no code implementations • 14 Sep 2022 • Y. -L. Mong, K. Ackley, T. L. Killestein, D. K. Galloway, M. Dyer, R. Cutter, M. J. I. Brown, J. Lyman, K. Ulaczyk, D. Steeghs, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. Breton, L. Nuttall, E. Palle, D. Pollacco, E. Thrane, S. Awiphan, U. Burhanudin, P. Chote, A. Chrimes, E. Daw, C. Duffy, R. Eyles-Ferris, B. P. Gompertz, T. Heikkila, P. Irawati, M. Kennedy, A. Levan, S. Littlefair, L. Makrygianni, T. Marsh, D. Mata Sanchez, S. Mattila, J. R. Maund, J. McCormac, D. Mkrtichian, J. Mullaney, E. Rol, U. Sawangwit, E. Stanway, R. Starling, P. Strom, S. Tooke, K. Wiersema
The identification of transient detections from the subtraction artifacts after the image differencing process is a key step in such classifiers, known as real-bogus classification problem.
no code implementations • 11 Jan 2021 • N. Casasayas-Barris, E. Palle, M. Stangret, V Bourrier, H. M. Tabernero, F. Yan, F. Borsa, R. Allart, M. R. Zapatero Osorio, C. Lovis, S. G. Sousa, G. Chen, M. Oshagh, N. C. Santos, F. Pepe, R. Rebolo, P. Molaro, S. Cristiani, V. Adibekyan, Y. Alibert, C. Allende Prieto, F. Bouchy, O. D. S. Demangeon, P. Di Marcantonio, V. D Odorico, D. Ehrenreich, P. Figueira, R. Génova Santos, J. I. González Hernández, B. Lavie, J. Lillo-Box, G. Lo Curto, C. J. A. P. Martins, A. Mehner, G. Micela, N. J. Nunes, E. Poretti, A. Sozzetti, A. Suárez Mascareño, S. Udry
We observed two transits of the iconic gas giant HD 209458b between 380 and 780 nm, using the high-resolution ESPRESSO spectrograph.
Earth and Planetary Astrophysics Solar and Stellar Astrophysics
no code implementations • 5 Jan 2021 • Vincent Van Eylen, N. Astudillo-Defru, X. Bonfils, J. Livingston, T. Hirano, R. Luque, K. W. F. Lam, A. B. Justesen, J. N. Winn, D. Gandolfi, G. Nowak, E. Palle, S. Albrecht, F. Dai, B. Campos Estrada, J. E. Owen, D. Foreman-Mackey, M. Fridlund, J. Korth, S. Mathur, T. Forveille, T. Mikal-Evans, H. L. M. Osborne, C. S. K. Ho, J. M. Almenara, E. Artigau, O. Barragán, F. Bouchy, J. Cabrera, D. A. Caldwell, D. Charbonneau, P. Chaturvedi, W. D. Cochran, S. Csizmadia, M. Damasso, X. Delfosse, J. R. De Medeiros, R. F. Díaz, R. Doyon, M. Esposito, G. Fűrész, P. Figueira, I. Georgieva, E. Goffo, S. Grziwa, E. Guenther, A. P. Hatzes, J. M. Jenkins, P. Kabath, E. Knudstrup, D. W. Latham, B. Lavie, C. Lovis, R. E. Mennickent, S. E. Mullally, F. Murgas, N. Narita, F. A. Pepe, C. M. Persson, S. Redfield, G. R. Ricker, N. C. Santos, S. Seager, L. M. Serrano, A. M. S. Smith, A. Suárez Mascareño, J. Subjak, J. D. Twicken, S. Udry, R. Vanderspek, M. R. Zapatero Osorio
The combination of radius and mass measurements suggests that the innermost planet has a rocky composition similar to that of Earth, while the outer two planets have lower densities.
