, additional, Gonzales, E J, additional, Günther, M N, additional, Güdel, M, additional, Heidari, N, additional, Henze, C E, additional, Howell, S, additional, Hoyer, S, additional, Frey, J I, additional, Isaak, K G, additional, Jenkins, J M, additional, Kiefer, F, additional, Kiss, L, additional, Korth, J, additional, Maxted, P F L, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lovis, C, additional, Lund, M B, additional, Luque, R, additional, Magrin, D, additional, Almenara, J M, additional, Martioli, E, additional, Mecina, M, additional, Medina, J V, additional, Moldovan, D, additional, Morales-Calderón, M, additional, Morello, G, additional, Moutou, C, additional, Murgas, F, additional, Jensen, E L N, additional, Nascimbeni, V, additional, Olofsson, G, additional, Ottensamer, R, additional, Pagano, I, 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, Ricker, G, additional, Demangeon, O D S, additional, Smith, A M S, additional, Santos, N, additional, Scandariato, G, additional, Seager, S, additional, Sousa, S G, additional, Steller, M, additional, Szabó, G M, additional, Ségransan, D, additional, Thomas, N, additional, Udry, S, additional, Ulmer, B, additional, Van Grootel, V, additional, Vanderspek, R, additional, Walton, N, additional, and Winn, J N, additional
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- 2023
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3. TESS and CHEOPS discover two warm sub-Neptunes transiting the bright K-dwarf HD 15906
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Tuson, A, primary, Queloz, D, additional, Osborn, H P, additional, Wilson, T G, additional, Hooton, M J, additional, Beck, M, additional, Lendl, M, additional, Olofsson, G, additional, Fortier, A, additional, Bonfanti, A, additional, Brandeker, A, additional, Buchhave, L A, additional, Collier Cameron, A, additional, Ciardi, D R, additional, Collins, K A, additional, Gandolfi, D, additional, Garai, Z, additional, Giacalone, S, additional, Gomes da Silva, J, additional, Howell, S B, additional, Patel, J A, additional, Persson, C M, additional, Serrano, L M, additional, Sousa, S G, additional, Ulmer-Moll, S, additional, Vanderburg, A, additional, Ziegler, C, additional, Alibert, Y, additional, Alonso, R, additional, Anglada, G, additional, Bárczy, T, additional, Barrado Navascues, D, additional, Barros, S C C, additional, Baumjohann, W, additional, Beck, T, additional, Benz, W, additional, Billot, N, additional, Bonfils, X, additional, Borsato, L, additional, Broeg, C, additional, Cabrera, J, additional, Charnoz, S, additional, Conti, D M, additional, Csizmadia, Sz, additional, Cubillos, P E, additional, Davies, M B, additional, Deleuil, M, additional, Delrez, L, additional, Demangeon, O D S, additional, Demory, B-O, additional, Dragomir, D, additional, Dressing, C D, additional, Ehrenreich, D, additional, Erikson, A, additional, Essack, Z, additional, Farinato, J, additional, Fossati, L, additional, Fridlund, M, additional, Furlan, E, additional, Gill, H, additional, Gillon, M, additional, Gnilka, C L, additional, Gonzales, E, additional, Güdel, M, additional, Günther, M N, additional, Hoyer, S, additional, Isaak, K G, additional, Jenkins, J M, additional, Kiss, L L, additional, Laskar, J, additional, Latham, D W, additional, Law, N, additional, Lecavelier des Etangs, A, additional, Curto, G Lo, additional, Lovis, C, additional, Luque, R, additional, Magrin, D, additional, Mann, A W, additional, Maxted, P F L, additional, Mayor, M, additional, McDermott, S, additional, Mecina, M, additional, Mordasini, C, additional, Mortier, A, additional, Nascimbeni, V, additional, Ottensamer, R, additional, Pagano, I, additional, Pallé, E, additional, Peter, G, additional, Piotto, G, additional, Pollacco, D, additional, Pritchard, T, additional, Ragazzoni, R, additional, Rando, N, additional, Ratti, F, additional, Rauer, H, additional, Ribas, I, additional, Ricker, G R, additional, Rieder, M, additional, Santos, N C, additional, Savel, A B, additional, Scandariato, G, additional, Schwarz, R P, additional, Seager, S, additional, Ségransan, D, additional, Shporer, A, additional, Simon, A E, additional, Smith, A M S, additional, Steller, M, additional, Stockdale, C, additional, Szabó, Gy M, additional, Thomas, N, additional, Torres, G, additional, Tronsgaard, R, additional, Udry, S, additional, Ulmer, B, additional, Van Grootel, V, additional, Vanderspek, R, additional, Venturini, J, additional, Walton, N A, additional, Winn, J N, additional, and Wohler, B, additional
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- 2023
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4. Can scallop-shell stars trap dust in their magnetic fields?
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Sanderson, H, primary, Jardine, M, additional, Collier Cameron, A, additional, Morin, J, additional, and Donati, J-F, additional
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- 2022
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5. Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS
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Lacedelli, G, Wilson, TG, Malavolta, L, Hooton, MJ, Collier Cameron, A, Alibert, Y, Mortier, A, Bonfanti, A, Haywood, RD, Hoyer, S, Piotto, G, Bekkelien, A, Vanderburg, AM, Benz, W, Dumusque, X, Deline, A, Lopez-Morales, M, Borsato, L, Rice, K, Fossati, L, Latham, DW, Brandeker, A, Poretti, E, Sousa, SG, Sozzetti, A, Salmon, S, Burke, CJ, Van Grootel, V, Fausnaugh, MM, Adibekyan, V, Huang, CX, Osborn, HP, Mustill, AJ, Palle, E, Bourrier, V, Nascimbeni, V, Alonso, R, Anglada, G, Barczy, T, Barrado Y Navascues, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Billot, N, Bonfils, X, Broeg, C, Buchhave, LA, Cabrera, J, Charnoz, S, Cosentino, R, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demangeon, O, Demory, BO, Ehrenreich, D, Erikson, A, Esparza-Borges, E, Floren, HG, Fortier, A, Fridlund, M, Futyan, D, Gandolfi, D, Ghedina, A, Gillon, M, Güdel, M, Guterman, P, Harutyunyan, A, Heng, K, Isaak, KG, Jenkins, JM, Kiss, L, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, Lovis, C, Magrin, D, Marafatto, L, Martinez Fiorenzano, AF, Maxted, PFL, Mayor, M, Micela, G, Molinari, E, Murgas, F, Narita, N, Olofsson, G, Ottensamer, R, Pagano, I, Pasetti, A, Pedani, M, Pepe, FA, Peter, G, Phillips, DF, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Lacedelli, G [0000-0002-4197-7374], Wilson, TG [0000-0001-8749-1962], Malavolta, L [0000-0002-6492-2085], Hooton, MJ [0000-0003-0030-332X], Collier Cameron, A [0000-0002-8863-7828], Mortier, A [0000-0001-7254-4363], Borsato, L [0000-0003-0066-9268], Rice, K [0000-0002-6379-9185], Sousa, SG [0000-0001-9047-2965], Sozzetti, A [0000-0002-7504-365X], Osborn, HP [0000-0002-4047-4724], Mustill, AJ [0000-0002-2086-3642], Nascimbeni, V [0000-0001-9770-1214], Buchhave, LA [0000-0003-1605-5666], Csizmadia, S [0000-0001-6803-9698], Delrez, L [0000-0001-6108-4808], Gandolfi, D [0000-0001-8627-9628], Lendl, M [0000-0001-9699-1459], Maxted, PFL [0000-0003-3794-1317], and Apollo - University of Cambridge Repository
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techniques: photometric ,stars: individual: TOI-561 (TIC 377064495, Gaia EDR3 3850421005290172416) ,techniques: radial velocities ,planets and satellites: fundamental parameters ,planets and satellites: interiors - Abstract
We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of $62$ HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b ($P = 0.45$ d, $R = 1.42$ R$_\oplus$, $M = 2.0$ M$_\oplus$), c ($P = 10.78$ d, $R = 2.91$ R$_\oplus$, $M = 5.4$ M$_\oplus$), d ($P = 25.7$ d, $R = 2.82$ R$_\oplus$, $M = 13.2$ M$_\oplus$) and e ($P = 77$ d, $R = 2.55$ R$_\oplus$, $M = 12.6$ M$_\oplus$). Moreover, we identify an additional, long-period signal ($>450$ d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density ($\rho_{\rm b} = 3.8 \pm 0.5$ g cm$^{-3}$) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies.
