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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. A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

Author: Espinoza, Néstor, Pallé, Enric, Kemmer, Jonas, Luque, Rafael, Caballero, José A., Cifuentes, Carlos, Herrero, Enrique, Béjar, Víctor J. Sánchez, Stock, Stephan, Molaverdikhani, Karan, Morello, Giuseppe, Kossakowski, Diana, Schlecker, Martin, Amado, Pedro J., Bluhm, Paz, Cortés-Contreras, Miriam, Henning, Thomas, Kreidberg, Laura, Kürster, Martin, Lafarga, Marina, Lodieu, Nicolas, Morales, Juan Carlos, Oshagh, Mahmoudreza, Passegger, Vera M., Pavlov, Alexey, Quirrenbach, Andreas, Reffert, Sabine, Reiners, Ansgar, Ribas, Ignasi, Rodríguez, Eloy, López, Cristina Rodríguez, Schweitzer, Andreas, Trifonov, Trifon, Chaturvedi, Priyanka, Dreizler, Stefan, Jeffers, Sandra V., Kaminski, Adrian, López-González, María José, Lillo-Box, Jorge, Montes, David, Nowak, Grzegorz, Pedraz, Santos, Vanaverbeke, Siegfried, Osorio, Maria R. Zapatero, Zechmeister, Mathias, Collins, Karen A., Girardin, Eric, Guerra, Pere, Naves, Ramon, Crossfield, Ian J. M., Matthews, Elisabeth C., Howell, Steve B., Ciardi, David R., Gonzales, Erica, Matson, Rachel A., Beichman, Charles A., Schlieder, Joshua E., Barclay, Thomas, Vezie, Michael, Villaseñor, Jesus Noel, Daylan, Tansu, Mireies, Ismael, Dragomir, Diana, Twicken, Joseph D., Jenkins, Jon, Winn, Joshua N., Latham, David, Ricker, George, and Seager, Sara
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery and characterization of TOI-1759~b, a temperate (400 K) sub-Neptune-sized exoplanet orbiting the M~dwarf TOI-1759 (TIC 408636441). TOI-1759 b was observed by TESS to transit on sectors 16, 17 and 24, with only one transit observed per sector, creating an ambiguity on the orbital period of the planet candidate. Ground-based photometric observations, combined with radial-velocity measurements obtained with the CARMENES spectrograph, confirm an actual period of $18.85019 \pm 0.00014$ d. A joint analysis of all available photometry and radial velocities reveal a radius of $3.17 \pm 0.10\,R_\oplus$ and a mass of $10.8 \pm 1.5\,M_\oplus$. Combining this with the stellar properties derived for TOI-1759 ($R_\star = 0.597 \pm 0.015\,R_\odot$; $M_\star = 0.606 \pm 0.020\,M_\odot$; $T_{\textrm{eff}} = 4065 \pm 51$ K), we compute a transmission spectroscopic metric (TSM) value of over 80 for the planet, making it a good target for transmission spectroscopy studies. TOI-1759 b is among the top five temperate, small exoplanets ($T_\textrm{eq} < 500$ K, $R_p < 4 \,R_\oplus$) with the highest TSM discovered to date. Two additional signals with periods of 80 d and $>$ 200 d seem to be present in our radial velocities. While our data suggest both could arise from stellar activity, the later signal's source and periodicity are hard to pinpoint given the $\sim 200$ d baseline of our radial-velocity campaign with CARMENES. Longer baseline radial-velocity campaigns should be performed in order to unveil the true nature of this long period signal., Comment: 22 pages, 10 figures, 7 tables. AJ in press
Published: 2022
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3. The Effect of Stellar Contamination on Low-resolution Transmission Spectroscopy: Needs Identified by NASA's Exoplanet Exploration Program Study Analysis Group 21

Author: Rackham, Benjamin V., Espinoza, Néstor, Berdyugina, Svetlana V., Korhonen, Heidi, MacDonald, Ryan J., Montet, Benjamin T., Morris, Brett M., Oshagh, Mahmoudreza, Shapiro, Alexander I., Unruh, Yvonne C., Quintana, Elisa V., Zellem, Robert T., Apai, Dániel, Barclay, Thomas, Barstow, Joanna K., Bruno, Giovanni, Carone, Ludmila, Casewell, Sarah L., Cegla, Heather M., Criscuoli, Serena, Fischer, Catherine, Fournier, Damien, Giampapa, Mark S., Giles, Helen, Iyer, Aishwarya, Kopp, Greg, Kostogryz, Nadiia M., Krivova, Natalie, Mallonn, Matthias, McGruder, Chima, Molaverdikhani, Karan, Newton, Elisabeth R., Panja, Mayukh, Peacock, Sarah, Reardon, Kevin, Roettenbacher, Rachael M., Scandariato, Gaetano, Solanki, Sami, Stassun, Keivan G., Steiner, Oskar, Stevenson, Kevin B., Tregloan-Reed, Jeremy, Valio, Adriana, Wedemeyer, Sven, Welbanks, Luis, Yu, Jie, Alam, Munazza K., Davenport, James R. A., Deming, Drake, Dong, Chuanfei, Ducrot, Elsa, Fisher, Chloe, Gilbert, Emily, Kostov, Veselin, López-Morales, Mercedes, Line, Mike, Močnik, Teo, Mullally, Susan, Paudel, Rishi R., Ribas, Ignasi, and Valenti, Jeff A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Study Analysis Group 21 (SAG21) of NASA's Exoplanet Exploration Program Analysis Group (ExoPAG) was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, plages, granules, and flares. This SAG brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current research needs that can be addressed in this context to make the most of transit studies from current NASA facilities like HST and JWST. The analysis produced 14 findings, which fall into three Science Themes encompassing (1) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities ("The Sun as the Stellar Benchmark"), (2) how stars other than the Sun extend our knowledge of heterogeneities ("Surface Heterogeneities of Other Stars") and (3) how to incorporate information gathered for the Sun and other stars into transit studies ("Mapping Stellar Knowledge to Transit Studies"). In this invited review, we largely reproduce the final report of SAG21 as a contribution to the peer-reviewed literature., Comment: Invited review in press at RASTI. Based on the ExoPAG SAG21 report (arXiv:2201.09905v1) and refined via feedback from three reviewers. 75 pages, 30 figures, 5 tables
Published: 2022

4. TOI-2285b: A 1.7 Earth-radius Planet Near the Habitable Zone around a Nearby M Dwarf

Author: Fukui, Akihiko, Kimura, Tadahiro, Hirano, Teruyuki, Narita, Norio, Kodama, Takanori, Hori, Yasunori, Ikoma, Masahiro, Pallé, Enric, Murgas, Felipe, Parviainen, Hannu, Kawauchi, Kiyoe, Mori, Mayuko, Esparza-Borges, Emma, Bieryla, Allyson, Irwin, Jonathan, Safonov, Boris S., Stassun, Keivan G., Alvarez-Hernandez, Leticia, Béjar, Víctor J. S., Casasayas-Barris, Núria, Chen, Guo, Crouzet, Nicolas, de Leon, Jerome P., Isogai, Keisuke, Kagetani, Taiki, Klagyivik, Peter, Korth, Judith, Kurita, Seiya, Kusakabe, Nobuhiko, Livingston, John, Luque, Rafael, Madrigal-Aguado, Alberto, Morello, Giuseppe, Nishiumi, Taku, Orell-Miquel, Jaume, Oshagh, Mahmoudreza, Sánchez-Benavente, Manuel, Stangret, Monika, Terada, Yuka, Watanabe, Noriharu, Zou, Yujie, Tamura, Motohide, Kurokawa, Takashi, Kuzuhara, Masayuki, Nishikawa, Jun, Omiya, Masashi, Vievard, Sébastien, Ueda, Akitoshi, Latham, David W., Quinn, Samuel N., Strakhov, Ivan S., Belinski, Alexandr A., Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua N., Charbonneau, David, Ciardi, David R., Collins, Karen A., Doty, John P., Bachelet, Etienne, and Harbeck, Daniel
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of TOI-2285b, a sub-Neptune-sized planet transiting a nearby (42 pc) M dwarf with a period of 27.3 days. We identified the transit signal from the Transiting Exoplanet Survey Satellite photometric data, which we confirmed with ground-based photometric observations using the multiband imagers MuSCAT2 and MuSCAT3. Combining these data with other follow-up observations including high resolution spectroscopy with the Tillinghast Reflector Echelle Spectrograph, high resolution imaging with the SPeckle Polarimeter, and radial velocity (RV) measurements with the InfraRed Doppler instrument, we find that the planet has a radius of 1.74 $\pm$ 0.08 $R_\oplus$, a mass of $<$ 19.5 $M_\oplus$ (95\% c.l.), and an insolation flux of 1.54 $\pm$ 0.14 times that of the Earth. Although the planet resides just outside the habitable zone for a rocky planet, if the planet harbors an H$_2$O layer under a hydrogen-rich atmosphere, then liquid water could exist on the surface of the H$_2$O layer depending on the planetary mass and water mass fraction. The bright host star in the near infrared ($K_s=9.0$) makes this planet an excellent target for further RV and atmospheric observations to improve our understanding on the composition, formation, and habitability of sub-Neptune-sized planets., Comment: 9 pages, 3 figures, published online in PASJ
Published: 2021
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5. Giant white-light flares on fully convective stars occur at high latitudes