Earth and Planetary Astrophysics Solar and Stellar Astrophysics
no code implementations • 5 Oct 2020 • A. Mortier, M. R. Zapatero Osorio, L. Malavolta, Y. Alibert, K. Rice, J. Lillo-Box, A. Vanderburg, M. Oshagh, L. Buchhave, V. Adibekyan, E. Delgado Mena, M. Lopez-Morales, D. Charbonneau, S. G. Sousa, C. Lovis, L. Affer, C. Allende Prieto, S. C. C. Barros, S. Benatti, A. S. Bonomo, W. Boschin, F. Bouchy, A. Cabral, A. Collier Cameron, R. Cosentino, S. Cristiani, O. D. S. Demangeon, P. Di Marcantonio, V. D'Odorico, X. Dumusque, D. Ehrenreich, P. Figueira, A. Fiorenzano, A. Ghedina, J. I. González Hernández, J. Haldemann, A. Harutyunyan, R. D. Haywood, D. W. Latham, B. Lavie, G. Lo Curto, J. Maldonado, A. Manescau, C. J. A. P. Martins, M. Mayor, D. Mégevand, A. Mehner, G. Micela, P. Molaro, E. Molinari, N. J. Nunes, F. A. Pepe, E. Palle, D. Phillips, G. Piotto, M. Pinamonti, E. Poretti, M. Riva, R. Rebolo, N. C. Santos, D. Sasselov, A. Sozzetti, A. Suárez Mascareño, S. Udry, R. G. West, C. A. Watson, T. G. Wilson
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.
Earth and Planetary Astrophysics
1 code implementation • 14 Apr 2020 • Benjamin F. Cooke, Don Pollacco, Y. Almleaky, K. Barkaoui, Z. Benkhaldoun, James A. Blake, François Bouchy, Panos Boumis, D. J. A. Brown, Ivan Bruni, A. Burdanov, Andrew Collier Cameron, Paul Chote, A. Daassou, Giuseppe D'ago, Shweta Dalal, Mario Damasso, L. Delrez, A. P. Doyle, E. Ducrot, M. Gillon, G. Hébrard, C. Hellier, Thomas Henning, E. Jehin, Flavien Kiefer, George W. King, Alexios Liakos, Théo Lopez, Luigi Mancini, Rosemary Mardling, P. F. L. Maxted, James McCormac, C. Murray, Louise D. Nielsen, Hugh Osborn, E. Palle, Francesco Pepe, F. J. Pozuelos, J. Prieto-Arranz, D. Queloz, Nicole Schanche, Damien Ségransan, Barry Smalley, John Southworth, S. Thompson, Oliver Turner, Stéphane Udry, S. Velasco, Richard West, Pete Wheatley, John Alikakos
We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b.
Earth and Planetary Astrophysics
1 code implementation • 26 Feb 2018 • J. Prieto-Arranz, E. Palle, D. Gandolfi, O. Barragán, E. W. Guenther, F. Dai, M. Fridlund, T. Hirano, J. Livingston, P. Niraula, C. M. Persson, S. Redfield, S. Albrecht, R. Alonso, G. Antoniciello, J. Cabrera, W. D. Cochran, Sz. Csizmadia, H. Deeg, Ph. Eigmüller, M. Endl, A. Erikson, M. E. Everett, A. Fukui, S. Grziwa, A. P. Hatzes, D. Hidalgo, M. Hjorth, J. Korth, D. Lorenzo-Oliveira, F. Murgas, N. Narita, D. Nespral, G. Nowak, M. Pätzold, P. Montañés Rodríguez, H. Rauer, I. Ribas, A. M. S. Smith, V. Van Eylen, J. N. Winn
We also find that the planetary bulk compositions are compatible with a scenario where all three planets formed with similar core/atmosphere compositions, and we speculate that while GJ 9827 b and GJ 9827 c lost their atmospheric envelopes, GJ 9827 d maintained its atmosphere, owing to the much lower stellar irradiation.
Earth and Planetary Astrophysics
1 code implementation • 11 May 2017 • E. W. Guenther, O. Barragan, F. Dai, D. Gandolfi, T. Hirano, M. Fridlund, L. Fossati, A. Chau, R. Helled, J. Korth, J. Prieto-Arranz, D. Nespral, G. Antoniciello, H. Deeg, M. Hjorth, S. Grziwa, S. Albrecht, A. P. Hatzes, H. Rauer, Sz. Csizmadia, A. M. S. Smith, J. Cabrera, N. Narita, P. Arriagada, J. Burt, R. P. Butler, W. D. Cochran, J. D. Crane, Ph. Eigmueller, A. Erikson, J. A. Johnson, A. Kiilerich, D. Kubyshkina, E. Palle, C. M. Persson, M. Paetzold, S. Sabotta, B. Sato, St. A. Shectman, J. K. Teske, I. B. Thompson, V. Van Eylen, G. Nowak, A. Vanderburg, R. A. Wittenmyer
The period of the outer planet is 13. 3 days. Although the two planets have similar masses, their densities are very different.
Earth and Planetary Astrophysics