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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. Masses, Revised Radii, and a Third Planet Candidate in the 'Inverted' Planetary System Around TOI-1266

Author: Cloutier, Ryan, Greklek-McKeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Is the population of close-in planets orbiting M dwarfs sculpted by thermally driven escape or is it a direct outcome of the planet formation process? A number of recent empirical results strongly suggest the latter. However, the unique architecture of the TOI-1266 system presents a challenge to models of planet formation and atmospheric escape given its seemingly "inverted" architecture of a large sub-Neptune ($P_b=10.9$ days, $R_{p,b}=2.62\pm 0.11\, \mathrm{R}_{\oplus}$) orbiting interior to that of the system's smaller planet ($P_c=18.8$ days, $R_{p,c}=2.13\pm 0.12\, \mathrm{R}_{\oplus}$). Here we present revised planetary radii based on new TESS and diffuser-assisted ground-based transit observations, and characterize both planetary masses using a set of 145 radial velocity measurements from HARPS-N ($M_{p,b}=4.23\pm 0.69\, \mathrm{M}_{\oplus}, M_{p,c}=2.88\pm 0.80\, \mathrm{M}_{\oplus}$). Our analysis also reveals a third planet candidate ($P_d=32.3$ days, $M_{p,d}\sin{i} = 4.59^{+0.96}_{-0.94}\, \mathrm{M}_{\oplus}$), which if real, would form a chain of near 5:3 period ratios, although the system is likely not in a mean motion resonance. Our results indicate that TOI-1266 b and c are among the lowest density sub-Neptunes around M dwarfs and likely exhibit distinct bulk compositions of a gas-enveloped terrestrial ($X_{\mathrm{env},b}=5.5\pm 0.7$%) and a water-rich world (WMF$_c=59\pm 14$%), which is supported by hydrodynamic escape models. If distinct bulk compositions are confirmed through atmospheric characterization, the system's unique architecture would represent an interesting test case of inside-out sub-Neptune formation at pebble traps., Comment: Accepted for publication in MNRAS. 21 pages. Our spectroscopic time series are included in the arXiv source files as table6.csv
Published: 2023

3. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author: Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., and Rose, Mark E.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation
Published: 2023
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4. Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

Author: DiTomasso, Victoria, Nava, Chantanelle, López-Morales, Mercedes, Bieryla, Allyson, Cloutier, Ryan, Malavolta, Luca, Mortier, Annelies, Buchhave, Lars A., Stassun, Keivan G., Sozzetti, Alessandro, Bonomo, Aldo Stefano, Charbonneau, David, Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martínez, Ghedina, Adriano, Harutyunyan, Avet, Haywood, R. D., Latham, David, Molinari, Emilio, Pepe, Francesco A., Pinamonti, Matteo, Poretti, Ennio, Rice, Ken, Sasselov, Dimitar, Stalport, Manu, Udry, Stéphane, Watson, Christopher, and Wilson, Thomas G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of $24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to $P=24.422\pm0.014$ days, $K=3.19\pm0.27$ m/s, $M$ sin $i = 10.6 \pm 1.2 M_\oplus$, and $a = 0.142 \pm0.005$ au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries., Comment: Accepted for publication in AJ, 29 pages, 17 figures
Published: 2022
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5. New Perspectives on the Exoplanet Radius Gap from a Mathematica Tool and Visualized Water Equation of State

Author: Zeng, Li, Jacobsen, Stein B., Hyung, Eugenia, Levi, Amit, Nava, Chantanelle, Kirk, James, Piaulet, Caroline, Lacedelli, Gaia, Sasselov, Dimitar D., Petaev, Michail I., Stewart, Sarah T., Alam, Munazza K., López-Morales, Mercedes, Damasso, Mario, and Latham, David W.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Recent astronomical observations obtained with the Kepler and TESS missions and their related ground-based follow-ups revealed an abundance of exoplanets with a size intermediate between Earth and Neptune. A low occurrence rate of planets has been identified at around twice the size of Earth, known as the exoplanet radius gap or radius valley. We explore the geometry of this gap in the mass-radius diagram, with the help of a Mathematica plotting tool developed with the capability of manipulating exoplanet data in multidimensional parameter space, and with the help of visualized water equations of state in the temperature-density graph and the entropy-pressure graph. We show that the radius valley can be explained by a compositional difference between smaller, predominantly rocky planets and larger planets that exhibit greater compositional diversity including cosmic ices (water, ammonia, methane) and gaseous envelopes. In particular, among the larger planets, when viewed from the perspective of planet equilibrium temperature, the hot ones are consistent with ice-dominated composition without significant gaseous envelopes, while the cold ones have more diverse compositions, including various amounts of gaseous envelopes., Comment: 30 pages, 15 figures
Published: 2022
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6. A super-massive Neptune-sized planet

Author: Naponiello, Luca, Mancini, Luigi, Sozzetti, Alessandro, Bonomo, Aldo S., Morbidelli, Alessandro, Dou, Jingyao, Zeng, Li, Leinhardt, Zoe M., Biazzo, Katia, Cubillos, Patricio E., Pinamonti, Matteo, Locci, Daniele, Maggio, Antonio, Damasso, Mario, Lanza, Antonino F., Lissauer, Jack J., Collins, Karen A., Carter, Philip J., Jensen, Eric L. N., Bignamini, Andrea, Boschin, Walter, Bouma, Luke G., Ciardi, David R., Cosentino, Rosario, Crossfield, Ian, Desidera, Silvano, Dumusque, Xavier, Fiorenzano, Aldo F. M., Fukui, Akihiko, Giacobbe, Paolo, Gnilka, Crystal L., Ghedina, Adriano, Guilluy, Gloria, Harutyunyan, Avet, Howell, Steve B., Jenkins, Jon M., Lund, Michael B., Kielkopf, John F., Lester, Katie V., Malavolta, Luca, Mann, Andrew W., Matson, Rachel A., Matthews, Elisabeth C., Nardiello, Domenico, Narita, Norio, Pace, Emanuele, Pagano, Isabella, Palle, Enric, Pedani, Marco, Seager, Sara, Schlieder, Joshua E., Schwarz, Richard P., Shporer, Avi, Twicken, Joseph D., Winn, Joshua N., Ziegler, Carl, and Zingales, Tiziano
Published: 2023
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7. Faint objects in motion: the new frontier of high precision astrometry

Author: Malbet, Fabien, Boehm, Céline, Krone-Martins, Alberto, Amorim, Antonio, Anglada-Escudé, Guillem, Brandeker, Alexis, Courbin, Frédéric, Enßlin, Torsten, Falcão, Antonio, Freese, Katherine, Holl, Berry, Labadie, Lucas, Léger, Alain, Mamon, Gary, Mcarthur, Barbara, Mora, Alcione, Shao, Mike, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Abbas, Ummi, Albertus, Conrado, Alves, João, Barnes, Rory, Bonomo, Aldo Stefano, Bouy, Hervé, Brown, Warren, Cardoso, Vitor, Castellani, Marco, Chemin, Laurent, Clark, Hamish, Correia, Alexandre, Crosta, Mariateresa, Crouzier, Antoine, Damasso, Mario, Darling, Jeremy, Davies, Melvyn, Diaferio, Antonaldo, Fortin, Morgane, Fridlund, Malcolm, Gai, Mario, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hall, David, Hambly, Nigel, Harrison, Diana, Hobbs, David, Holland, Andrew, Høg, Erik, Jordi, Carme, Klioner, Sergei, Lançon, Ariane, Laskar, Jacques, Lattanzi, Mario, Poncin-Lafitte, Christophe Le, Luri, Xavier, Michalik, Daniel, de Almeida, André Moitinho, Mourão, Ana, Moustakas, Leonidas, Murray, Neil, Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Portell, Jordi, Prost, Jean-Pierre, Quirrenbach, Andreas, Schneider, Jean, Scott, Pat, Siebert, Arnaud, Da Silva, Antonio, Silva, Manuel, Thébault, Philippe, Tomsick, John, Traub, Wesley, de Val-Borro, Miguel, Valluri, Monica, Walton, Nicholas, Watkins, Laura, White, Glenn, Wyrzykowski, Lukasz, Wyse, Rosemary, and Yamada, Yoshiyuki
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of Earth-mass habitable worlds around the nearest stars, to distant Milky Way objects, and out to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local Universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry missions: NEAT proposed for the ESA M3 opportunity, micro-NEAT for the S1 opportunity, and Theia for the M4 and M5 opportunities. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this White Paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review instrumentation and mission profiles., Comment: arXiv admin note: substantial text overlap with arXiv:1910.08028, arXiv:1707.01348
Published: 2021
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8. K2-79b and K2-222b: Mass measurements of two small exoplanets with periods beyond 10 days that overlap with periodic magnetic activity signals

Author: Nava, Chantanelle, López-Morales, Mercedes, Mortier, Annelies, Zeng, Li, Giles, Helen A. C., Bieryla, Allyson, Vanderburg, Andrew, Buchhave, Lars A., Poretti, Ennio, Saar, Steven H., Dumusque, Xavier, Latham, David W., Charbonneau, David, Damasso, Mario, Bonomo, Aldo S., Lovis, Christophe, Cameron, Andrew Collier, Eastman, Jason D., Sozzetti, Alessandro, Cosentino, Rosario, Pedani, Marco, Pepe, Francesco, Molinari, Emilio, Sasselov, Dimitar, Mayor, Michel, Stalport, Manu, Malavolta, Luca, Rice, Ken, Watson, Christopher A., Fiorenzano, A. F. Martinez, and Di Fabrizio, Luca
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present mass and radius measurements of K2-79b and K2-222b, two transiting exoplanets orbiting active G-type stars. Their respective 10.99d and 15.39d orbital periods fall near periods of signals induced by stellar magnetic activity. The two signals might therefore interfere and lead to an inaccurate estimate of exoplanet mass. We present a method to mitigate these effects when radial velocity and activity indicator observations are available over multiple observing seasons and the orbital period of the exoplanet is known. We perform correlation and periodogram analyses on sub-sets composed of each target's two observing seasons, in addition to the full data sets. For both targets, these analyses reveal an optimal season with little to no interference at the orbital period of the known exoplanet. We make a confident mass detection of each exoplanet by confirming agreement between fits to the full radial velocity set and the optimal season. For K2-79b, we measure a mass of 11.8 $\pm$ 3.6 $M_{Earth}$ and a radius of 4.09 $\pm$ 0.17 $R_{Earth}$. For K2-222b, we measure a mass of 8.0 $\pm$ 1.8 $M_{Earth}$ and a radius of 2.35 $\pm$ 0.08 $R_{Earth}$. According to model predictions, K2-79b is a highly irradiated Uranus-analog and K2-222b hosts significant amounts of water ice. We also present an RV solution for a candidate second companion orbiting K2-222 at 147.5d., Comment: 33 pages, 17 figures, 13 tables
Published: 2021
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9. Five carbon- and nitrogen-bearing species in a hot giant planet's atmosphere

