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1. 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, Cesar, 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, Acuña, Lorena, 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, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebastià 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, 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, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, 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, Jorgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, 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, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Degl'Innocenti, Scilla, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, 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, Estrela, Inês, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, 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, Galli, Emanuele, Garcia, 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, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, Grießbach, Denis, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Loïc, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, 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, 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, Kučinskas, 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, 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, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, Érico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, 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., Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Benoît, 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, Stefano, 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, Quirrenbach160, ndreas, Reina6, 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, Rodríguez, María Teresa Rodrigo, 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, Santoli, Francesco, Santos, Ângela 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, Švanda, 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, Weingril, 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

2. The $\beta$ Pictoris b Hill sphere transit campaign. Paper II: Searching for the signatures of the $\beta$ Pictoris exoplanets through time delay analysis of the $\delta$ Scuti pulsations

Author

Zieba, Sebastian, Zwintz, Konstanze, Kenworthy, Matthew, Hey, Daniel, Murphy, Simon J., Kuschnig, Rainer, Abe, Lyu, Agabi, Abdelkrim, Mekarnia, Djamel, Guillot, Tristan, Schmider, François-Xavier, Stee, Philippe, De Pra, Yuri, Buttu, Marco, Crouzet, Nicolas, Mellon, Samuel, Bailey III, Jeb, Stuik, Remko, Dorval, Patrick, Talens, Geert-Jan J., Crawford, Steven, Mamajek, Eric, Laginja, Iva, Ireland, Michael, Lomberg, Blaine, Kuhn, Rudi, Snellen, Ignas, Kalas, Paul, Wang, Jason J., Stevenson, Kevin B., de Mooij, Ernst, Lagrange, Anne-Marie, Lacour, Sylvestre, Nowak, Mathias, Strøm, Paul A., Hui, Zhang, and Wang, Lifan

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

The $\beta$ Pictoris system is the closest known stellar system with directly detected gas giant planets, an edge-on circumstellar disc, and evidence of falling sublimating bodies and transiting exocomets. The inner planet, $\beta$ Pictoris c, has also been indirectly detected with radial velocity (RV) measurements. The star is a known $\delta$ Scuti pulsator, and the long-term stability of these pulsations opens up the possibility of indirectly detecting the gas giant planets through time delays of the pulsations due to a varying light travel time. We search for phase shifts in the $\delta$ Scuti pulsations consistent with the known planets $\beta$ Pictoris b and c and carry out an analysis of the stellar pulsations of $\beta$ Pictoris over a multi-year timescale. We used photometric data collected by the BRITE-Constellation, bRing, ASTEP, and TESS to derive a list of the strongest and most significant $\delta$ Scuti pulsations. We carried out an analysis with the open-source python package maelstrom to study the stability of the pulsation modes of $\beta$ Pictoris in order to determine the long-term trends in the observed pulsations. We did not detect the expected signal for $\beta$ Pictoris b or $\beta$ Pictoris c. The expected time delay is 6 seconds for $\beta$ Pictoris c and 24 seconds for $\beta$ Pictoris b. With simulations, we determined that the photometric noise in all the combined data sets cannot reach the sensitivity needed to detect the expected timing drifts. An analysis of the pulsational modes of $\beta$ Pictoris using maelstrom showed that the modes themselves drift on the timescale of a year, fundamentally limiting our ability to detect exoplanets around $\beta$ Pictoris via pulsation timing., Comment: 16 pages, 16 figures, 4 tables, accepted for publication in A&A

Published
2024
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3. Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey: III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-Transit Jupiter Orbiting TOI-2010

Author

Mann, Christopher R., Dalba, Paul A., Lafrenière, David, Fulton, Benjamin J., Hébrard, Guillaume, Boisse, Isabelle, Dalal, Shweta, Deleuil, Magali, Delfosse, Xavier, Demangeon, Olivier, Forveille, Thierry, Heidari, Neda, Kiefer, Flavien, Martioli, Eder, Moutou, Claire, Endl, Michael, Cochran, William D., MacQueen, Phillip, Marchis, Franck, Dragomir, Diana, Gupta, Arvind F., Feliz, Dax L., Nicholson, Belinda A., Ziegler, Carl, Villanueva Jr., Steven, Rowe, Jason, Talens, Geert Jan, Thorngren, Daniel, LaCourse, Daryll, Jacobs, Tom, Howard, Andrew W., Bieryla, Allyson, Latham, David W., Rabus, Markus, Fetherolf, Tara, Hellier, Coel, Howell, Steve B., Plavchan, Peter, Reefe, Michael, Combs, Deven, Bowen, Michael, Wittrock, Justin, Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Barclay, Thomas, Watanabe, David, Collins, Karen A., Eastman, Jason D., and Ting, Eric B.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Large-scale exoplanet surveys like the TESS mission are powerful tools for discovering large numbers of exoplanet candidates. Single-transit events are commonplace within the resulting candidate list due to the unavoidable limitation of observing baseline. These single-transit planets often remain unverified due to their unknown orbital period and consequent difficulty in scheduling follow up observations. In some cases, radial velocity (RV) follow up can constrain the period enough to enable a future targeted transit detection. We present the confirmation of one such planet: TOI-2010 b. Nearly three years of RV coverage determined the period to a level where a broad window search could be undertaken with the Near-Earth Object Surveillance Satellite (NEOSSat), detecting an additional transit. An additional detection in a much later TESS sector solidified our final parameter estimation. We find TOI-2010 b to be a Jovian planet ($M_P = 1.29 \ M_{\rm Jup}$, $R_P = 1.05 \ R_{\rm Jup}$) on a mildly eccentric orbit ($e = 0.21$) with a period of $P = 141.83403$ days. Assuming a simple model with no albedo and perfect heat redistribution, the equilibrium temperature ranges from about 360 K to 450 K from apoastron to periastron. Its wide orbit and bright host star ($V=9.85$) make TOI-2010 b a valuable test-bed for future low-insolation atmospheric analysis., Comment: 27 pages, 10 figures, 6 tables