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- 2022
6. The EBLM project – IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves
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D Sebastian, M I Swayne, P F L Maxted, A H M J Triaud, S G Sousa, G Olofsson, M Beck, N Billot, S Hoyer, S Gill, N Heidari, D V Martin, C M Persson, M R Standing, Y Alibert, R Alonso, G Anglada, J Asquier, T Bárczy, D Barrado, S C C Barros, M P Battley, W Baumjohann, T Beck, W Benz, M Bergomi, I Boisse, X Bonfils, A Brandeker, C Broeg, J Cabrera, S Charnoz, A Collier Cameron, Sz Csizmadia, M B Davies, M Deleuil, L Delrez, O D S Demangeon, B-O Demory, G Dransfield, D Ehrenreich, A Erikson, A Fortier, L Fossati, M Fridlund, D Gandolfi, M Gillon, M Güdel, J Hasiba, G Hébrard, K Heng, K G Isaak, L L Kiss, E Kopp, V Kunovac, J Laskar, A Lecavelier des Etangs, M Lendl, C Lovis, D Magrin, J McCormac, N J Miller, V Nascimbeni, R Ottensamer, I Pagano, E Pallé, F A Pepe, G Peter, G Piotto, D Pollacco, D Queloz, R Ragazzoni, N Rando, H Rauer, I Ribas, S Lalitha, A Santerne, N C Santos, G Scandariato, D Ségransan, A E Simon, A M S Smith, M Steller, Gy M Szabó, N Thomas, S Udry, V Van Grootel, N A Walton, 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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stars fundamental parameters ,530 Physics ,FOS: Physical sciences ,techniques spectroscopic ,610 Medicine & health ,000 Computer science, knowledge & systems ,fundamental parameters [Stars] ,spectroscopic [Techniques] ,techniques: photometric ,low-mass [Stars] ,stars: low-mass ,QB460 ,QB Astronomy ,binaries eclipsing ,Solar and Stellar Astrophysics (astro-ph.SR) ,QB600 ,QC ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,MCC ,stars low-mass ,520 Astronomy ,eclipsing [Binaries] ,photometric [Techniques] ,binaries: eclipsing ,Astronomy and Astrophysics ,3rd-DAS ,620 Engineering ,techniques photometric ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,570 Life sciences ,biology ,stars: fundamental parameters ,techniques: spectroscopic ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Eclipsing binaries are important benchmark objects to test and calibrate stellar structure and evolution models. This is especially true for binaries with a fully convective M-dwarf component for which direct measurements of these stars' masses and radii are difficult using other techniques. Within the potential of M-dwarfs to be exoplanet host stars, the accuracy of theoretical predictions of their radius and effective temperature as a function of their mass is an active topic of discussion. Not only the parameters of transiting exoplanets but also the success of future atmospheric characterisation rely on accurate theoretical predictions. We present the analysis of five eclipsing binaries with low-mass stellar companions out of a sub-sample of 23, for which we obtained ultra high-precision light curves using the CHEOPS satellite. The observation of their primary and secondary eclipses are combined with spectroscopic measurements to precisely model the primary parameters and derive the M-dwarfs mass, radius, surface gravity, and effective temperature estimates using the PYCHEOPS data analysis software. Combining these results to the same set of parameters derived from TESS light curves, we find very good agreement (better than 1\% for radius and better than 0.2% for surface gravity). We also analyse the importance of precise orbits from radial velocity measurements and find them to be crucial to derive M-dwarf radii in a regime below 5% accuracy. These results add five valuable data points to the mass-radius diagram of fully-convective M-dwarfs., 19 pages, 12 figures, accepted for publication in MNRAS
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- 2022
7. The EBLM project – IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves
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Sebastian, D, primary, Swayne, M I, additional, Maxted, P F L, additional, Triaud, A H M J, additional, Sousa, S G, additional, Olofsson, G, additional, Beck, M, additional, Billot, N, additional, Hoyer, S, additional, Gill, S, additional, Heidari, N, additional, Martin, D V, additional, Persson, C M, additional, Standing, M R, additional, Alibert, Y, additional, Alonso, R, additional, Anglada, G, additional, Asquier, J, additional, Bárczy, T, additional, Barrado, D, additional, Barros, S C C, additional, Battley, M P, additional, Baumjohann, W, additional, Beck, T, additional, Benz, W, additional, Bergomi, M, additional, Boisse, I, additional, Bonfils, X, additional, Brandeker, A, additional, Broeg, C, additional, Cabrera, J, additional, Charnoz, S, additional, Collier Cameron, A, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Delrez, L, additional, Demangeon, O D S, additional, Demory, B-O, additional, Dransfield, G, additional, Ehrenreich, D, additional, Erikson, A, additional, Fortier, A, additional, Fossati, L, additional, Fridlund, M, additional, Gandolfi, D, additional, Gillon, M, additional, Güdel, M, additional, Hasiba, J, additional, Hébrard, G, additional, Heng, K, additional, Isaak, K G, additional, Kiss, L L, additional, Kopp, E, additional, Kunovac, V, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, McCormac, J, additional, Miller, N J, additional, Nascimbeni, V, additional, Ottensamer, R, additional, Pagano, I, additional, Pallé, E, additional, Pepe, F A, additional, Peter, G, additional, Piotto, G, additional, Pollacco, D, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Ribas, I, additional, Lalitha, S, additional, Santerne, A, additional, Santos, N C, additional, Scandariato, G, additional, Ségransan, D, additional, Simon, A E, additional, Smith, A M S, additional, Steller, M, additional, Szabó, Gy M, additional, Thomas, N, additional, Udry, S, additional, Van Grootel, V, additional, and Walton, N A, additional
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- 2022
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8. The impact of two non-transiting planets and stellar activity on mass determinations for the super-Earth CoRoT-7b
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Anna John, Ancy, primary, Collier Cameron, Andrew, additional, and Wilson, Thomas G, additional
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- 2022
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9. K2-111: an old system with two planets in near-resonance†
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Lars A. Buchhave, Valentina D'Odorico, Laura Affer, Dimitar Sasselov, Annelies Mortier, C. Allende Prieto, Christopher A. Watson, Aldo F. M. Fiorenzano, Paolo Molaro, A. Collier Cameron, Nuno C. Santos, Marco Riva, C. Lovis, Nelson J. Nunes, David Charbonneau, Jesus Maldonado, S. G. Sousa, Enric Palle, Giampaolo Piotto, Aldo S. Bonomo, Adriano Ghedina, Cristina Martins, Richard G. West, Andrew Vanderburg, David W. Latham, Giuseppina Micela, Vardan Adibekyan, Francesco Pepe, G. Lo Curto, Ken Rice, Mahmoudreza Oshagh, Avet Harutyunyan, Alexandre Cabral, Andrea Mehner, P. Di Marcantonio, Antonio Manescau, Rafael Rebolo, Matteo Pinamonti, M. R. Zapatero Osorio, François Bouchy, Baptiste Lavie, Denis Mégevand, Luca Malavolta, Stéphane Udry, David F. Phillips, David Ehrenreich, Jorge Lillo-Box, A. Suárez Mascareño, T. G. Wilson, S. C. C. Barros, Rosario Cosentino, Olivier Demangeon, M. Mayor, Xavier Dumusque, Mercedes López-Morales, Walter Boschin, E. Delgado Mena, Emilio Molinari, Serena Benatti, Alessandro Sozzetti, P. Figueira, Raphaëlle D. Haywood, Ennio Poretti, Stefano Cristiani, J. Haldemann, Yann Alibert, J. I. González Hernández, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Science and Technology Facilities Council (STFC), Istituto Nazionale di Astrofisica (INAF), Swiss National Science Foundation (SNSF), Fundação para a Ciência e a Tecnologia (FCT), National Aeronautics and Space Administration (NASA), European Research Council (ERC), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Cabral, A. [0000-0002-9433-871X], Suárez Mascareño, A. [0000-0002-3814-5323], Molaro, P. [0000-0002-0571-4163], Mena, E. D. [0000-0003-4434-2195], Buchhave, L. A. [0000-0003-1605-5666], Vanderburg, A. [0000-0001-7246-5438], Barros, S. [0000-0003-2434-3625], Haldemann, J. [0000-0003-1231-2389], Cosentino, R. [0000-0003-1784-1431], Sozzetti, A. [0000-0002-7504-365X], Adibekyan, V. [0000-0002-0601-6199], Wilson, T. G. [0000-0001-8749-1962], Cameron, A. [0000-0002-8863-7828], Santos, N. [0000-0003-4422-2919], Ministerio de Ciencia e Innovación (MICINN), Science and Technology Facilities Council (STFC), ST/R000824/1 ST/P000312/1 PTDC/FIS-AST/32113/2017, Istituto Nazionale Astrofisica (INAF) Agenzia Spaziale Italiana (ASI), 2018-16-HH.0, Swiss National Science Foundation (SNSF), 140649 152721 166227 184618, Fundação para a Ciência e a Tecnologia (FCT) through Investigador FCT, IF/00650/2015/CP1273/CT0001 IF/00849/2015/CP1273/CT0003 IF/00028/2014/CP1215/CT0002 IF/01312/2014/CP1215/CT0004 DL 57/2016/CP1364/CT0004, FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao, National Aeronautics and Space Administration (NASA), NNX17AB59G NAS5-26555 NNX13AC07G, Research Projects of National Relevance (PRIN), 201278X4FL, MCTES, PTDC/FIS-AST/32113/2017, European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES), ITA, USA, GBR, DEU, ESP, CHL, DNK, PRT, CHE, Mortier, Annelies [0000-0001-7254-4363], and Apollo - University of Cambridge Repository
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planets and satellites: detection ,010504 meteorology & atmospheric sciences ,530 Physics ,stars: individual (K2-111) ,FOS: Physical sciences ,Astrophysics ,Spectroscopic ,01 natural sciences ,spectroscopic [Techniques] ,techniques: photometric ,Planet ,individual [Stars] ,techniques: radial velocities ,0103 physical sciences ,QB Astronomy ,010303 astronomy & astrophysics ,QC ,QB ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,radial velocities [Techniques] ,520 Astronomy ,individual (K2-111) [Stars] ,photometric [Techniques] ,Astronomy and Astrophysics ,3rd-DAS ,Radius ,500 Science ,Planetary system ,620 Engineering ,Orbital period ,Radial velocity ,detection [Planets and satellites] ,Photometry (astronomy) ,QC Physics ,13. Climate action ,Space and Planetary Science ,astro-ph.EP ,Terrestrial planet ,techniques: spectroscopic ,K2-111 ,Planetary mass ,Astrophysics - Earth and Planetary Astrophysics - Abstract
This paper reports on the detailed characterisation of the K2-111 planetary system with K2, WASP, and ASAS-SN photometry as well as high-resolution spectroscopic data from HARPS-N and ESPRESSO. The host, K2-111, is confirmed to be a mildly evolved ($\log g=4.17$), iron-poor ([Fe/H]$=-0.46$), but alpha-enhanced ([$\alpha$/Fe]$=0.27$), chromospherically quiet, very old thick disc G2 star. A global fit, performed by using PyORBIT shows that the transiting planet, K2-111b, orbits with a period $P_b=5.3518\pm0.0004$ d, and has a planet radius of $1.82^{+0.11}_{-0.09}$ R$_\oplus$ and a mass of $5.29^{+0.76}_{-0.77}$ M$_\oplus$, resulting in a bulk density slightly lower than that of the Earth. The stellar chemical composition and the planet properties are consistent with K2-111b being a terrestrial planet with an iron core mass fraction lower than the Earth. We announce the existence of a second signal in the radial velocity data that we attribute to a non-transiting planet, K2-111c, with an orbital period of $15.6785\pm 0.0064$ days, orbiting in near-3:1 mean-motion resonance with the transiting planet, and a minimum planet mass of $11.3\pm1.1$ M$_\oplus$. Both planet signals are independently detected in the HARPS-N and ESPRESSO data when fitted separately. There are potentially more planets in this resonant system, but more well-sampled data are required to confirm their presence and physical parameters., Comment: Accepted for publication in MNRAS on 28 Sept 2020. Paper is 18 pages with an additional 12 pages of supplementary material. Data is available at https://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/MNRAS/499/5004