Author: Giacobbe, Paolo, Brogi, Matteo, Gandhi, Siddharth, Cubillos, Patricio E., Bonomo, Aldo S., Sozzetti, Alessandro, Fossati, Luca, Guilluy, Gloria, Carleo, Ilaria, Rainer, Monica, Harutyunyan, Avet, Borsa, Francesco, Pino, Lorenzo, Nascimbeni, Valerio, Benatti, Serena, Biazzo, Katia, Bignamini, Andrea, Chubb, Katy L., Claudi, Riccardo, Cosentino, Rosario, Covino, Elvira, Damasso, Mario, Desidera, Silvano, Fiorenzano, Aldo F. M., Ghedina, Adriano, Lanza, Antonino F., Leto, Giuseppe, Maggio, Antonio, Malavolta, Luca, Maldonado, Jesus, Micela, Giuseppina, Molinari, Emilio, Pagano, Isabella, Pedani, Marco, Piotto, Giampaolo, Poretti, Ennio, Scandariato, Gaetano, Yurchenko, Sergei N., Fantinel, Daniela, Galli, Alberto, Lodi, Marcello, Sanna, Nicoletta, and Tozzi, Andrea
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: The atmospheres of gaseous giant exoplanets orbiting close to their parent stars (hot Jupiters) have been probed for nearly two decades. They allow us to investigate the chemical and physical properties of planetary atmospheres under extreme irradiation conditions. Previous observations of hot Jupiters as they transit in front of their host stars have revealed the frequent presence of water vapour and carbon monoxide in their atmospheres; this has been studied in terms of scaled solar composition under the usual assumption of chemical equilibrium. Both molecules as well as hydrogen cyanide were found in the atmosphere of HD 209458b, a well studied hot Jupiter (with equilibrium temperature around 1,500 kelvin), whereas ammonia was tentatively detected there and subsequently refuted. Here we report observations of HD 209458b that indicate the presence of water (H2O), carbon monoxide (CO), hydrogen cyanide (HCN), methane (CH4), ammonia (NH3) and acetylene (C2H2), with statistical significance of 5.3 to 9.9 standard deviations per molecule. Atmospheric models in radiative and chemical equilibrium that account for the detected species indicate a carbon-rich chemistry with a carbon-to-oxygen ratio close to or greater than 1, higher than the solar value (0.55). According to existing models relating the atmospheric chemistry to planet formation and migration scenarios, this would suggest that HD 209458b formed far from its present location and subsequently migrated inwards. Other hot Jupiters may also show a richer chemistry than has been previously found, which would bring into question the frequently made assumption that they have solar-like and oxygen-rich compositions., Comment: As part of the Springer Nature Content Sharing Initiative, it is possible to access a view-only version of this paper by using the following SharedIt link: https://rdcu.be/cifrz
Published: 2021
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10. The GAPS Programme at TNG XXVIII -- A pair of hot-Neptunes orbiting the young star TOI-942

Author: Carleo, Ilaria, Desidera, Silvano, Nardiello, Domenico, Malavolta, Luca, Lanza, Antonino F., Livingston, John, Locci, Daniele, Marzari, Francesco, Messina, Sergio, Turrini, Diego, Baratella, Martina, Borsa, Francesco, D'Orazi, Valentina, Nascimbeni, Valerio, Pinamonti, Matteo, Rainer, Monica, Alei, Eleonora, Bignamini, Andrea, Gratton, Raffaele, Micela, Giuseppina, Montalto, Marco, Sozzetti, Alessandro, Squicciarini, Vito, Affer, Laura, Benatti, Serena, Biazzo, Katia, Bonomo, Aldo S., Claudi, Riccardo, Cosentino, Rosario, Covino, Elvira, Damasso, Mario, Esposito, Massimiliano, Fiorenzano, Aldo, Frustagli, Giuseppe, Giacobbe, Paolo, Harutyunyan, Avet, Leto, Giuseppe, Magazzú, Antonio, Maggio, Antonio, Mainella, Giovanni, Maldonado, Jesus, Mallonn, Matthias, Mancini, Luigi, Molinari, Emilio, Molinaro, Marco, Pagano, Isabella, Pedani, Marco, Piotto, Giampaolo, Poretti, Ennio, Redfield, Seth, and Scandariato, Gaetano
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Both young stars and multi-planet systems are primary objects that allow us to study, understand and constrain planetary formation and evolution theories. We validate the physical nature of two Neptune-type planets transiting TOI-942 (TYC 5909-319-1), a previously unacknowledged young star (50+30-20 Myr) observed by the TESS space mission in Sector 5. Thanks to a comprehensive stellar characterization, TESS light curve modelling and precise radial-velocity measurements, we validated the planetary nature of the TESS candidate and detect an additional transiting planet in the system on a larger orbit. From photometric and spectroscopic observations we performed an exhaustive stellar characterization and derived the main stellar parameters. TOI-942 is a relatively active K2.5V star (logR'hk = -4.17+-0.01) with rotation period Prot = 3.39+-0.01 days, a projected rotation velocity vsini=13.8+-0.5 km/s and a radius of ~0.9 Rsun. We found that the inner planet, TOI-942b, has an orbital period Pb=4.3263+-0.0011 days, a radius Rb=4.242-0.313+0.376 Rearth and a mass upper limit of 16 Mearth at 1-sigma confidence level. The outer planet, TOI-942c, has an orbital period Pc=10.1605-0.0053+0.0056 days, a radius Rc=4.793-0.351+0.410 Rearth and a mass upper limit of 37 Mearth at 1-sigma confidence level.
Published: 2020
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11. TOI-1235 b: a keystone super-Earth for testing radius valley emergence models around early M dwarfs

Author: Cloutier, Ryan, Rodriguez, Joseph E., Irwin, Jonathan, Charbonneau, David, Stassun, Keivan G., Mortier, Annelies, Latham, David W., Isaacson, Howard, Howard, Andrew W., Udry, Stéphane, Wilson, Thomas G., Watson, Christopher A., Pinamonti, Matteo, Lienhard, Florian, Giacobbe, Paolo, Guerra, Pere, Collins, Karen A., Beiryla, Allyson, Esquerdo, Gilbert A., Matthews, Elisabeth, Matson, Rachel A., Howell, Steve B., Furlan, Elise, Crossfield, Ian J. M., Winters, Jennifer G., Nava, Chantanelle, Ment, Kristo, Lopez, Eric D., Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Tenenbaum, Peter, Sozzetti, Alessandro, Sha, Lizhou, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Roy, Arpita, Robertson, Paul, Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepper, Joshua, Pepe, Francesco, Molinari, Emilio, Mocnik, Teo, Micela, Giuseppina, Mayor, Michel, Fiorenzano, Aldo F. Martinez, Mallia, Franco, Lubin, Jack, Lovis, Christophe, López-Morales, Mercedes, Kosiarek, Molly R., Kielkopf, John F., Kane, Stephen R., Jensen, Eric L. N., Isopi, Giovanni, Huber, Daniel, Hill, Michelle L., Harutyunyan, Avet, Gonzales, Erica, Giacalone, Steven, Ghedina, Adriano, Ercolino, Andrea, Dumusque, Xavier, Dressing, Courtney D., Damasso, Mario, Dalba, Paul A., Cosentino, Rosario, Conti, Dennis M., Colón, Knicole D., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Christiansen, Jessie, Chontos, Ashley, Cecconi, Massimo, Caldwell, Douglas A., Burke, Christopher, Buchhave, Lars, Beichman, Charles, Behmard, Aida, Beard, Corey, and Murphy, Joseph M. Akana
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally-driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/non-rocky transition in period-radius space. Here we present the confirmation of TOI-1235 b ($P=3.44$ days, $r_p=1.738^{+0.087}_{-0.076}$ R$_{\oplus}$), a planet whose size and period are intermediate between the competing model predictions thus making the system an important test case for emergence models of the rocky/non-rocky transition around early M dwarfs ($R_s=0.630\pm 0.015$ R$_{\odot}$, $M_s=0.640\pm 0.016$ M$_{\odot}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial-velocities from HARPS-N and HIRES. We measure a planet mass of $6.91^{+0.75}_{-0.85}$ M$_{\oplus}$, which implies an iron core mass fraction of $20^{+15}_{-12}$% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like and we constrain a H/He envelope mass fraction to be $<0.5$% at 90% confidence. Our results are consistent with model predictions from thermally-driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remain efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically-determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin ($P=21.8^{+0.9}_{-0.8}$ days, $m_p\sin{i}=13.0^{+3.8}_{-5.3}$ M$_{\oplus}$) that cannot be firmly ruled out by our data., Comment: Accepted to The Astronomical Journal. 8 figures & 5 tables. Table 2 is provided in the arXiv source code
Published: 2020
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12. Two transiting hot Jupiters from the WASP survey: WASP-150b and WASP-176b

Author: Cooke, Benjamin F., Pollacco, Don, Almleaky, Y., Barkaoui, K., Benkhaldoun, Z., Blake, James A., Bouchy, François, Boumis, Panos, Brown, D. J. A., Bruni, Ivan, Burdanov, A., Cameron, Andrew Collier, Chote, Paul, Daassou, A., D'ago, Giuseppe, Dalal, Shweta, Damasso, Mario, Delrez, L., Doyle, A. P., Ducrot, E., Gillon, M., Hébrard, G., Hellier, C., Henning, Thomas, Jehin, E., Kiefer, Flavien, King, George W., Liakos, Alexios, Lopez, Théo, Mancini, Luigi, Mardling, Rosemary, Maxted, P. F. L., McCormac, James, Murray, C., Nielsen, Louise D., Osborn, Hugh, Palle, E., Pepe, Francesco, Pozuelos, F. J., Prieto-Arranz, J., Queloz, D., Schanche, Nicole, Ségransan, Damien, Smalley, Barry, Southworth, John, Thompson, S., Turner, Oliver, Udry, Stéphane, Velasco, S., West, Richard, Wheatley, Pete, and Alikakos, John
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b. WASP-150b is an eccentric ($e$ = 0.38) hot Jupiter on a 5.6 day orbit around a $V$ = 12.03, F8 main-sequence host. The host star has a mass and radius of 1.4 $\rm M_{\odot}$ and 1.7 $\rm R_{\odot}$ respectively. WASP-150b has a mass and radius of 8.5 $\rm M_J$ and 1.1 $\rm R_J$, leading to a large planetary bulk density of 6.4 $\rm \rho_J$. WASP-150b is found to be $\sim3$ Gyr old, well below its circularisation timescale, supporting the eccentric nature of the planet. WASP-176b is a hot Jupiter planet on a 3.9 day orbit around a $V$ = 12.01, F9 sub-giant host. The host star has a mass and radius of 1.3 $\rm M_{\odot}$ and 1.9 $\rm R_{\odot}$. WASP-176b has a mass and radius of 0.86 $\rm M_J$ and 1.5 $\rm R_J$ respectively, leading to a planetary bulk density of 0.23 $\rm \rho_J$., Comment: 15 pages, 14 figures. Accepted for publication in The Astronomical Journal
Published: 2020
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13. Expectations for the confirmation of Proxima c from a long-term radial velocity follow-up

Author: Damasso, Mario and Del Sordo, Fabio
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Proxima c, a candidate second planet orbiting Proxima Centauri, was detected with the radial velocity method. The announced long orbital period (5.21$^{+0.26}_{-0.22}$ years), and small semi-amplitude of the induced Doppler signal (1.2$\pm$0.4 m/s), make this detection challenging and the target worthy of a follow-up in the next years. We intend to evaluate the impact of future data on the statistical significance of the detection through realistic simulated radial velocities to be added to the published dataset, spanning up to one orbital period of Proxima c in the time range 2019-2023. We find that the detection significance of Proxima c increases depending not only on the amount of data collected, but also on the number of instruments used, and especially on the timespan covered by the observational campaign. However, on average we do not get strong statistical evidence and we predict that, in the best-case scenario, in the next 5 years the detection of Proxima c can become significant at 4$\sigma$ level. If instead Proxima c does not exist, the detected signal may lower its significance down to 2$\sigma$., Comment: Accepted for publication in MNRAS, 2020
Published: 2020
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14. A pair of TESS planets spanning the radius valley around the nearby mid-M dwarf LTT 3780