Published
2023
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4. The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope -- III. Single Object Slitless Spectroscopy

Author

Albert, Loic, Lafreniere, David, Doyon, Rene, Artigau, Etienne, Volk, Kevin, Goudfrooij, Paul, Martel, Andre R., Radica, Michael, Rowe, Jason, Espinoza, Nestor, Roy, Arpita, Filippazzo, Joseph C., Darveau-Bernier, Antoine, Talens, Geert Jan, Sivaramakrishnan, Anand, Willott, Chris J., Fullerton, Alexander W., LaMassa, Stephanie, Hutchings, John B., Rowlands, Neil, Vila, M. Begona, Zhou, Julia, Aldridge, David, Maszkiewicz, Michael, Beaulieu, Mathilde, Cook, Neil J., Piaulet, Caroline, Roy, Pierre-Alexis, Lamontagne, Pierrot, Morel, Kim, Frost, William, Salhi, Salma, Coulombe, Louis-Philippe, Benneke, Bjorn, MacDonald, Ryan J., Johnstone, Doug, Turner, Jake D., Fournier-Tondreau, Marylou, Allart, Romain, and Kaltenegger, Lisa

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

The Near Infrared Imager and Slitless Spectrograph instrument (NIRISS) is the Canadian Space Agency (CSA) contribution to the suite of four science instruments of JWST. As one of the three NIRISS observing modes, the Single Object Slitless Spectroscopy (SOSS) mode is tailor-made to undertake time-series observations of exoplanets to perform transit spectroscopy. The SOSS permits observing point sources between 0.6 and 2.8 um at a resolving power of 650 at 1.25 um using a slit-less cross-dispersing grism while its defocussing cylindrical lens enables observing targets as bright as J=6.7 by spreading light across 23 pixels along the cross-dispersion axis. This paper officially presents the design of the SOSS mode, its operation, characterization, and its performance, from ground-based testing and flight-based Commissioning. On-sky measurements demonstrate a peak photon conversion efficiency of 55% at 1.2 um. The first time-series on the A-type star BD+60o1753 achieves a flux stability close to the photon-noise limit, so far tested to a level of 20 parts per million on 40-minute time-scales after simply subtracting a long-term trend. Uncorrected 1/f noise residuals underneath the spectral traces add an extra source of noise equivalent to doubling the readout noise. Preliminary analysis of a HAT-P-14b transit time-series indicates that it is difficult to remove all the noise in pixels with partially saturated ramps. Overall, the SOSS delivers performance at the level required to tackle key exoplanet science programs such as detecting secondary atmospheres on terrestrial planets and measuring abundances of several chemical species in gas giants., Comment: 41 pages, 28 figures, accepted for publication in PASP

Published
2023
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5. The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope -- I. Instrument Overview and in-Flight Performance

Author

Doyon, Rene, Willott, C. J, Hutchings, John B., Sivaramakrishnan, Anand, Albert, Loic, Lafreniere, David, Rowlands, Neil, Vila, M. Begona, Martel, Andre R., LaMassa, Stephanie, Aldridge, David, Artigau, Etienne, Cameron, Peter, Chayer, Pierre, Cook, Neil J., Cooper, Rachel A., Darveau-Bernier, Antoine, Dupuis, Jean, Earnshaw, Colin, Espinoza, Nestor, Filippazzo, Joseph C., Fullerton, Alexander W., Gaudreau, Daniel, Gawlik, Roman, Goudfrooij, Paul, Haley, Craig, Kammerer, Jens, Kendall, David, Lambros, Scott D., Ignat, Luminita Ilinca, Maszkiewicz, Michael, McColgan, Ashley, Morishita, Takahiro, Ouellette, Nathalie N. -Q., Pacifici, Camilla, Philippi, Natasha, Radica, Michael, Ravindranath, Swara, Rowe, Jason, Roy, Arpita, Saad, Karl, Sohn, Sangmo Tony, Talens, Geert Jan, Thatte, Deepashri, Taylor, Joanna M., Vandal, Thomas, Volk, Kevin, Wander, Michel, Warner, Gerald, Zheng, Sheng-Hai, Zhou, Julia, Abraham, Roberto, Beaulieu, Mathilde, Benneke, Bjorn, Ferrarese, Laura, Johnstone, Doug, Kaltenegger, Lisa, Meyer, Michael R., Pipher, Judy L., Rameau, Julien, Rieke, Marcia, Salhi, Salma, and Sawicki, Marcin