Author: Ilin, Ekaterina, Poppenhaeger, Katja, Schmidt, Sarah J., Järvinen, Silva P., Newton, Elisabeth R., Alvarado-Gómez, Julián D., Pineda, J. Sebastian, Davenport, James R. A., Oshagh, Mahmoudreza, and Ilyin, Ilya
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: White-light flares are magnetically driven localized brightenings on the surfaces of stars. Their temporal, spectral, and statistical properties present a treasury of physical information about stellar magnetic fields. The spatial distributions of magnetic spots and associated flaring regions help constrain dynamo theories. Moreover, flares are thought to crucially affect the habitability of exoplanets that orbit these stars. Measuring the location of flares on stars other than the Sun is challenging due to the lack of spatial resolution. Here we present four fully convective stars observed with the Transiting Exoplanet Survey Satellite (TESS) that displayed large, long-duration flares in white-light which were modulated in brightness by the stars' fast rotation. This allowed us to determine the loci of these flares directly from the light curves. All four flares occurred at latitudes between 55 deg and 81 deg, far higher than typical solar flare latitudes. Our findings are evidence that strong magnetic fields tend to emerge close to the stellar rotational poles for fully convective stars, and suggest that the impact of flares on the habitability of exoplanets around small stars could be weaker than previously thought., Comment: 23 pages, 18 figures, accepted to MNRAS, see conference poster https://doi.org/10.5281/zenodo.4558791 for short summary
Published: 2021
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6. Transit detection of the long-period volatile-rich super-Earth $\nu^2$ Lupi d with $CHEOPS$

Author: Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Escudé, Guillem Anglada, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Cameron, Andrew Collier, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Muñoz, Antonio Garcia, Gillon, Michaël, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Etangs, Alain Lecavelier des, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, and Walton, Nicholas A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Exoplanets transiting bright nearby stars are key objects for advancing our knowledge of planetary formation and evolution. The wealth of photons from the host star gives detailed access to the atmospheric, interior, and orbital properties of the planetary companions. $\nu^2$ Lupi (HD 136352) is a naked-eye ($V = 5.78$) Sun-like star that was discovered to host three low-mass planets with orbital periods of 11.6, 27.6, and 107.6 days via radial velocity monitoring (Udry et al. 2019). The two inner planets (b and c) were recently found to transit (Kane et al. 2020), prompting a photometric follow-up by the brand-new $CHaracterising\:ExOPlanets\:Satellite\:(CHEOPS)$. Here, we report that the outer planet d is also transiting, and measure its radius and mass to be $2.56\pm0.09$ $R_{\oplus}$ and $8.82\pm0.94$ $M_{\oplus}$, respectively. With its bright Sun-like star, long period, and mild irradiation ($\sim$5.7 times the irradiation of Earth), $\nu^2$ Lupi d unlocks a completely new region in the parameter space of exoplanets amenable to detailed characterization. We refine the properties of all three planets: planet b likely has a rocky mostly dry composition, while planets c and d seem to have retained small hydrogen-helium envelopes and a possibly large water fraction. This diversity of planetary compositions makes the $\nu^2$ Lupi system an excellent laboratory for testing formation and evolution models of low-mass planets., Comment: Published in Nature Astronomy. 60 pages, 18 Figures, 6 Tables. This is the authors' version of the manuscript. The final authenticated version is available online at https://www.nature.com/articles/s41550-021-01381-5
Published: 2021
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7. A compositional link between rocky exoplanets and their host stars

Author: Adibekyan, Vardan, Dorn, Caroline, Sousa, Sérgio G., Santos, Nuno C., Bitsch, Bertram, Israelian, Garik, Mordasini, Christoph, Barros, Susana C. C., Mena, Elisa Delgado, Demangeon, Olivier D. S., Faria, João P., Figueira, Pedro, Hakobyan, Artur A., Oshagh, Mahmoudreza, Soares, Barbara M. T. B., Kunitomo, Masanobu, Takeda, Yoichi, Jofré, Emiliano, Petrucci, Romina, and Martioli, Eder
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Stars and planets both form by accreting material from a surrounding disk. Because they grow from the same material, theory predicts that there should be a relationship between their compositions. In this study, we search for a compositional link between rocky exoplanets and their host stars. We estimate the iron-mass fraction of rocky exoplanets from their masses and radii and compare it with the compositions of their host stars, which we assume reflect the compositions of the protoplanetary disks. We find a correlation (but not a 1:1 relationship) between these two quantities, with a slope of >4, which we interpret as being attributable to planet formation processes. Super-Earths and super-Mercuries appear to be distinct populations with differing compositions, implying differences in their formation processes., Comment: Authors' version of the manuscript. Published in Science
Published: 2021
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8. A new orbital ephemeris for WASP-128b

Author: Smith, Alexis M. S., Eigmüller, Philipp, Oshagh, Mahmoudreza, and Southworth, John
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: WASP-128 is a relatively bright (V= 12.37) G0-dwarf, known to host a transiting brown dwarf in a short-period orbit (Hod\v{z}i\'c et al. 2018 arXiv:1807.07557 (H18)). Very few such objects are known, which makes WASP-128 a prime target for further observations to better understand giant planet / brown dwarf properties,including formation and migration histories. To facilitate the planning of future observations of WASP-128b, we improve the orbital ephemeris of the system, by using the seven transits of WASP-128 observed by TESS. We note that our orbital period differs significantly from that of H18: it is more than $14\,\sigma$ (using their uncertainty) larger. This results in our ephemeris predicting a mid-2020 transit to occur almost eight hours later than the H18 ephemeris. We find, however, no evidence for any period variation., Comment: Published in Research Notes of the American Astronomical Society (RNAAS)
Published: 2020
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9. The Detailed Science Case for the Maunakea Spectroscopic Explorer, 2019 edition

