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1. Synergies between Roman Galactic Plane Survey and other major surveys

Author: Kruszyńska, Katarzyna, Street, Rachel A., Gough-Kelly, Steven, Bonito, Rosaria, Prisinzano, Loredana, Trivedi, Oem, Gandhi, Poshak, Hundertmark, Markus, Tsapras, Yiannis, Di Criscienzo, Marcella, Musella, Ilaria, Dall'Ora, Massimo, Bachelet, Etienne, Abrams, Natasha S., Khakpash, Somayeh, Rabus, Markus, Szkody, Paula, and Holt, Carrie
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Nancy Grace Roman Space Telescope will revolutionize our understanding of the Galactic Bulge with its Galactic Bulge Time Domain survey. At the same time, Rubin Observatories's Legacy Survey of Space and Time (LSST) will monitor billions of stars in the Milky Way. The proposed Roman survey of the Galactic Plane, with its NIR passbands and exquisite spacial resolution, promises groundbreaking insights for a wide range of time-domain galactic astrophysics. In this white paper, we describe the scientific returns possible from the combination of the Roman Galactic Plane Survey with the data from LSST., Comment: 8 pages, 1 figure, submitted to the 2024 Call for Community Input into the Definition of a Roman Galactic Plane Survey
Published: 2024

2. The PLATO Mission

Author: Rauer, Heike, Aerts, Conny, Cabrera, Juan, Deleuil, Magali, Erikson, Anders, Gizon, Laurent, Goupil, Mariejo, Heras, Ana, Lorenzo-Alvarez, Jose, Marliani, Filippo, Martin-Garcia, César, Mas-Hesse, J. Miguel, O'Rourke, Laurence, Osborn, Hugh, Pagano, Isabella, Piotto, Giampaolo, Pollacco, Don, Ragazzoni, Roberto, Ramsay, Gavin, Udry, Stéphane, Appourchaux, Thierry, Benz, Willy, Brandeker, Alexis, Güdel, Manuel, Janot-Pacheco, Eduardo, Kabath, Petr, Kjeldsen, Hans, Min, Michiel, Santos, Nuno, Smith, Alan, Suarez, Juan-Carlos, Werner, Stephanie C., Aboudan, Alessio, Abreu, Manuel, a, Lorena Acu, Adams, Moritz, Adibekyan, Vardan, Affer, Laura, Agneray, François, Agnor, Craig, Børsen-Koch, Victor Aguirre, Ahmed, Saad, Aigrain, Suzanne, Al-Bahlawan, Ashraf, Gil, M de los Angeles Alcacera, Alei, Eleonora, Alencar, Silvia, Alexander, Richard, Alfonso-Garzón, Julia, Alibert, Yann, Prieto, Carlos Allende, Almeida, Leonardo, Sobrino, Roi Alonso, Altavilla, Giuseppe, Althaus, Christian, Trujillo, Luis Alonso Alvarez, Amarsi, Anish, Eiff, Matthias Ammler-von, Amôres, Eduardo, Andrade, Laerte, Antoniadis-Karnavas, Alexandros, António, Carlos, del Moral, Beatriz Aparicio, Appolloni, Matteo, Arena, Claudio, Armstrong, David, Aliaga, Jose Aroca, Asplund, Martin, Audenaert, Jeroen, Auricchio, Natalia, Avelino, Pedro, Baeke, Ann, Baillié, Kevin, Balado, Ana, Balagueró, Pau Ballber, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebasti Barceló, Barker, Adrian, Barklem, Paul, Barnes, Sydney, Navascues, David Barrado, Barragan, Oscar, Baruteau, Clément, Basu, Sarbani, Baudin, Frederic, Baumeister, Philipp, Bayliss, Daniel, Bazot, Michael, Beck, Paul G., Bedding, Tim, Belkacem, Kevin, Bellinger, Earl, Benatti, Serena, Benomar, Othman, Bérard, Diane, Bergemann, Maria, Bergomi, Maria, Bernardo, Pierre, Biazzo, Katia, Bignamini, Andrea, Bigot, Lionel, Billot, Nicolas, Binet, Martin, Biondi, David, Biondi, Federico, Birch, Aaron