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- 2020
10. BEBOP III. Observations and an independent mass measurement of Kepler-16 (AB) b – the first circumbinary planet detected with radial velocities
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Triaud, Amaury H M J, primary, Standing, Matthew R, additional, Heidari, Neda, additional, Martin, David V, additional, Boisse, Isabelle, additional, Santerne, Alexandre, additional, Correia, Alexandre C M, additional, Acuña, Lorena, additional, Battley, Matthew, additional, Bonfils, Xavier, additional, Carmona, Andrés, additional, Collier Cameron, Andrew, additional, Cortés-Zuleta, Pía, additional, Dransfield, Georgina, additional, Dalal, Shweta, additional, Deleuil, Magali, additional, Delfosse, Xavier, additional, Faria, João, additional, Forveille, Thierry, additional, Hara, Nathan C, additional, Hébrard, Guillaume, additional, Hoyer, Sergio, additional, Kiefer, Flavien, additional, Kunovac, Vedad, additional, Maxted, Pierre F L, additional, Martioli, Eder, additional, Miller, Nicola J, additional, Nelson, Richard P, additional, Poveda, Mathilde, additional, Rein, Hanno, additional, Sairam, Lalitha, additional, Udry, Stéphane, additional, and Willett, Emma, additional
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- 2022
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11. Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS
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Lacedelli, G, primary, Wilson, T G, additional, Malavolta, L, additional, Hooton, M J, additional, Collier Cameron, A, additional, Alibert, Y, additional, Mortier, A, additional, Bonfanti, A, additional, Haywood, R D, additional, Hoyer, S, additional, Piotto, G, additional, Bekkelien, A, additional, Vanderburg, A M, additional, Benz, W, additional, Dumusque, X, additional, Deline, A, additional, López-Morales, M, additional, Borsato, L, additional, Rice, K, additional, Fossati, L, additional, Latham, D W, additional, Brandeker, A, additional, Poretti, E, additional, Sousa, S G, additional, Sozzetti, A, additional, Salmon, S, additional, Burke, C J, additional, Van Grootel, V, additional, Fausnaugh, M M, additional, Adibekyan, V, additional, Huang, C X, additional, Osborn, H P, additional, Mustill, A J, additional, Pallé, E, additional, Bourrier, V, additional, Nascimbeni, V, additional, Alonso, R, additional, Anglada, G, additional, Bárczy, T, additional, Barrado y Navascues, D, additional, Barros, S C C, additional, Baumjohann, W, additional, Beck, M, additional, Beck, T, additional, Billot, N, additional, Bonfils, X, additional, Broeg, C, additional, Buchhave, L A, additional, Cabrera, J, additional, Charnoz, S, additional, Cosentino, R, 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, Esparza-Borges, E, additional, Florén, H G, additional, Fortier, A, additional, Fridlund, M, additional, Futyan, D, additional, Gandolfi, D, additional, Ghedina, A, additional, Gillon, M, additional, Güdel, M, additional, Guterman, P, additional, Harutyunyan, A, additional, Heng, K, additional, Isaak, K G, additional, Jenkins, J M, additional, Kiss, L, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, Marafatto, L, additional, Martinez Fiorenzano, A F, additional, Maxted, P F L, additional, Mayor, M, additional, Micela, G, additional, Molinari, E, additional, Murgas, F, additional, Narita, N, additional, Olofsson, G, additional, Ottensamer, R, additional, Pagano, I, additional, Pasetti, A, additional, Pedani, M, additional, Pepe, F A, additional, Peter, G, additional, Phillips, D F, additional, Pollacco, D, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Ratti, F, additional, Rauer, H, additional, Ribas, I, additional, Santos, N C, additional, Sasselov, D, additional, Scandariato, G, additional, Seager, S, additional, Ségransan, D, additional, Serrano, L M, additional, Simon, A E, additional, Smith, A M S, additional, Steinberger, M, additional, Steller, M, additional, Szabó, Gy, additional, Thomas, N, additional, Twicken, J D, additional, Udry, S, additional, Walton, N, additional, and Winn, J N, additional
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- 2022
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12. A pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 characterized with CHEOPS
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Wilson, Thomas G, primary, Goffo, Elisa, additional, Alibert, Yann, additional, Gandolfi, Davide, additional, Bonfanti, Andrea, additional, Persson, Carina M, additional, Collier Cameron, Andrew, additional, Fridlund, Malcolm, additional, Fossati, Luca, additional, Korth, Judith, additional, Benz, Willy, additional, Deline, Adrien, additional, Florén, Hans-Gustav, additional, Guterman, Pascal, additional, Adibekyan, Vardan, additional, Hooton, Matthew J, additional, Hoyer, Sergio, additional, Leleu, Adrien, additional, Mustill, Alexander James, additional, Salmon, Sébastien, additional, Sousa, Sérgio G, additional, Suarez, Olga, additional, Abe, Lyu, additional, Agabi, Abdelkrim, additional, Alonso, Roi, additional, Anglada, Guillem, additional, Asquier, Joel, additional, Bárczy, Tamas, additional, Barrado Navascues, David, additional, Barros, Susana C C, additional, Baumjohann, Wolfgang, additional, Beck, Mathias, additional, Beck, Thomas, additional, Billot, Nicolas, additional, Bonfils, Xavier, additional, Brandeker, Alexis, additional, Broeg, Christopher, additional, Bryant, Edward M, additional, Burleigh, Matthew R, additional, Buttu, Marco, additional, Cabrera, Juan, additional, Charnoz, Sébastien, additional, Ciardi, David R, additional, Cloutier, Ryan, additional, Cochran, William D, additional, Collins, Karen A, additional, Colón, Knicole D, additional, Crouzet, Nicolas, additional, Csizmadia, Szilard, additional, Davies, Melvyn B, additional, Deleuil, Magali, additional, Delrez, Laetitia, additional, Demangeon, Olivier, additional, Demory, Brice-Olivier, additional, Dragomir, Diana, additional, Dransfield, Georgina, additional, Ehrenreich, David, additional, Erikson, Anders, additional, Fortier, Andrea, additional, Gan, Tianjun, additional, Gill, Samuel, additional, Gillon, Michaël, additional, Gnilka, Crystal L, additional, Grieves, Nolan, additional, Grziwa, Sascha, additional, Güdel, Manuel, additional, Guillot, Tristan, additional, Haldemann, Jonas, additional, Heng, Kevin, additional, Horne, Keith, additional, Howell, Steve B, additional, Isaak, Kate G, additional, Jenkins, Jon M, additional, Jensen, Eric L N, additional, Kiss, Laszlo, additional, Lacedelli, Gaia, additional, Lam, Kristine, additional, Laskar, Jacques, additional, Latham, David W, additional, Lecavelier des Etangs, Alain, additional, Lendl, Monika, additional, Lester, Kathryn V, additional, Levine, Alan M, additional, Livingston, John, additional, Lovis, Christophe, additional, Luque, Rafael, additional, Magrin, Demetrio, additional, Marie-Sainte, Wenceslas, additional, Maxted, Pierre F L, additional, Mayo, Andrew W, additional, McLean, Brian, additional, Mecina, Marko, additional, Mékarnia, Djamel, additional, Nascimbeni, Valerio, additional, Nielsen, Louise D, additional, Olofsson, Göran, additional, Osborn, Hugh P, additional, Osborne, Hannah L M, additional, Ottensamer, Roland, additional, Pagano, Isabella, additional, Pallé, Enric, additional, Peter, Gisbert, additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Ragazzoni, Roberto, additional, Rando, Nicola, additional, Rauer, Heike, additional, Redfield, Seth, additional, Ribas, Ignasi, additional, Ricker, George R, additional, Rieder, Martin, additional, Santos, Nuno C, additional, Scandariato, Gaetano, additional, Schmider, François-Xavier, additional, Schwarz, Richard P, additional, Scott, Nicholas J, additional, Seager, Sara, additional, Ségransan, Damien, additional, Serrano, Luisa Maria, additional, Simon, Attila E, additional, Smith, Alexis M S, additional, Steller, Manfred, additional, Stockdale, Chris, additional, Szabó, Gyula, additional, Thomas, Nicolas, additional, Ting, Eric B, additional, Triaud, Amaury H M J, additional, Udry, Stéphane, additional, Van Eylen, Vincent, additional, Van Grootel, Valérie, additional, Vanderspek, Roland K, additional, Viotto, Valentina, additional, Walton, Nicholas, additional, and Winn, Joshua N, additional
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- 2022
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13. The EBLM project – VII. Spin–orbit alignment for the circumbinary planet host EBLM J0608-59 A/TOI-1338 A
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Damien Ségransan, Samuel Gill, William F. Welsh, Don Pollacco, Pierre F. L. Maxted, Andrew Collier Cameron, Stéphane Udry, Jerome A. Orosz, Veselin B. Kostov, Daniel C. Fabrycky, David V. Martin, H. M. Cegla, Amaury H. M. J. Triaud, Didier Queloz, Vedad Kunovac Hodžić, Coel Hellier, Francesco Pepe, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
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NDAS ,FOS: Physical sciences ,Library science ,01 natural sciences ,Categorical grant ,stars: low-mass ,stars: rotation ,low-mass [Stars] ,0103 physical sciences ,planets and satellites: formation ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,media_common.cataloged_instance ,TOI-1338) ,European union ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,QB600 ,QC ,Astrophysics::Galaxy Astrophysics ,QB ,media_common ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,eclipsing [Binaries] ,European research ,binaries: eclipsing ,Astronomy and Astrophysics ,rotation [Stars] ,Scholarship ,QC Physics ,individual (EBLM J0608-59 [Stars] ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,stars: individual: (EBLM J0608-59, TOI-1338) ,formation [Planets and satellites] ,QB799 ,Astrophysics - Earth and Planetary Astrophysics - Abstract
A dozen short-period detached binaries are known to host transiting circumbinary planets. In all circumbinary systems so far, the planetary and binary orbits are aligned within a couple of degrees. However, the obliquity of the primary star, which is an important tracer of their formation, evolution, and tidal history, has only been measured in one circumbinary system until now. EBLM J0608-59/TOI-1338 is a low-mass eclipsing binary system with a recently discovered circumbinary planet identified by TESS. Here, we perform high-resolution spectroscopy during primary eclipse to measure the projected stellar obliquity of the primary component. The obliquity is low, and thus the primary star is aligned with the binary and planetary orbits with a projected spin-orbit angle $\beta = 2.8 \pm 17.1$ deg. The rotation period of $18.1 \pm 1.6$ days implied by our measurement of $v\sin{i_\star}$ suggests that the primary has not yet pseudo-synchronized with the binary orbit, but is consistent with gyrochronology and weak tidal interaction with the binary companion. Our result, combined with the known coplanarity of the binary and planet orbits, is suggestive of formation from a single disc. Finally, we considered whether the spectrum of the faint secondary star could affect our measurements. We show through simulations that the effect is negligible for our system, but can lead to strong biases in $v\sin{i_\star}$ and $\beta$ for higher flux ratios. We encourage future studies in eclipse spectroscopy test the assumption of a dark secondary for flux ratios $\gtrsim 1$ ppt., Comment: 7 pages, 3 figures. Accepted in MNRAS. Fixed a few typos
