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1. NGTS-EB-7, an eccentric, long-period, low-mass eclipsing binary

Author

Rodel, Toby, Watson, Christopher. A., Ulmer-Moll, Solène, Gill, Samuel, Maxted, Pierre F. L., Casewell, Sarah L., Brahm, Rafael, Wilson, Thomas G, Costes, Jean C., Eschen, Yoshi Nike Emilia, Doyle, Lauren, Freckelton, Alix V., Alves, Douglas R., Apergis, Ioannis, Bayliss, Daniel, Bouchy, Francois, Burleigh, Matthew R., Dumusque, Xavier, Eberhardt, Jan, Fernández, Jorge Fernández, Gillen, Edward, Goad, Michael R., Hawthorn, Faith, Helled, Ravit, Henning, Thomas, Hobbs, Katlyn L., Jenkins, James S., Jordán, Andrés, Kendall, Alicia, Lendl, Monika, McCormac, James, de Mooij, Ernst J. W., O'Brien, Sean M., Saha, Suman, Pinto, Marcelo Tala, Trifonov, Trifon, Udry, Stéphane, and Wheatley, Peter J.

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

Despite being the most common types of stars in the Galaxy, the physical properties of late M dwarfs are often poorly constrained. A trend of radius inflation compared to evolutionary models has been observed for earlier type M dwarfs in eclipsing binaries, possibly caused by magnetic activity. It is currently unclear whether this trend also extends to later type M dwarfs below the convective boundary. This makes the discovery of lower-mass, fully convective, M dwarfs in eclipsing binaries valuable for testing evolutionary models especially in longer-period binaries where tidal interaction between the primary and secondary is negligible. With this context, we present the discovery of the NGTS-EB-7 AB system, an eclipsing binary containing a late M dwarf secondary and an evolved G-type primary star. The secondary star has a radius of $0.125 \pm 0.006 R_\odot$ , a mass of $0.096 \pm 0.004 M_\odot$ and follows a highly eccentric $(e=0.71436 \pm 0.00085)$ orbit every $193.35875 \pm 0.00034$ days. This makes NGTS-EB-7 AB the third longest-period eclipsing binary system with a secondary smaller than $200 M_J$ with the mass and radius constrained to better than $5 \%$. In addition, NGTS-EB-7 is situated near the centre of the proposed LOPS2 southern field of the upcoming PLATO mission, allowing for detection of the secondary eclipse and measurement of the companion`s temperature. With its long-period and well-constrained physical properties - NGTS-EB-7 B will make a valuable addition to the sample of M dwarfs in eclipsing binaries and help in determining accurate empirical mass/radius relations for later M dwarf stars., Comment: Main body: 14 pages, 6 figures, 5 tables. Appendices: 7 pages, 5 figures, 5 tables

Published
2025
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2. The PLATO Mission