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Near-Infrared Imager and Slitless Spectrograph (NIRISS) is the science module of the Canadian-built Fine Guidance Sensor (FGS) onboard the James Webb Space Telescope (JWST). NIRISS has four observing modes: 1) broadband imaging featuring seven of the eight NIRCam broadband filters, 2) wide-field slitless spectroscopy (WFSS) at a resolving power of $\sim$150 between 0.8 and 2.2 $\mu$m, 3) single-object cross-dispersed slitless spectroscopy (SOSS) enabling simultaneous wavelength coverage between 0.6 and 2.8 $\mu$m at R$\sim$700, a mode optimized for exoplanet spectroscopy of relatively bright ($J<6.3$) stars and 4) aperture masking interferometry (AMI) between 2.8 and 4.8 $\mu$m enabling high-contrast ($\sim10^{-3}-10^{-4}$) imaging at angular separations between 70 and 400 milliarcsec for relatively bright ($M<8$) sources. This paper presents an overview of the NIRISS instrument, its design, its scientific capabilities, and a summary of in-flight performance. NIRISS shows significantly better response shortward of $\sim2.5\,\mu$m resulting in 10-40% sensitivity improvement for broadband and low-resolution spectroscopy compared to pre-flight predictions. Two time-series observations performed during instrument commissioning in the SOSS mode yield very stable spectro-photometry performance within $\sim$10% of the expected noise. The first space-based companion detection of the tight binary star AB Dor AC through AMI was demonstrated.

Published
2023

6. Awesome SOSS: Transmission Spectroscopy of WASP-96b with NIRISS/SOSS

Author

Radica, Michael, Welbanks, Luis, Espinoza, Néstor, Taylor, Jake, Coulombe, Louis-Philippe, Feinstein, Adina D., Goyal, Jayesh, Scarsdale, Nicholas, Albert, Loic, Baghel, Priyanka, Bean, Jacob L., Blecic, Jasmina, Lafrenière, David, MacDonald, Ryan J., Zamyatina, Maria, Allart, Romain, Artigau, Étienne, Batalha, Natasha E., Cook, Neil James, Cowan, Nicolas B., Dang, Lisa, Doyon, René, Fournier-Tondreau, Marylou, Johnstone, Doug, Line, Michael R., Moran, Sarah E., Mukherjee, Sagnick, Pelletier, Stefan, Roy, Pierre-Alexis, Talens, Geert Jan, Filippazzo, Joseph, Pontoppidan, Klaus, and Volk, Kevin

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The future is now - after its long-awaited launch in December 2021, JWST began science operations in July 2022 and is already revolutionizing exoplanet astronomy. The Early Release Observations (ERO) program was designed to provide the first images and spectra from JWST, covering a multitude of science cases and using multiple modes of each on-board instrument. Here, we present transmission spectroscopy observations of the hot-Saturn WASP-96b with the Single Object Slitless Spectroscopy (SOSS) mode of the Near Infrared Imager and Slitless Spectrograph, observed as part of the ERO program. As the SOSS mode presents some unique data reduction challenges, we provide an in-depth walk-through of the major steps necessary for the reduction of SOSS data: including background subtraction, correction of 1/f noise, and treatment of the trace order overlap. We furthermore offer potential routes to correct for field star contamination, which can occur due to the SOSS mode's slitless nature. By comparing our extracted transmission spectrum with grids of atmosphere models, we find an atmosphere metallicity between 1x and 5x solar, and a solar carbon-to-oxygen ratio. Moreover, our models indicate that no grey cloud deck is required to fit WASP-96b's transmission spectrum, but find evidence for a slope shortward of 0.9$\mu$m, which could either be caused by enhanced Rayleigh scattering or the red wing of a pressure-broadened Na feature. Our work demonstrates the unique capabilities of the SOSS mode for exoplanet transmission spectroscopy and presents a step-by-step reduction guide for this new and exciting instrument., Comment: MNRAS, in press. Updated to reflect published version

Published
2023
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7. ATOCA: an algorithm to treat order contamination. Application to the NIRISS SOSS mode

Author

Darveau-Bernier, Antoine, Albert, Loïc, Talens, Geert Jan, Lafrenière, David, Radica, Michael, Doyon, René, Cook, Neil J., Rowe, Jason F., Artigau, Étienne, Benneke, Björn, Cowan, Nicolas, Dang, Lisa, Espinoza, Néstor, Johnstone, Doug, Kaltenegger, Lisa, Lim, Olivia, Pelletier, Stefan, Piaulet, Caroline, Roy, Arpita, Roy, Pierre-Alexis, Splinter, Jared, Taylor, Jake, and Turner, Jake D.