Author: The MSE Science Team, Babusiaux, Carine, Bergemann, Maria, Burgasser, Adam, Ellison, Sara, Haggard, Daryl, Huber, Daniel, Kaplinghat, Manoj, Li, Ting, Marshall, Jennifer, Martell, Sarah, McConnachie, Alan, Percival, Will, Robotham, Aaron, Shen, Yue, Thirupathi, Sivarani, Tran, Kim-Vy, Yeche, Christophe, Yong, David, Adibekyan, Vardan, Aguirre, Victor Silva, Angelou, George, Asplund, Martin, Balogh, Michael, Banerjee, Projjwal, Bannister, Michele, Barría, Daniela, Battaglia, Giuseppina, Bayo, Amelia, Bechtol, Keith, Beck, Paul G., Beers, Timothy C., Bellinger, Earl P., Berg, Trystyn, Bestenlehner, Joachim M., Bilicki, Maciej, Bitsch, Bertram, Bland-Hawthorn, Joss, Bolton, Adam S., Boselli, Alessandro, Bovy, Jo, Bragaglia, Angela, Buzasi, Derek, Caffau, Elisabetta, Cami, Jan, Carleton, Timothy, Casagrande, Luca, Cassisi, Santi, Catelan, Márcio, Chang, Chihway, Cortese, Luca, Damjanov, Ivana, Davies, Luke J. M., de Grijs, Richard, de Rosa, Gisella, Deason, Alis, di Matteo, Paola, Drlica-Wagner, Alex, Erkal, Denis, Escorza, Ana, Ferrarese, Laura, Fleming, Scott W., Font-Ribera, Andreu, Freeman, Ken, Gänsicke, Boris T., Gabdeev, Maksim, Gallagher, Sarah, Gandolfi, Davide, García, Rafael A., Gaulme, Patrick, Geha, Marla, Gennaro, Mario, Gieles, Mark, Gilbert, Karoline, Gordon, Yjan, Goswami, Aruna, Greco, Johnny P., Grillmair, Carl, Guiglion, Guillaume, Hénault-Brunet, Vincent, Hall, Patrick, Handler, Gerald, Hansen, Terese, Hathi, Nimish, Hatzidimitriou, Despina, Haywood, Misha, Santisteban, Juan V. Hernández, Hillenbrand, Lynne, Hopkins, Andrew M., Howlett, Cullan, Hudson, Michael J., Ibata, Rodrigo, Ilić, Dragana, Jablonka, Pascale, Ji, Alexander, Jiang, Linhua, Juneau, Stephanie, Karakas, Amanda, Karinkuzhi, Drisya, Kim, Stacy Y., Kong, Xu, Konstantopoulos, Iraklis, Krogager, Jens-Kristian, Lagos, Claudia, Lallement, Rosine, Laporte, Chervin, Lebreton, Yveline, Lee, Khee-Gan, Lewis, Geraint F., Lianou, Sophia, Liu, Xin, Lodieu, Nicolas, Loveday, Jon, Mészáros, Szabolcs, Makler, Martin, Mao, Yao-Yuan, Marchesini, Danilo, Martin, Nicolas, Mateo, Mario, Melis, Carl, Merle, Thibault, Miglio, Andrea, Mohammad, Faizan Gohar, Molaverdikhani, Karan, Monier, Richard, Morel, Thierry, Mosser, Benoit, Nataf, David, Necib, Lina, Neilson, Hilding R., Newman, Jeffrey A., Nierenberg, A. M., Nord, Brian, Noterdaeme, Pasquier, O'Dea, Chris, Oshagh, Mahmoudreza, Pace, Andrew B., Palanque-Delabrouille, Nathalie, Pandey, Gajendra, Parker, Laura C., Pawlowski, Marcel S., Peter, Annika H. G., Petitjean, Patrick, Petric, Andreea, Placco, Vinicius, Popović, Luka Č., Price-Whelan, Adrian M., Prsa, Andrej, Ravindranath, Swara, Rich, R. Michael, Ruan, John, Rybizki, Jan, Sakari, Charli, Sanderson, Robyn E., Schiavon, Ricardo, Schimd, Carlo, Serenelli, Aldo, Siebert, Arnaud, Siudek, Malgorzata, Smiljanic, Rodolfo, Smith, Daniel, Sobeck, Jennifer, Starkenburg, Else, Stello, Dennis, Szabó, Gyula M., Szabo, Robert, Taylor, Matthew A., Thanjavur, Karun, Thomas, Guillaume, Tollerud, Erik, Toonen, Silvia, Tremblay, Pier-Emmanuel, Tresse, Laurence, Tsantaki, Maria, Valentini, Marica, Van Eck, Sophie, Variu, Andrei, Venn, Kim, Villaver, Eva, Walker, Matthew G., Wang, Yiping, Wang, Yuting, Wilson, Michael J., Wright, Nicolas, Xu, Siyi, Yildiz, Mutlu, Zhang, Huawei, Zwintz, Konstanze, Anguiano, Borja, Bedell, Megan, Chaplin, William, Collet, Remo, Cuillandre, Jean-Charles, Duc, Pierre-Alain, Flagey, Nicolas, Hermes, JJ, Hill, Alexis, Kamath, Devika, Laychak, Mary Beth, Małek, Katarzyna, Marley, Mark, Sheinis, Andy, Simons, Doug, Sousa, Sérgio G., Szeto, Kei, Ting, Yuan-Sen, Vegetti, Simona, Wells, Lisa, Babas, Ferdinand, Bauman, Steve, Bosselli, Alessandro, Côté, Pat, Colless, Matthew, Comparat, Johan, Courtois, Helene, Crampton, David, Croom, Scott, Davies, Luke, Denny, Kelly, Devost, Daniel, Driver, Simon, Fernandez-Lorenzo, Mirian, Guhathakurta, Raja, Han, Zhanwen, Higgs, Clare, Hill, Vanessa, Ho, Kevin, Hopkins, Andrew, Hudson, Mike, Isani, Sidik, Jarvis, Matt, Johnson, Andrew, Jullo, Eric, Kaiser, Nick, Kneib, Jean-Paul, Koda, Jun, Koshy, George, Mignot, Shan, Murowinski, Rick, Newman, Jeff, Nusser, Adi, Pancoast, Anna, Peng, Eric, Peroux, Celine, Pichon, Christophe, Poggianti, Bianca, Richard, Johan, Salmon, Derrick, Seibert, Arnaud, Shastri, Prajval, Smith, Dan, Sutaria, Firoza, Tao, Charling, Taylor, Edwar, Tully, Brent, van Waerbeke, Ludovic, Vermeulen, Tom, Walker, Matthew, Willis, Jon, Willot, Chris, and Withington, Kanoa
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: (Abridged) The Maunakea Spectroscopic Explorer (MSE) is an end-to-end science platform for the design, execution and scientific exploitation of spectroscopic surveys. It will unveil the composition and dynamics of the faint Universe and impact nearly every field of astrophysics across all spatial scales, from individual stars to the largest scale structures in the Universe. Major pillars in the science program for MSE include (i) the ultimate Gaia follow-up facility for understanding the chemistry and dynamics of the distant Milky Way, including the outer disk and faint stellar halo at high spectral resolution (ii) galaxy formation and evolution at cosmic noon, via the type of revolutionary surveys that have occurred in the nearby Universe, but now conducted at the peak of the star formation history of the Universe (iii) derivation of the mass of the neutrino and insights into inflationary physics through a cosmological redshift survey that probes a large volume of the Universe with a high galaxy density. MSE is positioned to become a critical hub in the emerging international network of front-line astronomical facilities, with scientific capabilities that naturally complement and extend the scientific power of Gaia, the Large Synoptic Survey Telescope, the Square Kilometer Array, Euclid, WFIRST, the 30m telescopes and many more., Comment: 9 chapters, 301 pages, 100 figures. This version of the DSC is a comprehensive update of the original version, released in 2016, which can be downloaded at arXiv:1606.00043. A detailed summary of the design of MSE is available in the MSE Book 2018, available at arXiv:1810.08695
Published: 2019

10. Stellar Astrophysics and Exoplanet Science with the Maunakea Spectroscopic Explorer (MSE)

Author: Bergemann, Maria, Huber, Daniel, Adibekyan, Vardan, Angelou, George, Barría, Daniela, Beers, Timothy C., Beck, Paul G., Bellinger, Earl P., Bestenlehner, Joachim M., Bitsch, Bertram, Burgasser, Adam, Buzasi, Derek, Cassisi, Santi, Catelan, Márcio, Escorza, Ana, Fleming, Scott W., Gänsicke, Boris T., Gandolfi, Davide, García, Rafael A., Gieles, Mark, Karakas, Amanda, Lebreton, Yveline, Lodieu, Nicolas, Melis, Carl, Merle, Thibault, Mészáros, Szabolcs, Miglio, Andrea, Molaverdikhani, Karan, Monier, Richard, Morel, Thierry, Neilson, Hilding R., Oshagh, Mahmoudreza, Rybizki, Jan, Serenelli, Aldo, Smiljanic, Rodolfo, Szabó, Gyula M., Toonen, Silvia, Tremblay, Pier-Emmanuel, Valentini, Marica, Van Eck, Sophie, Zwintz, Konstanze, Bayo, Amelia, Cami, Jan, Casagrande, Luca, Gabdeev, Maksim, Gaulme, Patrick, Guiglion, Guillaume, Handler, Gerald, Hillenbrand, Lynne, Yildiz, Mutlu, Marley, Mark, Mosser, Benoit, Price-Whelan, Adrian M., Prsa, Andrej, Santisteban, Juan V. Hernández, Aguirre, Victor Silva, Sobeck, Jennifer, Stello, Dennis, Szabo, Robert, Tsantaki, Maria, Villaver, Eva, Wright, Nicholas J., Xu, Siyi, Zhang, Huawei, Anguiano, Borja, Bedell, Megan, Chaplin, Bill, Collet, Remo, Kamath, Devika, Martell, Sarah, Sousa, Sérgio G., Ting, Yuan-Sen, and Venn, Kim
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Maunakea Spectroscopic Explorer (MSE) is a planned 11.25-m aperture facility with a 1.5 square degree field of view that will be fully dedicated to multi-object spectroscopy. A rebirth of the 3.6m Canada-France-Hawaii Telescope on Maunakea, MSE will use 4332 fibers operating at three different resolving powers (R ~ 2500, 6000, 40000) across a wavelength range of 0.36-1.8mum, with dynamical fiber positioning that allows fibers to match the exposure times of individual objects. MSE will enable spectroscopic surveys with unprecedented scale and sensitivity by collecting millions of spectra per year down to limiting magnitudes of g ~ 20-24 mag, with a nominal velocity precision of ~100 m/s in high-resolution mode. This white paper describes science cases for stellar astrophysics and exoplanet science using MSE, including the discovery and atmospheric characterization of exoplanets and substellar objects, stellar physics with star clusters, asteroseismology of solar-like oscillators and opacity-driven pulsators, studies of stellar rotation, activity, and multiplicity, as well as the chemical characterization of AGB and extremely metal-poor stars., Comment: 31 pages, 11 figures; To appear as a chapter for the Detailed Science Case of the Maunakea Spectroscopic Explorer
Published: 2019

11. Detection of titanium oxide in the atmosphere of a hot Jupiter

Author: Sedaghati, Elyar, Boffin, Henri M. J., MacDonald, Ryan J., Gandhi, Siddharth, Madhusudhan, Nikku, Gibson, Neale P., Oshagh, Mahmoudreza, Claret, Antonio, and Rauer, Heike
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: As an exoplanet transits its host star, some of the light from the star is absorbed by the atoms and molecules in the planet's atmosphere, causing the planet to seem bigger; plotting the planet's observed size as a function of the wavelength of the light produces a transmission spectrum. Measuring the tiny variations in the transmission spectrum, together with atmospheric modelling, then gives clues to the properties of the exoplanet's atmosphere. Chemical species composed of light elements$-$such as hydrogen, oxygen, carbon, sodium and potassium$-$have in this way been detected in the atmospheres of several hot giant exoplanets, but molecules composed of heavier elements have thus far proved elusive. Nonetheless, it has been predicted that metal oxides such as titanium oxide (TiO) and vanadium oxide occur in the observable regions of the very hottest exoplanetary atmospheres, causing thermal inversions on the dayside. Here we report the detection of TiO in the atmosphere of the hot-Jupiter planet WASP-19b. Our combined spectrum, with its wide spectral coverage, reveals the presence of TiO (to a confidence level of 7.7{\sigma}), a strongly scattering haze (7.4{\sigma}) and sodium (3.4{\sigma}), and confirms the presence of water (7.9{\sigma}) in the atmosphere., Comment: Main article: 9 pages, 3 figures. Methods: 21 pages, 7 extended data figures, 3 extended data tables. Published in Nature
Published: 2017
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12. Noise Sources in Photometry and Radial Velocities