Author: Cloutier, Ryan, Eastman, Jason D., Rodriguez, Joseph E., Astudillo-Defru, Nicola, Bonfils, Xavier, Mortier, Annelies, Watson, Christopher A., Stalport, Manu, Pinamonti, Matteo, Lienhard, Florian, Harutyunyan, Avet, Damasso, Mario, Latham, David W., Collins, Karen A., Massey, Robert, Irwin, Jonathan, Winters, Jennifer G., Charbonneau, David, Ziegler, Carl, Matthews, Elisabeth, Crossfield, Ian J. M., Kreidberg, Laura, Quinn, Samuel N., Ricker, George, Vanderspek, Roland, Seager, Sara, Winn, Joshua, Jenkins, Jon M., Vezie, Michael, Udry, Stéphane, Twicken, Joseph D., Tenenbaum, Peter, Sozzetti, Alessandro, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Santos, Nuno C., Rice, Ken, Rackham, Benjamin V., Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Molinari, Emilio, Mignon, Lucile, Micela, Giuseppina, Melo, Claudio, de Medeiros, José R., Mayor, Michel, Matson, Rachel, Fiorenzano, Aldo F. Martinez, Mann, Andrew W., Magazzú, Antonio, Lovis, Christophe, López-Morales, Mercedes, Lopez, Eric, Lissauer, Jack J., Lépine, Sébastien, Law, Nicholas, Kielkopf, John F., Johnson, John A., Jensen, Eric L. N., Howell, Steve B., Gonzales, Erica, Ghedina, Adriano, Forveille, Thierry, Figueira, Pedro, Dumusque, Xavier, Dressing, Courtney D., Doyon, René, Díaz, Rodrigo F., Di Fabrizio, Luca, Delfosse, Xavier, Cosentino, Rosario, Conti, Dennis M., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Caldwell, Douglas A., Burke, Christopher, Buchhave, Lars, Briceño, César, Boyd, Patricia, Bouchy, François, Beichman, Charles, Artigau, Étienne, and Almenara, Jose M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, $V=13.07$, $K_s=8.204$, $R_s$=0.374 R$_{\odot}$, $M_s$=0.401 M$_{\odot}$, d=22 pc). The two planet candidates are identified in a single TESS sector and are validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of $P_b=0.77$ days, $P_c=12.25$ days and sizes $r_{p,b}=1.33\pm 0.07$ R$_{\oplus}$, $r_{p,c}=2.30\pm 0.16$ R$_{\oplus}$, the two planets span the radius valley in period-radius space around low mass stars thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial-velocity measurements from HARPS and HARPS-N, we measure planet masses of $m_{p,b}=2.62^{+0.48}_{-0.46}$ M$_{\oplus}$ and $m_{p,c}=8.6^{+1.6}_{-1.3}$ M$_{\oplus}$, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and from core-powered mass loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley., Comment: Accepted to AJ. 8 figures, 6 tables. CSV file of the RV measurements (i.e. Table 2) are included in the source code
Published: 2020
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15. Author Correction: A super-massive Neptune-sized planet

Author: Naponiello, Luca, Mancini, Luigi, Sozzetti, Alessandro, Bonomo, Aldo S., Morbidelli, Alessandro, Dou, Jingyao, Zeng, Li, Leinhardt, Zoe M., Biazzo, Katia, Cubillos, Patricio E., Pinamonti, Matteo, Locci, Daniele, Maggio, Antonio, Damasso, Mario, Lanza, Antonino F., Lissauer, Jack J., Collins, Karen A., Carter, Philip J., Jensen, Eric L. N., Bignamini, Andrea, Boschin, Walter, Bouma, Luke G., Ciardi, David R., Cosentino, Rosario, Crossfield, Ian, Desidera, Silvano, Dumusque, Xavier, Fiorenzano, Aldo F. M., Fukui, Akihiko, Giacobbe, Paolo, Gnilka, Crystal L., Ghedina, Adriano, Guilluy, Gloria, Harutyunyan, Avet, Howell, Steve B., Jenkins, Jon M., Lund, Michael B., Kielkopf, John F., Lester, Katie V., Malavolta, Luca, Mann, Andrew W., Matson, Rachel A., Matthews, Elisabeth C., Nardiello, Domenico, Narita, Norio, Pace, Emanuele, Pagano, Isabella, Palle, Enric, Pedani, Marco, Seager, Sara, Schlieder, Joshua E., Schwarz, Richard P., Shporer, Avi, Twicken, Joseph D., Winn, Joshua N., Ziegler, Carl, and Zingales, Tiziano
Published: 2023
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16. An 11 Earth-Mass, Long-Period Sub-Neptune Orbiting a Sun-like Star

Author: Mayo, Andrew W., Rajpaul, Vinesh M., Buchhave, Lars A., Dressing, Courtney D., Mortier, Annelies, Zeng, Li, Fortenbach, Charles D., Aigrain, Suzanne, Bonomo, Aldo S., Cameron, Andrew Collier, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martinez, Haywood, Raphaëlle D., Latham, David W., López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Rice, Ken, Sozzetti, Alessandro, and Udry, Stephane
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Although several thousands of exoplanets have now been detected and characterized, observational biases have led to a paucity of long-period, low-mass exoplanets with measured masses and a corresponding lag in our understanding of such planets. In this paper we report the mass estimation and characterization of the long-period exoplanet Kepler-538b. This planet orbits a Sun-like star (V = 11.27) with M_* = 0.892 +/- (0.051, 0.035) M_sun and R_* = 0.8717 +/- (0.0064, 0.0061) R_sun. Kepler-538b is a 2.215 +/- (0.040, 0.034) R_earth sub-Neptune with a period of P = 81.73778 +/- 0.00013 d. It is the only known planet in the system. We collected radial velocity (RV) observations with HIRES on Keck I and HARPS-N on the TNG. We characterized stellar activity by a Gaussian process with a quasi-periodic kernel applied to our RV and cross correlation function full width at half maximum (FWHM) observations. By simultaneously modeling Kepler photometry, RV, and FWHM observations, we found a semi-amplitude of K = 1.68 +/- (0.39, 0.38) m s^-1 and a planet mass of M_p = 10.6 +/- (2.5, 2.4) M_earth. Kepler-538b is the smallest planet beyond P = 50 d with an RV mass measurement. The planet likely consists of a significant fraction of ices (dominated by water ice), in addition to rocks/metals, and a small amount of gas. Sophisticated modeling techniques such as those used in this paper, combined with future spectrographs with ultra high-precision and stability will be vital for yielding more mass measurements in this poorly understood exoplanet regime. This in turn will improve our understanding of the relationship between planet composition and insolation flux and how the rocky to gaseous transition depends on planetary equilibrium temperature., Comment: Published in AJ, 17 pages, 8 figures, 3 tables
Published: 2019
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17. Growth Model Interpretation of Planet Size Distribution

Author: Zeng, Li, Jacobsen, Stein B., Sasselov, Dimitar D., Petaev, Michail I., Vanderburg, Andrew, Lopez-Morales, Mercedes, Perez-Mercader, Juan, Mattsson, Thomas R., Li, Gongjie, Heising, Matthew Z., Bonomo, Aldo S., Damasso, Mario, Berger, Travis A., Cao, Hao, Levi, Amit, and Wordsworth, Robin D.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Physics - Geophysics
Abstract: The radii and orbital periods of 4000+ confirmed/candidate exoplanets have been precisely measured by the Kepler mission. The radii show a bimodal distribution, with two peaks corresponding to smaller planets (likely rocky) and larger intermediate-size planets, respectively. While only the masses of the planets orbiting the brightest stars can be determined by ground-based spectroscopic observations, these observations allow calculation of their average densities placing constraints on the bulk compositions and internal structures. Yet an important question about the composition of planets ranging from 2 to 4 Earth radii still remains. They may either have a rocky core enveloped in a H2-He gaseous envelope (gas dwarfs) or contain a significant amount of multi-component, H2O-dominated ices/fluids (water worlds). Planets in the mass range of 10-15 Earth masses, if half-ice and half-rock by mass, have radii of 2.5 Earth radii, which exactly match the second peak of the exoplanet radius bimodal distribution. Any planet in the 2-4 Earth radii range requires a gas envelope of at most a few mass percentage points, regardless of the core composition. To resolve the ambiguity of internal compositions, we use a growth model and conduct Monte Carlo simulations to demonstrate that many intermediate-size planets are water worlds., Comment: PNAS link: https://www.pnas.org/content/116/20/9723 Complete data and mass-radius tables are available at: https://www.cfa.harvard.edu/~lzeng/planetmodels.html
Published: 2019
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18. A giant impact as the likely origin of different twins in the Kepler-107 exoplanet system

Author: Bonomo, Aldo S., Zeng, Li, Damasso, Mario, Leinhardt, Zoë M., Justesen, Anders B., Lopez, Eric, Lund, Mikkel N., Malavolta, Luca, Aguirre, Victor Silva, Buchhave, Lars A., Corsaro, Enrico, Denman, Thomas, Lopez-Morales, Mercedes, Mills, Sean M., Mortier, Annelies, Rice, Ken, Sozzetti, Alessandro, Vanderburg, Andrew, Affer, Laura, Arentoft, Torben, Benbakoura, Mansour, Bouchy, François, Christensen-Dalsgaard, Jørgen, Cameron, Andrew Collier, Cosentino, Rosario, Dressing, Courtney D., Dumusque, Xavier, Figueira, Pedro, Fiorenzano, Aldo F. M., García, Rafael A., Handberg, Rasmus, Harutyunyan, Avet, Johnson, John A., Kjeldsen, Hans, Latham, David W., Lovis, Christophe, Lundkvist, Mia S., Mathur, Savita, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Motalebi, Fatemeh, Nascimbeni, Valerio, Nava, Chantanelle, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Poretti, Ennio, Sasselov, Dimitar, Ségransan, Damien, Udry, Stéphane, and Watson, Chris
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Measures of exoplanet bulk densities indicate that small exoplanets with radius less than 3 Earth radii ($R_\oplus$) range from low-density sub-Neptunes containing volatile elements to higher density rocky planets with Earth-like or iron-rich (Mercury-like) compositions. Such astonishing diversity in observed small exoplanet compositions may be the product of different initial conditions of the planet-formation process and/or different evolutionary paths that altered the planetary properties after formation. Planet evolution may be especially affected by either photoevaporative mass loss induced by high stellar X-ray and extreme ultraviolet (XUV) flux or giant impacts. Although there is some evidence for the former, there are no unambiguous findings so far about the occurrence of giant impacts in an exoplanet system. Here, we characterize the two innermost planets of the compact and near-resonant system Kepler-107. We show that they have nearly identical radii (about $1.5-1.6~R_\oplus$), but the outer planet Kepler-107c is more than twice as dense (about $12.6~\rm g\,cm^{-3}$) as the innermost Kepler-107b (about $5.3~\rm g\,cm^{-3}$). In consequence, Kepler-107c must have a larger iron core fraction than Kepler-107b. This imbalance cannot be explained by the stellar XUV irradiation, which would conversely make the more-irradiated and less-massive planet Kepler-107b denser than Kepler-107c. Instead, the dissimilar densities are consistent with a giant impact event on Kepler-107c that would have stripped off part of its silicate mantle. This hypothesis is supported by theoretical predictions from collisional mantle stripping, which match the mass and radius of Kepler-107c., Comment: Published in Nature Astronomy on 4 February 2019, 35 pages including Supplementary Information material
Published: 2019
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19. K2-291 b: A rocky super-Earth in a 2.2 day orbit