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

After a successful launch, the James Webb Space Telescope is preparing to undertake one of its principal missions, the characterization of the atmospheres of exoplanets. The Single Object Slitless Spectroscopy (SOSS) mode of the Near Infrared Imager and Slitless Spectrograph (NIRISS) is the only observing mode that has been specifically designed for this objective. It features a wide simultaneous spectral range (0.6--2.8\,\micron) through two spectral diffraction orders. However, due to mechanical constraints, these two orders overlap slightly over a short range, potentially introducing a ``contamination'' signal in the extracted spectrum. We show that for a typical box extraction, this contaminating signal amounts to 1\% or less over the 1.6--2.8\,\micron\ range (order 1), and up to 1\% over the 0.85--0.95\,\micron\ range (order 2). For observations of exoplanet atmospheres (transits, eclipses or phase curves) where only temporal variations in flux matter, the contamination signal typically biases the results by order of 1\% of the planetary atmosphere spectral features strength. To address this problem, we developed the Algorithm to Treat Order ContAmination (ATOCA). By constructing a linear model of each pixel on the detector, treating the underlying incident spectrum as a free variable, ATOCA is able to perform a simultaneous extraction of both orders. We show that, given appropriate estimates of the spatial trace profiles, the throughputs, the wavelength solutions, as well as the spectral resolution kernels for each order, it is possible to obtain an extracted spectrum accurate to within 10\,ppm over the full spectral range., Comment: Submitted to PASP. 22 pages, 12 figures

Published
2022
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8. APPLESOSS: A Producer of ProfiLEs for SOSS. Application to the NIRISS SOSS Mode

Author

Radica, Michael, Albert, Loïc, Taylor, Jake, Lafrenière, David, Coulombe, Louis-Philippe, Darveau-Bernier, Antoine, Doyon, René, Cook, Neil, Cowan, Nicolas, Espinoza, Néstor, Johnstone, Doug, Kaltenegger, Lisa, Piaulet, Caroline, Roy, Arpita, and Talens, Geert Jan

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

The SOSS mode of the NIRISS instrument is poised to be one of the workhorse modes for exoplanet atmosphere observations with the newly launched James Webb Space Telescope. One of the challenges of the SOSS mode, however, is the physical overlap of the first two diffraction orders of the G700XD grism on the detector. Recently, the ATOCA algorithm was developed and implemented as an option in the official JWST pipeline, as a method to extract SOSS spectra by decontaminating the detector -- that is, separating the first and second orders. Here, we present APPLESOSS (A Producer of ProfiLEs for SOSS), which generates the spatial profiles for each diffraction order upon which ATOCA relies. We validate APPLESOSS using simulated SOSS time series observations of WASP-52\,b, and compare it to ATOCA extractions using two other spatial profiles (a best and worst case scenario on-sky), as well as a simple box extraction performed without taking into account the order contamination. We demonstrate that APPLESOSS profiles retain a high degree of fidelity to the true underlying spatial profiles, and therefore yield accurate extracted spectra. We further confirm that the effects of the order contamination for relative measurements (e.g., exoplanet transmission or emission observations) is small -- the transmission spectrum obtained from each of our four tests, including the contaminated box extraction, is consistent at the $\sim$1$\sigma$ level with the atmosphere model input into our noiseless simulations. We further confirm via a retrieval analysis that the atmosphere parameters (metallicity and C/O) obtained from each transmission spectrum are consistent with the true underlying values., Comment: 11 pages, 10 figures. Published in PASP

Published
2022
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9. TOI-1431b/MASCARA-5b: A Highly Irradiated Ultra-Hot Jupiter Orbiting One of the Hottest & Brightest Known Exoplanet Host Stars

Author

Addison, Brett Christopher, Knudstrup, Emil, Wong, Ian, Hebrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier, Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, Rene, Antoci, Victoria, Buchhave, Lars A., Gunther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hanse, Jens, Palle, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., and McLean, Brian

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery of a highly irradiated and moderately inflated ultra-hot Jupiter, TOI-1431b/MASCARA-5b (HD 201033b), first detected by NASA's Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky CAmeRA (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of $K=294.1\pm1.1$ m s$^{-1}$. A joint analysis of the TESS and ground-based photometry and radial velocity measurements reveals that TOI-1431b has a mass of $M_{p}=3.12\pm0.18$ $\rm{M_J}$ ($990\pm60$ M$_{\oplus}$), an inflated radius of $R_{p}=1.49\pm0.05$ $\rm{R_J}$ ($16.7\pm0.6$ R$_{\oplus}$), and an orbital period of $P=2.650237\pm0.000003$ d. Analysis of the spectral energy distribution of the host star reveals that the planet orbits a bright ($\mathrm{V}=8.049$ mag) and young ($0.29^{+0.32}_{-0.19}$ Gyr) Am type star with $T_{\rm eff}=7690^{+400}_{-250}$ $\rm{K}$, resulting in a highly irradiated planet with an incident flux of $\langle F \rangle=7.24^{+0.68}_{-0.64}\times$10$^9$ erg s$^{-1}$ cm$^{-2}$ ($5300^{+500}_{-470}\mathrm{S_{\oplus}}$) and an equilibrium temperature of $T_{eq}=2370\pm70$ K. TESS photometry also reveals a secondary eclipse with a depth of $127^{+4}_{-5}$ppm as well as the full phase curve of the planet's thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as $T_\mathrm{day}=3004\pm64$ K and $T_\mathrm{night}=2583\pm63$ K, the second hottest measured nightside temperature. The planet's low day/night temperature contrast ($\sim$420 K) suggests very efficient heat transport between the dayside and nightside hemispheres., Comment: Accepted for publication in the Astronomical Journal. 39 pages, 18 figures, and 4 tables

Published
2021
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10. Gravity-Darkening Analysis of Misaligned Hot Jupiter MASCARA-4 b

Author

Ahlers, John P., Kruse, Ethan, Colon, Knicole D., Dorval, Patrick, Talens, Geert Jan, Snellen, Ignas, Albrecht, Simon, Otten, Gilles, Ricker, George, Vanderspek, Roland, Latham, David, Seager, Sara, Winn, Joshua, Jenkins, Jon M., Haworth, Kari, Cartwright, Scott, Morris, Robert, Rowden, Pam, Tenenbaum, Peter, and TIng, Eric B.