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- 2020
14. The first Doppler imaging of the active binary prototype RS Canum Venaticorum
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Yue Xiang, S. Kohl, A. Collier Cameron, John R. Barnes, V. Perdelwitz, Shenghong Gu, U. Wolter, J. H. M. M. Schmitt, M. Mittag, University of St Andrews. St Andrews Centre for Exoplanet Science, and University of St Andrews. School of Physics and Astronomy
- Subjects
FOS: Physical sciences ,Astrophysics ,Star (graph theory) ,binaries: eclipsing [Stars] ,01 natural sciences ,Doppler imaging ,Spectral line ,symbols.namesake ,star-spots [Stars] ,0103 physical sciences ,Binary star ,Astrophysics::Solar and Stellar Astrophysics ,QB Astronomy ,Differential rotation ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,QC ,QB ,Physics ,010308 nuclear & particles physics ,DAS ,Astronomy and Astrophysics ,individual: RS CVn [Stars] ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,imaging [Stars] ,symbols ,Polar ,Astrophysics::Earth and Planetary Astrophysics ,Deconvolution ,Doppler effect ,activity [Stars] - Abstract
We present the first Doppler images of the prototypical active binary star RS CVn, derived from high-resolution spectra observed in 2004, 2016 and 2017, using three different telescopes and observing sites. We apply the least-squares deconvolution technique to all observed spectra to obtain high signal-to-noise line profiles, which are used to derive the surface images of the active K-type component. Our images show a complex spot pattern on the K star, distributed widely in longitude. All starspots revealed by our Doppler images are located below a latitude of about 70$^{\circ}$. In accordance with previous light-curve modeling studies, we find no indication of a polar spot on the K star. Using Doppler images derived from two consecutive rotational cycles, we estimate a surface differential rotation rate of $\Delta\Omega = -0.039 \pm 0.003 ~rad~d^{-1}$ and $\alpha = \Delta\Omega/\Omega_{eq} = -0.030 \pm 0.002$ for the K star. Given the limited phase coverage during those two rotations, the uncertainty of our differential rotation estimate is presumably higher., Comment: 11 pages, 10 figures, accepted for publication in MNRAS
- Published
- 2020
15. The EBLM project-VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves
- Author
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Swayne, MI, Maxted, PFL, Triaud, AHMJ, Sousa, SG, Broeg, C, Florén, HG, Guterman, P, Simon, AE, Boisse, I, Bonfanti, A, Martin, D, Santerne, A, Salmon, S, Standing, MR, Van Grootel, V, Wilson, TG, Alibert, Y, Alonso, R, Anglada Escudé, G, Asquier, J, Bárczy, T, Barrado, D, Barros, SCC, Battley, M, Baumjohann, W, Beck, M, Beck, T, Bekkelien, A, Benz, W, Billot, N, Bonfils, X, Brandeker, A, Busch, MD, Cabrera, J, Charnoz, S, Collier Cameron, A, Csizmadia, S, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, BO, Dransfield, G, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Futyan, D, Gandolfi, D, Gillon, M, Guedel, M, Hébrard, G, Heidari, N, Hellier, C, Heng, K, Hobson, M, Hoyer, S, Isaak, KG, Kiss, L, Kunovac Hodžić, V, Lalitha, S, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, Lovis, C, Magrin, D, Marafatto, L, McCormac, J, Miller, N, 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, NC, Scandariato, G, Ségransan, D, Smith, AMS, Steinberger, M, Steller, M, Szabó, GM, Thomas, N, Udry, S, Walter, I, Walton, NA, Willett, E, Swayne, MI [0000-0002-2609-3159], Triaud, AHMJ [0000-0002-5510-8751], Sousa, SG [0000-0001-9047-2965], Santerne, A [0000-0002-3586-1316], Wilson, TG [0000-0001-8749-1962], Battley, M [0000-0002-1357-9774], Baumjohann, W [0000-0001-6271-0110], Collier Cameron, A [0000-0002-8863-7828], Csizmadia, S [0000-0001-6803-9698], Delrez, L [0000-0001-6108-4808], Fridlund, M [0000-0002-0855-8426], Gandolfi, D [0000-0001-8627-9628], Hoyer, S [0000-0003-3477-2466], Lendl, M [0000-0001-9699-1459], Miller, N [0000-0001-9550-1198], and Apollo - University of Cambridge Repository
- Subjects
techniques: photometric ,stars: low-mass ,Astrophysics::Solar and Stellar Astrophysics ,binaries: eclipsing ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,stars: fundamental parameters ,Astrophysics::Galaxy Astrophysics ,techniques: spectroscopic - Abstract
The accuracy of theoretical mass, radius and effective temperature values for M-dwarf stars is an active topic of debate. Differences between observed and theoretical values have raised the possibility that current theoretical stellar structure and evolution models are inaccurate towards the low-mass end of the main sequence. To explore this issue we use the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low mass stellar companions. We use these light curves combined with the spectroscopic orbit for the solar-type companion to measure the mass, radius and effective temperature of the M-dwarf star. Here we present the analysis of three eclipsing binaries. We use the pycheops data analysis software to fit the observed transit and eclipse events of each system. Two of our systems were also observed by the TESS satellite -- we similarly analyse these light curves for comparison. We find consistent results between CHEOPS and TESS, presenting three stellar radii and two stellar effective temperature values of low-mass stellar objects. These initial results from our on-going observing programme with CHEOPS show that we can expect to have ~24 new mass, radius and effective temperature measurements for very low mass stars within the next few years.
- Published
- 2021
16. WASP-South hot Jupiters: WASP-178b, WASP-184b, WASP-185b, and WASP-192b
- Author
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Michaël Gillon, David R. Anderson, Khalid Barkaoui, Francesco Pepe, Francisco J. Pozuelos, Laetitia Delrez, Stéphane Udry, Zouhair Benkhaldoun, Louise D. Nielsen, Amaury H. M. J. Triaud, Pierre F. L. Maxted, A. Collier Cameron, Don Pollacco, Didier Queloz, Artem Burdanov, Damien Ségransan, Oliver Turner, Richard G. West, Coel Hellier, Barry Smalley, François Bouchy, Emmanuel Jehin, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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FOS: Physical sciences ,Orbital eccentricity ,Astrophysics ,individual: WASP-192 [Stars] ,01 natural sciences ,Planet ,0103 physical sciences ,Hot Jupiter ,QB Astronomy ,Transit (astronomy) ,individual: WASP-178 [Stars] ,010303 astronomy & astrophysics ,QC ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,individual: WASP-184 [Stars] ,Astronomy and Astrophysics ,3rd-DAS ,Radius ,Planetary system ,Orbital period ,Planetary systems ,Stars ,QC Physics ,individual: WASP-185 [Stars] ,Space and Planetary Science ,QB799 ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report on four new transiting hot Jupiters discovered by the WASP-South survey. WASP-178b transits a V = 9.9, A1V star with Teff = 9350 +/- 150 K, the second-hottest transit host known. It has a highly bloated radius of 1.81 +/- 0.09 Rjup, in line with the known correlation between high irradiation and large size. With an estimated temperature of 2470 +/- 60 K, the planet is one of the best targets for studying ultra-hot Jupiters that is visible from the Southern hemisphere. The three host stars WASP-184, WASP-185 and WASP-192 are all post-main-sequence G0 stars of ages 4-8 Gyr. The larger stellar radii (1.3-1.7 Msun) mean that the transits are relatively shallow (0.7-0.9%) even though the planets have moderately inflated radii of 1.2-1.3 Rjup. WASP-185b has an eccentric orbit (e = 0.24) and a relatively long orbital period of 9.4 d. A star that is 4.6 arcsec from WASP-185 and 4.4 mag fainter might be physically associated., Version as Accepted for MNRAS (RV table added)
- Published
- 2019
17. WASP-180Ab: Doppler tomography of a hot Jupiter orbiting the primary star in a visual binary
- Author
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Don Pollacco, Stéphane Udry, Oliver Turner, Richard G. West, James McCormac, Damien Ségransan, L. Y. Temple, B. Zouhair, L. Delrez, François Bouchy, Amaury H. M. J. Triaud, Emmanuel Jehin, Daniel F. Evans, Pierre F. L. Maxted, Monika Lendl, A. Collier Cameron, Susan E. Thompson, Francesco Pepe, David R. Anderson, Michaël Gillon, Khalid Barkaoui, Barry Smalley, D. J. A. Brown, D. Queloz, Louise D. Nielsen, Coel Hellier, C. Murray, Elsa Ducrot, Artem Burdanov, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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FOS: Physical sciences ,Star (graph theory) ,01 natural sciences ,spectroscopic [Techniques] ,Primary (astronomy) ,QB460 ,0103 physical sciences ,Hot Jupiter ,QB Astronomy ,010303 astronomy & astrophysics ,QC ,QB ,Visual binary ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,European research ,photometric [Techniques] ,Astronomy ,DAS ,Astronomy and Astrophysics ,Doppler tomography ,Planetary system ,rotation [Stars] ,Planetary systems ,QC Physics ,Space and Planetary Science ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery and characterisation of WASP-180Ab, a hot Jupiter confirmed by the detection of its Doppler shadow and by measuring its mass using radial velocities. We find the 0.9 $\pm$ 0.1 $M_{\rm Jup}$, 1.24 $\pm$ 0.04 $R_{\rm Jup}$ planet to be in a misaligned, retrograde orbit around an F7 star with $T_{\rm eff}$ = 6500K and a moderate rotation speed of vsini = 19.9 km s$^{-1}$. The host star is the primary of a $V$ = 10.7 binary, where a secondary separated by 5$''$ ($\sim$1200 AU) contributes $\sim$30% of the light. WASP-180Ab therefore adds to a small sample of transiting hot Jupiters known in binary systems. A 4.6-day modulation seen in the WASP data is likely to be the rotational modulation of the companion star, WASP-180B., Comment: 9 pages, 6 figures, accepted by MNRAS
- Published
- 2019
18. SuperWASP dispositions and false positive catalogue
- Author
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Magali Deleuil, Howard M. Relles, J. Bochinski, Jose-Manuel Almenara, Guillaume Hébrard, Don Pollacco, François Bouchy, David R. Anderson, R. Busuttil, D. Queloz, Ulrich Kolb, K. L. Hay, Emmanuel Jehin, Laetitia Delrez, Aldo S. Bonomo, Amaury H. M. J. Triaud, Francisco J. Pozuelos, Leslie Hebb, Barry Smalley, Grant Miller, A. Collier Cameron, Pierre F. L. Maxted, Peter J. Wheatley, S. C. C. Barros, Stéphane Udry, David J. Armstrong, Michaël Gillon, D. J. A. Brown, N. Schanche, Artem Burdanov, Francesca Faedi, Khalid Al-Subai, Richard G. West, Khalid Barkaoui, Louise D. Nielsen, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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. St Andrews Centre for Exoplanet Science, and University of St Andrews. School of Physics and Astronomy