Author

Rauer, Heike, Aerts, Conny, Cabrera, Juan, Deleuil, Magali, Erikson, Anders, Gizon, Laurent, Goupil, Mariejo, Heras, Ana, Lorenzo-Alvarez, Jose, Marliani, Filippo, Martin-Garcia, César, Mas-Hesse, J. Miguel, O'Rourke, Laurence, Osborn, Hugh, Pagano, Isabella, Piotto, Giampaolo, Pollacco, Don, Ragazzoni, Roberto, Ramsay, Gavin, Udry, Stéphane, Appourchaux, Thierry, Benz, Willy, Brandeker, Alexis, Güdel, Manuel, Janot-Pacheco, Eduardo, Kabath, Petr, Kjeldsen, Hans, Min, Michiel, Santos, Nuno, Smith, Alan, Suarez, Juan-Carlos, Werner, Stephanie C., Aboudan, Alessio, Abreu, Manuel, a, Lorena Acu, Adams, Moritz, Adibekyan, Vardan, Affer, Laura, Agneray, François, Agnor, Craig, Børsen-Koch, Victor Aguirre, Ahmed, Saad, Aigrain, Suzanne, Al-Bahlawan, Ashraf, Gil, M de los Angeles Alcacera, Alei, Eleonora, Alencar, Silvia, Alexander, Richard, Alfonso-Garzón, Julia, Alibert, Yann, Prieto, Carlos Allende, Almeida, Leonardo, Sobrino, Roi Alonso, Altavilla, Giuseppe, Althaus, Christian, Trujillo, Luis Alonso Alvarez, Amarsi, Anish, Eiff, Matthias Ammler-von, Amôres, Eduardo, Andrade, Laerte, Antoniadis-Karnavas, Alexandros, António, Carlos, del Moral, Beatriz Aparicio, Appolloni, Matteo, Arena, Claudio, Armstrong, David, Aliaga, Jose Aroca, Asplund, Martin, Audenaert, Jeroen, Auricchio, Natalia, Avelino, Pedro, Baeke, Ann, Baillié, Kevin, Balado, Ana, Balagueró, Pau Ballber, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebasti Barceló, Barker, Adrian, Barklem, Paul, Barnes, Sydney, Navascues, David Barrado, Barragan, Oscar, Baruteau, Clément, Basu, Sarbani, Baudin, Frederic, Baumeister, Philipp, Bayliss, Daniel, Bazot, Michael, Beck, Paul G., Bedding, Tim, Belkacem, Kevin, Bellinger, Earl, Benatti, Serena, Benomar, Othman, Bérard, Diane, Bergemann, Maria, Bergomi, Maria, Bernardo, Pierre, Biazzo, Katia, Bignamini, Andrea, Bigot, Lionel, Billot, Nicolas, Binet, Martin, Biondi, David, Biondi, Federico, Birch, Aaron C., Bitsch, Bertram, Ceballos, Paz Victoria Bluhm, Bódi, Attila, Bognár, Zsófia, Boisse, Isabelle, Bolmont, Emeline, Bonanno, Alfio, Bonavita, Mariangela, Bonfanti, Andrea, Bonfils, Xavier, Bonito, Rosaria, Bonomo, Aldo Stefano, Börner, Anko, Saikia, Sudeshna Boro, Martín, Elisa Borreguero, Borsa, Francesco, Borsato, Luca, Bossini, Diego, Bouchy, Francois, Boué, Gwenaël, Boufleur, Rodrigo, Boumier, Patrick, Bourrier, Vincent, Bowman, Dominic M., Bozzo, Enrico, Bradley, Louisa, Bray, John, Bressan, Alessandro, Breton, Sylvain, Brienza, Daniele, Brito, Ana, Brogi, Matteo, Brown, Beverly, Brown, David J. A., Brun, Allan Sacha, Bruno, Giovanni, Bruns, Michael, Buchhave, Lars A., Bugnet, Lisa, Buldgen, Gaël, Burgess, Patrick, Busatta, Andrea, Busso, Giorgia, Buzasi, Derek, Caballero, José A., Cabral, Alexandre, Gomez, Juan-Francisco Cabrero, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, Gestal, Néstor Campos, Martins, Bruno Leonardo Canto, Cara, Christophe, Carone, Ludmila, Carrasco, Josep Manel, Casagrande, Luca, Casewell, Sarah L., Cassisi, Santi, Castellani, Marco, Castro, Matthieu, Catala, Claude, Fernández, Irene Catalán, Catelan, Márcio, Cegla, Heather, Cerruti, Chiara, Cessa, Virginie, Chadid, Merieme, Chaplin, William, Charpinet, Stephane, Chiappini, Cristina, Chiarucci, Simone, Chiavassa, Andrea, Chinellato, Simonetta, Chirulli, Giovanni, Christensen-Dalsgaard, Jørgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, García, Fernando Conde, Conseil, Simon, Corbard, Thierry, Correia, Alexandre C. M., Corsaro, Enrico, Cosentino, Rosario, Costes, Jean, Cottinelli, Andrea, Covone, Giovanni, Creevey, Orlagh L., Crida, Aurelien, Csizmadia, Szilard, Cunha, Margarida, Curry, Patrick, da Costa, Jefferson, da Silva, Francys, Dalal, Shweta, Damasso, Mario, Damiani, Cilia, Damiani, Francesco, Chagas, Maria Liduina das, Davies, Melvyn, Davies, Guy, Davies, Ben, Davison, Gary, de Almeida, Leandro, de Angeli, Francesca, de Barros, Susana Cristina Cabral, Leão, Izan de Castro, de Freitas, Daniel Brito, de Freitas, Marcia Cristina, De Martino, Domitilla, de Medeiros, José Renan, de Paula, Luiz Alberto, Gómez, Álvaro de Pedraza, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Innocenti, Scilla Degl, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, Desert, Jean-Michel, Desidera, Silvano, Dexet, Marc, Di Criscienzo, Marcella, Di Giorgio, Anna Maria, Di Mauro, Maria Pia, Rial, Federico Jose Diaz, Díaz-García, José-Javier, Dima, Marco, Dinuzzi, Giacomo, Dionatos, Odysseas, Distefano, Elisa, Nascimento Jr., Jose-Dias do, Domingo, Albert, D'Orazi, Valentina, Dorn, Caroline, Doyle, Lauren, Duarte, Elena, Ducellier, Florent, Dumaye, Luc, Dumusque, Xavier, Dupret, Marc-Antoine, Eggenberger, Patrick, Ehrenreich, David, Eigmüller, Philipp, Eising, Johannes, Emilio, Marcelo, Eriksson, Kjell, Ermocida, Marco, Giribaldi, Riano Isidoro Escate, Eschen, Yoshi, ez, Lucía Espinosa Yá, Estrela, In s, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, Fernández, Miguel, Ferrari, Lorenza, Ferraz-Mello, Sylvio, Fialho, Fabio, Fienga, Agnes, Figueira, Pedro, Fiori, Laura, Flaccomio, Ettore, Focardi, Mauro, Foley, Steve, Fontignie, Jean, Ford, Dominic, Fornazier, Karin, Forveille, Thierry, Fossati, Luca, Franca, Rodrigo de Marca, da Silva, Lucas Franco, Frasca, Antonio, Fridlund, Malcolm, Furlan, Marco, Gabler, Sarah-Maria, Gaido, Marco, Gallagher, Andrew, Sempere, Paloma I. Gallego, Galli, Emanuele, García, Rafael A., Hernández, Antonio García, Munoz, Antonio Garcia, García-Vázquez, Hugo, Haba, Rafael Garrido, Gaulme, Patrick, Gauthier, Nicolas, Gehan, Charlotte, Gent, Matthew, Georgieva, Iskra, Ghigo, Mauro, Giana, Edoardo, Gill, Samuel, Girardi, Leo, Winter, Silvia Giuliatti, Giusi, Giovanni, da Silva, João Gomes, Zazo, Luis Jorge Gómez, Gomez-Lopez, Juan Manuel, Hernández, Jonay Isai González, Murillo, Kevin Gonzalez, Melchor, Alejandro Gonzalo, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, bach, Denis Grie, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Lo c, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, Guillot, Tristan, Guiot, Pierre, Guterman, Pascal, Gutiérrez, Antonio, Gutiérrez-Canales, Fernando, Hagelberg, Janis, Haldemann, Jonas, Hall, Cassandra, Handberg, Rasmus, Harrison, Ian, Harrison, Diana L., Hasiba, Johann, Haswell, Carole A., Hatalova, Petra, Hatzes, Artie, Haywood, Raphaelle, Hébrard, Guillaume, Heckes, Frank, Heiter, Ulrike, Hekker, Saskia, Heller, René, Helling, Christiane, Helminiak, Krzysztof, Hemsley, Simon, Heng, Kevin, Herbst, Konstantin, Hermans, Aline, Hermes, JJ, Torres, Nadia Hidalgo, Hinkel, Natalie, Hobbs, David, Hodgkin, Simon, Hofmann, Karl, Hojjatpanah, Saeed, Houdek, Günter, Huber, Daniel, Huesler, Joseph, Hui-Bon-Hoa, Alain, Huygen, Rik, Huynh, Duc-Dat, Iro, Nicolas, Irwin, Jonathan, Irwin, Mike, Izidoro, André, Jacquinod, Sophie, Jannsen, Nicholas Emborg, Janson, Markus, Jeszenszky, Harald, Jiang, Chen, Mancebo, Antonio José Jimenez, Jofre, Paula, Johansen, Anders, Johnston, Cole, Jones, Geraint, Kallinger, Thomas, Kálmán, Szilárd, Kanitz, Thomas, Karjalainen, Marie, Karjalainen, Raine, Karoff, Christoffer, Kawaler, Steven, Kawata, Daisuke, Keereman, Arnoud, Keiderling, David, Kennedy, Tom, Kenworthy, Matthew, Kerschbaum, Franz, Kidger, Mark, Kiefer, Flavien, Kintziger, Christian, Kislyakova, Kristina, Kiss, László, Klagyivik, Peter, Klahr, Hubert, Klevas, Jonas, Kochukhov, Oleg, Köhler, Ulrich, Kolb, Ulrich, Koncz, Alexander, Korth, Judith, Kostogryz, Nadiia, Kovács, Gábor, Kovács, József, Kozhura, Oleg, Krivova, Natalie, Kucinskas, Arunas, Kuhlemann, Ilyas, Kupka, Friedrich, Laauwen, Wouter, Labiano, Alvaro, Lagarde, Nadege, Laget, Philippe, Laky, Gunter, Lam, Kristine