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

MASCARA-4 b is a hot Jupiter in a highly-misaligned orbit around a rapidly-rotating A3V star that was observed for 54 days by the Transiting Exoplanet Survey Satellite (\tess). We perform two analyses of MASCARA-4 b using a stellar gravity-darkened model. First, we measure MASCARA-4 b's misaligned orbital configuration by modeling its \tess~photometric light curve. We take advantage of the asymmetry in MASCARA-4 b's transit due to its host star's gravity-darkened surface to measure MASCARA-4 b's true spin-orbit angle to be $104^{\circ+7^\circ}_{-13^\circ}$. We also detect a $\sim4\sigma$ secondary eclipse at $0.491\pm0.007$ orbital phase, proving that the orbit is slightly eccentric. Second, we model MASCARA-4 b's insolation including gravity-darkening and find that the planet's received XUV flux varies by $4$\% throughout its orbit. MASCARA-4 b's short-period, polar orbit suggests that the planet likely underwent dramatic orbital evolution to end up in its present-day configuration and that it receives a varying stellar irradiance that perpetually forces the planet out of thermal equilibrium. These findings make MASCARA-4 b an excellent target for follow-up characterization to better understand orbital evolution and current-day of planets around high-mass stars., Comment: Accepted for publication in ApJ

Published
2019
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11. An unusually large gaseous transit in a debris disc

Author

Iglesias, Daniela P., Olofsson, Johan, Bayo, Amelia, Zieba, Sebastian, Montesinos, Matías, Smoker, Jonathan, Kennedy, Grant M., Godoy, Nicolás, Pantoja, Blake, Talens, Geert Jan, Wahhaj, Zahed, and Zamora, Catalina

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

We present the detection of an unusually large transient gas absorption in several ionized species in the debris disc star HD 37306 using high-resolution optical spectra. We have been analysing a large sample of debris discs searching for circumstellar gas absorptions aiming to determine the frequency of gas in debris discs. HD 37306 stood out showing remarkably broad absorptions superimposed onto several photospheric Ca ii, Fe ii and Ti ii lines. The observed absorptions, unlike typical exocometary transits, lasted for at least eight days. Here we analyse simultaneous spectroscopic and photometric data of the event and evaluate different scenarios that might explain the observed features. We conclude that the most likely scenario might be an exocometary break-up releasing a significant amount of gas close to the star, producing an occulting "ring"/"torus" shape., Comment: 11 pages, 10 figures, accepted in MNRAS

Published
2019
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12. Bright Southern Variable Stars in the bRing Survey

Author

Mellon, Samuel N., Mamajek, Eric E., Stuik, Remko, Zwintz, Konstanze, Kenworthy, Matthew A., Talens, Geert Jan J., Burggraaff, Olivier, Bailey III, John I., Dorval, Patrick, Lomberg, Blaine B. D., Kuhn, Rudi B., and Ireland, Michael J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Besides monitoring the bright star $\beta$ Pic during the near transit event for its giant exoplanet, the $\beta$ Pictoris b Ring (bRing) observatories at Siding Springs Observatory, Australia and Sutherland, South Africa have monitored the brightnesses of bright stars ($V$ $\simeq$ 4--8 mag) centered on the south celestial pole ($\delta$ $\leq$ -30$^{\circ}$) for approximately two years. Here we present a comprehensive study of the bRing time series photometry for bright southern stars monitored between 2017 June and 2019 January. Of the 16762 stars monitored by bRing, 353 of them were found to be variable. Of the variable stars, 80% had previously known variability and 20% were new variables. Each of the new variables was classified, including 3 new eclipsing binaries (HD 77669, HD 142049, HD 155781), 26 $\delta$ Scutis, 4 slowly pulsating B stars, and others. This survey also reclassified four stars based on their period of pulsation, light curve, spectral classification, and color-magnitude information. The survey data were searched for new examples of transiting circumsecondary disk systems, but no candidates were found., Comment: Accepted by ApJS, 35 pages, 5 figures, 10 tables

Published
2019
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13. Discovery of {\delta} Scuti Pulsations in the Young Hybrid Debris Disk Star HD 156623