Author: Oshagh, Mahmoudreza, Campante, Tiago L., editor, Santos, Nuno C., editor, and Monteiro, Mário J. P. F. G., editor
Published: 2018
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13. New analytical expressions of the Rossiter-McLaughlin effect adapted to different observation techniques

Author: Boué, Gwenaël, Montalto, Marco, Boisse, Isabelle, Oshagh, Mahmoudreza, and Santos, Nuno C.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The Rossiter-McLaughlin (hereafter RM) effect is a key tool for measuring the projected spin-orbit angle between stellar spin axes and orbits of transiting planets. However, the measured radial velocity (RV) anomalies produced by this effect are not intrinsic and depend on both instrumental resolution and data reduction routines. Using inappropriate formulas to model the RM effect introduces biases, at least in the projected velocity Vsin(i) compared to the spectroscopic value. Currently, only the iodine cell technique has been modeled, which corresponds to observations done by, e.g., the HIRES spectrograph of the Keck telescope. In this paper, we provide a simple expression of the RM effect specially designed to model observations done by the Gaussian fit of a cross-correlation function (CCF) as in the routines performed by the HARPS team. We derived also a new analytical formulation of the RV anomaly associated to the iodine cell technique. For both formulas, we modeled the subplanet mean velocity v_p and dispersion beta_p accurately taking the rotational broadening on the subplanet profile into account. We compare our formulas adapted to the CCF technique with simulated data generated with the numerical software SOAP-T and find good agreement up to Vsin(i) < 20 km/s. In contrast, the analytical models simulating the two different observation techniques can disagree by about 10 sigma in Vsin(i) for large spin-orbit misalignments. It is thus important to apply the adapted model when fitting data., Comment: 16 pages, 11, figures, accepted in Astronomy and Astrophysics. Public code available at http://www.astro.up.pt/resources/arome
Published: 2012
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14. Degeneracy in the characterization of non-transiting planets from transit timing variations

Author: Boué, Gwenaël, Oshagh, Mahmoudreza, Montalto, Marco, and Santos, Nuno C.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The transit timing variation (TTV) method allows the detection of non-transiting planets through their gravitational perturbations. Since TTVs are strongly enhanced in systems close to mean-motion resonances (MMR), even a low mass planet can produce an observable signal. This technique has thus been proposed to detect terrestrial planets. In this letter, we analyse TTV signals for systems in or close to MMR in order to illustrate the difficulties arising in the determination of planetary parameters. TTVs are computed numerically with an n-body integrator for a variety of systems close to MMR. The main features of these TTVs are also derived analytically. Systems deeply inside MMR do not produce particularly strong TTVs, while those close to MMR generate quasiperiodic TTVs characterised by a dominant long period term and a low amplitude remainder. If the remainder is too weak to be detected, then the signal is strongly degenerate and this prevents the determination of the planetary parameters. Even though an Earth mass planet can be detected by the TTV method if it is close to a MMR, it may not be possible to assert that this planet is actually an Earth mass planet. On the other hand, if the system is right in the center of a MMR, the high amplitude oscillation of the TTV signal vanishes and the detection of the perturber becomes as difficult as it is far from MMR., Comment: 5 pages, 3 figures, submitted to MNRAS
Published: 2012
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15. A Survey of M Stars in the Field of View of Kepler Space Telescope

Author: Oshagh, Mahmoudreza, Haghighipour, Nader, and Santos, Nuno C.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: M dwarfs constitute more than 70% of the stars in the solar neighborhood. They are cooler and smaller than Sun-like stars and have less-massive disks which suggests that planets around these stars are more likely to be Neptune-size or smaller. The transit depths and transit times of planets around M stars are large and well-matched to the Kepler temporal resolution. As a result, M stars have been of particular interest for searching for planets in both radial velocity and transit photometry surveys. We have recently started a project on searching for possible planet-hosting M stars in the publicly available data from Kepler space telescope. We have used four criteria, namely, the magnitude, proper motion, H-Ks and J-H colors, and searched for M stars in Q0 and Q1 data sets. We have been able to find 108 M stars among which 54 had not been previously identified among Kepler's targets. We discuss the details of our selection process and present the results., Comment: 2 pages, 1 table, To be published in proceedings of the IAU Symposium No.276
Published: 2010
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16. The effect of stellar contamination on low-resolution transmission spectroscopy: needs identified by NASA’s Exoplanet Exploration Program Study Analysis Group 21

Author: Rackham, Benjamin V, primary, Espinoza, Néstor, additional, Berdyugina, Svetlana V, additional, Korhonen, Heidi, additional, MacDonald, Ryan J, additional, Montet, Benjamin T, additional, Morris, Brett M, additional, Oshagh, Mahmoudreza, additional, Shapiro, Alexander I, additional, Unruh, Yvonne C, additional, Quintana, Elisa V, additional, Zellem, Robert T, additional, Apai, Dániel, additional, Barclay, Thomas, additional, Barstow, Joanna K, additional, Bruno, Giovanni, additional, Carone, Ludmila, additional, Casewell, Sarah L, additional, Cegla, Heather M, additional, Criscuoli, Serena, additional, Fischer, Catherine, additional, Fournier, Damien, additional, Giampapa, Mark S, additional, Giles, Helen, additional, Iyer, Aishwarya, additional, Kopp, Greg, additional, Kostogryz, Nadiia M, additional, Krivova, Natalie, additional, Mallonn, Matthias, additional, McGruder, Chima, additional, Molaverdikhani, Karan, additional, Newton, Elisabeth R, additional, Panja, Mayukh, additional, Peacock, Sarah, additional, Reardon, Kevin, additional, Roettenbacher, Rachael M, additional, Scandariato, Gaetano, additional, Solanki, Sami, additional, Stassun, Keivan G, additional, Steiner, Oskar, additional, Stevenson, Kevin B, additional, Tregloan-Reed, Jeremy, additional, Valio, Adriana, additional, Wedemeyer, Sven, additional, Welbanks, Luis, additional, Yu, Jie, additional, Alam, Munazza K, additional, Davenport, James R A, additional, Deming, Drake, additional, Dong, Chuanfei, additional, Ducrot, Elsa, additional, Fisher, Chloe, additional, Gilbert, Emily, additional, Kostov, Veselin, additional, López-Morales, Mercedes, additional, Line, Mike, additional, Močnik, Teo, additional, Mullally, Susan, additional, Paudel, Rishi R, additional, Ribas, Ignasi, additional, and Valenti, Jeff A, additional
Published: 2023
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17. Noise Sources in Photometry and Radial Velocities

Author: Oshagh, Mahmoudreza, primary
Published: 2017
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18. Final Report for SAG 21: The Effect of Stellar Contamination on Space-based Transmission Spectroscopy