C., Bitsch, Bertram, Ceballos, Paz Victoria Bluhm, Bódi, Attila, Bognár, Zsófia, Boisse, Isabelle, Bolmont, Emeline, Bonanno, Alfio, Bonavita, Mariangela, Bonfanti, Andrea, Bonfils, Xavier, Bonito, Rosaria, Bonomo, Aldo Stefano, Börner, Anko, Saikia, Sudeshna Boro, Martín, Elisa Borreguero, Borsa, Francesco, Borsato, Luca, Bossini, Diego, Bouchy, Francois, Boué, Gwenaël, Boufleur, Rodrigo, Boumier, Patrick, Bourrier, Vincent, Bowman, Dominic M., Bozzo, Enrico, Bradley, Louisa, Bray, John, Bressan, Alessandro, Breton, Sylvain, Brienza, Daniele, Brito, Ana, Brogi, Matteo, Brown, Beverly, Brown, David J. A., Brun, Allan Sacha, Bruno, Giovanni, Bruns, Michael, Buchhave, Lars A., Bugnet, Lisa, Buldgen, Gaël, Burgess, Patrick, Busatta, Andrea, Busso, Giorgia, Buzasi, Derek, Caballero, José A., Cabral, Alexandre, Gomez, Juan-Francisco Cabrero, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, Gestal, Néstor Campos, Martins, Bruno Leonardo Canto, Cara, Christophe, Carone, Ludmila, Carrasco, Josep Manel, Casagrande, Luca, Casewell, Sarah L., Cassisi, Santi, Castellani, Marco, Castro, Matthieu, Catala, Claude, Fernández, Irene Catalán, Catelan, Márcio, Cegla, Heather, Cerruti, Chiara, Cessa, Virginie, Chadid, Merieme, Chaplin, William, Charpinet, Stephane, Chiappini, Cristina, Chiarucci, Simone, Chiavassa, Andrea, Chinellato, Simonetta, Chirulli, Giovanni, Christensen-Dalsgaard, Jørgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, García, Fernando Conde, Conseil, Simon, Corbard, Thierry, Correia, Alexandre C. M., Corsaro, Enrico, Cosentino, Rosario, Costes, Jean, Cottinelli, Andrea, Covone, Giovanni, Creevey, Orlagh L., Crida, Aurelien, Csizmadia, Szilard, Cunha, Margarida, Curry, Patrick, da Costa, Jefferson, da Silva, Francys, Dalal, Shweta, Damasso, Mario, Damiani, Cilia, Damiani, Francesco, Chagas, Maria Liduina das, Davies, Melvyn, Davies, Guy, Davies, Ben, Davison, Gary, de Almeida, Leandro, de Angeli, Francesca, de Barros, Susana Cristina Cabral, Leão, Izan de Castro, de Freitas, Daniel Brito, de Freitas, Marcia Cristina, De Martino, Domitilla, de Medeiros, José Renan, de Paula, Luiz Alberto, Gómez, Álvaro de Pedraza, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Innocenti, Scilla Degl, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, Desert, Jean-Michel, Desidera, Silvano, Dexet, Marc, Di Criscienzo, Marcella, Di Giorgio, Anna Maria, Di Mauro, Maria Pia, Rial, Federico Jose Diaz, Díaz-García, José-Javier, Dima, Marco, Dinuzzi, Giacomo, Dionatos, Odysseas, Distefano, Elisa, Nascimento Jr., Jose-Dias do, Domingo, Albert, D'Orazi, Valentina, Dorn, Caroline, Doyle, Lauren, Duarte, Elena, Ducellier, Florent, Dumaye, Luc, Dumusque, Xavier, Dupret, Marc-Antoine, Eggenberger, Patrick, Ehrenreich, David, Eigmüller, Philipp, Eising, Johannes, Emilio, Marcelo, Eriksson, Kjell, Ermocida, Marco, Giribaldi, Riano Isidoro Escate, Eschen, Yoshi, ez, Lucía Espinosa Yá, Estrela, In s, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, Fernández, Miguel, Ferrari, Lorenza, Ferraz-Mello, Sylvio, Fialho, Fabio, Fienga, Agnes, Figueira, Pedro, Fiori, Laura, Flaccomio, Ettore, Focardi, Mauro, Foley, Steve, Fontignie, Jean, Ford, Dominic, Fornazier, Karin, Forveille, Thierry, Fossati, Luca, Franca, Rodrigo