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planets and satellites: detection ,media_common.quotation_subject ,law.invention ,Telescope ,Observatory ,Planet ,law ,QB460 ,QB Astronomy ,observational [Methods] ,QC ,catalogues ,QB ,media_common ,Physics ,Northern Hemisphere ,Astronomy ,DAS ,Astronomy and Astrophysics ,Catalogues ,Methods observational ,detection [Planets and satellites] ,QC Physics ,[SDU]Sciences of the Universe [physics] ,Space and Planetary Science ,Sky ,methods: observational - Abstract
NS acknowledges the support of the National Priorities Research Program (NPRP) grant #X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). ACC acknowledges support from the Science & Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. SuperWASP, the Northern hemisphere WASP observatory, has been observing the skies from La Palma since 2004. In that time, more than 50 planets have been discovered with data contributions from SuperWASP. In the process of validating planets, many false-positive candidates have also been identified. The TESS telescope is set to begin observations of the northern sky in 2019. Similar to the WASP survey, the TESS pixel size is relatively large (13arcsec for WASP and 21arcsec for TESS), making it susceptible to many blended signals and false detections caused principally by grazing and blended stellar eclipsing binary systems. In order to reduce duplication of effort on targets, we present a catalogue of 1041 Northern hemisphere SuperWASP targets that have been rejected as planetary transits through follow-up observation. Publisher PDF
- Published
- 2019
19. High-resolution spectroscopy of Boyajian’s star during optical dimming events
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Carlos González-Fernández, Sergio Simón-Díaz, Emilio Molinari, Thomas Masseron, G. Holgado, Tabetha S. Boyajian, Jason T. Wright, A. Collier Cameron, Grant M. Kennedy, J. Saario, Hector Socas-Navarro, M. J. Martínez González, B. Toledo-Padrón, J. I. González Hernández, A. Asensio Ramos, C. Westendorp Plaza, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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Epoch (astronomy) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Star (graph theory) ,01 natural sciences ,circumstellar matter [Stars] ,0103 physical sciences ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,observational [Methods] ,010303 astronomy & astrophysics ,Chromosphere ,Solar and Stellar Astrophysics (astro-ph.SR) ,QC ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,010308 nuclear & particles physics ,Stellar atmosphere ,DAS ,Astronomy and Astrophysics ,Light curve ,findamental parameters [Stars] ,Interstellar medium ,Radial velocity ,QC Physics ,Radiative equilibrium ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,activity [Stars] - Abstract
Boyajian's star is an apparently normal main sequence F-type star with a very unusual light curve. The dipping activity of the star, discovered during the Kepler mission, presents deep, asymmetric, and aperiodic events. Here we present high resolution spectroscopic follow-up during some dimming events recorded post-Kepler observations, from ground-based telescopes. We analise data from the HERMES, HARPS-N and FIES spectrographs to characterise the stellar atmosphere and to put some constraints on the hypotheses that have appeared in the literature concerning the occulting elements. The star's magnetism, if existing, is not extreme. The spots on the surface, if present, would occupy 0.02% of the area, at most. The chromosphere, irrespective of the epoch of observation, is hotter than the values expected from radiative equilibrium, meaning that the star has some degree of activity. We find no clear evidence of the interstellar medium nor exocoments being responsible for the dimmings of the light curve. However, we detect at 1-2 sigma level, a decrease of the radial velocity of the star during the first dip recorded after the \emph{\emph{Kepler}} observations. We claim the presence of an optically thick object with likely inclined and high impact parameter orbits that produces the observed Rossiter-McLaughlin effect., Comment: submitted to MNRAS
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- 2019
20. Three hot-Jupiters on the upper edge of the mass–radius distribution: WASP-177, WASP-181, and WASP-183
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Barry Smalley, Francisco J. Pozuelos, Louise D. Nielsen, Oliver Turner, Richard G. West, Emmanuel Jehin, Khalid Barkaoui, Zouhair Benkhaldoun, Stéphane Udry, Damien Ségransan, Coel Hellier, Francesco Pepe, F. Bouchy, Didier Queloz, Amaury H. M. J. Triaud, Artem Burdanov, A. Collier Cameron, Michaël Gillon, D. J. A. Brown, Elsa Ducrot, Monika Lendl, Don Pollacco, David R. Anderson, Pierre F. L. Maxted, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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individual: WASP-177b [Planets and satellites] ,FOS: Physical sciences ,Astrophysics ,Star (graph theory) ,01 natural sciences ,Upper and lower bounds ,Planet ,individual: WASP-181b [Planets and satellites] ,0103 physical sciences ,Hot Jupiter ,QB Astronomy ,010303 astronomy & astrophysics ,QC ,QB600 ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,DAS ,Astronomy and Astrophysics ,Radius ,detection [Planets and satellites] ,QC Physics ,Distribution (mathematics) ,Space and Planetary Science ,Orbit (control theory) ,individual: WASP-183b [Planets and satellites] ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery of 3 transiting planets from the WASP survey, two hot-Jupiters: WASP-177b (~0.5 M_Jup, ~1.6 R_Jup) in a 3.07-d orbit of a V = 12.6 K2 star, WASP-183b (~0.5 M_Jup, ~1.5 R_Jup) in a 4.11-d orbit of a V = 12.8 G9/K0 star; and one hot-Saturn planet WASP-181b (~0.3 M_Jup, ~1.2 R_Jup) in a 4.52-d orbit of a V = 12.9 G2 star. Each planet is close to the upper bound of mass-radius space and has a scaled semi-major axis, a/R_star, between 9.6 and 12.1. These lie in the transition between systems that tend to be in orbits that are well aligned with their host-star's spin and those that show a higher dispersion., 11 pages, 9 figures, 5 tables
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- 2019
21. The EBLM project – VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves
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Swayne, M I, primary, Maxted, P F L, additional, Triaud, A H M J, additional, Sousa, S G, additional, Broeg, C, additional, Florén, H-G, additional, Guterman, P, additional, Simon, A E, additional, Boisse, I, additional, Bonfanti, A, additional, Martin, D, additional, Santerne, A, additional, Salmon, S, additional, Standing, M R, additional, Van Grootel, V, additional, Wilson, T G, additional, Alibert, Y, additional, Alonso, R, additional, Anglada Escudé, G, additional, Asquier, J, additional, Bárczy, T, additional, Barrado, D, additional, Barros, S C C, additional, Battley, M, additional, Baumjohann, W, additional, Beck, M, additional, Beck, T, additional, Bekkelien, A, additional, Benz, W, additional, Billot, N, additional, Bonfils, X, additional, Brandeker, A, additional, Busch, M-D, additional, Cabrera, J, additional, Charnoz, S, additional, Collier Cameron, A, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Deline, A, additional, Delrez, L, additional, Demangeon, O D S, additional, Demory, B-O, additional, Dransfield, G, additional, Ehrenreich, D, additional, Erikson, A, additional, Fortier, A, additional, Fossati, L, additional, Fridlund, M, additional, Futyan, D, additional, Gandolfi, D, additional, Gillon, M, additional, Guedel, M, additional, Hébrard, G, additional, Heidari, N, additional, Hellier, C, additional, Heng, K, additional, Hobson, M, additional, Hoyer, S, additional, Isaak, K G, additional, Kiss, L, additional, Kunovac Hodžić, V, additional, Lalitha, S, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, Marafatto, L, additional, McCormac, J, additional, Miller, N, 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, Walter, I, additional, Walton, N A, additional, and Willett, E, additional
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- 2021
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22. Separating planetary reflex Doppler shifts from stellar variability in the wavelength domain
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Collier Cameron, A, primary, Ford, E B, additional, Shahaf, S, additional, Aigrain, S, additional, Dumusque, X, additional, Haywood, R D, additional, Mortier, A, additional, Phillips, D F, additional, Buchhave, L, additional, Cecconi, M, additional, Cegla, H, additional, Cosentino, R, additional, Crétignier, M, additional, Ghedina, A, additional, González, M, additional, Latham, D W, additional, Lodi, M, additional, López-Morales, M, additional, Micela, G, additional, Molinari, E, additional, Pepe, F, additional, Piotto, G, additional, Poretti, E, additional, Queloz, D, additional, Juan, J San, additional, Ségransan, D, additional, Sozzetti, A, additional, Szentgyorgyi, A, additional, Thompson, S, additional, Udry, S, additional, and Watson, C, additional
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- 2021
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23. An unusually low density ultra-short period super-Earth and three mini-Neptunes around the old star TOI-561
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Lacedelli, G, primary, Malavolta, L, additional, Borsato, L, additional, Piotto, G, additional, Nardiello, D, additional, Mortier, A, additional, Stalport, M, additional, Collier Cameron, A, additional, Poretti, E, additional, Buchhave, L A, additional, López-Morales, M, additional, Nascimbeni, V, additional, Wilson, T G, additional, Udry, S, additional, Latham, D W, additional, Bonomo, A S, additional, Damasso, M, additional, Dumusque, X, additional, Jenkins, J M, additional, Lovis, C, additional, Rice, K, additional, Sasselov, D, additional, Winn, J N, additional, Andreuzzi, G, additional, Cosentino, R, additional, Charbonneau, D, additional, Di Fabrizio, L, additional, Martnez Fiorenzano, A F, additional, Ghedina, A, additional, Harutyunyan, A, additional, Lienhard, F, additional, Micela, G, additional, Molinari, E, additional, Pagano, I, additional, Pepe, F, additional, Phillips, D F, additional, Pinamonti, M, additional, Ricker, G, additional, Scandariato, G, additional, Sozzetti, A, additional, and Watson, C A, additional
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- 2020
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24. K2-111: an old system with two planets in near-resonance†
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Mortier, A, primary, Zapatero Osorio, M R, additional, Malavolta, L, additional, Alibert, Y, additional, Rice, K, additional, Lillo-Box, J, additional, Vanderburg, A, additional, Oshagh, M, additional, Buchhave, L, additional, Adibekyan, V, additional, Delgado Mena, E, additional, Lopez-Morales, M, additional, Charbonneau, D, additional, Sousa, S G, additional, Lovis, C, additional, Affer, L, additional, Allende Prieto, C, additional, Barros, S C C, additional, Benatti, S, additional, Bonomo, A S, additional, Boschin, W, additional, Bouchy, F, additional, Cabral, A, additional, Collier Cameron, A, additional, Cosentino, R, additional, Cristiani, S, additional, Demangeon, O D S, additional, Di Marcantonio, P, additional, D’Odorico, V, additional, Dumusque, X, additional, Ehrenreich, D, additional, Figueira, P, additional, Fiorenzano, A, additional, Ghedina, A, additional, González Hernández, J I, additional, Haldemann, J, additional, Harutyunyan, A, additional, Haywood, R D, additional, Latham, D W, additional, Lavie, B, additional, Lo Curto, G, additional, Maldonado, J, additional, Manescau, A, additional, Martins, C J A P, additional, Mayor, M, additional, Mégevand, D, additional, Mehner, A, additional, Micela, G, additional, Molaro, P, additional, Molinari, E, additional, Nunes, N J, additional, Pepe, F A, additional, Palle, E, additional, Phillips, D, additional, Piotto, G, additional, Pinamonti, M, additional, Poretti, E, additional, Riva, M, additional, Rebolo, R, additional, Santos, N C, additional, Sasselov, D, additional, Sozzetti, A, additional, Suárez Mascareño, A, additional, Udry, S, additional, West, R G, additional, Watson, C A, additional, and Wilson, T G, additional