Wai Fun, Lambrechts, Michiel, Lammer, Helmut, Lanza, Antonino Francesco, Lanzafame, Alessandro, Martiz, Mariel Lares, Laskar, Jacques, Latter, Henrik, Lavanant, Tony, Lawrenson, Alastair, Lazzoni, Cecilia, Lebre, Agnes, Lebreton, Yveline, Etangs, Alain Lecavelier des, Lee, Katherine, Leinhardt, Zoe, Leleu, Adrien, Lendl, Monika, Leto, Giuseppe, Levillain, Yves, Libert, Anne-Sophie, Lichtenberg, Tim, Ligi, Roxanne, Lignieres, Francois, Lillo-Box, Jorge, Linsky, Jeffrey, Liu, John Scige, Loidolt, Dominik, Longval, Yuying, Lopes, Ilídio, Lorenzani, Andrea, Ludwig, Hans-Guenter, Lund, Mikkel, Lundkvist, Mia Sloth, Luri, Xavier, Maceroni, Carla, Madden, Sean, Madhusudhan, Nikku, Maggio, Antonio, Magliano, Christian, Magrin, Demetrio, Mahy, Laurent, Maibaum, Olaf, Malac-Allain, LeeRoy, Malapert, Jean-Christophe, Malavolta, Luca, Maldonado, Jesus, Mamonova, Elena, Manchon, Louis, Manjón, Andres, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, rico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, Vodopivec, Iris Martín, Figueiredo, Ana Carolina Mattiuci, Maxted, Pierre F. L., Mazeh, Tsevi, Mazevet, Stephane, Mazzei, Francesco, McCormac, James, McMillan, Paul, Menou, Lucas, Merle, Thibault, Meru, Farzana, Mesa, Dino, Messina, Sergio, Mészáros, Szabolcs, Meunier, Nadége, Meunier, Jean-Charles, Micela, Giuseppina, Michaelis, Harald, Michel, Eric, Michielsen, Mathias, Michtchenko, Tatiana, Miglio, Andrea, Miguel, Yamila, Milligan, David, Mirouh, Giovanni, Mitchell, Morgan, Moedas, Nuno, Molendini, Francesca, Molnár, László, Mombarg, Joey, Montalban, Josefina, Montalto, Marco, Monteiro, Mário J. P. F. G., Sánchez, Francisco Montoro, Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Beno t, Mourard, Denis, Mousis, Olivier, Moutou, Claire, Mowlavi, Nami, Moya, Andrés, Muehlmann, Prisca, Muirhead, Philip, Munari, Matteo, Musella, Ilaria, Mustill, Alexander James, Nardetto, Nicolas, Nardiello, Domenico, Narita, Norio, Nascimbeni, Valerio, Nash, Anna, Neiner, Coralie, Nelson, Richard P., Nettelmann, Nadine, Nicolini, Gianalfredo, Nielsen, Martin, Niemi, Sami-Matias, Noack, Lena, Noels-Grotsch, Arlette, Noll, Anthony, Norazman, Azib, Norton, Andrew J., Nsamba, Benard, Ofir, Aviv, Ogilvie, Gordon, Olander, Terese, Olivetto, Christian, Olofsson, Göran, Ong, Joel, Ortolani, Sergio, Oshagh, Mahmoudreza, Ottacher, Harald, Ottensamer, Roland, Ouazzani, Rhita-Maria, Paardekooper, Sijme-Jan, Pace, Emanuele, Pajas, Miriam, Palacios, Ana, Palandri, Gaelle, Palle, Enric, Paproth, Carsten, Parro, Vanderlei, Parviainen, Hannu, Granado, Javier Pascual, Passegger, Vera Maria, Pastor-Morales, Carmen, Pätzold, Martin, Pedersen, May Gade, Hidalgo, David Pena, Pepe, Francesco, Pereira, Filipe, Persson, Carina M., Pertenais, Martin, Peter, Gisbert, Petit, Antoine C., Petit, Pascal, Pezzuto, Stefania, Pichierri, Gabriele, Pietrinferni, Adriano, Pinheiro, Fernando, Pinsonneault, Marc, Plachy, Emese, Plasson, Philippe, Plez, Bertrand, Poppenhaeger, Katja, Poretti, Ennio, Portaluri, Elisa, Portell, Jordi, de Mello, Gustavo Frederico Porto, Poyatos, Julien, Pozuelos, Francisco J., Moroni, Pier Giorgio Prada, Pricopi, Dumitru, Prisinzano, Loredana, Quade, Matthias, Quirrenbach, Andreas, Reina, Julio Arturo Rabanal, Soares, Maria Cristina Rabello, Raimondo, Gabriella, Rainer, Monica, Rodón, Jose Ramón, Ramón-Ballesta, Alejandro, Zapata, Gonzalo Ramos, Rätz, Stefanie, Rauterberg, Christoph, Redman, Bob, Redmer, Ronald, Reese, Daniel, Regibo, Sara, Reiners, Ansgar, Reinhold, Timo, Renie, Christian, Ribas, Ignasi, Ribeiro, Sergio, Ricciardi, Thiago Pereira, Rice, Ken, Richard, Olivier, Riello, Marco, Rieutord, Michel, Ripepi, Vincenzo, Rixon, Guy, Rockstein, Steve, Ortiz, José Ramón Rodón, Rodríguez, María Teresa Rodrigo, Amor, Alberto Rodríguez, Díaz, Luisa Fernanda Rodríguez, Garcia, Juan Pablo Rodriguez, Rodriguez-Gomez, Julio, Roehlly, Yannick, Roig, Fernando, Rojas-Ayala, Bárbara, Rolf, Tobias, Rørsted, Jakob Lysgaard, Rosado, Hugo, Rosotti, Giovanni, Roth, Olivier, Roth, Markus, Rousseau, Alex, Roxburgh, Ian, Roy, Fabrice, Royer, Pierre, Ruane, Kirk, Mastropasqua, Sergio Rufini, de Galarreta, Claudia Ruiz, Russi, Andrea, Saar, Steven, Saillenfest, Melaine, Salaris, Maurizio, Salmon, Sebastien, Saltas, Ippocratis, Samadi, Réza, Samadi, Aunia, Samra, Dominic, da Silva, Tiago Sanches, Carrasco, Miguel Andrés Sánchez, Santerne, Alexandre, Pé, Amaia Santiago, Santoli, Francesco, Santos, ngela R. G., Mesa, Rosario Sanz, Sarro, Luis Manuel, Scandariato, Gaetano, Schäfer, Martin, Schlafly, Edward, Schmider, François-Xavier, Schneider, Jean, Schou, Jesper, Schunker, Hannah, Schwarzkopf, Gabriel Jörg, Serenelli, Aldo, Seynaeve, Dries, Shan, Yutong, Shapiro, Alexander, Shipman, Russel, Sicilia, Daniela, sanmartin, Maria Angeles Sierra, Sigot, Axelle, Silliman, Kyle, Silvotti, Roberto, Simon, Attila E., Napoli, Ricardo Simoyama, Skarka, Marek, Smalley, Barry, Smiljanic, Rodolfo, Smit, Samuel, Smith, Alexis, Smith, Leigh, Snellen, Ignas, Sódor, Ádám, Sohl, Frank, Solanki, Sami K., Sortino, Francesca, Sousa, Sérgio, Southworth, John, Souto, Diogo, Sozzetti, Alessandro, Stamatellos, Dimitris, Stassun, Keivan, Steller, Manfred, Stello, Dennis, Stelzer, Beate, Stiebeler, Ulrike, Stokholm, Amalie, Storelvmo, Trude, Strassmeier, Klaus, Strøm, Paul Anthony, Strugarek, Antoine, Sulis, Sophia, vanda, Michal, Szabados, László, Szabó, Róbert, Szabó, Gyula M., Szuszkiewicz, Ewa, Talens, Geert Jan, Teti, Daniele, Theisen, Tom, Thévenin, Frédéric, Thoul, Anne, Tiphene, Didier, Titz-Weider, Ruth, Tkachenko, Andrew, Tomecki, Daniel, Tonfat, Jorge, Tosi, Nicola, Trampedach, Regner, Traven, Gregor, Triaud, Amaury, Trønnes, Reidar, Tsantaki, Maria, Tschentscher, Matthias, Turin, Arnaud, Tvaruzka, Adam, Ulmer, Bernd, Ulmer-Moll, Solène, Ulusoy, Ceren, Umbriaco, Gabriele, Valencia, Diana, Valentini, Marica, Valio, Adriana, Guijarro, Ángel Luis Valverde, Van Eylen, Vincent, Van Grootel, Valerie, van Kempen, Tim A., Van Reeth, Timothy, Van Zelst, Iris, Vandenbussche, Bart, Vasiliou, Konstantinos, Vasilyev, Valeriy, de Mascarenhas, David Vaz, Vazan, Allona, Nunez, Marina Vela, Velloso, Eduardo Nunes, Ventura, Rita, Ventura, Paolo, Venturini, Julia, Trallero, Isabel Vera, Veras, Dimitri, Verdugo, Eva, Verma, Kuldeep, Vibert, Didier, Martinez, Tobias Vicanek, Vida, Krisztián, Vigan, Arthur, Villacorta, Antonio, Villaver, Eva, Aparicio, Marcos Villaverde, Viotto, Valentina, Vorobyov, Eduard, Vorontsov, Sergey, Wagner, Frank W., Walloschek, Thomas, Walton, Nicholas, Walton, Dave, Wang, Haiyang, Waters, Rens, Watson, Christopher, Wedemeyer, Sven, Weeks, Angharad, Weingrill, Jörg, Weiss, Annita, Wendler, Belinda, West, Richard, Westerdorff, Karsten, Westphal, Pierre-Amaury, Wheatley, Peter, White, Tim, Whittaker, Amadou, Wickhusen, Kai, Wilson, Thomas, Windsor, James, Winter, Othon, Winther, Mark Lykke, Winton, Alistair, Witteck, Ulrike, Witzke, Veronika, Woitke, Peter, Wolter, David, Wuchterl, Günther, Wyatt, Mark, Yang, Dan, Yu, Jie, Sanchez, Ricardo Zanmar, Osorio, María Rosa Zapatero, Zechmeister, Mathias, Zhou, Yixiao, Ziemke, Claas, and Zwintz, Konstanze