de Marca, da Silva, Lucas Franco, Frasca, Antonio, Fridlund, Malcolm, Furlan, Marco, Gabler, Sarah-Maria, Gaido, Marco, Gallagher, Andrew, Sempere, Paloma I. Gallego, Galli, Emanuele, García, Rafael A., Hernández, Antonio García, Munoz, Antonio Garcia, García-Vázquez, Hugo, Haba, Rafael Garrido, Gaulme, Patrick, Gauthier, Nicolas, Gehan, Charlotte, Gent, Matthew, Georgieva, Iskra, Ghigo, Mauro, Giana, Edoardo, Gill, Samuel, Girardi, Leo, Winter, Silvia Giuliatti, Giusi, Giovanni, da Silva, João Gomes, Zazo, Luis Jorge Gómez, Gomez-Lopez, Juan Manuel, Hernández, Jonay Isai González, Murillo, Kevin Gonzalez, Melchor, Alejandro Gonzalo, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, bach, Denis Grie, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Lo c, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, Guillot, Tristan, Guiot, Pierre, Guterman, Pascal, Gutiérrez, Antonio, Gutiérrez-Canales, Fernando, Hagelberg, Janis, Haldemann, Jonas, Hall, Cassandra, Handberg, Rasmus, Harrison, Ian, Harrison, Diana L., Hasiba, Johann, Haswell, Carole A., Hatalova, Petra, Hatzes, Artie, Haywood, Raphaelle, Hébrard, Guillaume, Heckes, Frank, Heiter, Ulrike, Hekker, Saskia, Heller, René, Helling, Christiane, Helminiak, Krzysztof, Hemsley, Simon, Heng, Kevin, Herbst, Konstantin, Hermans, Aline, Hermes, JJ, Torres, Nadia Hidalgo, Hinkel, Natalie, Hobbs, David, Hodgkin, Simon, Hofmann, Karl, Hojjatpanah, Saeed, Houdek, Günter, Huber, Daniel, Huesler, Joseph, Hui-Bon-Hoa, Alain, Huygen, Rik, Huynh, Duc-Dat, Iro, Nicolas, Irwin, Jonathan, Irwin, Mike, Izidoro, André, Jacquinod, Sophie, Jannsen, Nicholas Emborg, Janson, Markus, Jeszenszky, Harald, Jiang, Chen, Mancebo, Antonio José Jimenez, Jofre, Paula, Johansen, Anders, Johnston, Cole, Jones, Geraint, Kallinger, Thomas, Kálmán, Szilárd, Kanitz, Thomas, Karjalainen, Marie, Karjalainen, Raine, Karoff, Christoffer, Kawaler, Steven, Kawata, Daisuke, Keereman, Arnoud, Keiderling, David, Kennedy, Tom, Kenworthy, Matthew, Kerschbaum, Franz, Kidger, Mark, Kiefer, Flavien, Kintziger, Christian, Kislyakova, Kristina, Kiss, László, Klagyivik, Peter, Klahr, Hubert, Klevas, Jonas, Kochukhov, Oleg, Köhler, Ulrich, Kolb, Ulrich, Koncz, Alexander, Korth, Judith, Kostogryz, Nadiia, Kovács, Gábor, Kovács, József, Kozhura, Oleg, Krivova, Natalie, Kucinskas, Arunas, Kuhlemann, Ilyas, Kupka, Friedrich, Laauwen, Wouter, Labiano, Alvaro, Lagarde, Nadege, Laget, Philippe, Laky, Gunter, Lam, Kristine Wai Fun, Lambrechts, Michiel, Lammer, Helmut, Lanza, Antonino Francesco, Lanzafame, Alessandro, Martiz, Mariel Lares, Laskar, Jacques, Latter, Henrik, Lavanant, Tony, Lawrenson, Alastair, Lazzoni, Cecilia, Lebre, Agnes, Lebreton, Yveline, Etangs, Alain Lecavelier des, Lee, Katherine, Leinhardt, Zoe, Leleu, Adrien, Lendl, Monika, Leto, Giuseppe, Levillain, Yves, Libert, Anne-Sophie, Lichtenberg, Tim, Ligi, Roxanne, Lignieres, Francois, Lillo-Box, Jorge, Linsky, Jeffrey, Liu, John Scige, Loidolt, Dominik, Longval, Yuying, Lopes, Ilídio, Lorenzani, Andrea, Ludwig, Hans-Guenter, Lund, Mikkel, Lundkvist, Mia