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- 2020
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25. WASP-186 and WASP-187: two hot Jupiters discovered by SuperWASP and SOPHIE with additional observations by TESS
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Schanche, N, primary, Hébrard, G, additional, Collier Cameron, A, additional, Dalal, S, additional, Smalley, B, additional, Wilson, T G, additional, Boisse, I, additional, Bouchy, F, additional, Brown, D J A, additional, Demangeon, O, additional, Haswell, C A, additional, Hellier, C, additional, Kolb, U C, additional, Lopez, T, additional, Maxted, P F L, additional, Pollacco, D L, additional, West, R G, additional, and Wheatley, P J, additional
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- 2020
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26. The EBLM project – VII. Spin–orbit alignment for the circumbinary planet host EBLM J0608-59 A/TOI-1338 A
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Kunovac Hodžić, Vedad, primary, Triaud, Amaury H M J, additional, Martin, David V, additional, Fabrycky, Daniel C, additional, Cegla, Heather M, additional, Collier Cameron, Andrew, additional, Gill, Samuel, additional, Hellier, Coel, additional, Kostov, Veselin B, additional, Maxted, Pierre F L, additional, Orosz, Jerome A, additional, Pepe, Francesco, additional, Pollacco, Don, additional, Queloz, Didier, additional, Ségransan, Damien, additional, Udry, Stéphane, additional, and Welsh, William F, additional
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- 2020
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27. The spectral impact of magnetic activity on disc-integrated HARPS-N solar observations: exploring new activity indicators
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Thompson, A P G, primary, Watson, C A, additional, Haywood, R D, additional, Costes, J C, additional, de Mooij, E, additional, Collier Cameron, A, additional, Dumusque, X, additional, Phillips, D F, additional, Saar, S H, additional, Mortier, A, additional, Milbourne, T W, additional, Aigrain, S, additional, Cegla, H M, additional, Charbonneau, D, additional, Cosentino, R, additional, Ghedina, A, additional, Latham, D W, additional, López-Morales, M, additional, Micela, G, additional, Molinari, E, additional, Poretti, E, additional, Sozzetti, A, additional, Thompson, S, additional, and Walsworth, R, additional
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- 2020
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28. A Kepler study of starspot lifetimes with respect to light-curve amplitude and spectral type
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H. Giles, Andrew Collier Cameron, Raphaëlle D. Haywood, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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NDAS ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Kepler ,0103 physical sciences ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,QC ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,photometric [Techniques] ,Starspot ,Astronomy ,Astronomy and Astrophysics ,Light curve ,Starspots ,rotation [Stars] ,QC Physics ,Amplitude ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,activity [Stars] ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Wide-field high precision photometric surveys such as Kepler have produced reams of data suitable for investigating stellar magnetic activity of cooler stars. Starspot activity produces quasi-sinusoidal light curves whose phase and amplitude vary as active regions grow and decay over time. Here we investigate, firstly, whether there is a correlation between the size of starspots - assumed to be related to the amplitude of the sinusoid - and their decay timescale and, secondly, whether any such correlation depends on the stellar effective temperature. To determine this, we computed the autocorrelation functions of the light curves of samples of stars from Kepler and fitted them with apodised periodic functions. The light curve amplitudes, representing spot size were measured from the root-mean-squared scatter of the normalised light curves. We used a Monte Carlo Markov Chain to measure the periods and decay timescales of the light curves. The results show a correlation between the decay time of starspots and their inferred size. The decay time also depends strongly on the temperature of the star. Cooler stars have spots that last much longer, in particular for stars with longer rotational periods. This is consistent with current theories of diffusive mechanisms causing starspot decay. We also find that the Sun is not unusually quiet for its spectral type - stars with solar-type rotation periods and temperatures tend to have (comparatively) smaller starspots than stars with mid-G or later spectral types., Comment: Accepted for publication in MNRAS, 11 pages, 8 figures
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- 2017
29. Using HARPS-N to characterise the long-period planets in the PH-2 and Kepler-103 systems
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Chantanelle Nava, Sophie C Dubber, Francesco Pepe, Raphaëlle D. Haywood, Ennio Poretti, Andrew Collier Cameron, Stéphane Udry, Alessandro Sozzetti, David W. Latham, A. Coffinet, Aldo S. Bonomo, Walter Boschin, Giampaolo Piotto, David Charbonneau, H. Giles, Luca Malavolta, Xavier Dumusque, Ken Rice, Andrew Vanderburg, Avet Harutyunyan, Adriano Ghedina, Mercedes López-Morales, Emilio Molinari, Rosario Cosentino, Giuseppina Micela, Annelies Mortier, David F. Phillips, Lars A. Buchhave, Dimitar Sasselov, Mortier, Annelies [0000-0001-7254-4363], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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NDAS ,FOS: Physical sciences ,Astrophysics ,Type (model theory) ,01 natural sciences ,Single star ,spectroscopic [Techniques] ,techniques: photometric ,Planet ,Long period ,0103 physical sciences ,techniques: radial velocities ,Astrophysics::Solar and Stellar Astrophysics ,QB Astronomy ,010303 astronomy & astrophysics ,QC ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,radial velocities [Techniques] ,010308 nuclear & particles physics ,photometric [Techniques] ,planets and satellites: composition ,Astronomy and Astrophysics ,Radius ,Planets and satellites ,composition ,Orbital period ,Exoplanet ,QC Physics ,Space and Planetary Science ,composition [Planets and satellites] ,astro-ph.EP ,techniques: spectroscopic ,Astrophysics::Earth and Planetary Astrophysics ,Planetary mass ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely-populated category of exoplanet. We use {\it Kepler} light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5-$\sigma$ mass estimate of $M_p = 109^{+30}_{-32}$ M$_\oplus$ and a radius of $R_p = 9.49\pm0.16$ R$_\oplus$. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period $P > 200$ days that orbits a single star. We find that Kepler-103b has a mass of $M_{\text{p,b}} = 11.7^{+4.31}_{-4.72}$ M$_{\oplus}$ and Kepler-103c has a mass of $M_{\text{p,c}} = 58.5^{+11.2}_{-11.4}$ M$_{\oplus}$. These are 2.5$\sigma$ and 5$\sigma$ results, respectively. With radii of $R_{\text{p,b}} = 3.49^{+0.06}_{-0.05}$ R$_\oplus$, and $R_{\text{p,c}} = 5.45^{+0.18}_{-0.17}$ R$_\oplus$, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period $P > 100$ days. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass-radius relation across the full range of exoplanet masses and radii., The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), the University of St Andrews, Queen’s University Belfast, and the University of Edinburgh. AM acknowledges support from Senior Kavli Institute Fellowships at the University of Cambridge. ACC acknowledges support from the Science & Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. AV’s and RDH’s work was performed under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. LM acknowledges support from PLATO ASI-INAF agreement n.2015-019-R.1-2018 This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is partly based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. Some of this work has been carried out in the frame of the National Centre for Competence in Research ‘PlanetS’ supported by the Swiss National Science Foundation (SNSF).
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- 2019
30. High-precision multiwavelength eclipse photometry of the ultra-hot gas giant exoplanetWASP-103 b
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Delrez, L, Madhusudhan, N, Lendl, M, Gillon, M, Anderson, DR, Neveu-VanMalle, M, Bouchy, F, Burdanov, A, Collier-Cameron, A, Demory, BO, Hellier, C, Jehin, E, Magain, P, Maxted, PFL, Queloz, D, Smalley, B, Triaud, AHMJ, Delrez, Laetitia [0000-0001-6108-4808], Nikku, Madhusudhan [0000-0002-4869-000X], Queloz, Didier [0000-0002-3012-0316], Triaud, Amaury [0000-0002-5510-8751], and Apollo - University of Cambridge Repository
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planets and satellites: atmospheres ,stars: individual: WASP-103 ,techniques: photometric ,techniques: radial velocities ,Astrophysics::Earth and Planetary Astrophysics ,planetary systems - Abstract
© 2017 The Author(s). We present 16 occultation and three transit light curves for the ultra-short period hot Jupiter WASP-103b, in addition to five new radial velocity measurements. We combine these observations with archival data and perform a global analysis of the resulting extensive data set, accounting for the contamination from a nearby star. We detect the thermal emission of the planet in both the z' and KS bands, the measured occultation depths being 699±110 ppm (6.4σ) and 3567 -350 +400 ppm (10.2σ), respectively. We use these two measurements, together with recently published HST/WFC3 data, to derive joint constraints on the properties of WASP- 103b's dayside atmosphere. On one hand, we find that the z' band and WFC3 data are best fit by an isothermal atmosphere at 2900K or an atmosphere with a low H 2 O abundance. On the other hand, we find an unexpected excess in the K S band measured flux compared to these models, which requires confirmation with additional observations before any interpretation can be given. From our global data analysis, we also derive a broad-band optical transmission spectrum that shows a minimum around 700 nm and increasing values towards both shorter and longer wavelengths. This is in agreement with a previous study based on a large fraction of the archival transit light curves used in our analysis. The unusual profile of this transmission spectrum is poorly matched by theoretical spectra and is not confirmed by more recent observations at higher spectral resolution. Additional data, in both emission and transmission, are required to better constrain the atmospheric properties of WASP-103b.