Author: Rackham, Benjamin V., Espinoza, Néstor, Berdyugina, Svetlana V., Korhonen, Heidi, MacDonald, Ryan J., Montet, Benjamin T., Morris, Brett M., Oshagh, Mahmoudreza, Shapiro, Alexander I., Unruh, Yvonne C., Quintana, Elisa V., Zellem, Robert T., Apai, Dániel, Barclay, Thomas, Barstow, Joanna K., Bruno, Giovanni, Carone, Ludmila, Casewell, Sarah L., Cegla, Heather M., Criscuoli, Serena, Fischer, Catherine, Fournier, Damien, Giampapa, Mark S., Giles, Helen, Iyer, Aishwarya, Kopp, Greg, Kostogryz, Nadiia M., Krivova, Natalie, Mallonn, Matthias, McGruder, Chima, Molaverdikhani, Karan, Newton, Elisabeth R., Panja, Mayukh, Peacock, Sarah, Reardon, Kevin, Roettenbacher, Rachael M., Scandariato, Gaetano, Solanki, Sami, Stassun, Keivan G., Steiner, Oskar, Stevenson, Kevin B., Tregloan-Reed, Jeremy, Valio, Adriana, Wedemeyer, Sven, Welbanks, Luis, Yu, Jie, Alam, Munazza K., Davenport, James R. A., Deming, Drake, Dong, Chuanfei, Ducrot, Elsa, Fisher, Chloe, Gilbert, Emily, Kostov, Veselin, López-Morales, Mercedes, Line, Mike, Močnik, Teo, Mullally, Susan, Paudel, Rishi R., Ribas, Ignasi, Valenti, Jeff A., Rackham, Benjamin V., Espinoza, Néstor, Berdyugina, Svetlana V., Korhonen, Heidi, MacDonald, Ryan J., Montet, Benjamin T., Morris, Brett M., Oshagh, Mahmoudreza, Shapiro, Alexander I., Unruh, Yvonne C., Quintana, Elisa V., Zellem, Robert T., Apai, Dániel, Barclay, Thomas, Barstow, Joanna K., Bruno, Giovanni, Carone, Ludmila, Casewell, Sarah L., Cegla, Heather M., Criscuoli, Serena, Fischer, Catherine, Fournier, Damien, Giampapa, Mark S., Giles, Helen, Iyer, Aishwarya, Kopp, Greg, Kostogryz, Nadiia M., Krivova, Natalie, Mallonn, Matthias, McGruder, Chima, Molaverdikhani, Karan, Newton, Elisabeth R., Panja, Mayukh, Peacock, Sarah, Reardon, Kevin, Roettenbacher, Rachael M., Scandariato, Gaetano, Solanki, Sami, Stassun, Keivan G., Steiner, Oskar, Stevenson, Kevin B., Tregloan-Reed, Jeremy, Valio, Adriana, Wedemeyer, Sven, Welbanks, Luis, Yu, Jie, Alam, Munazza K., Davenport, James R. A., Deming, Drake, Dong, Chuanfei, Ducrot, Elsa, Fisher, Chloe, Gilbert, Emily, Kostov, Veselin, López-Morales, Mercedes, Line, Mike, Močnik, Teo, Mullally, Susan, Paudel, Rishi R., Ribas, Ignasi, and Valenti, Jeff A.
Abstract: Study Analysis Group 21 (SAG21) of the Exoplanet Exploration Program Analysis Group (ExoPAG) was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, and plages. This SAG has brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current needs that can be addressed in this context to make the most of transit studies from current NASA facilities like HST and JWST. The analysis produced 14 findings, which fall into three Science Themes encompassing (1) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities ("The Sun as the Stellar Benchmark"), (2) how stars other than the Sun extend our knowledge of heterogeneities ("Surface Heterogeneities of Other Stars") and (3) how to incorporate information gathered for the Sun and other stars into transit studies ("Mapping Stellar Knowledge to Transit Studies")., Comment: 122 pages, 30 figures
Published: 2022

19. A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS

Author: Espinoza, Néstor, primary, Pallé, Enric, additional, Kemmer, Jonas, additional, Luque, Rafael, additional, Caballero, José A., additional, Cifuentes, Carlos, additional, Herrero, Enrique, additional, Sánchez Béjar, Víctor J., additional, Stock, Stephan, additional, Molaverdikhani, Karan, additional, Morello, Giuseppe, additional, Kossakowski, Diana, additional, Schlecker, Martin, additional, Amado, Pedro J., additional, Bluhm, Paz, additional, Cortés-Contreras, Miriam, additional, Henning, Thomas, additional, Kreidberg, Laura, additional, Kürster, Martin, additional, Lafarga, Marina, additional, Lodieu, Nicolas, additional, Morales, Juan Carlos, additional, Oshagh, Mahmoudreza, additional, Passegger, Vera M., additional, Pavlov, Alexey, additional, Quirrenbach, Andreas, additional, Reffert, Sabine, additional, Reiners, Ansgar, additional, Ribas, Ignasi, additional, Rodríguez, Eloy, additional, López, Cristina Rodríguez, additional, Schweitzer, Andreas, additional, Trifonov, Trifon, additional, Chaturvedi, Priyanka, additional, Dreizler, Stefan, additional, Jeffers, Sandra V., additional, Kaminski, Adrian, additional, López-González, María José, additional, Lillo-Box, Jorge, additional, Montes, David, additional, Nowak, Grzegorz, additional, Pedraz, Santos, additional, Vanaverbeke, Siegfried, additional, Zapatero Osorio, Maria R., additional, Zechmeister, Mathias, additional, Collins, Karen A., additional, Girardin, Eric, additional, Guerra, Pere, additional, Naves, Ramon, additional, Crossfield, Ian J. M., additional, Matthews, Elisabeth C., additional, Howell, Steve B., additional, Ciardi, David R., additional, Gonzales, Erica, additional, Matson, Rachel A., additional, Beichman, Charles A., additional, Schlieder, Joshua E., additional, Barclay, Thomas, additional, Vezie, Michael, additional, Villaseñor, Jesus Noel, additional, Daylan, Tansu, additional, Mireies, Ismael, additional, Dragomir, Diana, additional, Twicken, Joseph D., additional, Jenkins, Jon, additional, Winn, Joshua N., additional, Latham, David, additional, Ricker, George, additional, and Seager, Sara, additional
Published: 2022
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20. TOI-178: a window into the formation and evolution of planetary systems

Author: Hooton, Matthew J., Fisher, Chloe, Alibert, Yann, Hara, Nathan, Heng, Kevin, Leleu, Adrien, Palle, Enric, Wilson, Thomas G., Adibekyan, Vardan, Allart, Romain, Barros, Susana C. C., Billot, Nicolas, Boué, Gwenaël, Bourrier, Vincent, Brandeker, Alexis, Bruno, Giovanni, Correia, Alexandre C. M., Demory, Brice-Olivier, Ehrenreich, David, Espinoza, Néstor, Fossati, Luca, Fridlund, Malcolm, Haldemann, Jonas, Hoyer, Sergio, Kitzmann, Daniel, Lavie, Baptiste, Lendl, Monika, Lillo-Box, Jorge, Morris, Brett, Osborn, Hugh, Oshagh, Mahmoudreza, Persson, Carina, Pozuelos, Francisco J., Allende-Prieto, Carlos, Santos, Nuno, Schneider, Jean, Sozzetti, Alessandro, and Beaussier, Catherine
Subjects: [SDU] Sciences of the Universe [physics]
Abstract: Laplacian resonant chains — where astronomical bodies are in mean motion resonance with two or more other bodies — are rare phenomena observed in systems such as the TRAPPIST-1 exoplanets and the Galilean moons of Jupiter. Laplacian chains are an important tool to study the history of planetary systems occupying this configuration, as the fragility of the chain significantly constrains the possible pathways through which the planets can form and evolve. Whilst initial TESS observations suggested that TOI-178 — a nearby system of exoplanets orbiting a relatively cool K-dwarf — hosted the first known planets occupying a horseshoe-coorbital configuration, follow-up observations by CHEOPS, NGTS and SPECULOOS revealed a compact system of six transiting exoplanets all smaller than Neptune: five of which form a chain of Laplacian resonance. Precise measurements of the host's radial velocity using the ESPRESSO spectrograph revealed uncommon planet-to-planet density variations: a stark departure from the monotonic decrease in density with orbital separation common to most systems. JWST time awarded in Cycle 1 to acquire transmission spectroscopy of planets b, d and g promises to make the evolution of the TOI-178 planets amongst the best-understood of any planetary system for the foreseeable future.
Published: 2022

21. TOI-2285b: A 1.7 Earth-radius planet near the habitable zone around a nearby M dwarf

Author: Fukui, Akihiko, primary, Kimura, Tadahiro, additional, Hirano, Teruyuki, additional, Narita, Norio, additional, Kodama, Takanori, additional, Hori, Yasunori, additional, Ikoma, Masahiro, additional, Pallé, Enric, additional, Murgas, Felipe, additional, Parviainen, Hannu, additional, Kawauchi, Kiyoe, additional, Mori, Mayuko, additional, Esparza-Borges, Emma, additional, Bieryla, Allyson, additional, Irwin, Jonathan, additional, Safonov, Boris S, additional, Stassun, Keivan G, additional, Alvarez-Hernandez, Leticia, additional, Béjar, Víctor J S, additional, Casasayas-Barris, Núria, additional, Chen, Guo, additional, Crouzet, Nicolas, additional, de Leon, Jerome P, additional, Isogai, Keisuke, additional, Kagetani, Taiki, additional, Klagyivik, Peter, additional, Korth, Judith, additional, Kurita, Seiya, additional, Kusakabe, Nobuhiko, additional, Livingston, John, additional, Luque, Rafael, additional, Madrigal-Aguado, Alberto, additional, Morello, Giuseppe, additional, Nishiumi, Taku, additional, Orell-Miquel, Jaume, additional, Oshagh, Mahmoudreza, additional, Sánchez-Benavente, Manuel, additional, Stangret, Monika, additional, Terada, Yuka, additional, Watanabe, Noriharu, additional, Zou, Yujie, additional, Tamura, Motohide, additional, Kurokawa, Takashi, additional, Kuzuhara, Masayuki, additional, Nishikawa, Jun, additional, Omiya, Masashi, additional, Vievard, Sébastien, additional, Ueda, Akitoshi, additional, Latham, David W, additional, Quinn, Samuel N, additional, Strakhov, Ivan S, additional, Belinski, Alexandr A, additional, Jenkins, Jon M, additional, Ricker, George R, additional, Seager, Sara, additional, Vanderspek, Roland, additional, Winn, Joshua N, additional, Charbonneau, David, additional, Ciardi, David R, additional, Collins, Karen A, additional, Doty, John P, additional, Bachelet, Etienne, additional, and Harbeck, Daniel, additional
Published: 2021
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22. CHOCOLATE: a new Chromatic Line-Profile Tomography Technique to retrieve Transmission Spectroscopy