Author

Mellon, Samuel N., Mamajek, Eric E., Zwintz, Konstanze, David, Trevor J., Stuik, Remko, Talens, Geert Jan J., Dorval, Patrick, Burggraaff, Olivier, Kenworthy, Matthew A., Bailey III, John I., Lomberg, Blaine B. D., Kuhn, Rudi B., Ireland, Michael J., and Crawford, Steven M.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The bRing robotic observatory network was built to search for circumplanetary material within the transiting Hill sphere of the exoplanet $\beta$ Pic b across its bright host star $\beta$ Pic. During the bRing survey of $\beta$ Pic, it simultaneously monitored the brightnesses of thousands of bright stars in the southern sky ($V$ $\simeq$ 4-8, $\delta$ $\lesssim$ -30$^{\circ}$). In this work, we announce the discovery of $\delta$ Scuti pulsations in the A-type star HD 156623 using bRing data. HD 156623 is notable as it is a well-studied young star with a dusty and gas-rich debris disk, previously detected using ALMA. We present the observational results on the pulsation periods and amplitudes for HD 156623, discuss its evolutionary status, and provide further constraints on its nature and age. We find strong evidence of frequency regularity and grouping. We do not find evidence of frequency, amplitude, or phase modulation for any of the frequencies over the course of the observations. We show that HD 156623 is consistent with other hot and high frequency pre-MS and early ZAMS $\delta$ Scutis as predicted by theoretical models and corresponding evolutionary tracks, although we observe that HD 156623 lies hotter than the theoretical blue edge of the classical instability strip. This, coupled with our characterization and Sco-Cen membership analyses, suggest that the star is most likely an outlying ZAMS member of the $\sim$16 Myr Upper Centaurus-Lupus subgroup of the Sco-Cen association., Comment: Accepted by ApJ, 15 pages, 7 figures, 6 tables

Published
2018
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14. The relationship between the morphology and kinematics of galaxies and its dependence on dark matter halo structure in EAGLE

Author

Thob, Adrien C. R., Crain, Robert A., McCarthy, Ian G., Schaller, Matthieu, Lagos, Claudia D. P., Schaye, Joop, Talens, Geert Jan J., James, Philip A., Theuns, Tom, and Bower, Richard G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We investigate the connection between the morphology and internal kinematics of the stellar component of central galaxies with mass $M_\star > {10}^{9.5} {\rm M}_\odot$ in the EAGLE simulations. We compare several kinematic diagnostics commonly used to describe simulated galaxies, and find good consistency between them. We model the structure of galaxies as ellipsoids and quantify their morphology via the ratios of their principal axes. We show that the differentiation of blue star-forming and red quiescent galaxies using morphological diagnostics can be achieved with similar efficacy to the use of kinematical diagnostics, but only if one is able to measure both the flattening and the triaxiality of the galaxy. Flattened oblate galaxies exhibit greater rotational support than their spheroidal counterparts, but there is significant scatter in the relationship between morphological and kinematical diagnostics, such that kinematically-similar galaxies can exhibit a broad range of morphologies. The scatter in the relationship between the flattening and the ratio of the rotation and dispersion velocities ($v/\sigma$) correlates strongly with the anisotropy of the stellar velocity dispersion: at fixed $v/\sigma$, flatter galaxies exhibit greater dispersion in the plane defined by the intermediate and major axes than along the minor axis, indicating that the morphology of simulated galaxies is influenced significantly by the structure of their velocity dispersion. The simulations reveal that this anisotropy correlates with the intrinsic morphology of the galaxy's inner dark matter halo, i.e. the halo's morphology that emerges in the absence of dissipative baryonic physics. This implies the existence of a causal relationship between the morphologies of galaxies and that of their host dark matter haloes., Comment: Accepted for publication in MNRAS. 16 pages and 8 figures. Morphological and kinematical diagnostics presented here have been added to the public EAGLE database at http://galaxy-catalogue.dur.ac.uk, and routines enabling their calculation are publicly available at http://github.com/athob/morphokinematics/

Published
2018
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15. Giant Outer Transiting Exoplanet Mass (GOT ’EM) Survey. III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-transit Jupiter Orbiting TOI-2010

Author

Mann, Christopher R., primary, Dalba, Paul A., additional, Lafrenière, David, additional, Fulton, Benjamin J., additional, Hébrard, Guillaume, additional, Boisse, Isabelle, additional, Dalal, Shweta, additional, Deleuil, Magali, additional, Delfosse, Xavier, additional, Demangeon, Olivier, additional, Forveille, Thierry, additional, Heidari, Neda, additional, Kiefer, Flavien, additional, Martioli, Eder, additional, Moutou, Claire, additional, Endl, Michael, additional, Cochran, William D., additional, MacQueen, Phillip, additional, Marchis, Franck, additional, Dragomir, Diana, additional, Gupta, Arvind F., additional, Feliz, Dax L., additional, Nicholson, Belinda A., additional, Ziegler, Carl, additional, Villanueva, Steven, additional, Rowe, Jason, additional, Talens, Geert Jan, additional, Thorngren, Daniel, additional, LaCourse, Daryll, additional, Jacobs, Tom, additional, Howard, Andrew W., additional, Bieryla, Allyson, additional, Latham, David W., additional, Rabus, Markus, additional, Fetherolf, Tara, additional, Hellier, Coel, additional, Howell, Steve B., additional, Plavchan, Peter, additional, Reefe, Michael, additional, Combs, Deven, additional, Bowen, Michael, additional, Wittrock, Justin, additional, Ricker, George R., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Barclay, Thomas, additional, Watanabe, David, additional, Collins, Karen A., additional, Eastman, Jason D., additional, and Ting, Eric B., additional

Published
2023
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16. The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope. I. Instrument Overview and In-flight Performance