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

PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.

Published
2024

3. $\beta$ Pictoris b through the eyes of the upgraded CRIRES+

Author

Landman, Rico, Stolker, Tomas, Snellen, Ignas, Costes, Jean, de Regt, Sam, Zhang, Yapeng, Gandhi, Siddharth, Mollière, Paul, Kesseli, Aurora, Vigan, Arthur, and Sánchez-López, Alejandro

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

Context: High-resolution spectrographs fed by adaptive optics (AO) provide a unique opportunity to characterize directly imaged exoplanets. Observations with such instruments allow us to probe the atmospheric composition, spin rotation, and radial velocity of the planet, thereby helping to reveal information on its formation and migration history. The recent upgrade of the Cryogenic High-Resolution Infrared Echelle Spectrograph (CRIRES+) at the VLT makes it a highly suitable instrument for characterizing directly imaged exoplanets. Aims: In this work, we report on observations of $\beta$ Pictoris b with CRIRES+ and use them to constrain the planets atmospheric properties and update the estimation of its spin rotation. Methods: The data were reduced using the open-source \textit{pycrires} package. We subsequently forward-modeled the stellar, planetary, and systematic contribution to the data to detect molecules in the planet's atmosphere. We also used atmospheric retrievals to provide new constraints on its atmosphere. Results: We confidently detected water and carbon monoxide in the atmosphere of $\beta$ Pictoris b and retrieved a slightly sub-solar carbon-to-oxygen ratio, which is in agreement with previous results. The interpretation is hampered by our limited knowledge of the C/O ratio of the host star. We also obtained a much improved constraint on its spin rotation of $19.9 \pm 1.0$ km/s, which gives a rotation period of $8.7 \pm 0.8$ hours, assuming no obliquity. We find that there is a degeneracy between the metallicity and clouds, but this has minimal impact on the retrieved C/O, $v\sin{i}$, and radial velocity. Our results show that CRIRES+ is performing well and stands as a highly useful instrument for characterizing directly imaged planets., Comment: Accepted for publication in A&A

Published
2023

4. The discovery of three hot Jupiters, NGTS-23b, 24b and 25b, and updated parameters for HATS-54b from the Next Generation Transit Survey

Author

Jackson, David G., Watson, Christopher A., de Mooij, Ernst J. W., Acton, Jack S., Alves, Douglas R., Anderson, David R., Armstrong, David J., Bayliss, Daniel, Belardi, Claudia, Bouchy, François, Bryant, Edward M., Burleigh, Matthew R., Casewell, Sarah L., Costes, Jean C., Eigmüller, Phillip, Goad, Michael R., Gill, Samuel, Gillen, Edward, Günther, Maximilian N., Hawthorn, Faith, Henderson, Beth A., Jackman, James A. G., Jenkins, James S., Lendl, Monika, Kendall, Alicia, McCormac, James, Moyano, Maximiliano, Nielsen, Louise. D., Osborn, Ares, Sefako, Ramotholo R., Smith, Alexis M. S., Tilbrook, Rosanna H., Turner, Oliver, Udry, Stéphane, Vines, Jose I., West, Richard G., Wheatley, Peter J., and Worters, Hannah

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of three new hot Jupiters with the Next Generation Transit Survey (NGTS) as well as updated parameters for HATS-54b, which was independently discovered by NGTS. NGTS-23b, NGTS-24b and NGTS-25b have orbital periods of 4.076, 3.468, and 2.823 days and orbit G-, F- and K-type stars, respectively. NGTS-24 and HATS-54 appear close to transitioning off the main-sequence (if they are not already doing so), and therefore are interesting targets given the observed lack of Hot Jupiters around sub-giant stars. By considering the host star luminosities and the planets' small orbital separations (0.037 - 0.050 au), we find that all four hot Jupiters are above the minimum irradiance threshold for inflation mechanisms to be effective. NGTS-23b has a mass of 0.61 $M_{J}$ and radius of 1.27 $R_{J}$ and is likely inflated. With a radius of 1.21 $R_{J}$ and mass of 0.52 $M_{J}$, NGTS-24b has a radius larger than expected from non-inflated models but its radius is smaller than the predicted radius from current Bayesian inflationary models. Finally, NGTS-25b is intermediate between the inflated and non-inflated cases, having a mass of 0.64 $M_{J}$ and a radius of 1.02 $R_{J}$. The physical processes driving radius inflation remain poorly understood, and by building the sample of hot Jupiters we can aim to identify the additional controlling parameters, such as metallicity and stellar age., Comment: 17 pages, 8 figures. Accepted for publication in MNRAS