Sloth, Luri, Xavier, Maceroni, Carla, Madden, Sean, Madhusudhan, Nikku, Maggio, Antonio, Magliano, Christian, Magrin, Demetrio, Mahy, Laurent, Maibaum, Olaf, Malac-Allain, LeeRoy, Malapert, Jean-Christophe, Malavolta, Luca, Maldonado, Jesus, Mamonova, Elena, Manchon, Louis, Manjón, Andres, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, rico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, Vodopivec, Iris Martín, Figueiredo, Ana Carolina Mattiuci, Maxted, Pierre F. L., Mazeh, Tsevi, Mazevet, Stephane, Mazzei, Francesco, McCormac, James, McMillan, Paul, Menou, Lucas, Merle, Thibault, Meru, Farzana, Mesa, Dino, Messina, Sergio, Mészáros, Szabolcs, Meunier, Nadége, Meunier, Jean-Charles, Micela, Giuseppina, Michaelis, Harald, Michel, Eric, Michielsen, Mathias, Michtchenko, Tatiana, Miglio, Andrea, Miguel, Yamila, Milligan, David, Mirouh, Giovanni, Mitchell, Morgan, Moedas, Nuno, Molendini, Francesca, Molnár, László, Mombarg, Joey, Montalban, Josefina, Montalto, Marco, Monteiro, Mário J. P. F. G., Sánchez, Francisco Montoro, Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Beno t, Mourard, Denis, Mousis, Olivier, Moutou, Claire, Mowlavi, Nami, Moya, Andrés, Muehlmann, Prisca, Muirhead, Philip, Munari, Matteo, Musella, Ilaria, Mustill, Alexander James, Nardetto, Nicolas, Nardiello, Domenico, Narita, Norio, Nascimbeni, Valerio, Nash, Anna, Neiner, Coralie, Nelson, Richard P., Nettelmann, Nadine, Nicolini, Gianalfredo, Nielsen, Martin, Niemi, Sami-Matias, Noack, Lena, Noels-Grotsch, Arlette, Noll, Anthony, Norazman, Azib, Norton, Andrew J., Nsamba, Benard, Ofir, Aviv, Ogilvie, Gordon, Olander, Terese, Olivetto, Christian, Olofsson, Göran, Ong, Joel, Ortolani, Sergio, Oshagh, Mahmoudreza, Ottacher, Harald, Ottensamer, Roland, Ouazzani, Rhita-Maria, Paardekooper, Sijme-Jan, Pace, Emanuele, Pajas, Miriam, Palacios, Ana, Palandri, Gaelle, Palle, Enric, Paproth, Carsten, Parro, Vanderlei, Parviainen, Hannu, Granado, Javier Pascual, Passegger, Vera Maria, Pastor-Morales, Carmen, Pätzold, Martin, Pedersen, May Gade, Hidalgo, David Pena, Pepe, Francesco, Pereira, Filipe, Persson, Carina M., Pertenais, Martin, Peter, Gisbert, Petit, Antoine C., Petit, Pascal, Pezzuto, Stefania, Pichierri, Gabriele, Pietrinferni, Adriano, Pinheiro, Fernando, Pinsonneault, Marc, Plachy, Emese, Plasson, Philippe, Plez, Bertrand, Poppenhaeger, Katja, Poretti, Ennio, Portaluri, Elisa, Portell, Jordi, de Mello, Gustavo Frederico Porto, Poyatos, Julien, Pozuelos, Francisco J., Moroni, Pier Giorgio Prada, Pricopi, Dumitru, Prisinzano, Loredana, Quade, Matthias, Quirrenbach, Andreas, Reina, Julio Arturo Rabanal, Soares, Maria Cristina Rabello, Raimondo, Gabriella, Rainer, Monica, Rodón, Jose Ramón, Ramón-Ballesta, Alejandro, Zapata, Gonzalo Ramos, Rätz, Stefanie, Rauterberg, Christoph, Redman, Bob, Redmer, Ronald, Reese, Daniel, Regibo, Sara, Reiners, Ansgar, Reinhold, Timo, Renie, Christian, Ribas, Ignasi, Ribeiro, Sergio, Ricciardi, Thiago Pereira, Rice, Ken, Richard, Olivier, Riello, Marco, Rieutord, Michel, Ripepi, Vincenzo, Rixon, Guy, Rockstein, Steve, Ortiz, José Ramón Rodón, Rodríguez, María Teresa Rodrigo, Amor, Alberto Rodríguez, Díaz, Luisa Fernanda Rodríguez, Garcia, Juan Pablo Rodriguez, Rodriguez-Gomez, Julio, Roehlly, Yannick, Roig, Fernando, Rojas-Ayala, Bárbara, Rolf, Tobias, Rørsted, Jakob