Author: Esparza-Borges, Emma, Oshagh, Mahmoudreza, Casasayas-Barris, Núria, and Pallé, Enric
Subjects: Astrophysics::Earth and Planetary Astrophysics
Abstract: Multi-bandphotometrictransitobservationsorlowresolutionspectroscopy(spectro-photometry)arenormallyusedtoretrievethebroadbandtransmissionspectraoftransitingexoplanetsinordertoassessthechemicalcompositionoftheiratmospheres.Here,wepresentanalternativeapproachforrecoveringthebroadbandtransmissionspectrausingchromaticDopplerTomography.Tovalidatethemethodandexamineitsperformance,weusednewobservationaldataobtainedwiththeESPRESSOinstrumenttoretrievethe transmissionspectraofthearchetypalhotJupiterHD209458b.Ourfindingsindicatethattherecoveredtransmissionspectrumisingoodagreementwiththeresultspresentedinpreviousstudies,whichuseddifferentmethodologiestoextractthespectrum.
Published: 2021
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23. Retrieving the Transmission Spectrum of HD209458b using CHOCOLATE: a new Chromatic Line-Profile Technique

Author: Esparza-Borges, Emma, Oshagh, Mahmoudreza, and Pallé, Enric
Subjects: Astrophysics::Earth and Planetary Astrophysics
Abstract: Multi-band photometric transit observations or low resolution spectroscopy (spectro-photometry) are normally used to retrieve the broadband transmission spectra of transiting exoplanets in order to assess the chemical composition of their atmospheres. In this work, we present an alternative approach for recovering the broadband transmission spectra using chromatic Line-Profile Tomography. To validate the method and examine its performance, we used new observational data obtained with the ESPRESSO instruments to retrieve the transmission spectra of the archetypal hot Jupiter HD209458b. Our findings indicate that the recovered transmission spectrum is in good agreement with the results presented in previous studies, which used different methodologies to extract the spectrum.
Published: 2021
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24. A compositional link between rocky exoplanets and their host stars

Author: Adibekyan, Vardan, primary, Dorn, Caroline, additional, Sousa, Sérgio G., additional, Santos, Nuno C., additional, Bitsch, Bertram, additional, Israelian, Garik, additional, Mordasini, Christoph, additional, Barros, Susana C. C., additional, Delgado Mena, Elisa, additional, Demangeon, Olivier D. S., additional, Faria, João P., additional, Figueira, Pedro, additional, Hakobyan, Artur A., additional, Oshagh, Mahmoudreza, additional, Soares, Bárbara M. T. B., additional, Kunitomo, Masanobu, additional, Takeda, Yoichi, additional, Jofré, Emiliano, additional, Petrucci, Romina, additional, and Martioli, Eder, additional
Published: 2021
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25. Giant white-light flares on fully convective stars occur at high latitudes

Author: Ilin, Ekaterina, primary, Poppenhaeger, Katja, additional, Schmidt, Sarah J, additional, Järvinen, Silva P, additional, Newton, Elisabeth R, additional, Alvarado-Gómez, Julián D, additional, Pineda, J Sebastian, additional, Davenport, James R A, additional, Oshagh, Mahmoudreza, additional, and Ilyin, Ilya, additional
Published: 2021
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26. Transit detection of the long-period volatile-rich super-Earth ν2 Lupi d with CHEOPS

Author: Delrez, Laetitia, primary, Ehrenreich, David, additional, Alibert, Yann, additional, Bonfanti, Andrea, additional, Borsato, Luca, additional, Fossati, Luca, additional, Hooton, Matthew J., additional, Hoyer, Sergio, additional, Pozuelos, Francisco J., additional, Salmon, Sébastien, additional, Sulis, Sophia, additional, Wilson, Thomas G., additional, Adibekyan, Vardan, additional, Bourrier, Vincent, additional, Brandeker, Alexis, additional, Charnoz, Sébastien, additional, Deline, Adrien, additional, Guterman, Pascal, additional, Haldemann, Jonas, additional, Hara, Nathan, additional, Oshagh, Mahmoudreza, additional, Sousa, Sergio G., additional, Van Grootel, Valérie, additional, Alonso, Roi, additional, Anglada-Escudé, Guillem, additional, Bárczy, Tamás, additional, Barrado, David, additional, Barros, Susana C. C., additional, Baumjohann, Wolfgang, additional, Beck, Mathias, additional, Bekkelien, Anja, additional, Benz, Willy, additional, Billot, Nicolas, additional, Bonfils, Xavier, additional, Broeg, Christopher, additional, Cabrera, Juan, additional, Collier Cameron, Andrew, additional, Davies, Melvyn B., additional, Deleuil, Magali, additional, Delisle, Jean-Baptiste, additional, Demangeon, Olivier D. S., additional, Demory, Brice-Olivier, additional, Erikson, Anders, additional, Fortier, Andrea, additional, Fridlund, Malcolm, additional, Futyan, David, additional, Gandolfi, Davide, additional, Garcia Muñoz, Antonio, additional, Gillon, Michaël, additional, Guedel, Manuel, additional, Heng, Kevin, additional, Kiss, László, additional, Laskar, Jacques, additional, Lecavelier des Etangs, Alain, additional, Lendl, Monika, additional, Lovis, Christophe, additional, Maxted, Pierre F. L., additional, Nascimbeni, Valerio, additional, Olofsson, Göran, additional, Osborn, Hugh P., additional, Pagano, Isabella, additional, Pallé, Enric, additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Rauer, Heike, additional, Ragazzoni, Roberto, additional, Ribas, Ignasi, additional, Santos, Nuno C., additional, Scandariato, Gaetano, additional, Ségransan, Damien, additional, Simon, Attila E., additional, Smith, Alexis M. S., additional, Steller, Manfred, additional, Szabó, Gyula M., additional, Thomas, Nicolas, additional, Udry, Stéphane, additional, and Walton, Nicholas A., additional
Published: 2021
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27. Dynamical masses of two infant giant planets

Author: Mascareño, Alejandro Suárez, primary, Damasso, Mario, additional, Lodieu, Nicolas, additional, Sozzetti, Alessandro, additional, Béjar, Víctor, additional, Benatti, Serena, additional, Osorio, María Rosa Zapatero, additional, Micela, Giusi, additional, Rebolo, Rafael, additional, Desidera, Silvano, additional, Murgas, Felipe, additional, Claudi, Riccardo, additional, González-Hernández, Jonay, additional, Malavolta, Luca, additional, Burgo, Carlos del, additional, D'Orazi, Valentina, additional, Amado, Pedro, additional, Locci, Daniele, additional, Tabernero, Hugo, additional, Marzari, Francesco, additional, Aguado, David, additional, Turrini, Diego, additional, Guillén, Carlos Cardona, additional, Padrón, Borja Toledo, additional, Maggio, Antonio, additional, Aceituno, Jesús, additional, Bauer, Florian, additional, Caballero, Jose, additional, Chinchilla, Patricia, additional, Esparza-Borges, Emma, additional, González-Álvarez, Esther, additional, Granzer, Thomas, additional, Luque, Rafael, additional, Guerrero, Eduardo Martín, additional, Nowak, Grzegorz, additional, Oshagh, Mahmoudreza, additional, Pallé, Enric, additional, Parviainen, Hannu, additional, Quirrenbach, Andreas, additional, Reiners, Ansgar, additional, Ribas, Ignasi, additional, Strassmeier, Klaus, additional, and Weber, Michael, additional
Published: 2021
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28. Transit detection of the long-period volatile-rich super-Earth ν² Lupi d with CHEOPS

Author: Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sebastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sérgio G., Van Grootel, Valérie, Alonso Sobrino, Roi, Anglada-Escudé, Guillem, Bárczy, Tamás, Barrado, David, Barros, Susana C.C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera Perez, Juan, Collier Cameron, Andrew, Davies, Melvyn. B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D.S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Garcia Muñoz, Antonio, Gillon, Michael, Guedel, Manuel, Heng, Kevin, Kiss, Laszlo, Laskar, Jacques, Lecavelier des Etangs, Alain, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Palle, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M S, Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stephane, and Walton, Nicholas A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Published: 2021