Author: Kosiarek, Molly R., Blunt, Sarah, Lopez-Morales, Mercedes, Crossfield, Ian J. M., Sinukoff, Evan, Petigura, Erik A., Gonzales, Erica J., Poretti, Ennio, Malavolta, Luca, Howard, Andrew W., Isaacson, Howard, Haywood, Raphaelle D., Ciardi, David R., Bristow, Makennah, Cameron, Andrew Collier, Charbonneau, David, Dressing, Courtney D., Figueira, Pedro, Fulton, Benjamin J., Hardee, Bronwen J., Hirsch, Lea A., Latham, David W., Mortier, Annelies, Nava, Chantanelle, Schlieder, Joshua E., Vanderburg, Andrew, Weiss, Lauren, Bonomo, Aldo S., Bouchy, Francois, Buchhave, Lars A., Coffinet, Adrien, Damasso, Mario, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Segransan, Damien, Sozzetti, Alessandro, Udry, Stephane, and Watson, Chris
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: K2-291 (EPIC 247418783) is a solar-type star with a radius of R_star = 0.899 $\pm$ 0.034 R_sun and mass of M_star=0.934 $\pm$ 0.038 M_sun. From K2 C13 data, we found one super-Earth planet (R_p = 1.589+0.095-0.072 R_Earth) transiting this star on a short period orbit (P = 2.225177 +6.6e-5 -6.8e-5 days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using HIRES on Keck I and HARPS-N on Telescopio Nazionale Galileo, we constrained the mass of EPIC 247418783b to M_p = 6.49 $\pm$ 1.16 M_Earth. We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process in order to more accurately model the effect of stellar noise on our data; the addition of the Gaussian process also improved the precision of this mass measurement. With a bulk density of 8.84+2.50-2.03 g cm-3, the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photo-evaporation during the first billion years of the star's lifetime., Comment: Accepted to AJ, 15 pages, 8 figures
Published: 2019
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20. Erratum: “An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star” (2019, AJ, 158, 165)

Author: Mayo, Andrew W, Rajpaul, Vinesh M, Buchhave, Lars A, Dressing, Courtney D, Mortier, Annelies, Zeng, Li, Fortenbach, Charles D, Aigrain, Suzanne, Bonomo, Aldo S, Cameron, Andrew Collier, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, AF Martinez, Haywood, Raphaëlle D, Latham, David W, López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Rice, Ken, Sozzetti, Alessandro, and Udry, Stephane
Subjects: Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: The semimajor axis and planet insolation flux of Kepler-538b were incorrectly calculated in the published article. This error did not impact any other parameters or any other results in the paper. Table 2 has been included in full here with the corrected semimajor axis and planet insolation flux values. We thank Arbab I. Arbab and Charles D. Fortenbach for bringing this to our attention.(Table Presented).
Published: 2020

21. An ultra-short period rocky super-Earth with a secondary eclipse and a Neptune-like companion around K2-141

Author: Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Crossfield, Ian J. M., Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Ultra-short period (USP) planets are a class of low mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in-situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of an USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b we thus inferred a radius of $1.51\pm0.05~R_\oplus$ and a mass of $5.08\pm0.41~M_\oplus$, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV dataset, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of $0.30 \pm 0.06$ in the Kepler bandpass, or by thermal emission from the surface of the planet at $\sim$3000K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios., Comment: 16 pages, 10 figures., accepted for publication in AJ
Published: 2018
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22. K2-291b: A Rocky Super-Earth in a 2.2 day Orbit* * Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the University of California and the California Institute of Technology. Keck time has been granted by NASA, the University of Hawaii, the California Institute of Technology, and the University of California. † † Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated by the Fundación Galileo Galilei (FGG) of the Istituto Nazionale di Astrofisica (INAF) at the Observatorio del Roque de los Muchachos (La Palma, Canary Islands, Spain).

Author: Kosiarek, Molly R, Blunt, Sarah, López-Morales, Mercedes, Crossfield, Ian JM, Sinukoff, Evan, Petigura, Erik A, Gonzales, Erica J, Poretti, Ennio, Malavolta, Luca, Howard, Andrew W, Isaacson, Howard, Haywood, Raphaëlle D, Ciardi, David R, Bristow, Makennah, Cameron, Andrew Collier, Charbonneau, David, Dressing, Courtney D, Figueira, Pedro, Fulton, Benjamin J, Hardee, Bronwen J, Hirsch, Lea A, Latham, David W, Mortier, Annelies, Nava, Chantanelle, Schlieder, Joshua E, Vanderburg, Andrew, Weiss, Lauren, Bonomo, Aldo S, Bouchy, François, Buchhave, Lars A, Coffinet, Adrien, Damasso, Mario, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris
Subjects: planets and satellites: composition, planets and satellites: detection, techniques: radial velocities, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: K2-291 is a solar-type star with a radius of R ∗ = 0.899 ±0.034 R and mass of M ∗ = 0.934 ±0.038 M . From the K2 C13 data, we found one super-Earth planet (R p = 1.589 -0.072+0.095 R ⊕ ) transiting this star on a short period orbit (P = 2.225177 -6.8e-5+6.6e-5 days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M p = 6.49 ±1.16 M ⊕ . We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84 -2.03+2.50 g cm -3 , the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star's lifetime.
Published: 2019

23. Theia: Faint objects in motion or the new astrometry frontier

Author: The Theia Collaboration, Boehm, Celine, Krone-Martins, Alberto, Amorim, Antonio, Anglada-Escude, Guillem, Brandeker, Alexis, Courbin, Frederic, Ensslin, Torsten, Falcao, Antonio, Freese, Katherine, Holl, Berry, Labadie, Lucas, Leger, Alain, Malbet, Fabien, Mamon, Gary, McArthur, Barbara, Mora, Alcione, Shao, Michael, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Albertus, Conrado, Bertone, Stefano, Bouy, Herve, Boylan-Kolchin, Michael, Brown, Anthony, Brown, Warren, Cardoso, Vitor, Chemin, Laurent, Claudi, Riccardo, Correia, Alexandre C. M., Crosta, Mariateresa, Crouzier, Antoine, Cyr-Racine, Francis-Yan, Damasso, Mario, da Silva, Antonio, Davies, Melvyn, Das, Payel, Dayal, Pratika, de Val-Borro, Miguel, Diaferio, Antonaldo, Erickcek, Adrienne, Fairbairn, Malcolm, Fortin, Morgane, Fridlund, Malcolm, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hambly, Nigel, Hara, Nathan, Hobbs, David, Hog, Erik, Holland, Andrew, Ibata, Rodrigo, Jordi, Carme, Klioner, Sergei, Kopeikin, Sergei, Lacroix, Thomas, Laskar, Jacques, Poncin-Lafitte, Christophe Le, Luri, Xavier, Majumdar, Subhabrata, Makarov, Valeri, Massey, Richard, Mennesson, Bertrand, Michalik, Daniel, de Almeida, Andre Moitinho, Mourao, Ana, Moustakas, Leonidas, Murray, Neil, Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Perez-Garcia, Angeles, Platais, Imants, de Mora, Jordi Portell i, Quirrenbach, Andreas, Randall, Lisa, Read, Justin, Regos, Eniko, Rory, Barnes, Rybicki, Krzysztof, Scott, Pat, Schneider, Jean, Scholtz, Jakub, Siebert, Arnaud, Tereno, Ismael, Tomsick, John, Traub, Wesley, Valluri, Monica, Walker, Matt, Walton, Nicholas, Watkins, Laura, White, Glenn, Evans, Dafydd Wyn, Wyrzykowski, Lukasz, and Wyse, Rosemary
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: In the context of the ESA M5 (medium mission) call we proposed a new satellite mission, Theia, based on relative astrometry and extreme precision to study the motion of very faint objects in the Universe. Theia is primarily designed to study the local dark matter properties, the existence of Earth-like exoplanets in our nearest star systems and the physics of compact objects. Furthermore, about 15 $\%$ of the mission time was dedicated to an open observatory for the wider community to propose complementary science cases. With its unique metrology system and "point and stare" strategy, Theia's precision would have reached the sub micro-arcsecond level. This is about 1000 times better than ESA/Gaia's accuracy for the brightest objects and represents a factor 10-30 improvement for the faintest stars (depending on the exact observational program). In the version submitted to ESA, we proposed an optical (350-1000nm) on-axis TMA telescope. Due to ESA Technology readiness level, the camera's focal plane would have been made of CCD detectors but we anticipated an upgrade with CMOS detectors. Photometric measurements would have been performed during slew time and stabilisation phases needed for reaching the required astrometric precision., Comment: http://theia.phyip3.dur.ac.uk
Published: 2017

24. SIOUX project: a simultaneous multiband camera for exoplanet atmospheres studies

Author: Christille, Jean Marc, Bonomo, Aldo Stefano, Borsa, Francesco, Busonero, Deborah, Calcidese, Paolo, Claudi, Riccardo, Damasso, Mario, Giacobbe, Paolo, Molinari, Emilio, Pace, Emanuele, Riva, Alberto, Sozzetti, Alessandro, Toso, Giorgio, and Tresoldi, Daniela
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The exoplanet revolution is well underway. The last decade has seen order-of-magnitude increases in the number of known planets beyond the Solar system. Detailed characterization of exoplanetary atmospheres provide the best means for distinguishing the makeup of their outer layers, and the only hope for understanding the interplay between initial composition chemistry, temperature-pressure atmospheric profiles, dynamics and circulation. While pioneering work on the observational side has produced the first important detections of atmospheric molecules for the class of transiting exoplanets, important limitations are still present due to the lack of sys- tematic, repeated measurements with optimized instrumentation at both visible (VIS) and near-infrared (NIR) wavelengths. It is thus of fundamental importance to explore quantitatively possible avenues for improvements. In this paper we report initial results of a feasibility study for the prototype of a versatile multi-band imaging system for very high-precision differential photometry that exploits the choice of specifically selected narrow-band filters and novel ideas for the execution of simultaneous VIS and NIR measurements. Starting from the fundamental system requirements driven by the science case at hand, we describe a set of three opto-mechanical solutions for the instrument prototype: 1) a radial distribution of the optical flux using dichroic filters for the wavelength separation and narrow-band filters or liquid crystal filters for the observations; 2) a tree distribution of the optical flux (implying 2 separate foci), with the same technique used for the beam separation and filtering; 3) an exotic solution consisting of the study of a complete optical system (i.e. a brand new telescope) that exploits the chromatic errors of a reflecting surface for directing the different wavelengths at different foci.
Published: 2016
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25. Masses, revised radii, and a third planet candidate in the 'Inverted' planetary system around TOI-1266