Lysgaard, Rosado, Hugo, Rosotti, Giovanni, Roth, Olivier, Roth, Markus, Rousseau, Alex, Roxburgh, Ian, Roy, Fabrice, Royer, Pierre, Ruane, Kirk, Mastropasqua, Sergio Rufini, de Galarreta, Claudia Ruiz, Russi, Andrea, Saar, Steven, Saillenfest, Melaine, Salaris, Maurizio, Salmon, Sebastien, Saltas, Ippocratis, Samadi, Réza, Samadi, Aunia, Samra, Dominic, da Silva, Tiago Sanches, Carrasco, Miguel Andrés Sánchez, Santerne, Alexandre, Pé, Amaia Santiago, Santoli, Francesco, Santos, ngela R. G., Mesa, Rosario Sanz, Sarro, Luis Manuel, Scandariato, Gaetano, Schäfer, Martin, Schlafly, Edward, Schmider, François-Xavier, Schneider, Jean, Schou, Jesper, Schunker, Hannah, Schwarzkopf, Gabriel Jörg, Serenelli, Aldo, Seynaeve, Dries, Shan, Yutong, Shapiro, Alexander, Shipman, Russel, Sicilia, Daniela, sanmartin, Maria Angeles Sierra, Sigot, Axelle, Silliman, Kyle, Silvotti, Roberto, Simon, Attila E., Napoli, Ricardo Simoyama, Skarka, Marek, Smalley, Barry, Smiljanic, Rodolfo, Smit, Samuel, Smith, Alexis, Smith, Leigh, Snellen, Ignas, Sódor, Ádám, Sohl, Frank, Solanki, Sami K., Sortino, Francesca, Sousa, Sérgio, Southworth, John, Souto, Diogo, Sozzetti, Alessandro, Stamatellos, Dimitris, Stassun, Keivan, Steller, Manfred, Stello, Dennis, Stelzer, Beate, Stiebeler, Ulrike, Stokholm, Amalie, Storelvmo, Trude, Strassmeier, Klaus, Strøm, Paul Anthony, Strugarek, Antoine, Sulis, Sophia, vanda, Michal, Szabados, László, Szabó, Róbert, Szabó, Gyula M., Szuszkiewicz, Ewa, Talens, Geert Jan, Teti, Daniele, Theisen, Tom, Thévenin, Frédéric, Thoul, Anne, Tiphene, Didier, Titz-Weider, Ruth, Tkachenko, Andrew, Tomecki, Daniel, Tonfat, Jorge, Tosi, Nicola, Trampedach, Regner, Traven, Gregor, Triaud, Amaury, Trønnes, Reidar, Tsantaki, Maria, Tschentscher, Matthias, Turin, Arnaud, Tvaruzka, Adam, Ulmer, Bernd, Ulmer-Moll, Solène, Ulusoy, Ceren, Umbriaco, Gabriele, Valencia, Diana, Valentini, Marica, Valio, Adriana, Guijarro, Ángel Luis Valverde, Van Eylen, Vincent, Van Grootel, Valerie, van Kempen, Tim A., Van Reeth, Timothy, Van Zelst, Iris, Vandenbussche, Bart, Vasiliou, Konstantinos, Vasilyev, Valeriy, de Mascarenhas, David Vaz, Vazan, Allona, Nunez, Marina Vela, Velloso, Eduardo Nunes, Ventura, Rita, Ventura, Paolo, Venturini, Julia, Trallero, Isabel Vera, Veras, Dimitri, Verdugo, Eva, Verma, Kuldeep, Vibert, Didier, Martinez, Tobias Vicanek, Vida, Krisztián, Vigan, Arthur, Villacorta, Antonio, Villaver, Eva, Aparicio, Marcos Villaverde, Viotto, Valentina, Vorobyov, Eduard, Vorontsov, Sergey, Wagner, Frank W., Walloschek, Thomas, Walton, Nicholas, Walton, Dave, Wang, Haiyang, Waters, Rens, Watson, Christopher, Wedemeyer, Sven, Weeks, Angharad, Weingrill, Jörg, Weiss, Annita, Wendler, Belinda, West, Richard, Westerdorff, Karsten, Westphal, Pierre-Amaury, Wheatley, Peter, White, Tim, Whittaker, Amadou, Wickhusen, Kai, Wilson, Thomas, Windsor, James, Winter, Othon, Winther, Mark Lykke, Winton, Alistair, Witteck, Ulrike, Witzke, Veronika, Woitke, Peter, Wolter, David, Wuchterl, Günther, Wyatt, Mark, Yang, Dan, Yu, Jie, Sanchez, Ricardo Zanmar, Osorio, María Rosa Zapatero, Zechmeister, Mathias, Zhou, Yixiao, Ziemke, Claas, and Zwintz, Konstanze
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.