Published
2022
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5. NGTS-21b: An Inflated Super-Jupiter Orbiting a Metal-poor K dwarf

Author

Alves, Douglas R., Jenkins, James S., Vines, Jose I., Nielsen, Louise D., Gill, Samuel, Acton, Jack S., Anderson, D. R., Bayliss, Daniel, Bouchy, François, Breytenbach, Hannes, Bryant, Edward M., Burleigh, Matthew R., Casewell, Sarah L., Eigmüller, Philipp, Gillen, Edward, Goad, Michael R., Günther, Maximilian N., Henderson, Beth A., Kendall, Alicia, Lendl, Monika, Moyano, Maximiliano, Sefako, Ramotholo R., Smith, Alexis M. S., Costes, Jean C., Tilbrook, Rosanne H., Thomas, Jessymol K., Udry, Stéphane, Watson, Christopher A., West, Richard G., Wheatley, Peter J., Worters, Hannah L., and Osborn, Ares

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of NGTS-21b, a massive hot Jupiter orbiting a low-mass star as part of the Next Generation Transit Survey (NGTS). The planet has a mass and radius of $2.36 \pm 0.21$ M$_{\rm J}$, and $1.33 \pm 0.03$ R$_{\rm J}$, and an orbital period of 1.543 days. The host is a K3V ($T_{\rm eff}=4660 \pm 41$, K) metal-poor (${\rm [Fe/H]}=-0.26 \pm 0.07$, dex) dwarf star with a mass and radius of $0.72 \pm 0.04$, M$_{\odot}$,and $0.86 \pm 0.04$, R$_{\odot}$. Its age and rotation period of $10.02^{+3.29}_{-7.30}$, Gyr and $17.88 \pm 0.08$, d respectively, are in accordance with the observed moderately low stellar activity level. When comparing NGTS-21b with currently known transiting hot Jupiters with similar equilibrium temperatures, it is found to have one of the largest measured radii despite its large mass. Inflation-free planetary structure models suggest the planet's atmosphere is inflated by $\sim21\%$, while inflationary models predict a radius consistent with observations, thus pointing to stellar irradiation as the probable origin of NGTS-21b's radius inflation. Additionally, NGTS-21b's bulk density ($1.25 \pm 0.15$, g/cm$^3$) is also amongst the largest within the population of metal-poor giant hosts ([Fe/H] < 0.0), helping to reveal a falling upper boundary in metallicity-planet density parameter space that is in concordance with core accretion formation models. The discovery of rare planetary systems such as NGTS-21 greatly contributes towards better constraints being placed on the formation and evolution mechanisms of massive planets orbiting low-mass stars., Comment: 12 pages, 13 figures, accepted for publication in MNRAS

Published
2022
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8. Periodic stellar variability from almost a million NGTS light curves

Author

Briegal, Joshua T., Gillen, Edward, Queloz, Didier, Hodgkin, Simon, Acton, Jack S., Anderson, David R., Armstrong, David J., Battley, Matthew P., Bayliss, Daniel, Burleigh, Matthew R., Bryant, Edward M., Casewell, Sarah L., Costes, Jean C., Eigmuller, Philipp, Gill, Samuel, Goad, Michael R., Gunther, Maximilian N., Henderson, Beth A., Jackman, James A. G., Jenkins, James S., Kreutzer, Lars T., Moyano, Maximiliano, Lendl, Monika, Smith, Gareth D., Tilbrook, Rosanna H., Watson, Christopher A., West, Richard G., and Wheatley, Peter J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We analyse 829,481 stars from the Next Generation Transit Survey (NGTS) to extract variability periods. We utilise a generalisation of the autocorrelation function (the G-ACF), which applies to irregularly sampled time series data. We extract variability periods for 16,880 stars from late-A through to mid-M spectral types and periods between 0.1 and 130 days with no assumed variability model. We find variable signals associated with a number of astrophysical phenomena, including stellar rotation, pulsations and multiple-star systems. The extracted variability periods are compared with stellar parameters taken from Gaia DR2, which allows us to identify distinct regions of variability in the Hertzsprung-Russell Diagram. We explore a sample of rotational main-sequence objects in period-colour space, in which we observe a dearth of rotation periods between 15 and 25 days. This 'bi-modality' was previously only seen in space-based data. We demonstrate that stars in sub-samples above and below the period gap appear to arise from a stellar population not significantly contaminated by excess multiple systems. We also observe a small population of long-period variable M-dwarfs, which highlight a departure from the predictions made by rotational evolution models fitted to solar-type main-sequence objects. The NGTS data spans a period and spectral type range that links previous rotation studies such as those using data from Kepler, K2 and MEarth., Comment: 22 pages, 13 figures, 3 tables. Accepted for publication in MNRAS

Published
2022
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10. Long-term stellar activity variations and their effect on radial-velocity measurements

Author

Costes, Jean C., Watson, Christopher A., de Mooij, Ernst, Saar, Steven H., Dumusque, Xavier, Cameron, Andrew Collier, Phillips, David F., Günther, Maximilian N., Jenkins, James S., Mortier, Annelies, and Thompson, Andrew P. G.

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

Long-term stellar activity variations can affect the detectability of long-period and Earth-analogue extrasolar planets. We have, for 54 stars, analysed the long-term trend of five activity indicators: log$R'_\mathrm{{HK}}$, the cross-correlation function (CCF) bisector span, CCF full-width-at-half-maximum, CCF contrast, and the area of the Gaussian fit to the CCF; and studied their correlation with the RVs. The sign of the correlations appears to vary as a function of stellar spectral type, and the transition in sign signals a noteworthy change in the stellar activity properties where earlier type stars appear more plage dominated. These transitions become more clearly defined when considered as a function of the convective zone depth. Therefore, it is the convective zone depth (which can be altered by stellar metallicity) that appears to be the underlying fundamental parameter driving the observed activity correlations. In addition, for most of the stars, we find that the RVs become increasingly red-shifted as activity levels increase, which can be explained by the increase in the suppression of convective blue-shift. However, we also find a minority of stars where the RVs become increasingly blue-shifted as activity levels increase. Finally, using the correlation found between activity indicators and RVs, we removed RV signals generated by long-term changes in stellar activity. We find that performing simple cleaning of such long-term signals enables improved planet detection at longer orbital periods., Comment: 22 pages, 9 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society