Author

Doyon, René, primary, Willott, Chris J., additional, Hutchings, John B., additional, Sivaramakrishnan, Anand, additional, Albert, Loïc, additional, Lafrenière, David, additional, Rowlands, Neil, additional, Begoña Vila, M., additional, Martel, André R., additional, LaMassa, Stephanie, additional, Aldridge, David, additional, Artigau, Étienne, additional, Cameron, Peter, additional, Chayer, Pierre, additional, Cook, Neil J., additional, Cooper, Rachel A., additional, Darveau-Bernier, Antoine, additional, Dupuis, Jean, additional, Earnshaw, Colin, additional, Espinoza, Néstor, additional, Filippazzo, Joseph C., additional, Fullerton, Alexander W., additional, Gaudreau, Daniel, additional, Gawlik, Roman, additional, Goudfrooij, Paul, additional, Haley, Craig, additional, Kammerer, Jens, additional, Kendall, David, additional, Lambros, Scott D., additional, Ignat, Luminita Ilinca, additional, Maszkiewicz, Michael, additional, McColgan, Ashley, additional, Morishita, Takahiro, additional, Ouellette, Nathalie N.-Q., additional, Pacifici, Camilla, additional, Philippi, Natasha, additional, Radica, Michael, additional, Ravindranath, Swara, additional, Rowe, Jason, additional, Roy, Arpita, additional, Roy, Niladri, additional, Saad, Karl, additional, Sohn, Sangmo Tony, additional, Talens, Geert Jan, additional, Touahri, Driss, additional, Thatte, Deepashri, additional, Taylor, Joanna M., additional, Vandal, Thomas, additional, Volk, Kevin, additional, Wander, Michel, additional, Warner, Gerald, additional, Zheng, Sheng-Hai, additional, Zhou, Julia, additional, Abraham, Roberto, additional, Beaulieu, Mathilde, additional, Benneke, Björn, additional, Ferrarese, Laura, additional, Jayawardhana, Ray, additional, Johnstone, Doug, additional, Kaltenegger, Lisa, additional, Meyer, Michael R., additional, Pipher, Judy L., additional, Rameau, Julien, additional, Rieke, Marcia, additional, Salhi, Salma, additional, and Sawicki, Marcin, additional

Published
2023
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17. The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope. III. Single Object Slitless Spectroscopy

Author

Albert, Loïc, primary, Lafrenière, David, additional, René, Doyon,, additional, Artigau, Étienne, additional, Volk, Kevin, additional, Goudfrooij, Paul, additional, Martel, André R., additional, Radica, Michael, additional, Rowe, Jason, additional, Espinoza, Néstor, additional, Roy, Arpita, additional, Filippazzo, Joseph C., additional, Darveau-Bernier, Antoine, additional, Talens, Geert Jan, additional, Sivaramakrishnan, Anand, additional, Willott, Chris J., additional, Fullerton, Alexander W., additional, LaMassa, Stephanie, additional, Hutchings, John B., additional, Rowlands, Neil, additional, Vila, M. Begoña, additional, Zhou, Julia, additional, Aldridge, David, additional, Maszkiewicz, Michael, additional, Beaulieu, Mathilde, additional, Cook, Neil J., additional, Piaulet, Caroline, additional, Roy, Pierre-Alexis, additional, Lamontagne, Pierrot, additional, Morel, Kim, additional, Frost, William, additional, Salhi, Salma, additional, Coulombe, Louis-Philippe, additional, Benneke, Björn, additional, MacDonald, Ryan J., additional, Johnstone, Doug, additional, Turner, Jake D., additional, Fournier-Tondreau, Marylou, additional, Allart, Romain, additional, and Kaltenegger, Lisa, additional

Published
2023
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18. APPLESOSS: A Producer of ProfiLEs for SOSS. Application to the NIRISS SOSS Mode

Author

Radica, Michael, primary, Albert, Loïc, additional, Taylor, Jake, additional, Lafrenière, David, additional, Coulombe, Louis-Philippe, additional, Darveau-Bernier, Antoine, additional, Doyon, René, additional, Cook, Neil, additional, Cowan, Nicolas, additional, Espinoza, Néstor, additional, Johnstone, Doug, additional, Kaltenegger, Lisa, additional, Piaulet, Caroline, additional, Roy, Arpita, additional, and Talens, Geert Jan, additional

Published
2022
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19. ATOCA: an Algorithm to Treat Order Contamination. Application to the NIRISS SOSS Mode

Author

Darveau-Bernier, Antoine, primary, Albert, Loïc, additional, Talens, Geert Jan, additional, Lafrenière, David, additional, Radica, Michael, additional, Doyon, René, additional, Cook, Neil J., additional, Rowe, Jason F., additional, Allart, Romain, additional, Artigau, Étienne, additional, Benneke, Björn, additional, Cowan, Nicolas, additional, Dang, Lisa, additional, Espinoza, Néstor, additional, Johnstone, Doug, additional, Kaltenegger, Lisa, additional, Lim, Olivia, additional, Pauly, Tyler, additional, Pelletier, Stefan, additional, Piaulet, Caroline, additional, Roy, Arpita, additional, Roy, Pierre-Alexis, additional, Splinter, Jared, additional, Taylor, Jake, additional, and Turner, Jake D., additional