Published: 2024

3. The Wide-field Spectroscopic Telescope (WST) Science White Paper

Author: Mainieri, Vincenzo, Anderson, Richard I., Brinchmann, Jarle, Cimatti, Andrea, Ellis, Richard S., Hill, Vanessa, Kneib, Jean-Paul, McLeod, Anna F., Opitom, Cyrielle, Roth, Martin M., Sanchez-Saez, Paula, Smiljanic, Rodolfo, Tolstoy, Eline, Bacon, Roland, Randich, Sofia, Adamo, Angela, Annibali, Francesca, Arevalo, Patricia, Audard, Marc, Barsanti, Stefania, Battaglia, Giuseppina, Aran, Amelia M. Bayo, Belfiore, Francesco, Bellazzini, Michele, Bellini, Emilio, Beltran, Maria Teresa, Berni, Leda, Bianchi, Simone, Biazzo, Katia, Bisero, Sofia, Bisogni, Susanna, Bland-Hawthorn, Joss, Blondin, Stephane, Bodensteiner, Julia, Boffin, Henri M. J., Bonito, Rosaria, Bono, Giuseppe, Bouche, Nicolas F., Bowman, Dominic, Braga, Vittorio F., Bragaglia, Angela, Branchesi, Marica, Brucalassi, Anna, Bryant, Julia J., Bryson, Ian, Busa, Innocenza, Camera, Stefano, Carbone, Carmelita, Casali, Giada, Casali, Mark, Casasola, Viviana, Castro, Norberto, Catelan, Marcio, Cavallo, Lorenzo, Chiappini, Cristina, Cioni, Maria-Rosa, Colless, Matthew, Colzi, Laura, Contarini, Sofia, Couch, Warrick, D'Ammando, Filippo, D., William d'Assignies, D'Orazi, Valentina, da Silva, Ronaldo, Dainotti, Maria Giovanna, Damiani, Francesco, Danielski, Camilla, De Cia, Annalisa, de Jong, Roelof S., Dhawan, Suhail, Dierickx, Philippe, Driver, Simon P., Dupletsa, Ulyana, Escoffier, Stephanie, Escorza, Ana, Fabrizio, Michele, Fiorentino, Giuliana, Fontana, Adriano, Fontani, Francesco, Sanchez, Daniel Forero, Franois, Patrick, Galindo-Guil, Francisco Jose, Gallazzi, Anna Rita, Galli, Daniele, Garcia, Miriam, Garcia-Rojas, Jorge, Garilli, Bianca, Grand, Robert, Guarcello, Mario Giuseppe, Hazra, Nandini, Helmi, Amina, Herrero, Artemio, Iglesias, Daniela, Ilic, Dragana, Irsic, Vid, Ivanov, Valentin D., Izzo, Luca, Jablonka, Pascale, Joachimi, Benjamin, Kakkad, Darshan, Kamann, Sebastian, Koposov, Sergey, Kordopatis, Georges, Kovacevic, Andjelka B., Kraljic, Katarina, Kuncarayakti, Hanindyo, Kwon, Yuna, La Forgia, Fiorangela, Lahav, Ofer, Laigle, Clotilde, Lazzarin, Monica, Leaman, Ryan, Leclercq, Floriane, Lee, Khee-Gan, Lee, David, Lehnert, Matt D., Lira, Paulina, Loffredo, Eleonora, Lucatello, Sara, Magrini, Laura, Maguire, Kate, Mahler, Guillaume, Majidi, Fatemeh Zahra, Malavasi, Nicola, Mannucci, Filippo, Marconi, Marcella, Martin, Nicolas, Marulli, Federico, Massari, Davide, Matsuno, Tadafumi, Mattheee, Jorryt, McGee, Sean, Merc, Jaroslav, Merle, Thibault, Miglio, Andrea, Migliorini, Alessandra, Minchev, Ivan, Minniti, Dante, Miret-Roig, Nuria, Ibero, Ana Monreal, Montano, Federico, Montet, Ben T., Moresco, Michele, Moretti, Chiara, Moscardini, Lauro, Moya, Andres, Mueller, Oliver, Nanayakkara, Themiya, Nicholl, Matt, Nordlander, Thomas, Onori, Francesca, Padovani, Marco, Pala, Anna Francesca, Panda, Swayamtrupta, Pandey-Pommier, Mamta, Pasquini, Luca, Pawlak, Michal, Pessi, Priscila J., Pisani, Alice, Popovic, Lukav C., Prisinzano, Loredana, Raddi, Roberto, Rainer, Monica, Rebassa-Mansergas, Alberto, Richard, Johan, Rigault, Mickael, Rocher, Antoine, Romano, Donatella, Rosati, Piero, Sacco, Germano, Sanchez-Janssen, Ruben, Sander, Andreas A. C., Sanders, Jason L., Sargent, Mark, Sarpa, Elena, Schimd, Carlo, Schipani, Pietro, Sefusatti, Emiliano, Smith, Graham P., Spina, Lorenzo, Steinmetz, Matthias, Tacchella, Sandro, Tautvaisiene, Grazina, Theissen, Christopher, Thomas, Guillaume, Ting, Yuan-Sen, Travouillon, Tony, Tresse, Laurence, Trivedi, Oem, Tsantaki, Maria, Tsedrik, Maria, Urrutia, Tanya, Valenti, Elena, Van der Swaelmen, Mathieu, Van Eck, Sophie, Verdiani, Francesco, Verdier, Aurelien, Vergani, Susanna Diana, Verhamme, Anne, Vernet, Joel, Verza, Giovanni, Viel, Matteo, Vielzeuf, Pauline, Vietri, Giustina, Vink, Jorick S., Vazquez, Carlos Viscasillas, Wang, Hai-Feng, Weilbacher, Peter M., Wendt, Martin, Wright, Nicholas, Ye, Quanzhi, Yeche, Christophe, Yu, Jiaxi, Zafar, Tayyaba, Zibetti, Stefano, Ziegler, Bodo, and Zinchenko, Igor