Published
2021
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11. NGTS 15b, 16b, 17b and 18b: four hot Jupiters from the Next Generation Transit Survey

Author

Tilbrook, Rosanna H., Burleigh, Matthew R., Costes, Jean C., Gill, Samuel, Nielsen, Louise D., Vines, José I., Queloz, Didier, Hodgkin, Simon T., Worters, Hannah L., Goad, Michael R., Acton, Jack S., Henderson, Beth A., Armstrong, David J., Anderson, David R., Bayliss, Daniel, Bouchy, François, Briegal, Joshua T., Bryant, Edward M., Casewell, Sarah L., Chaushev, Alexander, Cooke, Benjamin F., Eigmüller, Philipp, Gillen, Edward, Günther, Maximilian N., Hogan, Aleisha, Jenkins, James S., Lendl, Monika, McCormac, James, Moyano, Maximiliano, Raynard, Liam, Smith, Alexis M. S., Udry, Stéphane, Watson, Christopher A., West, Richard G., Wheatley, Peter J., Breytenbach, Hannes, Sefako, Ramotholo R., Thomas, Jessymol K., and Alves, Douglas R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of four new hot Jupiters with the Next Generation Transit Survey (NGTS). NGTS-15b, NGTS-16b, NGTS-17b, and NGTS-18b are short-period ($P<5$d) planets orbiting G-type main sequence stars, with radii and masses between $1.10-1.30$ $R_J$ and $0.41-0.76$ $M_J$. By considering the host star luminosities and the planets' small orbital separations ($0.039-0.052$ AU), we find that all four hot Jupiters are highly irradiated and therefore occupy a region of parameter space in which planetary inflation mechanisms become effective. Comparison with statistical studies and a consideration of the planets' high incident fluxes reveals that NGTS-16b, NGTS-17b, and NGTS-18b are indeed likely inflated, although some disparities arise upon analysis with current Bayesian inflationary models. However, the underlying relationships which govern radius inflation remain poorly understood. We postulate that the inclusion of additional hyperparameters to describe latent factors such as heavy element fraction, as well as the addition of an updated catalogue of hot Jupiters, would refine inflationary models, thus furthering our understanding of the physical processes which give rise to inflated planets., Comment: Accepted for publication in MNRAS

Published
2021
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13. Understand thy star, understand thy planet

Author

Costes, Jean, Watson, Christopher, and de Mooij, Ernst

Subjects
Convection, radial velocities, planets and satellites detection, activity of stars, star chromospheres, stars, solar and stellar astrophysics, earth and planetary astrophysics, photometric, planetary systems, plages, astrophysics, solar type of stars
Abstract

Instrumental precision is no longer the biggest impediment to the discovery of Earth-like planets. Indeed, future space missions and next generation spectrographs are technically capable at finding and characterising Earth-analogue planets. However, it is now stellar activity that poses a critical challenge on the pathway to detect habitable Earth-like worlds. This thesis is therefore dedicated to understanding the effect stellar activity has on spectroscopically observed radial-velocity (RV) variations used to detect the Doppler wobble reflex motion induced by orbiting planets on their host star. In this thesis, I first outline one of the most common processes by which exoplanets are detected by presenting the discovery of two hot Jupiters by NGTS. Following this discovery, I investigate how to detect smaller exoplanets using our best example: the Sun. Using the HARPS-N solar telescope, I study the possibility of detecting Venus using the RV method. However, finding Venus is proven to be impossible unless solar activity can be corrected for to some certain level. Therefore, in order to better understand stellar activity, I compare the Sun with a large number of relatively inactive stars, from F-type to M-type stars, over long timescales, with the aim of improving our detection of long-period exoplanets. I analyse the long-term changes seen for multiple activity indicators and study their correlation with the RVs. The sign of the correlations appears to vary as a function of stellar spectral type, and the transition in sign signals a noteworthy change in the stellar activity properties where earlier type stars appear more plage dominated. These transitions become more clearly defined when considered as a function of the convective zone depth. Therefore, it is the convective zone depth (which can be altered by stellar metallicity) that appears to be the underlying fundamental parameter driving the observed activity correlations. In addition, for most of the stars, I find that the RVs become increasingly red-shifted as activity levels increase, which can be explained by the increase in the suppression of convective blue-shift. However, I also find that for a minority of stars, those with deeper convective envelopes, the RVs become increasingly blue-shifted as activity levels increase. Then, using the correlations found between activity indicators and RVs, I perform a simple cleaning of the long-term RV signals induced by stellar activity. This RV noise cleaning allows me to improve the planetary detection at longer orbital periods. Using these cleaned curves, some new planetary candidates are identified. Finally, I present a new approach to search for activity indicators. By comparing active spectra from inactive ones, I aim to classify individual lines as either sensitive or insensitive to stellar activity. Such classification would then improve our data-reduction techniques, by reducing the RV variations due to stellar activity, by analysing the activity insensitive lines, or conversely providing more precise information on the stellar surface variability.

Published
2021

15. NGTS-8b and NGTS-9b: two non-inflated hot-Jupiters

Author

Costes, Jean C., Watson, Christopher A., Belardi, Claudia, Braker, Ian P., Burleigh, Matthew R., Casewell, Sarah L., Eigmüller, Philipp, Günther, Maximilian N., Jackman, James A. G., Nielsen, Louise D., Soto, Maritza G., Turner, Oliver, Anderson, David R., Bayliss, Daniel, Bouchy, François, Briegal, Joshua T., Bryant, Edward M., Cabrera, Juan, Chaushev, Alexander, Csizmadia, Szilard, Erikson, Anders, Gill, Samuel, Gillen, Edward, Goad, Michael R., Hooton, Matthew J., Jenkins, James S., McCormac, James, Moyano, Maximiliano, Queloz, Didier, Rauer, Heike, Raynard, Liam, Smith, Alexis M. S., Thompson, Andrew P. G., Tilbrook, Rosanna H., Udry, Stephane, Vines, Jose I., West, Richard G., and Wheatley, Peter J.