Author: Cloutier, Ryan, Greklek-Mckeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris A., Cloutier, Ryan, Greklek-Mckeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris A.
Abstract: Is the population of close-in planets orbiting M dwarfs sculpted by thermally driven escape or is it a direct outcome of the planet formation process? A number of recent empirical results strongly suggest the latter. However, the unique architecture of the TOI-1266 system presents a challenge to models of planet formation and atmospheric escape given its seemingly ‘inverted’ architecture of a large sub-Neptune (Pb = 10.9 d, ⁠) orbiting interior to that of the system’s smaller planet (Pc = 18.8 d, ⁠). Here, we present revised planetary radii based on new TESS and diffuser-assisted ground-based transit observations, and characterize both planetary masses using a set of 145 radial velocity measurements from HARPS-N (⁠⁠). Our analysis also reveals a third planet candidate (Pd = 32.3 d, ⁠), which if real, would form a chain of near 5:3 period ratios, although the system is likely not in a mean motion resonance. Our results indicate that TOI-1266 b and c are among the lowest density sub-Neptunes around M dwarfs and likely exhibit distinct bulk compositions of a gas-enveloped terrestrial (Xenv,b = 5.5 ± 0.7 per cent) and a water-rich world (WMFc = 59 ± 14 per cent), which is supported by hydrodynamic escape models. If distinct bulk compositions are confirmed through atmospheric characterization, the system’s unique architecture would represent an interesting test case of inside-out sub-Neptune formation at pebble traps.
Published: 2024

26. Masses, revised radii, and a third planet candidate in the ‘Inverted’ planetary system around TOI-1266

Author: Cloutier, Ryan, primary, Greklek-McKeon, Michael, additional, Wurmser, Serena, additional, Cherubim, Collin, additional, Gillis, Erik, additional, Vanderburg, Andrew, additional, Hadden, Sam, additional, Cadieux, Charles, additional, Artigau, Étienne, additional, Vissapragada, Shreyas, additional, Mortier, Annelies, additional, López-Morales, Mercedes, additional, Latham, David W, additional, Knutson, Heather, additional, Haywood, Raphaëlle D, additional, Pallé, Enric, additional, Doyon, René, additional, Cook, Neil, additional, Andreuzzi, Gloria, additional, Cecconi, Massimo, additional, Cosentino, Rosario, additional, Ghedina, Adriano, additional, Harutyunyan, Avet, additional, Pinamonti, Matteo, additional, Stalport, Manu, additional, Damasso, Mario, additional, Rescigno, Federica, additional, Wilson, Thomas G, additional, Buchhave, Lars A, additional, Charbonneau, David, additional, Cameron, Andrew Collier, additional, Dumusque, Xavier, additional, Lovis, Christophe, additional, Mayor, Michel, additional, Molinari, Emilio, additional, Pepe, Francesco, additional, Piotto, Giampaolo, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Udry, Stéphane, additional, and Watson, Chris A, additional
Published: 2023
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27. LHS 1903 provides evidence for gas-depleted formation of planets around M-dwarfs

Author: Wilson, Thomas, primary, Simpson, Anna, additional, Cameron, Andrew Collier, additional, Cloutier, Ryan, additional, Adibekyan, Vardan, additional, John, Ancy Anna, additional, Alibert, Y, additional, Stalport, Manu, additional, Egger, J, additional, Bonfanti, Andrea, additional, Billot, Nicolas, additional, Guterman, Pascal, additional, Maxted, Pierre, additional, Simon, Attila, additional, Sousa, Sergio, additional, Fridlund, Malcolm, additional, Beck, M, additional, Bekkelien, Anja, additional, Salmon, S, additional, Grootel, Valerie Van, additional, Fossati, Luca, additional, Mustill, Alexander, additional, Osborn, Hugh, additional, Zingales, Tiziano, additional, Hooton, M, additional, Affer, Laura, additional, Aigrain, Suzanne, additional, Alonso, Roi, additional, Anglada-Escude, G, additional, Antoniadis-Karnavas, Alexandros, additional, Barczy, T, additional, Barrado, David, additional, Barros, Susana, additional, Baumjohann, Wolfgang, additional, Beck, T, additional, Benz, W, additional, Biondi, Federico, additional, Bonfils, Xavier, additional, Borsato, Luca, additional, Brandeker, Alexis, additional, Broeg, Christopher, additional, Buchhave, Lars, additional, Buder, Maximilian, additional, Cabrera, Juan, additional, Gaxiola, S Carrazco, additional, Charnoz, Sébastien, additional, Ciardi, David, additional, Collins, Karen, additional, Collins, Kevin, additional, Cosentino, Rosario, additional, Csizmadia, Szilard, additional, Cubillos, P, additional, Dalal, Shweta, additional, Damasso, Mario, additional, Davenport, James, additional, Davies, Melvyn, additional, Deleuil, Magali, additional, Delrez, L, additional, Demangeon, Olivier, additional, Demory, Brice-Olivier, additional, DiTomasso, Victoria, additional, Dragomir, Diana, additional, Dressing, Courtney, additional, Dumusque, Xavier, additional, Ehrenreich, David, additional, Erikson, Anders, additional, Esparza-Borges, Emma, additional, Fortier, Andrea, additional, Fukuda, Izuru, additional, Fukui, Akihiko, additional, Gandolfi, Davide, additional, Ghedina, Adriano, additional, Giacalone, Steven, additional, Gill, Holden, additional, Gillon, Michaël, additional, Chew, Y Gomez Maqueo, additional, Güdel, Manuel, additional, Guerra, Pere, additional, Günther, Maximilian, additional, Hara, Nathan, additional, Harutyunyan, Avet, additional, Hayashi, Yuya, additional, Haywood, Raphaëlle, additional, Holcomb, Rae, additional, Horne, Keith, additional, Hoyer, S, additional, Huang, Chelsea, additional, Ikoma, Masahiro, additional, Isaak, K, additional, Jackman, James, additional, Jenkins, Jon, additional, Jensen, Eric, additional, Jontof-Hutter, Daniel, additional, Kawai, Yugo, additional, Kiss, Laszlo, additional, Lakeland, Ben, additional, Laskar, J, additional, Latham, David, additional, des Etangs, Alain Lecavelier, additional, Leleu, Adrien, additional, Lendl, Monika, additional, de Leon, J, additional, Lienhard, Florian, additional, López-Morales, Mercedes, additional, Lovis, Christophe, additional, Lund, Michael, additional, Luque, Rafael, additional, Magrin, D, additional, Malavolta, Luca, additional, Fiorenzano, Aldo, additional, Mayo, Andrew, additional, Mayor, Michel, additional, Mordasini, C, additional, Mortier, Annelies, additional, Murgas, Felipe, additional, Narita, Norio, additional, Nascimbeni, Valerio, additional, Nicholson, Belinda, additional, Olofsson, Göran, additional, Ottensamer, Roland, additional, Pagano, Isabella, additional, Palethorpe, Larissa, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Pedani, Marco, additional, Pepe, Francesco, additional, Peter, Gisbert, additional, Pinamonti, Matteo, additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Poretti, Ennio, additional, Queloz, Didier, additional, Quinn, Sam, additional, Ragazzoni, R, additional, Rando, N, additional, Rapetti, David, additional, Ratti, F, additional, Rauer, Heike, additional, Rescigno, Federica, additional, Ribas, Ignasi, additional, Rice, William, additional, Ricker, George, additional, Robertson, Paul, additional, de Roche, Thierry, additional, Sabin, L, additional, Santos, Nuno, additional, Sasselov, Dimitar, additional, Savel, Arjun, additional, Scandariato, Gaetano, additional, Schanche, Nicole, additional, Schroffenegger, Urs, additional, Schwarz, Richard, additional, Seager, Sara, additional, Sefako, Ramotholo, additional, Ségransan, Damien, additional, Shporer, Avi, additional, Silva, André, additional, Smith, Alexis, additional, Sozzetti, Alessandro, additional, Steller, Manfred, additional, Szabo, Gyula, additional, Tamura, Motohide, additional, Thomas, Nicolas, additional, Tuson, Amy, additional, Udry, Stéphane, additional, Vanderburg, Andrew, additional, Vanderspek, Roland, additional, Venturini, J, additional, Verrecchia, Francesco, additional, Walton, Nicholas, additional, Watson, Christopher, additional, Wells, Robert, additional, Winn, Joshua, additional, Zambelli, Roberto, additional, and Ziegler, Carl, additional
Published: 2023
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28. A chemical survey of exoplanets with ARIEL

Author: Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Heske, Astrid, Leconte, Jérémy, Micela, Giusi, Ollivier, Marc, Pilbratt, Göran, Puig, Ludovic, Turrini, Diego, Vandenbussche, Bart, Wolkenberg, Paulina, Beaulieu, Jean-Philippe, Buchave, Lars A., Ferus, Martin, Griffin, Matt, Guedel, Manuel, Justtanont, Kay, Lagage, Pierre-Olivier, Machado, Pedro, Malaguti, Giuseppe, Min, Michiel, Nørgaard-Nielsen, Hans Ulrik, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Swain, Mark, Szabo, Robert, Werner, Stephanie, Barstow, Joanna, Burleigh, Matt, Cho, James, du Foresto, Vincent Coudé, Coustenis, Athena, Decin, Leen, Encrenaz, Therese, Galand, Marina, Gillon, Michael, Helled, Ravit, Morales, Juan Carlos, Muñoz, Antonio García, Moneti, Andrea, Pagano, Isabella, Pascale, Enzo, Piccioni, Giuseppe, Pinfield, David, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Triaud, Amaury, Venot, Olivia, Waldmann, Ingo, Waltham, David, Wright, Gillian, Amiaux, Jerome, Auguères, Jean-Louis, Berthé, Michel, Bezawada, Naidu, Bishop, Georgia, Bowles, Neil, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Crouzet, Pierre-Elie, Da Peppo, Vania, Sanz, Isabel Escudero, Focardi, Mauro, Frericks, Martin, Hunt, Tom, Kohley, Ralf, Middleton, Kevin, Morgante, Gianluca, Ottensamer, Roland, Pace, Emanuele, Pearson, Chris, Stamper, Richard, Symonds, Kate, Rengel, Miriam, Renotte, Etienne, Ade, Peter, Affer, Laura, Alard, Christophe, Allard, Nicole, Altieri, Francesca, André, Yves, Arena, Claudio, Argyriou, Ioannis, Aylward, Alan, Baccani, Cristian, Bakos, Gaspar, Banaszkiewicz, Marek, Barlow, Mike, Batista, Virginie, Bellucci, Giancarlo, Benatti, Serena, Bernardi, Pernelle, Bézard, Bruno, Blecka, Maria, Bolmont, Emeline, Bonfond, Bertrand, Bonito, Rosaria, Bonomo, Aldo S., Brucato, John Robert, Brun, Allan Sacha, Bryson, Ian, Bujwan, Waldemar, Casewell, Sarah, Charnay, Bejamin, Pestellini, Cesare Cecchi, Chen, Guo, Ciaravella, Angela, Claudi, Riccardo, Clédassou, Rodolphe, Damasso, Mario, Damiano, Mario, Danielski, Camilla, Deroo, Pieter, Di Giorgio, Anna Maria, Dominik, Carsten, Doublier, Vanessa, Doyle, Simon, Doyon, René, Drummond, Benjamin, Duong, Bastien, Eales, Stephen, Edwards, Billy, Farina, Maria, Flaccomio, Ettore, Fletcher, Leigh, Forget, François, Fossey, Steve, Fränz, Markus, Fujii, Yuka, García-Piquer, Álvaro, Gear, Walter, Geoffray, Hervé, Gérard, Jean Claude, Gesa, Lluis, Gomez, H., Graczyk, Rafał, Griffith, Caitlin, Grodent, Denis, Guarcello, Mario Giuseppe, Gustin, Jacques, Hamano, Keiko, Hargrave, Peter, Hello, Yann, Heng, Kevin, Herrero, Enrique, Hornstrup, Allan, Hubert, Benoit, Ida, Shigeru, Ikoma, Masahiro, Iro, Nicolas, Irwin, Patrick, Jarchow, Christopher, Jaubert, Jean, Jones, Hugh, Julien, Queyrel, Kameda, Shingo, Kerschbaum, Franz, Kervella, Pierre, Koskinen, Tommi, Krijger, Matthijs, Krupp, Norbert, Lafarga, Marina, Landini, Federico, Lellouch, Emanuel, Leto, Giuseppe, Luntzer, A., Rank-Lüftinger, Theresa, Maggio, Antonio, Maldonado, Jesus, Maillard, Jean-Pierre, Mall, Urs, Marquette, Jean-Baptiste, Mathis, Stephane, Maxted, Pierre, Matsuo, Taro, Medvedev, Alexander, Miguel, Yamila, Minier, Vincent, Morello, Giuseppe, Mura, Alessandro, Narita, Norio, Nascimbeni, Valerio, Nguyen Tong, N., Noce, Vladimiro, Oliva, Fabrizio, Palle, Enric, Palmer, Paul, Pancrazzi, Maurizio, Papageorgiou, Andreas, Parmentier, Vivien, Perger, Manuel, Petralia, Antonino, Pezzuto, Stefano, Pierrehumbert, Ray, Pillitteri, Ignazio, Piotto, Giampaolo, Pisano, Giampaolo, Prisinzano, Loredana, Radioti, Aikaterini, Réess, Jean-Michel, Rezac, Ladislav, Rocchetto, Marco, Rosich, Albert, Sanna, Nicoletta, Santerne, Alexandre, Savini, Giorgio, Scandariato, Gaetano, Sicardy, Bruno, Sierra, Carles, Sindoni, Giuseppe, Skup, Konrad, Snellen, Ignas, Sobiecki, Mateusz, Soret, Lauriane, Sozzetti, Alessandro, Stiepen, A., Strugarek, Antoine, Taylor, Jake, Taylor, William, Terenzi, Luca, Tessenyi, Marcell, Tsiaras, Angelos, Tucker, C., Valencia, Diana, Vasisht, Gautam, Vazan, Allona, Vilardell, Francesc, Vinatier, Sabrine, Viti, Serena, Waters, Rens, Wawer, Piotr, Wawrzaszek, Anna, Whitworth, Anthony, Yung, Yuk L., Yurchenko, Sergey N., Osorio, María Rosa Zapatero, Zellem, Robert, Zingales, Tiziano, and Zwart, Frans
Published: 2018
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29. Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N