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The Wide-field Spectroscopic Telescope (WST) is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys. This white paper summarises the initial concept as well as the corresponding science cases. WST will feature simultaneous operation of a large field-of-view (3 sq. degree), a high multiplex (20,000) multi-object spectrograph (MOS) and a giant 3x3 sq. arcmin integral field spectrograph (IFS). In scientific capability these requirements place WST far ahead of existing and planned facilities. Given the current investment in deep imaging surveys and noting the diagnostic power of spectroscopy, WST will fill a crucial gap in astronomical capability and work synergistically with future ground and space-based facilities. This white paper shows that WST can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; origin of stars and planets; time domain and multi-messenger astrophysics. WST's uniquely rich dataset will deliver unforeseen discoveries in many of these areas. The WST Science Team (already including more than 500 scientists worldwide) is open to the all astronomical community. To register in the WST Science Team please visit https://www.wstelescope.com/for-scientists/participate, Comment: 194 pages, 66 figures. Comments are welcome (wstelescope@gmail.com)
Published: 2024

4. An Evenly-Spaced LSST Cadence for Rapidly Variable Stars

Author: Feigelson, Eric D., Bianco, Federica B., and Bonito, Rosaria
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Stars exhibit a bewildering variety of rapidly variable behaviors ranging from explosive magnetic flares to stochastically changing accretion to periodic pulsations or rotation. The principal Rubin Observatory Legacy Survey of Space and Time (LSST) surveys will have cadences too sparse and irregular to capture many of these phenomena. We propose here a LSST micro-survey to observe a single Galactic field, rich in unobscured stars, in a continuous sequence of 30 second exposures for one long winter night in a single photometric band. The result will be a unique dataset of $\sim 1$ million regularly spaced stellar light curves (LCs). The LCs will constitute a comprehensive collection of late-type stellar flaring, but also other classes like short-period binary systems and cataclysmic variables, young stellar objects and ultra-short period exoplanets. An unknown variety of anomalous Solar System, Galactic and extragalactic variables and transients may also be present. A powerful array of statistical procedures can be applied to individual LCs from the long-standing fields of time series analysis, signal processing and econometrics. Dozens of `features' describing the variability can be extracted and the ensemble of light curves can be subject to advanced machine learning clustering procedures. This will give a unique, authoritative, objective taxonomy of the rapidly variable sky derived from identically cadenced LCs. This micro-survey is best performed early in the Rubin Observatory program, and the results can inform the wider community on the best approaches to variable star identification and classification from the sparse, irregular cadences that dominate the planned surveys., Comment: Accepted for publication in Astrophysical Journal Supplements. 11 pages
Published: 2023

5. Anti-Black Racism Workshop during the Vera C. Rubin Observatory Virtual 2021 Project and Community Workshop

Author: Plazas Malagón, Andrés A, primary, Bianco, Federica, additional, Gill, Ranpal, additional, Blum, Robert D, additional, Bonito, Rosaria (Sara), additional, O’Mullane, Wil, additional, Shugart, Alsyha, additional, Street, Rachel, additional, and Verma, Aprajita, additional
Published: 2024
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6. Rubin Observatory LSST Transients and Variable Stars Roadmap