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

We report the discovery, by the Next Generation Transit Survey (NGTS), of two hot-Jupiters NGTS-8b and NGTS-9b. These orbit a V = 13.68 K0V star (Teff = 5241 +/- 50 K) with a period of 2.49970 days, and a V = 12.80 F8V star (Teff = 6330 +/- 130 K) in 4.43527 days, respectively. The transits were independently verified by follow-up photometric observations with the SAAO 1.0-m and Euler telescopes, and we report on the planetary parameters using HARPS, FEROS and CORALIE radial velocities. NGTS-8b has a mass, 0.93 +0.04 -0.03 MJ and a radius, 1.09 +/- 0.03 RJ similar to Jupiter, resulting in a density of 0.89 +0.08 -0.07 g cm-3. This is in contrast to NGTS-9b, which has a mass of 2.90 +/- 0.17 MJ and a radius of 1.07 +/- 0.06 RJ , resulting in a much greater density of 2.93 +0.53 -0.49 g cm-3. Statistically, the planetary parameters put both objects in the regime where they would be expected to exhibit larger than predicted radii. However, we find that their radii are in agreement with predictions by theoretical non-inflated models., Comment: 12 pages, 7 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society

Published
2019
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16. NGTS-10b: The shortest period hot Jupiter yet discovered

Author

McCormac, James, Gillen, Edward, Jackman, James A. G., Brown, David J. A., Bayliss, Daniel, Wheatley, Peter J., West, Richard G., Anderson, David R., Armstrong, David J., Bouchy, Francois, Briegal, Joshua T., Burleigh, Matthew R., Cabrera, Juan, Casewell, Sarah L., Chaushev, Alexander, Chazelas, Bruno, Chote, Paul, Cooke, Benjamin F., Costes, Jean C., Csizmadia, Szilard, Eigmuller, Philipp, Erikson, Anders, Foxell, Emma, Gaensicke, Boris T., Goad, Michael R., Gunther, Maximilian N., Hodgkin, Simon T., Hooton, Matthew J., Jenkins, James S., Lambert, Gregory, Lendl, Monika, Longstaff, Emma, Louden, Tom, Moyano, Maximiliano, Nielsen, Louise D., Pollacco, Don, Queloz, Didier, Rauer, Heike, Raynard, Liam, Smith, Alexis M. S., Smalley, Barry, Soto, Maritza, Turner, Oliver, Udry, Stephane, Vines, Jose I., Walker, Simon. R., and Watson, Christopher A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of a new ultra-short period transiting hot Jupiter from the Next Generation Transit Survey (NGTS). NGTS-10b has a mass and radius of $2.162\,^{+0.092}_{-0.107}$ M$_{\rm J}$ and $1.205\,^{+0.117}_{-0.083}$ R$_{\rm J}$ and orbits its host star with a period of $0.7668944\pm0.0000003$ days, making it the shortest period hot Jupiter yet discovered. The host is a $10.4\pm2.5$ Gyr old K5V star ($T_\mathrm{eff}$=$4400\pm100$\,K) of Solar metallicity ([Fe/H] = $-0.02\pm0.12$\,dex) showing moderate signs of stellar activity. NGTS-10b joins a short list of ultra-short period Jupiters that are prime candidates for the study of star-planet tidal interactions. NGTS-10b orbits its host at just $1.46\pm0.18$ Roche radii, and we calculate a median remaining inspiral time of $38$\,Myr and a potentially measurable transit time shift of $7$\,seconds over the coming decade, assuming a stellar tidal quality factor $Q'_{\rm s}=2\times10^{7}$., Comment: 16 pages, 19 figures and 5 tables. Submitted 27 Sept 2019. Accepted 10 Jan 2020. Published 20 Feb 2020

Published
2019
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17. NGTS-7Ab: An ultra-short period brown dwarf transiting a tidally-locked and active M dwarf

Author

Jackman, James A. G., Wheatley, Peter J., Bayliss, Dan, Gill, Samuel, Hodgkin, Simon T., Burleigh, Matthew R., Braker, Ian P., Günther, Maximilian N., Louden, Tom, Turner, Oliver, Anderson, David R., Belardi, Claudia, Bouchy, François, Briegal, Joshua T., Bryant, Edward M., Cabrera, Juan, Casewell, Sarah L., Chaushev, Alexander, Costes, Jean C., Csizmadia, Szilard, Eigmüller, Philipp, Erikson, Anders, Gänsicke, Boris T., Gillen, Edward, Goad, Michael R., Jenkins, James S., McCormac, James, Moyano, Maximiliano, Nielsen, Louise D., Pollacco, Don, Poppenhaeger, Katja, Queloz, Didier, Rauer, Heike, Raynard, Liam, Smith, Alexis M. S., Udry, Stéphane, Vines, Jose I., Watson, Christopher A., and West, Richard G.

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

We present the discovery of NGTS-7Ab, a high mass brown dwarf transiting an M dwarf with a period of 16.2 hours, discovered as part of the Next Generation Transit Survey (NGTS). This is the shortest period transiting brown dwarf around a main or pre-main sequence star to date. The M star host (NGTS-7A) has an age of roughly 55 Myr and is in a state of spin-orbit synchronisation, which we attribute to tidal interaction with the brown dwarf acting to spin up the star. The host star is magnetically active and shows multiple flares across the NGTS and follow up lightcurves, which we use to probe the flare-starspot phase relation. The host star also has an M star companion at a separation of 1.13 arcseconds with very similar proper motion and systemic velocity, suggesting the NGTS-7 system is a hierarchical triple. The combination of tidal synchronisation and magnetic braking is expected to drive ongoing decay of the brown dwarf orbit, with a remaining lifetime of only 5-10 Myr., Comment: 21 pages, 16 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society

Published
2019
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18. Author Correction: Pictograms to aid laypeople in identifying the addictiveness of gambling products (PictoGRRed study)

Author

Luquiens, Amandine, Guillou, Morgane, Giustiniani, Julie, Barrault, Servane, Caillon, Julie, Delmas, Helena, Achab, Sophia, Bento, Bruno, Billieux, Joël, Brevers, Damien, Brody, Aymeric, Brunault, Paul, Challet-Bouju, Gaëlle, Chóliz, Mariano, Clark, Luke, Cornil, Aurélien, Costes, Jean-Michel, Devos, Gaetan, Díaz, Rosa, Estevez, Ana, Grassi, Giacomo, Hakansson, Anders, Khazaal, Yasser, King, Daniel L., Labrador, Francisco, Lopez-Gonzalez, Hibai, Newall, Philip, Perales, José C., Ribadier, Aurélien, Sescousse, Guillaume, Sharman, Stephen, Taquet, Pierre, Varescon, Isabelle, Von Hammerstein, Cora, Bonjour, Thierry, Romo, Lucia, and Grall-Bronnec, Marie

Published
2023
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20. FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) I: Project Overview and Initial Results

Author

Umemoto, Tomofumi, Minamidani, Tetsuhiro, Kuno, Nario, Fujita, Shinji, Matsuo, Mitsuhiro, Nishimura, Atsushi, Torii, Kazufumi, Tosaki, Tomoka, Kohno, Mikito, Kuriki, Mika, Tsuda, Yuya, Hirota, Akihiko, Ohashi, Satoshi, Yamagishi, Mitsuyoshi, Handa, Toshihiro, Nakanishi, Hiroyuki, Omodaka, Toshihiro, Koide, Nagito, Matsumoto, Naoko, Onishi, Toshikazu, Tokuda, Kazuki, Seta, Masumichi, Kobayashi, Yukinori, Tachihara, Kengo, Sano, Hidetoshi, Hattori, Yusuke, Onodera, Sachiko, Oasa, Yumiko, Kamegai, Kazuhisa, Tsuboi, Masato, Sofue, Yoshiaki, Higuchi, Aya E., Chibueze, James O., Mizuno, Norikazu, Honma, Mareki, Muller, Erik, Inoue, Tsuyoshi, Morokuma-Matsui, Kana, Shinnaga, Hiroko, Ozawa, Takeaki, Takahashi, Ryo, Yoshiike, Satoshi, Costes, Jean, and Kuwahara, Sho