29. Transit detection of the long-period volatile-rich super-Earth nu(2) Lupi d with CHEOPS

Author: Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Anglada-Escudé, Guillem, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Collier Cameron, Andrew, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Garcia Muñoz, Antonio, Gillon, Michael, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Lecavelier des Etangs, Alain, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, Walton, Nicholas A., Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Anglada-Escudé, Guillem, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Collier Cameron, Andrew, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Garcia Muñoz, Antonio, Gillon, Michael, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Lecavelier des Etangs, Alain, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, and Walton, Nicholas A.
Abstract: Exoplanets transiting bright nearby stars are key objects for advancing our knowledge of planetary formation and evolution. The wealth of photons from the host star gives detailed access to the atmospheric, interior and orbital properties of the planetary companions. nu(2) Lupi (HD 136352) is a naked-eye (V = 5.78) Sun-like star that was discovered to host three low-mass planets with orbital periods of 11.6, 27.6 and 107.6 d via radial-velocity monitoring(1). The two inner planets (b and c) were recently found to transit(2), prompting a photometric follow-up by the brand new Characterising Exoplanets Satellite (CHEOPS). Here, we report that the outer planet d is also transiting, and measure its radius and mass to be 2.56 +/- 0.09 R-circle plus and 8.82 +/- 0.94 M-circle plus, respectively. With its bright Sun-like star, long period and mild irradiation (similar to 5.7 times the irradiation of Earth), nu(2) Lupi d unlocks a completely new region in the parameter space of exoplanets amenable to detailed characterization. We refine the properties of all three planets: planet b probably has a rocky mostly dry composition, while planets c and d seem to have retained small hydrogen-helium envelopes and a possibly large water fraction. This diversity of planetary compositions makes the nu(2) Lupi system an excellent laboratory for testing formation and evolution models of low-mass planets.
Published: 2021
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30. A compositional link between rocky exoplanets and their host stars

Author: Adibekyan, Vardan; https://orcid.org/0000-0002-0601-6199, Dorn, Caroline; https://orcid.org/0000-0001-6110-4610, Sousa, Sérgio G; https://orcid.org/0000-0001-9047-2965, Santos, Nuno C; https://orcid.org/0000-0003-4422-2919, Bitsch, Bertram, Israelian, Garik, Mordasini, Christoph; https://orcid.org/0000-0002-1013-2811, Barros, Susana C C; https://orcid.org/0000-0003-2434-3625, Delgado Mena, Elisa, Demangeon, Olivier D S; https://orcid.org/0000-0001-7918-0355, Faria, João P; https://orcid.org/0000-0002-6728-244X, Figueira, Pedro, Hakobyan, Artur A; https://orcid.org/0000-0001-7392-1765, Oshagh, Mahmoudreza; https://orcid.org/0000-0002-0715-8789, Soares, Bárbara M T B, Kunitomo, Masanobu; https://orcid.org/0000-0002-1932-3358, Takeda, Yoichi; https://orcid.org/0000-0002-7363-0447, Jofré, Emiliano; https://orcid.org/0000-0002-8177-7633, Petrucci, Romina; https://orcid.org/0000-0003-0742-6437, Martioli, Eder; https://orcid.org/0000-0002-5084-168X, Adibekyan, Vardan; https://orcid.org/0000-0002-0601-6199, Dorn, Caroline; https://orcid.org/0000-0001-6110-4610, Sousa, Sérgio G; https://orcid.org/0000-0001-9047-2965, Santos, Nuno C; https://orcid.org/0000-0003-4422-2919, Bitsch, Bertram, Israelian, Garik, Mordasini, Christoph; https://orcid.org/0000-0002-1013-2811, Barros, Susana C C; https://orcid.org/0000-0003-2434-3625, Delgado Mena, Elisa, Demangeon, Olivier D S; https://orcid.org/0000-0001-7918-0355, Faria, João P; https://orcid.org/0000-0002-6728-244X, Figueira, Pedro, Hakobyan, Artur A; https://orcid.org/0000-0001-7392-1765, Oshagh, Mahmoudreza; https://orcid.org/0000-0002-0715-8789, Soares, Bárbara M T B, Kunitomo, Masanobu; https://orcid.org/0000-0002-1932-3358, Takeda, Yoichi; https://orcid.org/0000-0002-7363-0447, Jofré, Emiliano; https://orcid.org/0000-0002-8177-7633, Petrucci, Romina; https://orcid.org/0000-0003-0742-6437, and Martioli, Eder; https://orcid.org/0000-0002-5084-168X
Abstract: The interior compositions of small rocky exoplanets cannot be observed directly but are expected to relate to the composition of the host star. Adibekyan et al. analyzed a sample of rocky exoplanets, inferring the planets’ iron fractions by combining their masses and radii with an interior structure model. The iron fractions of the host stars were calculated from stellar elemental abundances. The two iron fractions, that of the planets and that of the stars, correlate with each other, but the slope is steeper than 1, indicating that planet formation processes modify the compositions of rocky planets. —KTS Stars and planets both form by accreting material from a surrounding disk. Because they grow from the same material, theory predicts that there should be a relationship between their compositions. In this study, we search for a compositional link between rocky exoplanets and their host stars. We estimate the iron-mass fraction of rocky exoplanets from their masses and radii and compare it with the compositions of their host stars, which we assume reflect the compositions of the protoplanetary disks. We find a correlation (but not a 1:1 relationship) between these two quantities, with a slope of >4, which we interpret as being attributable to planet formation processes. Super-Earths and super-Mercuries appear to be distinct populations with differing compositions, implying differences in their formation processes.
Published: 2021

31. Widest broadband transmission spectra (0.38-1.71 micrometer) obtained through ground based chromatic Rossiter-McLaughlin observations

Author: Oshagh, Mahmoudreza, primary
Published: 2020
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32. A New Orbital Ephemeris for WASP-128b

Author: Smith, Alexis M. S., primary, Eigmüller, Philipp, additional, Oshagh, Mahmoudreza, additional, and Southworth, John, additional
Published: 2020
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33. TOI-2285b: A 1.7 Earth-radius planet near the habitable zone around a nearby M dwarf

Author: Fukui, Akihiko, Kimura, Tadahiro, Hirano, Teruyuki, Narita, Norio, Kodama, Takanori, Hori, Yasunori, Ikoma, Masahiro, Pallé, Enric, Murgas, Felipe, Parviainen, Hannu, Kawauchi, Kiyoe, Mori, Mayuko, Esparza-Borges, Emma, Bieryla, Allyson, Irwin, Jonathan, Safonov, Boris S, Stassun, Keivan G, Alvarez-Hernandez, Leticia, Béjar, Víctor J S, Casasayas-Barris, Núria, Chen, Guo, Crouzet, Nicolas, de Leon, Jerome P, Isogai, Keisuke, Kagetani, Taiki, Klagyivik, Peter, Korth, Judith, Kurita, Seiya, Kusakabe, Nobuhiko, Livingston, John, Luque, Rafael, Madrigal-Aguado, Alberto, Morello, Giuseppe, Nishiumi, Taku, Orell-Miquel, Jaume, Oshagh, Mahmoudreza, Sánchez-Benavente, Manuel, Stangret, Monika, Terada, Yuka, Watanabe, Noriharu, Zou, Yujie, Tamura, Motohide, Kurokawa, Takashi, Kuzuhara, Masayuki, Nishikawa, Jun, Omiya, Masashi, Vievard, Sébastien, Ueda, Akitoshi, Latham, David W, Quinn, Samuel N, Strakhov, Ivan S, Belinski, Alexandr A, Jenkins, Jon M, Ricker, George R, Seager, Sara, Vanderspek, Roland, Winn, Joshua N, Charbonneau, David, Ciardi, David R, Collins, Karen A, Doty, John P, Bachelet, Etienne, and Harbeck, Daniel
Abstract: We report the discovery of TOI-2285b, a sub-Neptune-sized planet transiting a nearby (42 pc) M dwarf with a period of 27.3 d. We identified the transit signal from the Transiting Exoplanet Survey Satellite photometric data, which we confirmed with ground-based photometric observations using the multiband imagers MuSCAT2 and MuSCAT3. Combining these data with other follow-up observations including high-resolution spectroscopy with the Tillinghast Reflector Echelle Spectrograph, high-resolution imaging with the SPeckle Polarimeter, and radial velocity (RV) measurements with the InfraRed Doppler instrument, we find that the planet has a radius of $1.74 \pm 0.08\, R_\oplus$, a mass of $\lt \!\!19.5\,M_\oplus$($95\%$c.l.), and an insolation flux of 1.54 ± 0.14 times that of the Earth. Although the planet resides just outside the habitable zone for a rocky planet, if the planet harbors an H2O layer under a hydrogen-rich atmosphere, then liquid water could exist on the surface of the H2O layer depending on the planetary mass and water mass fraction. The bright host star in the near-infrared (Ks= 9.0) makes this planet an excellent target for further RV and atmospheric observations to improve our understanding of the composition, formation, and habitability of sub-Neptune-sized planets.
Published: 2022
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34. Near-InfraRed Planet Searcher to Join HARPS on the ESO 3.6-metre Telescope