Author: DiTomasso, Victoria, Nava, Chantanelle, López-Morales, Mercedes, Bieryla, Allyson, Cloutier, Ryan, Malavolta, Luca, Mortier, Annelies, Buchhave, Lars A., Stassun, Keivan G., Sozzetti, Alessandro, Bonomo, Aldo Stefano, Charbonneau, David, Collier Cameron, Andrew, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Martínez Fiorenzano, A. F., Ghedina, Adriano, Harutyunyan, Avet, Haywood, R. D., Latham, David, Molinari, Emilio, Pepe, Francesco A., Pinamonti, Matteo, Poretti, Ennio, Rice, Ken, Sasselov, Dimitar, Stalport, Manu, Udry, Stéphane, Watson, Christopher, Wilson, Thomas G., DiTomasso, Victoria, Nava, Chantanelle, López-Morales, Mercedes, Bieryla, Allyson, Cloutier, Ryan, Malavolta, Luca, Mortier, Annelies, Buchhave, Lars A., Stassun, Keivan G., Sozzetti, Alessandro, Bonomo, Aldo Stefano, Charbonneau, David, Collier Cameron, Andrew, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Martínez Fiorenzano, A. F., Ghedina, Adriano, Harutyunyan, Avet, Haywood, R. D., Latham, David, Molinari, Emilio, Pepe, Francesco A., Pinamonti, Matteo, Poretti, Ennio, Rice, Ken, Sasselov, Dimitar, Stalport, Manu, Udry, Stéphane, Watson, Christopher, and Wilson, Thomas G.
Abstract: We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD 79210 and HD 79211, two M0V members of a gravitationally bound binary system. We detect a planet candidate with a period of days around HD 79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES, and RVs spanning a total of 25 yr, we further refine the planet candidate parameters to P = 24.422 ± 0.014 days, K = 3.19 ± 0.27 m s−1, M sin i = 10.6 ± 1.2M⊕, and a = 0.142 ± 0.005 au. We do not find any additional planet candidate signals in the data of HD 79211, nor do we find any planet candidate signals in HD 79210. This system adds to the number of exoplanets detected in binaries with M-dwarf members and serves as a case study for planet formation in stellar binaries.
Published: 2023

30. Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N

Author: DiTomasso, Victoria, primary, Nava, Chantanelle, additional, López-Morales, Mercedes, additional, Bieryla, Allyson, additional, Cloutier, Ryan, additional, Malavolta, Luca, additional, Mortier, Annelies, additional, Buchhave, Lars A., additional, Stassun, Keivan G., additional, Sozzetti, Alessandro, additional, Bonomo, Aldo Stefano, additional, Charbonneau, David, additional, Collier Cameron, Andrew, additional, Cosentino, Rosario, additional, Damasso, Mario, additional, Dumusque, Xavier, additional, Martínez Fiorenzano, A. F., additional, Ghedina, Adriano, additional, Harutyunyan, Avet, additional, Haywood, R. D., additional, Latham, David, additional, Molinari, Emilio, additional, Pepe, Francesco A., additional, Pinamonti, Matteo, additional, Poretti, Ennio, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Stalport, Manu, additional, Udry, Stéphane, additional, Watson, Christopher, additional, and Wilson, Thomas G., additional
Published: 2023
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31. GAPS2: the origin of planetary systems diversity

Author: AFFER, Laura, BENATTI, Serena, BIAZZO, Katia, BIGNAMINI, ANDREA, BORSA, Francesco, CARLEO, Ilaria, CLAUDI, Riccardo, COSENTINO, Rosario, COVINO, Elvira, DAMASSO, Mario, DESIDERA, Silvano, GIACOBBE, Paolo, GUILLUY, GLORIA, HARUTYUNYAN, Avet, LANZA, Antonino Francesco, LETO, Giuseppe, MAGGIO, Antonio, Malavolta, L., MALDONADO PRADO, Jesus, Mancini, Luigi, MICELA, Giuseppina, MOLINARI, Emilio Carlo, NARDIELLO, Domenico, NASCIMBENI, VALERIO, PAGANO, Isabella, PINAMONTI, Matteo, PIOTTO , GIAMPAOLO, PORETTI, Ennio, RAINER, Monica, SCANDARIATO, GAETANO, SOZZETTI, Alessandro, and ITA
Abstract: This report described the work done in the GAPS2 programme so far. The goal of the project was to take advantage of the unique capabilities of the instrumentation at the TNG to study the origin of the diversity of planetary systems, shaped by variable degrees of orbital evolution, exploring uncharted territories in the realm of planet formation and evolution with emphasis on the innermost regions.
Published: 2023

32. Searching for the Transit Signal of the Exoplanet Gl 514 b in the TESS Photometry

Author: Damasso, Mario, primary and Nardiello, Domenico, additional
Published: 2022
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33. The gaia survey contribution to EChO target selection and characterization

Author: Sozzetti, Alessandro and Damasso, Mario
Published: 2015
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34. A Pair of TESS Planets Spanning the Radius Valley around the Nearby Mid-M Dwarf LTT 3780

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Cloutier, Ryan, Eastman, Jason D., Rodriguez, Joseph E., Astudillo-Defru, Nicola, Bonfils, Xavier, Mortier, Annelies, Watson, Christopher A., Stalport, Manu, Pinamonti, Matteo, Lienhard, Florian, Harutyunyan, Avet, Damasso, Mario, Latham, David W., Collins, Karen A., Massey, Robert, Irwin, Jonathan, Winters, Jennifer G., Charbonneau, David, Ziegler, Carl, Matthews, Elisabeth C, Crossfield, Ian Jm, Kreidberg, Laura, Quinn, Samuel N., Ricker, George R, Vanderspek, Roland K, Seager, Sara, Winn, Joshua, Jenkins, Jon M., Vezie, Michael L., Udry, Stéphane, Twicken, Joseph D., Tenenbaum, Peter, Sozzetti, Alessandro, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Santos, Nuno C., Rice, Ken, Rackham, Benjamin V, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Molinari, Emilio, Mignon, Lucile, Micela, Giuseppina, Melo, Claudio, de Medeiros, José R., Mayor, Michel, Matson, Rachel A., Fiorenzano, Aldo F. Martinez, Mann, Andrew W., Magazzú, Antonio, Lovis, Christophe, López-Morales, Mercedes, Lopez, Eric, Lizzauer, Jack J., Lépine, Sébastien, Law, Nicholas, Kielkopf, John F., Johnson, John A., Jensen, Eric L. N., Howell, Steve B., Gonzales, Erica, Ghedina, Adriano, Forveille, Thierry, Figueira, Pedro, Dumusque, Xavier, Dressing, Courtney D., Doyon, René, Díaz, Rodrigo F., Fabrizio, Luca Di, Delfosse, Xavier, Cosentino, Rosario, Conti, Dennis M., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Caldwell, Douglas A., Burke, Christopher J., Buchhave, Lars, Briceño, César, Boyd, Patricia, Bouchy, François, Beichman, Charles, Artigau, Etienne, Almenara, Jose M., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Cloutier, Ryan, Eastman, Jason D., Rodriguez, Joseph E., Astudillo-Defru, Nicola, Bonfils, Xavier, Mortier, Annelies, Watson, Christopher A., Stalport, Manu, Pinamonti, Matteo, Lienhard, Florian, Harutyunyan, Avet, Damasso, Mario, Latham, David W., Collins, Karen A., Massey, Robert, Irwin, Jonathan, Winters, Jennifer G., Charbonneau, David, Ziegler, Carl, Matthews, Elisabeth C, Crossfield, Ian Jm, Kreidberg, Laura, Quinn, Samuel N., Ricker, George R, Vanderspek, Roland K, Seager, Sara, Winn, Joshua, Jenkins, Jon M., Vezie, Michael L., Udry, Stéphane, Twicken, Joseph D., Tenenbaum, Peter, Sozzetti, Alessandro, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Santos, Nuno C., Rice, Ken, Rackham, Benjamin V, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Molinari, Emilio, Mignon, Lucile, Micela, Giuseppina, Melo, Claudio, de Medeiros, José R., Mayor, Michel, Matson, Rachel A., Fiorenzano, Aldo F. Martinez, Mann, Andrew W., Magazzú, Antonio, Lovis, Christophe, López-Morales, Mercedes, Lopez, Eric, Lizzauer, Jack J., Lépine, Sébastien, Law, Nicholas, Kielkopf, John F., Johnson, John A., Jensen, Eric L. N., Howell, Steve B., Gonzales, Erica, Ghedina, Adriano, Forveille, Thierry, Figueira, Pedro, Dumusque, Xavier, Dressing, Courtney D., Doyon, René, Díaz, Rodrigo F., Fabrizio, Luca Di, Delfosse, Xavier, Cosentino, Rosario, Conti, Dennis M., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Caldwell, Douglas A., Burke, Christopher J., Buchhave, Lars, Briceño, César, Boyd, Patricia, Bouchy, François, Beichman, Charles, Artigau, Etienne, and Almenara, Jose M.
Abstract: © 2020. The American Astronomical Society. All rights reserved We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, V = 13.07, K s = 8.204, R s = 0.374 R o˙, M s = 0.401 M o˙, d = 22 pc). The two planet candidates are identified in a single Transiting Exoplanet Survey Satellite sector and validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of P b = 0.77, P c = 12.25 days and sizes r p,b = 1.33 ± 0.07, r p,c = 2.30 ± 0.16 R ⊕, the two planets span the radius valley in period-radius space around low-mass stars, thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial velocity measurements from the High Accuracy Radial velocity Planet Searcher (HARPS) and HARPS-N, we measure planet masses of mpb 2.62+ 0.48 and-0.46= mpc 8.6+1.6-1.3 M⊕, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and core-powered mass-loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley.
Published: 2022