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- 2018
31. WASP-180Ab: Doppler tomography of a hot Jupiter orbiting the primary star in a visual binary
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Temple, L Y, primary, Hellier, C, additional, Anderson, D R, additional, Barkaoui, K, additional, Bouchy, F, additional, Brown, D J A, additional, Burdanov, A, additional, Collier Cameron, A, additional, Delrez, L, additional, Ducrot, E, additional, Evans, D, additional, Gillon, M, additional, Jehin, E, additional, Lendl, M, additional, Maxted, P F L, additional, McCormac, J, additional, Murray, C, additional, Nielsen, L D, additional, Pepe, F, additional, Pollacco, D, additional, Queloz, D, additional, Ségransan, D, additional, Smalley, B, additional, Thompson, S, additional, Triaud, A H M J, additional, Turner, O D, additional, Udry, S, additional, West, R G, additional, and Zouhair, B, additional
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- 2019
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32. Magnetic field, activity, and companions of V410 Tau
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Yu, L, primary, Donati, J-F, additional, Grankin, K, additional, Collier Cameron, A, additional, Moutou, C, additional, Hussain, G, additional, Baruteau, C, additional, Jouve, L, additional, and MaTYSSE collaboration, the, additional
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- 2019
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33. SuperWASP dispositions and false positive catalogue
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Schanche, N, primary, Collier Cameron, A, additional, Almenara, J M, additional, Alsubai, K A, additional, Anderson, D R, additional, Armstrong, D J, additional, Barkaoui, K, additional, Barros, S C C, additional, Bochiński, J, additional, Bonomo, A S, additional, Bouchy, F, additional, Brown, D J A, additional, Burdanov, A, additional, Busuttil, R, additional, Deleuil, M, additional, Delrez, L, additional, Faedi, F, additional, Gillon, M, additional, Hay, K, additional, Hebb, L, additional, Hébrard, G, additional, Jehin, E, additional, Kolb, U, additional, Maxted, P F L, additional, Miller, G, additional, Nielsen, L D, additional, Pollacco, D L, additional, Pozuelos, F J, additional, Queloz, D, additional, Relles, H, additional, Smalley, B, additional, Triaud, A H M J, additional, Udry, S, additional, West, R, additional, and Wheatley, P J, additional
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- 2019
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34. WASP-166b: a bloated super-Neptune transiting a V = 9 star
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Hellier, Coel, primary, Anderson, D R, primary, Triaud, A H M J, primary, Bouchy, F, primary, Burdanov, A, primary, Collier Cameron, A, primary, Delrez, L, primary, Ehrenreich, D, primary, Gillon, M, primary, Jehin, E, primary, Lendl, M, primary, Linder, E, primary, Nielsen, L D, primary, Maxted, P F L, primary, Pepe, F, primary, Pollacco, D, primary, Queloz, D, primary, Ségransan, D, primary, Smalley, B, primary, Spake, J J, primary, Temple, L Y, primary, Udry, S, primary, West, R G, primary, and Wyttenbach, A, primary
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- 2019
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35. Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum
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Collier Cameron, A, primary, Mortier, A, primary, Phillips, D, primary, Dumusque, X, primary, Haywood, R D, primary, Langellier, N, primary, Watson, C A, primary, Cegla, H M, primary, Costes, J, primary, Charbonneau, D, primary, Coffinet, A, primary, Latham, D W, primary, Lopez-Morales, M, primary, Malavolta, L, primary, Maldonado, J, primary, Micela, G, primary, Milbourne, T, primary, Molinari, E, primary, Saar, S H, primary, Thompson, S, primary, Buchschacher, N, primary, Cecconi, M, primary, Cosentino, R, primary, Ghedina, A, primary, Glenday, A, primary, Gonzalez, M, primary, Li, C-H, primary, Lodi, M, primary, Lovis, C, primary, Pepe, F, primary, Poretti, E, primary, Rice, K, primary, Sasselov, D, primary, Sozzetti, A, primary, Szentgyorgyi, A, primary, Udry, S, primary, and Walsworth, R, primary
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- 2019
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36. Reducing activity-induced variations in a radial-velocity time series of the Sun as a star
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Lanza, A F, primary, Collier Cameron, A, primary, and Haywood, R D, primary
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- 2019
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37. High-resolution spectroscopy of Boyajian’s star during optical dimming events
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Martínez González, M J, primary, González-Fernández, C, additional, Asensio Ramos, A, additional, Socas-Navarro, H, additional, Westendorp Plaza, C, additional, Boyajian, T S, additional, Wright, J T, additional, Collier Cameron, A, additional, González Hernández, J I, additional, Holgado, G, additional, Kennedy, G M, additional, Masseron, T, additional, Molinari, E, additional, Saario, J, additional, Simón-Díaz, S, additional, and Toledo-Padrón, B, additional
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- 2019
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38. Three hot-Jupiters on the upper edge of the mass–radius distribution: WASP-177, WASP-181, and WASP-183
- Author
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Turner, Oliver D, primary, Anderson, D R, additional, Barkaoui, K, additional, Bouchy, F, additional, Benkhaldoun, Z, additional, Brown, D J A, additional, Burdanov, A, additional, Collier Cameron, A, additional, Ducrot, E, additional, Gillon, M, additional, Hellier, C, additional, Jehin, E, additional, Lendl, M, additional, Maxted, P F L, additional, Nielsen, L D, additional, Pepe, F, additional, Pollacco, D, additional, Pozuelos, F J, additional, Queloz, D, additional, Ségransan, D, additional, Smalley, B, additional, Triaud, A H M J, additional, Udry, S, additional, and West, R G, additional
- Published
- 2019
- Full Text
- View/download PDF
39. Slingshot prominences: nature’s wind gauges
- Author
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Jardine, Moira, primary and Collier Cameron, Andrew, additional
- Published
- 2018
- Full Text
- View/download PDF
40. The thermal emission of the exoplanet WASP-3b
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Andrew Collier Cameron, Jonathan J. Fortney, J. W. Rostron, David R. Anderson, Heather Knutson, Peter J. Wheatley, Don Pollacco, Joseph Harrington, Science & Technology Facilities Council, PPARC - Now STFC, and University of St Andrews. School of Physics and Astronomy
- Subjects
Physics ,Brightness ,Infrared ,individual: WASP-3 [Stars] ,individual: WASP-3b [Planets and satellites] ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Atmospheric model ,Light curve ,Exoplanet ,QC Physics ,Spitzer Space Telescope ,Space and Planetary Science ,Planet ,Hot Jupiter ,atmospheres [Planets and satellites] ,QB Astronomy ,data analysis [Methods] ,QC ,QB - Abstract
We report the detection of thermal emission from the transiting hot Jupiter WASP-3b at 3.6, 4.5 and 8.0 μm using the Spitzer Space Telescope. We obtain planet-to-star flux ratios of 0.209^(+0.040)_(−0.028), 0.282 ± 0.012 and 0.328^(+0.086)_(−0.055) per cent at these wavelengths, respectively, implying infrared brightness temperatures of T_(3.6μm) =2280^(+210)_(−150) K , T_(4.5 μm) = 2400 ± 80 K and T_(8.0μm) =2210^(+390)_(−250) K . We find that WASP-3b falls into an emerging class of highly irradiated planets whose measured temperatures suggest that the planets are dark and redistribute heat around the planet inefficiently. The latter is similarly concluded from 1D atmospheric model comparisons, which also favour the presence of an atmospheric temperature inversion. We compare the WASP-3 system to the proposed inversion–activity relation, finding that it hints at a more complex relation than a simple cut-off in activity implied by previous data. Using eclipse timings we also constrain e cos ω to be −0.0006^(+0.0010)_(−0.0006), suggesting that the eccentricity of WASP-3b can only be large for a narrow range of ω.
- Published
- 2014
41. High-frequency A-type pulsators discovered using SuperWASP★†
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Francesca Faedi, Laetitia Delrez, Michaël Gillon, Coel Hellier, Andrew Norton, Daniel Luke Holdsworth, John Southworth, Richard G. West, David R. Anderson, Don Pollacco, Emmanuel Jehin, Keith Horne, A. Collier Cameron, Alexis M. S. Smith, Peter J. Wheatley, Pierre F. L. Maxted, Kelsey I. Clubb, S. C. C. Barros, Carole A. Haswell, Barry Smalley, I. Skillen, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
- Subjects
Kepler observations ,Metallic-line ,oscillations [Stars] ,FOS: Physical sciences ,F500 ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Surveys ,01 natural sciences ,Asteroseismology ,Rapidly oscillating AP ,ROAP stars ,0103 physical sciences ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,Delta-scuti ,Sky survey ,010303 astronomy & astrophysics ,QC ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,chemically peculiar [Stars] ,QB ,Physics ,Planet-detection ,010308 nuclear & particles physics ,photometric [Techniques] ,Atmospheric parameters ,Astronomy ,Astronomy and Astrophysics ,Radial-velocity ,variables: δ Scuti [Sstars] ,Radial velocity ,Stars ,QC Physics ,Amplitude ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Catalog ,Astrophysics::Earth and Planetary Astrophysics ,Variable star - Abstract
We present the results of a survey using the WASP archive to search for high frequency pulsations in F-, A- and B-type stars. Over 1.5 million targets have been searched for pulsations with amplitudes greater than 0.5 millimagnitude. We identify over 350 stars which pulsate with periods less than 30 min. Spectroscopic follow-up of selected targets has enabled us to confirm 10 new rapidly oscillating Ap stars, 13 pulsating Am stars and the fastest known $\delta$ Scuti star. We also observe stars which show pulsations in both the high-frequency domain and in the low-frequency $\delta$ Scuti range. This work shows the power of the WASP photometric survey to find variable stars with amplitudes well below the nominal photometric precision per observation., Comment: 19 pages, 26 figures, accepted for publication in MNRAS
- Published
- 2014
42. Distribution and evolution of starspots on the RS CVn binary II Pegasi in 2004
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Yue Xiang, John R. Barnes, Shenghong Gu, A. Collier Cameron, Science & Technology Facilities Council, PPARC - Now STFC, and University of St Andrews. School of Physics and Astronomy
- Subjects
Physics ,individual: II Peg [Stars] ,Epoch (astronomy) ,Equator ,Starspot ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Ephemeris ,Orbital period ,Starspots ,Latitude ,symbols.namesake ,QC Physics ,Space and Planetary Science ,imaging [Stars] ,symbols ,QB Astronomy ,Longitude ,close [Binaries] ,Doppler effect ,activity [Stars] ,QC ,QB - Abstract
This work is supported by National Natural Science Foundation of China through grants Nos. 10373023, 10773027 and 11333006, Chinese Academy of Sciences through project KJCX2-YW-T24. We present Doppler images of RS CVn-type binary II Peg based on two data sets obtained in 2004 February and November. In order to improve signal-to-noise ratio and reliability,we apply least-squares deconvolution technique to calculate average profiles from 2032 photospheric absorption lines. Both of the resulting surface images show a wide latitude distribution of starspots. Most spots are concentrated at a high-latitude belt above 60° and a low-latitude belt near equator. The starspots evolved dramatically between two observing runs, which may indicate shorter time-scale evolution in this epoch, especially for low-latitude belt. There is no stable preferred active longitude that can be found in our images. We also find out a possible phenomenon that the intermediate-latitude spot migrated poleward and merged with the high-latitude spot to make it stronger, which may reveal a more complex behaviour of starspots on II Peg. A potential change of orbital ephemeris zero-point was detected. This may imply an orbital period change of II Peg like other active close binaries. Publisher PDF
- Published
- 2013
43. K2-263 b: a 50 d period sub-Neptune with a mass measurement using HARPS-N
- Author
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Mortier, A, primary, Bonomo, A S, additional, Rajpaul, V M, additional, Buchhave, L A, additional, Vanderburg, A, additional, Zeng, L, additional, López-Morales, M, additional, Malavolta, L, additional, Collier Cameron, A, additional, Dressing, C D, additional, Figueira, P, additional, Nascimbeni, V, additional, Rice, K, additional, Sozzetti, A, additional, Watson, C, additional, Affer, L, additional, Bouchy, F, additional, Charbonneau, D, additional, Harutyunyan, A, additional, Haywood, R D, additional, Johnson, J A, additional, Latham, D W, additional, Lovis, C, additional, Martinez Fiorenzano, A F, additional, Mayor, M, additional, Micela, G, additional, Molinari, E, additional, Motalebi, F, additional, Pepe, F, additional, Piotto, G, additional, Phillips, D, additional, Poretti, E, additional, Sasselov, D, additional, Ségransan, D, additional, and Udry, S, additional