Published
2022
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20. Exoplanet instrumentation in the 2020s: Canada's pathway towards searching for life on potentially Earth-like exoplanets

Author

Benneke, Bjorn, Cowan, Nick, Rowe, Jason, Marois, Christian, Metchev, Stanimir, Moores, John, Lee, Eve, Boley, Aaron, Doyon, Rene, Cumming, Andrew, Matthews, Jaymie, Lafreniere, David, Strong, Kimberly, Gladman, Brett, Menou, Kristen, Valencia, Diana, Mawet, Dimitri, Cook, Neil James, Ngo, Henry, Artigau, UdeM, Albert, Loic, Godin, Paul, Chauhan, Akash, Darveau-Bernier, Antoine, Lee, Junchan, Pelletier, Stefan, Coulombe, Louis-Phillippe, Miles-Paez, Paulo, Marquette, Melissa, Bell, Taylor, Radica, Michael, Gerard, Benjamin L., Ouelette, Nathalie, Dang, Lisa, Naud, Marie-Eve, Moore, Kevin, Lim, Olivia, Wu, Yanqin, Gupta, Prashansa, Bastien, Pierre, Malo, Lison, Gagne, Jonathan, Beauvais, Simon-Gabriel, Cloutier, Ryan, Cadieux, Charles, Talens, Geert Jan, Herman, Miranda, Mann, Christopher, Piaulet, Caroline, Weiss, Lauren, Chan, Jonathan, Speedie, Jessica, Hedgepeth, Josh, Ali-Dib, Mohamad, Ellery, Alex, Lee, Christopher, Thorngren, Daniel, Navarro, Thomas, Nguyen, Giang, Keating, Dylan, and Hallatt, Tim

Subjects
astrophysics
Abstract

The next decade presents a unique moment in the history of planetary astronomy. For the first time, we have the technologies at hand to discover and characterize a wide range of exoplanetary systems, possibly harboring true Earth analogues. The opportunity is no less than answering humanity’s millennia old questions of “Are we alone?” and “How did we get here?”. The best part: Canada can play a leading role in this historic endeavor, if we make deliberate strategic investments over the next decade. In this white paper, we lay out pathways to develop the necessary instrumentation in collaboration with national and international partners to address the most fundamental questions regarding the formation of planets, the diversity of planetary systems, and the frequency of life in the universe. We recommend critical investments in a portfolio of assets including high-dispersion coronagraphy instrumentation for the upcoming ground based 30-meter class telescopes, a strong (JWST-scale) Canadian involvement in the next generation space missions LUVOIR or HabEx, and support for small and large space missions led by Canada. Importantly, while the science case of searching for biomarkers on rocky exoplanets presents the most stringent design requirements, the proposed instrumentation will also be ideal for the characterization of giant exoplanets, sub-Neptunes, and super-Earths and address a wide range of science questions in the coming decade., White paper identifier W065

Published
2019
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21. Gravity-darkening Analysis of the Misaligned Hot Jupiter MASCARA-4 b

Author

Ahlers, John P., primary, Kruse, Ethan, additional, Colón, Knicole D., additional, Dorval, Patrick, additional, Talens, Geert Jan, additional, Snellen, Ignas, additional, Albrecht, Simon, additional, Otten, Gilles, additional, Ricker, George, additional, Vanderspek, Roland, additional, Latham, David, additional, Seager, Sara, additional, Winn, Joshua, additional, Jenkins, Jon M., additional, Haworth, Kari, additional, Cartwright, Scott, additional, Morris, Robert, additional, Rowden, Pam, additional, Tenenbaum, Peter, additional, and Ting, Eric B., additional

Published
2020
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22. An unusually large gaseous transit in a debris disc

Author

Iglesias, Daniela P, primary, Olofsson, Johan, additional, Bayo, Amelia, additional, Zieba, Sebastian, additional, Montesinos, Matías, additional, Smoker, Jonathan, additional, Kennedy, Grant M, additional, Godoy, Nicolás, additional, Pantoja, Blake, additional, Talens, Geert Jan, additional, Wahhaj, Zahed, additional, and Zamora, Catalina, additional

Published
2019
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23. Bright Southern Variable Stars in the bRing Survey

Author

Mellon, Samuel N., primary, Mamajek, Eric E., additional, Stuik, Remko, additional, Zwintz, Konstanze, additional, Kenworthy, Matthew A., additional, J. Talens, Geert Jan, additional, Burggraaff, Olivier, additional, Bailey, III, John I., additional, Dorval, Patrick, additional, Lomberg, Blaine B. D., additional, Kuhn, Rudi B., additional, and Ireland, Michael J., additional

Published
2019
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25. Discovery of δ Scuti Pulsations in the Young Hybrid Debris Disk Star HD 156623

Author

Mellon, Samuel N., primary, Mamajek, Eric E., additional, Zwintz, Konstanze, additional, David, Trevor J., additional, Stuik, Remko, additional, J. Talens, Geert Jan, additional, Dorval, Patrick, additional, Burggraaff, Olivier, additional, Kenworthy, Matthew A., additional, Bailey, III, John I., additional, Lomberg, Blaine B. D., additional, Kuhn, Rudi B., additional, Ireland, Michael J., additional, and Crawford, Steven M., additional

Published
2019
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