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) project is one of the legacy projects using the new multi-beam FOREST receiver installed on the Nobeyama 45-m telescope. This project aims to investigate the distribution, kinematics, and physical properties of both diffuse and dense molecular gas in the Galaxy at once by observing 12CO, 13CO, and C18O J=1-0 lines simultaneously. The mapping regions are a part of the 1st quadrant (10d < l < 50d, |b| < 1d) and the 3rd quadrant (198d < l <236d, |b| < 1d) of the Galaxy, where spiral arms, bar structure, and the molecular gas ring are included. This survey achieves the highest angular resolution to date (~20") for the Galactic plane survey in the CO J=1-0 lines, which makes it possible to find dense clumps located farther away than the previous surveys. FUGIN will provide us with an invaluable dataset for investigating the physics of the galactic interstellar medium (ISM), particularly the evolution of interstellar gas covering galactic scale structures to the internal structures of giant molecular clouds, such as small filament/clump/core. We present an overview of the FUGIN project, observation plan, and initial results, which reveal wide-field and detailed structures of molecular clouds, such as entangled filaments that have not been obvious in previous surveys, and large-scale kinematics of molecular gas such as spiral arms., Comment: 19 pages, 14 figures, accepted for publication in PASJ

Published
2017
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21. A new view of the giant molecular cloud M16 (Eagle Nebula) in 12CO J=1-0 and 2-1 transitions with NANTEN2

Author

Nishimura, Atsushi, Costes, Jean, Inaba, Tetsuta, Tachihara, Kengo, Hattori, Yusuke, Kohno, Mikito, Ohama, Akio, Torii, Kazufumi, Sano, Hidetoshi, Yamamoto, Hiroaki, Hasegawa, Yutaka, Kimura, Kimihiro, Ogawa, Hideo, and Fukui, Yasuo

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

M16, the Eagle Nebula, is an outstanding HII region where extensive high-mass star formation is taking place in the Sagittarius Arm, and hosts the remarkable "pillars" observed with HST. We made new CO observations of the region in the 12CO J=1--0 and J=2--1 transitions with NANTEN2. These observations revealed for the first time that a giant molecular cloud of $\sim 1.3 \times 10^5$ \Msun \ is associated with M16, which is elongated vertically to the Galactic plane over 35 pc at a distance of 1.8 kpc. We found a cavity of the molecular gas of $\sim 10$ pc diameter toward the heart of M16 at \lbeq (16.95\degree, 0.85\degree), where more than 10 O-type stars and $\sim 400$ stars are associated, in addition to a close-by molecular cavity toward a Spitzer bubble N19 at \lbeq (17.06\degree, 1.0\degree). We found three velocity components which show spatially complementary distribution in the entire M16 giant molecular cloud (GMC) including NGC6611 and N19, suggesting collisional interaction between them. Based on the above results we frame a hypothesis that collision between the red-shifted and blue-shifted components at a relative of $\sim 10$ \kms \ triggered formation of the O-type stars in the M16 GMC in the last 1-2 Myr. The collision is two fold in the sense that one of the collisional interactions is major toward the M16 cluster and the other toward N19 with a RCW120 type, the former triggered most of the O star formation with almost full ionization of the parent gas, and the latter an O star formation in N19., Comment: 20 pages, 10 figures, submitted to PASJ

Published
2017

22. Pictograms to aid laypeople in identifying the addictiveness of gambling products (PictoGRRed study)

Author

Luquiens, Amandine, Guillou, Morgane, Giustiniani, Julie, Barrault, Servane, Caillon, Julie, Delmas, Helena, Achab, Sophia, Bento, Bruno, Billieux, Joël, Brody, Aymeric, Brunault, Paul, Challet-Bouju, Gaëlle, Chóliz, Mariano, Clark, Luke, Cornil, Aurélien, Costes, Jean-Michel, Devos, Gaetan, Díaz, Rosa, Estevez, Ana, Grassi, Giacomo, Hakansson, Anders, Khazaal, Yasser, King, Daniel L., Labrador, Francisco, Lopez-Gonzalez, Hibai, Newall, Philip, Perales, José C., Ribadier, Aurélien, Sescousse, Guillaume, Sharman, Stephen, Taquet, Pierre, Varescon, Isabelle, Von Hammerstein, Cora, Bonjour, Thierry, Romo, Lucia, and Grall-Bronnec, Marie

Published
2022
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35. A simple reaction pathway allowing easy EPR characterization of N-oxyl radicals.

Author

Costes, Jean-Pierre

Subjects
*RADICALS (Chemistry), *SECONDARY amines, *RADICALS, *COPPER compounds, *TOLUENE
Abstract

Mixing a dinuclear CuII complex with an excess of primary or secondary amine in the presence of dioxygen with or without toluene yields N-oxyl radicals and CuI entities. The EPR spectra of these radicals clearly show their evolution from the initial to the final state. Under these mild conditions, it is not possible to obtain Tempo radicals, steric crowding impeding the approach of the corresponding amine into the CuII coordination sphere. [ABSTRACT FROM AUTHOR]

Published
2024
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41. A la recherche du mystérieux Cary Grant

Author

Costes, Jean-Philippe, Costes, Jean-Philippe, Costes, Jean-Philippe, and Costes, Jean-Philippe

Abstract

Mon premier est un acteur adulé par le public depuis 1937.?Mon deuxième s’est ingénié à garder le secret sur sa vie privée.?Mon troisième est l’incarnation de la classe et du charme.?Mon quatrième a brillé dans l’ensemble des genres cinématographiques, de la comédie au drame en passant par l’espionnage.?La réponse, vous l’avez devinée : Cary Grant.?Tout est dit et rien n’est dit : à force de nimber sa personnalité de mystère, Cary Grant est l’une des célébrités les plus méconnues du monde. Et ce ne sont pas les nombreux articles de presse ou les multiples biographies qui lui ont été consacrés qui lèveront totalement le voile. C’est en effet au sein même d’une œuvre en forme de charade que le malicieux complice d’Alfred Hitchcock a caché la vérité de son être. Une vérité qui, loin des conventions et des images immaculées du star-system, fera mentir vos certitudes d’admirateur ou d’amateur du septième art. Essayiste et docteur en sciences politiques de l’université Paris II Panthéon-Assas, Jean-Philippe Costes a pour ambition d’éclairer les grands enjeux éthiques et philosophiques de la vie à la lumière du cinéma et de la culture populaire. Aux éditions Liber, cet amateur de figures contestataires et de héros anticonformistes a récemment publié Les Subversifs hollywoodiens, Le Monde selon James Bond, La Sagesse du septième art et Tintin au pays du mal.

Published
2022

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