- Published
- 2018
- Full Text
- View/download PDF
44. High-precision multiwavelength eclipse photometry of the ultra-hot gas giant exoplanet WASP-103 b
- Author
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Delrez, L, primary, Madhusudhan, N, additional, Lendl, M, additional, Gillon, M, additional, Anderson, D R, additional, Neveu-VanMalle, M, additional, Bouchy, F, additional, Burdanov, A, additional, Collier-Cameron, A, additional, Demory, B-O, additional, Hellier, C, additional, Jehin, E, additional, Magain, P, additional, Maxted, P F L, additional, Queloz, D, additional, Smalley, B, additional, and Triaud, A H M J, additional
- Published
- 2017
- Full Text
- View/download PDF
45. A small survey of the magnetic fields of planet-host stars★
- Author
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Moira Jardine, Andrew Collier Cameron, Rim Fares, Evgenya L. Shkolnik, C. Moutou, C. Catala, Jean-François Donati, Magali Deleuil, Science & Technology Facilities Council, PPARC - Now STFC, University of St Andrews. School of Physics and Astronomy, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire de Paris, Université Paris sciences et lettres (PSL), and 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)
- Subjects
K-type main-sequence star ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,polarimetric [Techniques] ,01 natural sciences ,individual [Stars] ,0103 physical sciences ,Hot Jupiter ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Stellar collision ,Stellar magnetic field ,Flare star ,Astronomy ,Astronomy and Astrophysics ,magnetic field [Stars] ,Planetary systems ,T Tauri star ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,activity [Stars] ,Superflare - Abstract
Using spectropolarimetry, we investigate the large-scale magnetic topologies of stars hosting close-in exoplanets. A small survey of ten stars has been done with the twin instruments TBL/NARVAL and CFHT/ESPaDOnS between 2006 and 2011. Each target consists of circular-polarization observations covering 7 to 22 days. For each of the 7 targets in which a magnetic field was detected, we reconstructed the magnetic field topology using Zeeman-Doppler imaging. Otherwise, a detection limit has been estimated. Three new epochs of observations of Tau Boo are presented, which confirm magnetic polarity reversal. We estimate that the cycle period is 2 years, but recall that a shorter period of 240 days can not still be ruled out. The result of our survey is compared to the global picture of stellar magnetic field properties in the mass-rotation diagram. The comparison shows that these giant planet-host stars tend to have similar magnetic field topologies to stars without detected hot-Jupiters. This needs to be confirmed with a larger sample of stars., Comment: Accepted for publication in Monthly Notices of The Royal Astronomical Society
- Published
- 2013
46. Thermal emission at 3.6–8 μm from WASP-19b: a hot Jupiter without a stratosphere orbiting an active star
- Author
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Michaël Gillon, Coel Hellier, Don Pollacco, Amaury H. M. J. Triaud, Nikku Madhusudhan, Richard G. West, D. Queloz, Joseph Harrington, A. Collier Cameron, Pierre F. L. Maxted, David R. Anderson, Alexis M. S. Smith, Barry Smalley, Christopher J. Campo, Peter J. Wheatley, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
- Subjects
individual: WASP-19b [Planets and satellites] ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Atmosphere ,Spitzer Space Telescope ,Planet ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,QB Astronomy ,data analysis [Methods] ,Stratosphere ,Astrophysics::Galaxy Astrophysics ,QC ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,photometric [Techniques] ,Astronomy ,Astronomy and Astrophysics ,individual: WASP-19 [Stars] ,Exoplanet ,Stars ,QC Physics ,Space and Planetary Science ,atmospheres [Planets and satellites] ,Spectral energy distribution ,Astrophysics::Earth and Planetary Astrophysics ,Occultations ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report detection of thermal emission from the exoplanet WASP-19b at 3.6, 4.5, 5.8 and 8.0 micron. We used the InfraRed Array Camera on the Spitzer Space Telescope to observe two occultations of WASP-19b by its host star. We combine our new detections with previous measurements of WASP-19b's emission at 1.6 and 2.09 micron to construct a spectral energy distribution of the planet's dayside atmosphere. By comparing this with model-atmosphere spectra, we find that the dayside atmosphere of WASP-19b lacks a strong temperature inversion. As WASP-19 is an active star (log RHK = -4.50 +/- 0.03), this finding supports the hypothesis of Knutson, Howard & Isaacson (2010) that inversions are suppressed in hot Jupiters orbiting active stars. The available data are unable to differentiate between a carbon-rich and an oxygen-rich atmosphere., As accepted for publication in MNRAS. 12 pages, 5 figures, 3 tables
- Published
- 2013
47. Accurate spectroscopic parameters of WASP planet host stars★
- Author
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Richard G. West, David R. Anderson, Amanda P. Doyle, Amaury H. M. J. Triaud, Don Pollacco, A. Collier Cameron, Michaël Gillon, Coel Hellier, Pierre F. L. Maxted, Barry Smalley, and Didier Queloz
- Subjects
Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Metallicity ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Effective temperature ,Surface gravity ,Spectral line ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Planet ,Hot Jupiter ,ddc:520 ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Equivalent width ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We have made a detailed spectral analysis of eleven Wide Angle Search for Planets (WASP) planet host stars using high signal-to-noise (S/N) HARPS spectra. Our line list was carefully selected from the spectra of the Sun and Procyon, and we made a critical evaluation of the atomic data. The spectral lines were measured using equivalent widths. The procedures were tested on the Sun and Procyon prior to be being used on the WASP stars. The effective temperature, surface gravity, microturbulent velocity and metallicity were determined for all the stars. We show that abundances derived from high S/N spectra are likely to be higher than those obtained from low S/N spectra, as noise can cause the equivalent width to be underestimated. We also show that there is a limit to the accuracy of stellar parameters that can be achieved, despite using high S/N spectra, and the average uncertainty in effective temperature, surface gravity, microturbulent velocity and metallicity is 83 K, 0.11 dex, 0.11 km/s and 0.10 dex respectively., 9 pages, 5 figures, accepted for publication in MNRAS
- Published
- 2012
48. Seven transiting hot Jupiters from WASP-South, Euler and TRAPPIST: WASP-47b, WASP-55b, WASP-61b, WASP-62b, WASP-63b, WASP-66b and WASP-67b
- Author
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Coel Hellier, D. R. Anderson, A. Collier Cameron, A. P. Doyle, A. Fumel, M. Gillon, E. Jehin, M. Lendl, P. F. L. Maxted, F. Pepe, D. Pollacco, D. Queloz, D. Ségransan, B. Smalley, A. M. S. Smith, J. Southworth, A. H. M. J. Triaud, S. Udry, and R. G. West
- Subjects
Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Stars ,13. Climate action ,Space and Planetary Science ,Planet ,Physics::Space Physics ,0103 physical sciences ,Hot Jupiter ,High Energy Physics::Experiment ,TRAPPIST ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Line (formation) - Abstract
We present seven new transiting hot Jupiters from the WASP-South survey. The planets are all typical hot Jupiters orbiting stars from F4 to K0 with magnitudes of V = 10.3 to 12.5. The orbital periods are all in the range 3.9--4.6 d, the planetary masses range from 0.4--2.3 Mjup and the radii from 1.1--1.4 Mjup. In line with known hot Jupiters, the planetary densities range from Jupiter-like to inflated (rho = 0.13--1.07 rho_jup). We use the increasing numbers of known hot Jupiters to investigate the distribution of their orbital periods and the 3--4-d "pile-up".
- Published
- 2012
49. Tidal evolution of close-in giant planets: evidence of type II migration?
- Author
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J. Veljanoski, W. K. M. Rice, and A. Collier Cameron
- Subjects
Physics ,education.field_of_study ,Angular momentum ,media_common.quotation_subject ,Population ,Astronomy ,Astronomy and Astrophysics ,Radius ,Star (graph theory) ,Orbit ,Space and Planetary Science ,Planet ,Hot Jupiter ,Astrophysics::Earth and Planetary Astrophysics ,Eccentricity (behavior) ,education ,Astrophysics::Galaxy Astrophysics ,media_common - Abstract
It is well accepted that 'hot Jupiters' did not form in situ, as the temperature in the protoplanetary disc at the radius at which they now orbit would have been too high for planet formation to have occurred. These planets, instead, form at larger radii and then move into the region in which they now orbit. The exact process that leads to the formation of these close-in planets is, however, unclear and it seems that there may be more than one mechanism that can produce these short-period systems. Dynamical interactions in multiple-planet systems can scatter planets into highly eccentric orbits which, if the pericentre is sufficiently close to the parent star, can be tidally circularised by tidal interactions between the planet and star. Furthermore, systems with distant planetary or stellar companions can undergo Kozai cycles which can result in a planet orbiting very close to its parent star. However, the most developed model for the origin of short period planets is one in which the planet exchanges angular momentum with the surrounding protoplanetary disc and spirals in towards the central star. In the case of 'hot Jupiters', the planet is expected to open a gap in the disc and migrate through Type II .migration. If this is the dominant mechanism for producing `hot Jupiters' then we would expect the currect properties of observed close-in giant planets to be consistent with an initial population resulting from Type II migration followed by evolution due to tidal interactions with the central star. We consider initial distributions that are consistent with Type II migration and find that after tidal evolution, the final distributions can be consistent with that observed. Our results suggest that a modest initial pile-up at a ~ 0.05 au is required and that the initial eccentricity distribution must peak at e \sim 0.
- Published
- 2012
50. Magnetic field, differential rotation and activity of the hot-Jupiter-hosting star HD 179949
- Author
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Rim Fares, S. Dieters, Isabella Pagano, Evgenya L. Shkolnik, A. F. Martinez Fiorenzano, Moira Jardine, Andrew Collier Cameron, C. Moutou, Antonio Maggio, Antonino F. Lanza, Jean-François Donati, and David A. Bohlender
- Subjects
Rotation period ,Physics ,010504 meteorology & atmospheric sciences ,Giant planet ,Magnetosphere ,Astronomy and Astrophysics ,Astrophysics ,Orbital period ,Rotation ,01 natural sciences ,13. Climate action ,Space and Planetary Science ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,Polar ,Differential rotation ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences - Abstract
HD 179949 is an F8V star, orbited by a giant planet at ~8 R* every 3.092514 days. The system was reported to undergo episodes of stellar activity enhancement modulated by the orbital period, interpreted as caused by Star-Planet Interactions (SPIs). One possible cause of SPIs is the large-scale magnetic field of the host star in which the close-in giant planet orbits. In this paper we present spectropolarimetric observations of HD 179949 during two observing campaigns (2009 September and 2007 June). We detect a weak large-scale magnetic field of a few Gauss at the surface of the star. The field configuration is mainly poloidal at both observing epochs. The star is found to rotate differentially, with a surface rotation shear of dOmega=0.216\pm0.061 rad/d, corresponding to equatorial and polar rotation periods of 7.62\pm0.07 and 10.3\pm0.8 d respectively. The coronal field estimated by extrapolating the surface maps resembles a dipole tilted at ~70 degrees. We also find that the chromospheric activity of HD 179949 is mainly modulated by the rotation of the star, with two clear maxima per rotation period as expected from a highly tilted magnetosphere. In September 2009, we find that the activity of HD 179949 shows hints of low amplitude fluctuations with a period close to the beat period of the system.
- Published
- 2012
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