35. K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals

Author: Nava, Chantanelle, López-Morales, Mercedes, Mortier, Annelies, Zeng, Li, Giles, Helen A. C., Bieryla, Allyson, Vanderburg, Andrew, Buchhave, Lars A., Poretti, Ennio, Saar, Steven H., Dumusque, Xavier, Latham, David W., Charbonneau, David, Damasso, Mario, Bonomo, Aldo S., Lovis, Christophe, Collier Cameron, Andrew, Eastman, Jason D., Sozzetti, Alessandro, Cosentino, Rosario, Pedani, Marco, Pepe, Francesco, Molinari, Emilio, Sasselov, Dimitar, Mayor, Michel, Stalport, Manu, Malavolta, Luca, Rice, Ken, Watson, Christopher A., Martinez Fiorenzano, A. F., Di Fabrizio, Luca, Nava, Chantanelle, López-Morales, Mercedes, Mortier, Annelies, Zeng, Li, Giles, Helen A. C., Bieryla, Allyson, Vanderburg, Andrew, Buchhave, Lars A., Poretti, Ennio, Saar, Steven H., Dumusque, Xavier, Latham, David W., Charbonneau, David, Damasso, Mario, Bonomo, Aldo S., Lovis, Christophe, Collier Cameron, Andrew, Eastman, Jason D., Sozzetti, Alessandro, Cosentino, Rosario, Pedani, Marco, Pepe, Francesco, Molinari, Emilio, Sasselov, Dimitar, Mayor, Michel, Stalport, Manu, Malavolta, Luca, Rice, Ken, Watson, Christopher A., Martinez Fiorenzano, A. F., and Di Fabrizio, Luca
Abstract: We present mass and radius measurements of K2-79b and K2-222b, two transiting exoplanets orbiting active G-type stars observed with HARPS-N and K2. Their respective 10.99 day and 15.39 day orbital periods fall near periods of signals induced by stellar magnetic activity. The two signals might therefore interfere and lead to an inaccurate estimate of exoplanet mass. We present a method to mitigate these effects when radial velocity (RV) and activity-indicator observations are available over multiple observing seasons and the orbital period of the exoplanet is known. We perform correlation and periodogram analyses on subsets composed of each target's two observing seasons, in addition to the full data sets. For both targets, these analyses reveal an optimal season with little to no interference at the orbital period of the known exoplanet. We make a confident mass detection of each exoplanet by confirming agreement between fits to the full RV set and the optimal season. For K2-79b, we measure a mass of 11.8 ± 3.6 M⊕ and a radius of 4.09 ± 0.17 R⊕. For K2-222b, we measure a mass of 8.0 ± 1.8 M⊕ and a radius of 2.35 ± 0.08 R⊕. According to model predictions, K2-79b is a highly irradiated Uranus analog and K2-222b hosts significant amounts of water ice. We also present a RV solution for a candidate second companion orbiting K2-222 at 147.5 days.
Published: 2022

36. K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals

Author: Nava, Chantanelle, primary, López-Morales, Mercedes, additional, Mortier, Annelies, additional, Zeng, Li, additional, Giles, Helen A. C., additional, Bieryla, Allyson, additional, Vanderburg, Andrew, additional, Buchhave, Lars A., additional, Poretti, Ennio, additional, Saar, Steven H., additional, Dumusque, Xavier, additional, Latham, David W., additional, Charbonneau, David, additional, Damasso, Mario, additional, Bonomo, Aldo S., additional, Lovis, Christophe, additional, Collier Cameron, Andrew, additional, Eastman, Jason D., additional, Sozzetti, Alessandro, additional, Cosentino, Rosario, additional, Pedani, Marco, additional, Pepe, Francesco, additional, Molinari, Emilio, additional, Sasselov, Dimitar, additional, Mayor, Michel, additional, Stalport, Manu, additional, Malavolta, Luca, additional, Rice, Ken, additional, Watson, Christopher A., additional, Martinez Fiorenzano, A. F., additional, and Di Fabrizio, Luca, additional
Published: 2022
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37. New Perspectives on the Exoplanet Radius Gap from a Mathematica Tool and Visualized Water Equation of State

Author: Zeng, Li, primary, Jacobsen, Stein B., additional, Hyung, Eugenia, additional, Levi, Amit, additional, Nava, Chantanelle, additional, Kirk, James, additional, Piaulet, Caroline, additional, Lacedelli, Gaia, additional, Sasselov, Dimitar D., additional, Petaev, Michail I., additional, Stewart, Sarah T., additional, Alam, Munazza K., additional, López-Morales, Mercedes, additional, Damasso, Mario, additional, and Latham, David W., additional
Published: 2021
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38. Search and characterization of young planets with GAPS2

Author: Benatti, Serena, Desidera, Silvano, and Damasso, Mario
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Exoplanets, young transiting planets, radial velocities, evolution of planetary systems, Astrophysics::Galaxy Astrophysics
Abstract: The“GAPS” (Global Architecture of Planetary Systems)projectgathersa large part of the Italian community working onexoplanets.One of our aims is thesearch for young exoplanets with HARPS-N and GIARPS at TNG, since they are the key targets to study the ongoing planet formation and to investigate the role played by the migration mechanisms, the formation sites and the orbit evolution on their observed diversity.Transit space missions are significantly contributing in our view of young planetary systems at close separations, providing robust candidates to be followed-up with the radial velocity (RV) technique. The Young Objects sub-program of GAPS2 searches for young planets by surveying members in young (e.g., Taurus, Cepheus) and intermediate age (e.g. Coma Ber, Hyades) associations, and perform an RV follow-up of young transiting candidates, mainly provided by the NASA-TESS satellite. For a proper treatment of the high level of the stellar activity, typical for these objects, we work to improve the RV extraction and exploit the Gaussian process regression modelling, supported by an intensive RV monitoring. I will review the first results of our survey, including the confirmation and the retraction of known planet candidates, the stellar parameters such as stellar age and membership to groups, chemical composition, magnetic activity and high-energy emission and their link to planet detectability and evaporation of the atmospheres.
Published: 2021
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39. Radial velocity follow-up of young transiting planets: promising results from selected case studies

Author: Damasso, Mario
Abstract: Contributed talk to the PLATO mission conference 2021
Published: 2021
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40. A warm Neptune around the G5V dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N

Author: König, Pierre-Cécil, Damasso, Mario, Hébrard, Guillaume, Naponiello, Luca, and et al., including SOPHIE, GAPS and TESS Teams
Subjects: Stellar Astrophysics, Exoplanets, Techniques: Photometric, Planetary Systems, Techniques: Spectroscopic, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Techniques: Radial Velocities
Abstract: We report the detection and characterization of the new transiting extrasolar planet TOI-1710 b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite (TESS). Its planetary nature has been established from HARPS-N and SOPHIE spectroscopic observations via the radial velocity method. The stellar parameters for the host star are derived from the spectra and a joint Markov chain Monte-Carlo (MCMC) adjustment of the spectral energy distribution and evolutionary tracks of TOI-1710. Performed in a combined MCMC and quasi-periodic Gaussian process method, a simultaneous analysis of the TESS light curve and the radial velocity evolution concomitantly allows us to determine the planetary properties and inspect the stellar magnetic activity jitter. TOI-1710 b is a massive warm Neptune (30.0 ± 5.7 M_Earth and 5.84 ± 0.30 R_Earth) orbiting a G5V dwarf star on a 24.3 days circular compatible orbit (e = 0.13 ± 0.09)., König, Pierre-Cécil, et al., A&A, in prep., {"references":["Foreman-Mackey, Daniel, et al. (2017). Exoplanet Python Package associated to DOI:10.3847/1538-3881/aa9332"]}
Published: 2021
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41. the new frontier of high precision astrometry

Author: Malbet, Fabien, Boehm, Céline, Krone-Martins, Alberto, Amorim, Antonio, Anglada-Escudé, Guillem, Brandeker, Alexis, Courbin, Frédéric, Enßlin, Torsten, Falcão, Antonio, Freese, Katherine, Holl, Berry, Labadie, Lucas, Léger, Alain, Mamon, Gary A., McArthur, Barbara, Mora, Alcione, Shao, Mike, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Abbas, Ummi, Albertus, Conrado, Alves, João, Barnes, Rory, Bonomo, Aldo Stefano, Bouy, Hervé, Brown, Warren R., Cardoso, Vitor, Castellani, Marco, Chemin, Laurent, Clark, Hamish, Correia, Alexandre C.M., Crosta, Mariateresa, Crouzier, Antoine, Damasso, Mario, Darling, Jeremy, Davies, Melvyn B., Diaferio, Antonaldo, Fortin, Morgane, Fridlund, Malcolm, Gai, Mario, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hall, David, Hambly, Nigel, Harrison, Diana, Hobbs, David, Holland, Andrew, Høg, Erik, Jordi, Carme, Klioner, Sergei, Lançon, Ariane, Laskar, Jacques, Lattanzi, Mario, Le Poncin-Lafitte, Christophe, Luri, Xavier, Michalik, Daniel, de Almeida, André Moitinho, Mourão, Ana, Moustakas, Leonidas, Murray, Neil J., Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Portell, Jordi, Prost, Jean Pierre, Quirrenbach, Andreas, Schneider, Jean, Scott, Pat, Siebert, Arnaud, Silva, Antonio da, Silva, Manuel, Thébault, Philippe, Tomsick, John, Traub, Wesley, de Val-Borro, Miguel, Valluri, Monica, Walton, Nicholas A., White, Glenn, Watkins, Laura L., Wyrzykowski, Lukasz, Wyse, Rosemary, Yamada, Yoshiyuki, and UNINOVA-Instituto de Desenvolvimento de Novas Tecnologias
Subjects: Local universe, Space and Planetary Science, Exoplanets, Astronomy and Astrophysics, Astrometry, Space mission, Cosmology
Abstract: Open access funding provided by Istituto Nazionale di Astrofisica within the CRUI-CARE Agreement. Publisher Copyright: © 2021, The Author(s). Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of Earth-mass habitable worlds around the nearest stars, to distant Milky Way objects, and out to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local Universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry missions: NEAT proposed for the ESA M3 opportunity, micro-NEAT for the S1 opportunity, and Theia for the M4 and M5 opportunities. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this White Paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review instrumentation and mission profiles. publishersversion published
Published: 2021

42. The radiation environment observed by Liulin-Photo and R3D-B3 spectrum-dosimeters inside and outside Foton-M3 spacecraft