Author: Bouchy, François, Doyon, René, Artigau, Étienne, Melo, Claudio, Hernandez, Olivier, Wildi, François, Delfosse, Xavier, Lovis, Christophe, Figueira, Pedro, Canto Martins, Bruno L., González Hernández, Jonay I., Thibault, Simon, Reshetov, Vladimir, Pepe, Francesco, Santos, Nuno C., De Medeiros, José Renan, Rebolo, Rafael, Abreu, Manuel, Adibekyan, Vardan Z., Bandy, Timothy, Benz, Willy, Blind, Nicolas, Bohlender, David, Boisse, Isabelle, Bovay, Sébastien, Broeg, Christopher, Brousseau, Denis, Cabral, Alexandre, Chazelas, Bruno, Cloutier, Ryan, Coelho, João, Conod, Uriel, Cumming, Andrew, Delabre, Bernard, Genolet, Ludovic, Hagelberg, Janis, Jayawardhana, Ray, Käufl, Hans-Ulrich, Lafrenière, David, De Castro Leão, Izan, Malo, Lison, De Medeiros Martins, Allan, Matthews, Jaymie M., Metchev, Stanimir, Oshagh, Mahmoudreza, Ouellet, Mathieu, Parro, Vanderlei C., Rasilla Piñeiro, José Luis, Santos, Pedro, Sarajlic, Mirsad, Segovia, Alex, Sordet, Michael, Udry, Stéphane, Valencia, Diana, Vallée, Philippe, Venn, Kim, Wade, Gregg A., and Saddlemyer, Les
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Near-InfraRed Planet Searcher (NIRPS) is a new ultra-stable infrared (YJH) spectrograph that will be installed on ESO’s 3.6-metre Telescope in La Silla, Chile. Aiming to achieve a precision of 1 m s–1, NIRPS is designed to find rocky planets orbiting M dwarfs, and will operate together with the High Accuracy Radial velocity Planet Searcher (HARPS), also on the 3.6-metre Telescope. In this article we describe the NIRPS science cases and present its main technical characteristics., Published in The Messenger vol. 169, pp. 21-27, September 2017.
Published: 2017
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35. Detection of titanium oxide in the atmosphere of a hot Jupiter

Author: Sedaghati, Elyar, primary, Boffin, Henri M. J., additional, MacDonald, Ryan J., additional, Gandhi, Siddharth, additional, Madhusudhan, Nikku, additional, Gibson, Neale P., additional, Oshagh, Mahmoudreza, additional, Claret, Antonio, additional, and Rauer, Heike, additional
Published: 2017
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36. A survey of M stars in the field of view of Kepler space telescope

Author: Oshagh, Mahmoudreza, primary, Haghighipour, Nader, additional, and Santos, Nuno C., additional
Published: 2010
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37. Detection of titanium oxide in the atmosphere of a hot Jupiter

Author: Sedaghati, Elyar, Boffin, Henri MJ, MacDonald, Ryan J, Gandhi, Siddharth, Madhusudhan, Nikku, Gibson, Neale P, Oshagh, Mahmoudreza, Claret, Antonio, and Rauer, Heike
Subjects: 13. Climate action, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: As an exoplanet transits its host star, some of the light from the star is absorbed by the atoms and molecules in the planet's atmosphere, causing the planet to seem bigger; plotting the planet's observed size as a function of the wavelength of the light produces a transmission spectrum. Measuring the tiny variations in the transmission spectrum, together with atmospheric modelling, then gives clues to the properties of the exoplanet's atmosphere. Chemical species composed of light elements-such as hydrogen, oxygen, carbon, sodium and potassium-have in this way been detected in the atmospheres of several hot giant exoplanets, but molecules composed of heavier elements have thus far proved elusive. Nonetheless, it has been predicted that metal oxides such as titanium oxide (TiO) and vanadium oxide occur in the observable regions of the very hottest exoplanetary atmospheres, causing thermal inversions on the dayside. Here we report the detection of TiO in the atmosphere of the hot-Jupiter planet WASP-19b. Our combined spectrum, with its wide spectral coverage, reveals the presence of TiO (to a confidence level of 7.7σ), a strongly scattering haze (7.4σ) and sodium (3.4σ), and confirms the presence of water (7.9σ) in the atmosphere.

38. The effect of stellar contamination on low-resolution transmission spectroscopy: needs identified by NASA’s Exoplanet Exploration Program Study Analysis Group 21

Author: Rackham, Benjamin V, Espinoza, Néstor, Berdyugina, Svetlana V, Korhonen, Heidi, MacDonald, Ryan J, Montet, Benjamin T, Morris, Brett M, Oshagh, Mahmoudreza, Shapiro, Alexander I, Unruh, Yvonne C, Quintana, Elisa V, Zellem, Robert T, Apai, Dániel, Barclay, Thomas, Barstow, Joanna K, Bruno, Giovanni, Carone, Ludmila, Casewell, Sarah L, Cegla, Heather M, Criscuoli, Serena, Fischer, Catherine, Fournier, Damien, Giampapa, Mark S, Giles, Helen, Iyer, Aishwarya, Kopp, Greg, Kostogryz, Nadiia M, Krivova, Natalie, Mallonn, Matthias, McGruder, Chima, Molaverdikhani, Karan, Newton, Elisabeth R, Panja, Mayukh, Peacock, Sarah, Reardon, Kevin, Roettenbacher, Rachael M, Scandariato, Gaetano, Solanki, Sami, Stassun, Keivan G, Steiner, Oskar, Stevenson, Kevin B, Tregloan-Reed, Jeremy, Valio, Adriana, Wedemeyer, Sven, Welbanks, Luis, Yu, Jie, Alam, Munazza K, Davenport, James R A, Deming, Drake, Dong, Chuanfei, Ducrot, Elsa, Fisher, Chloe, Gilbert, Emily, Kostov, Veselin, López-Morales, Mercedes, Line, Mike, Močnik, Teo, Mullally, Susan, Paudel, Rishi R, Ribas, Ignasi, Valenti, Jeff A, Rackham, Benjamin V, Espinoza, Néstor, Berdyugina, Svetlana V, Korhonen, Heidi, MacDonald, Ryan J, Montet, Benjamin T, Morris, Brett M, Oshagh, Mahmoudreza, Shapiro, Alexander I, Unruh, Yvonne C, Quintana, Elisa V, Zellem, Robert T, Apai, Dániel, Barclay, Thomas, Barstow, Joanna K, Bruno, Giovanni, Carone, Ludmila, Casewell, Sarah L, Cegla, Heather M, Criscuoli, Serena, Fischer, Catherine, Fournier, Damien, Giampapa, Mark S, Giles, Helen, Iyer, Aishwarya, Kopp, Greg, Kostogryz, Nadiia M, Krivova, Natalie, Mallonn, Matthias, McGruder, Chima, Molaverdikhani, Karan, Newton, Elisabeth R, Panja, Mayukh, Peacock, Sarah, Reardon, Kevin, Roettenbacher, Rachael M, Scandariato, Gaetano, Solanki, Sami, Stassun, Keivan G, Steiner, Oskar, Stevenson, Kevin B, Tregloan-Reed, Jeremy, Valio, Adriana, Wedemeyer, Sven, Welbanks, Luis, Yu, Jie, Alam, Munazza K, Davenport, James R A, Deming, Drake, Dong, Chuanfei, Ducrot, Elsa, Fisher, Chloe, Gilbert, Emily, Kostov, Veselin, López-Morales, Mercedes, Line, Mike, Močnik, Teo, Mullally, Susan, Paudel, Rishi R, Ribas, Ignasi, and Valenti, Jeff A
Abstract: Study Analysis Group 21 (SAG21) of NASA’s Exoplanet Exploration Program Analysis Group was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, plages, granules, and flares. This SAG brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current research needs that can be addressed in this context to make the most of transit studies from current NASA facilities like Hubble Space Telescope and JWST. The analysis produced 14 findings, which fall into three science themes encompassing (i) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities (‘The Sun as the Stellar Benchmark’), (ii) how stars other than the Sun extend our knowledge of heterogeneities (‘Surface Heterogeneities of Other Stars’), and (iii) how to incorporate information gathered for the Sun and other stars into transit studies (‘Mapping Stellar Knowledge to Transit Studies’). In this invited review, we largely reproduce the final report of SAG21 as a contribution to the peer-reviewed literature.

39. Studying exoplanetary atmospheres using Chromatic Line-Profile Doppler Tomography technique

Author: Esparza Borges, Emma, Oshagh, Mahmoudreza, Pallé Bagó, Enric, and Máster Universitario en Astrofísica
Subjects: Astrophysics::Earth and Planetary Astrophysics
Abstract: We aim to probe the atmospheric composition of extrasolar planets, specifically hot Jupiters, retrieving their transmission spectra via the novel Chromatic LineProfile Tomography method. This new method relies on measuring the spectral line distortions caused by the planet shading parts of the rotating stellar surface, which are reflected in the Cross Correlation Functions (CCFs). Hence, once the transmission spectra is retrieved, it can reveal narrow and broadband features which can provide information about the composition of the planet’s atmosphere. In this project, we developed a Chromatic Doppler Tomography -based methodology able to fit observational data to extract transmission spectra. We used the publicly available SOAP code to produce the Doppler Tomography models which are used to fit observational data via an MCMC fitting procedure. Also, we tested our methodology with ESPRESSO and HARPS-N data of the well-studied hot Jupiter HD 209458b, which were obtained during several transits of the planet. The transmission spectra of HD 209458b obtained through this technique reproduced previous results published in the bibliography, proving that the Chromatic Line-Profile Doppler Tomography methodology presented in this work can be a useful and novel technique to explore the atmospheres of transiting planets
Published: 2021

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