Author: Damasso, Mario, Dachev, Tsvetan, Falzetta, Giuseppe, Giardi, Maria Teresa, Rea, Giuseppina, and Zanini, Alba
Published: 2009
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43. The gaia survey contribution to EChO target selection and characterization

Author: Sozzetti, Alessandro, primary and Damasso, Mario, additional
Published: 2014
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44. Faint objects in motion: the new frontier of high precision astrometry

Author: Malbet, Fabien, primary, Boehm, Céline, additional, Krone-Martins, Alberto, additional, Amorim, Antonio, additional, Anglada-Escudé, Guillem, additional, Brandeker, Alexis, additional, Courbin, Frédéric, additional, Enßlin, Torsten, additional, Falcão, Antonio, additional, Freese, Katherine, additional, Holl, Berry, additional, Labadie, Lucas, additional, Léger, Alain, additional, Mamon, Gary A., additional, McArthur, Barbara, additional, Mora, Alcione, additional, Shao, Mike, additional, Sozzetti, Alessandro, additional, Spolyar, Douglas, additional, Villaver, Eva, additional, Abbas, Ummi, additional, Albertus, Conrado, additional, Alves, João, additional, Barnes, Rory, additional, Bonomo, Aldo Stefano, additional, Bouy, Hervé, additional, Brown, Warren R., additional, Cardoso, Vitor, additional, Castellani, Marco, additional, Chemin, Laurent, additional, Clark, Hamish, additional, Correia, Alexandre C. M., additional, Crosta, Mariateresa, additional, Crouzier, Antoine, additional, Damasso, Mario, additional, Darling, Jeremy, additional, Davies, Melvyn B., additional, Diaferio, Antonaldo, additional, Fortin, Morgane, additional, Fridlund, Malcolm, additional, Gai, Mario, additional, Garcia, Paulo, additional, Gnedin, Oleg, additional, Goobar, Ariel, additional, Gordo, Paulo, additional, Goullioud, Renaud, additional, Hall, David, additional, Hambly, Nigel, additional, Harrison, Diana, additional, Hobbs, David, additional, Holland, Andrew, additional, Høg, Erik, additional, Jordi, Carme, additional, Klioner, Sergei, additional, Lançon, Ariane, additional, Laskar, Jacques, additional, Lattanzi, Mario, additional, Le Poncin-Lafitte, Christophe, additional, Luri, Xavier, additional, Michalik, Daniel, additional, de Almeida, André Moitinho, additional, Mourão, Ana, additional, Moustakas, Leonidas, additional, Murray, Neil J., additional, Muterspaugh, Matthew, additional, Oertel, Micaela, additional, Ostorero, Luisa, additional, Portell, Jordi, additional, Prost, Jean-Pierre, additional, Quirrenbach, Andreas, additional, Schneider, Jean, additional, Scott, Pat, additional, Siebert, Arnaud, additional, Silva, Antonio da, additional, Silva, Manuel, additional, Thébault, Philippe, additional, Tomsick, John, additional, Traub, Wesley, additional, de Val-Borro, Miguel, additional, Valluri, Monica, additional, Walton, Nicholas A., additional, Watkins, Laura L., additional, White, Glenn, additional, Wyrzykowski, Lukasz, additional, Wyse, Rosemary, additional, and Yamada, Yoshiyuki, additional
Published: 2021
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45. 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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46. Faint objects in motion:the new frontier of high precision astrometry

Author: Malbet, Fabien, Boehm, Celine, Krone-Martins, Alberto, Amorim, Antonio, Anglada-Escude, Guillem, Brandeker, Alexis, Courbin, Frederic, Ensslin, Torsten, Falcao, Antonio, Freese, Katherine, Holl, Berry, Labadie, Lucas, Leger, Alain, Mamon, Gary A., McArthur, Barbara, Mora, Alcione, Shao, Mike, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Abbas, Ummi, Albertus, Conrado, Alves, Joao, Barnes, Rory, Bonomo, Aldo Stefano, Bouy, Herve, Brown, Warren R., Cardoso, Vitor, Castellani, Marco, Chemin, Laurent, Clark, Hamish, Correia, Alexandre C. M., Crosta, Mariateresa, Crouzier, Antoine, Damasso, Mario, Darling, Jeremy, Davies, Melvyn B., Diaferio, Antonaldo, Fortin, Morgane, Fridlund, Malcolm, Gai, Mario, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hall, David, Hambly, Nigel, Harrison, Diana, Hobbs, David, Holland, Andrew, Hog, Erik, Jordi, Carme, Klioner, Sergei, Lancon, Ariane, Laskar, Jacques, Lattanzi, Mario, Le Poncin-Lafitte, Christophe, Luri, Xavier, Michalik, Daniel, de Almeida, Andre Moitinho, Mourao, Ana, Moustakas, Leonidas, Murray, Neil J., Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Portell, Jordi, Prost, Jean-Pierre, Quirrenbach, Andreas, Schneider, Jean, Scott, Pat, Siebert, Arnaud, da Silva, Antonio, Silva, Manuel, Thebault, Philippe, Tomsick, John, Traub, Wesley, de Val-Borro, Miguel, Valluri, Monica, Walton, Nicholas A., Watkins, Laura L., White, Glenn, Wyrzykowski, Lukasz, Wyse, Rosemary, Yamada, Yoshiyuki, Malbet, Fabien, Boehm, Celine, Krone-Martins, Alberto, Amorim, Antonio, Anglada-Escude, Guillem, Brandeker, Alexis, Courbin, Frederic, Ensslin, Torsten, Falcao, Antonio, Freese, Katherine, Holl, Berry, Labadie, Lucas, Leger, Alain, Mamon, Gary A., McArthur, Barbara, Mora, Alcione, Shao, Mike, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Abbas, Ummi, Albertus, Conrado, Alves, Joao, Barnes, Rory, Bonomo, Aldo Stefano, Bouy, Herve, Brown, Warren R., Cardoso, Vitor, Castellani, Marco, Chemin, Laurent, Clark, Hamish, Correia, Alexandre C. M., Crosta, Mariateresa, Crouzier, Antoine, Damasso, Mario, Darling, Jeremy, Davies, Melvyn B., Diaferio, Antonaldo, Fortin, Morgane, Fridlund, Malcolm, Gai, Mario, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hall, David, Hambly, Nigel, Harrison, Diana, Hobbs, David, Holland, Andrew, Hog, Erik, Jordi, Carme, Klioner, Sergei, Lancon, Ariane, Laskar, Jacques, Lattanzi, Mario, Le Poncin-Lafitte, Christophe, Luri, Xavier, Michalik, Daniel, de Almeida, Andre Moitinho, Mourao, Ana, Moustakas, Leonidas, Murray, Neil J., Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Portell, Jordi, Prost, Jean-Pierre, Quirrenbach, Andreas, Schneider, Jean, Scott, Pat, Siebert, Arnaud, da Silva, Antonio, Silva, Manuel, Thebault, Philippe, Tomsick, John, Traub, Wesley, de Val-Borro, Miguel, Valluri, Monica, Walton, Nicholas A., Watkins, Laura L., White, Glenn, Wyrzykowski, Lukasz, Wyse, Rosemary, and Yamada, Yoshiyuki
Abstract: Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of Earth-mass habitable worlds around the nearest stars, to distant Milky Way objects, and out to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local Universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry missions: NEAT proposed for the ESA M3 opportunity, micro-NEAT for the S1 opportunity, and Theia for the M4 and M5 opportunities. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this White Paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review instrumentation and mission profiles.
Published: 2021

47. An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Author: Massachusetts Institute of Technology. Department of Physics, Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Crossfield, Ian Jm, Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris, Massachusetts Institute of Technology. Department of Physics, Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Crossfield, Ian Jm, Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris
Abstract: Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios., United States. National Aeronautics and Space Administration (Grant NNX15AC90G), United States. National Aeronautics and Space Administration (Grant NNX17AB59G)
Published: 2021

48. PyExoRaMa: An Interactive Tool in Python to Investigate the Radius–Mass Diagram for Exoplanets

Author: Amadori Francesco, Damasso Mario, Zeng Li, and Sozzetti Alessandro
Subjects: Astrophysics::Earth and Planetary Astrophysics, General Medicine
Abstract: We present the python version of the software originally developed with Mathematica by Zeng et al. The code represents a useful tool for visualizing and manipulating data related to extrasolar planets and their host stars in a multi-dimensional parameter space. Its versatility enables statistical studies based on the large and constantly increasing number of detected exoplanets. It can be used to identify possible interdependence among several physical parameters, and to compare observables with theoretical models describing the exoplanet composition and structure. Our transposition to python presents some new features with respect to the original version, and due to the popularity of this programming language in the astrophysics community, the tool is made accessible to a larger number of users interested in exoplanet studies.
Published: 2022

49. Five carbon- and nitrogen-bearing species in a hot giant planet’s atmosphere

Author: Giacobbe, Paolo, primary, Brogi, Matteo, additional, Gandhi, Siddharth, additional, Cubillos, Patricio E., additional, Bonomo, Aldo S., additional, Sozzetti, Alessandro, additional, Fossati, Luca, additional, Guilluy, Gloria, additional, Carleo, Ilaria, additional, Rainer, Monica, additional, Harutyunyan, Avet, additional, Borsa, Francesco, additional, Pino, Lorenzo, additional, Nascimbeni, Valerio, additional, Benatti, Serena, additional, Biazzo, Katia, additional, Bignamini, Andrea, additional, Chubb, Katy L., additional, Claudi, Riccardo, additional, Cosentino, Rosario, additional, Covino, Elvira, additional, Damasso, Mario, additional, Desidera, Silvano, additional, Fiorenzano, Aldo F. M., additional, Ghedina, Adriano, additional, Lanza, Antonino F., additional, Leto, Giuseppe, additional, Maggio, Antonio, additional, Malavolta, Luca, additional, Maldonado, Jesus, additional, Micela, Giuseppina, additional, Molinari, Emilio, additional, Pagano, Isabella, additional, Pedani, Marco, additional, Piotto, Giampaolo, additional, Poretti, Ennio, additional, Scandariato, Gaetano, additional, Yurchenko, Sergei N., additional, Fantinel, Daniela, additional, Galli, Alberto, additional, Lodi, Marcello, additional, Sanna, Nicoletta, additional, and Tozzi, Andrea, additional
Published: 2021
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50. Erratum: 'An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star' (2019, AJ, 158, 165)

Author: Mayo, Andrew W., Rajpaul, Vinesh M., Buchhave, Lars A., Dressing, Courtney D., Mortier, Annelies, Zeng, Li, Fortenbach, Charles D., Aigrain, Suzanne, Bonomo, Aldo S., Cameron, Andrew Collier, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martinez, Haywood, Raphaëlle D., Latham, David W., López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Rice, Ken, Sozzetti, Alessandro, Udry, Stephane, Mayo, Andrew W., Rajpaul, Vinesh M., Buchhave, Lars A., Dressing, Courtney D., Mortier, Annelies, Zeng, Li, Fortenbach, Charles D., Aigrain, Suzanne, Bonomo, Aldo S., Cameron, Andrew Collier, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martinez, Haywood, Raphaëlle D., Latham, David W., López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Rice, Ken, Sozzetti, Alessandro, and Udry, Stephane
Abstract: The semimajor axis and planet insolation flux of Kepler-538b were incorrectly calculated in the published article. This error did not impact any other parameters or any other results in the paper. Table 2 has been included in full here with the corrected semimajor axis and planet insolation flux values.
Published: 2020

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