Author: Hambleton, Kelly M., Bianco, Federica B., Street, Rachel, Bell, Keaton, Buckley, David, Graham, Melissa, Hernitschek, Nina, Lund, Michael B., Mason, Elena, Pepper, Joshua, Prsa, Andrej, Rabus, Markus, Raiteri, Claudia M., Szabo, Robert, Szkody, Paula, Andreoni, Igor, Antoniucci, Simone, Balmaverde, Barbara, Bellm, Eric, Bonito, Rosaria, Bono, Giuseppe, Botticella, Maria Teresa, Brocato, Enzo, Bricman, Katja Bucar, Cappellaro, Enrico, Carnerero, Maria Isabel, Chornock, Ryan, Clarke, Riley, Cowperthwaite, Phil, Cucchiara, Antonino, D'Ammando, Filippo, Dage, Kristen C., Dall'Ora, Massimo, Davenport, James R. A., de Martino, Domitilla, de Somma, Giulia, Di Criscienzo, Marcella, Di Stefano, Rosanne, Drout, Maria, Fabrizio, Michele, Fiorentino, Giuliana, Gandhi, Poshak, Garofalo, Alessia, Giannini, Teresa, Gomboc, Andreja, Greggio, Laura, Hartigan, Patrick, Hundertmark, Markus, Johnson, Elizabeth, Johnson, Michael, Jurkic, Tomislav, Khakpash, Somayeh, Leccia, Silvio, Li, Xiaolong, Magurno, Davide, Malanchev, Konstantin, Marconi, Marcella, Margutti, Raffaella, Marinoni, Silvia, Mauron, Nicolas, Molinaro, Roberto, Moller, Anais, Moniez, Marc, Muraveva, Tatiana, Musella, Ilaria, Ngeow, Chow-Choong, Pastorello, Andrea, Petrecca, Vincenzo, Piranomonte, Silvia, Ragosta, Fabio, Reguitti, Andrea, Righi, Chiara, Ripepi, Vincenzo, Sandoval, Liliana Rivera, Stassun, Keivan G., Stroh, Michael, Terreran, Giacomo, Trimble, Virginia, Tsapras, Yiannis, van Velzen, Sjoert, Venuti, Laura, and Vink, Jorick S.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: The Vera C. Rubin Legacy Survey of Space and Time holds the potential to revolutionize time domain astrophysics, reaching completely unexplored areas of the Universe and mapping variability time scales from minutes to a decade. To prepare to maximize the potential of the Rubin LSST data for the exploration of the transient and variable Universe, one of the four pillars of Rubin LSST science, the Transient and Variable Stars Science Collaboration, one of the eight Rubin LSST Science Collaborations, has identified research areas of interest and requirements, and paths to enable them. While our roadmap is ever-evolving, this document represents a snapshot of our plans and preparatory work in the final years and months leading up to the survey's first light., Comment: 202 pages (in book format) 34 figures plus chapter heading figures (13)
Published: 2022

7. From Data to Software to Science with the Rubin Observatory LSST

Author: Breivik, Katelyn, Connolly, Andrew J., Ford, K. E. Saavik, Jurić, Mario, Mandelbaum, Rachel, Miller, Adam A., Norman, Dara, Olsen, Knut, O'Mullane, William, Price-Whelan, Adrian, Sacco, Timothy, Sokoloski, J. L., Villar, Ashley, Acquaviva, Viviana, Ahumada, Tomas, AlSayyad, Yusra, Alves, Catarina S., Andreoni, Igor, Anguita, Timo, Best, Henry J., Bianco, Federica B., Bonito, Rosaria, Bradshaw, Andrew, Burke, Colin J., de Campos, Andresa Rodrigues, Cantiello, Matteo, Caplar, Neven, Chandler, Colin Orion, Chan, James, da Costa, Luiz Nicolaci, Danieli, Shany, Davenport, James R. A., Fabbian, Giulio, Fagin, Joshua, Gagliano, Alexander, Gall, Christa, Camargo, Nicolás Garavito, Gawiser, Eric, Gezari, Suvi, Gomboc, Andreja, Gonzalez-Morales, Alma X., Graham, Matthew J., Gschwend, Julia, Guy, Leanne P., Holman, Matthew J., Hsieh, Henry H., Hundertmark, Markus, Ilić, Dragana, Ishida, Emille E. O., Jurkić, Tomislav, Kannawadi, Arun, Kosakowski, Alekzander, Kovačević, Andjelka B., Kubica, Jeremy, Lanusse, François, Lazar, Ilin, Levine, W. Garrett, Li, Xiaolong, Lu, Jing, Luna, Gerardo Juan Manuel, Mahabal, Ashish A., Malz, Alex I., Mao, Yao-Yuan, Medan, Ilija, Moeyens, Joachim, Nikolić, Mladen, Nikutta, Robert, O'Dowd, Matt, Olsen, Charlotte, Pearson, Sarah, Pedraza, Ilhuiyolitzin Villicana, Popinchalk, Mark, Popović, Luka C., Pritchard, Tyler A., Quint, Bruno C., Radović, Viktor, Ragosta, Fabio, Riccio, Gabriele, Riley, Alexander H., Rożek, Agata, Sánchez-Sáez, Paula, Sarro, Luis M., Saunders, Clare, Savić, Đorđe V., Schmidt, Samuel, Scott, Adam, Shirley, Raphael, Smotherman, Hayden R., Stetzler, Steven, Storey-Fisher, Kate, Street, Rachel A., Trilling, David E., Tsapras, Yiannis, Ustamujic, Sabina, van Velzen, Sjoert, Vázquez-Mata, José Antonio, Venuti, Laura, Wyatt, Samuel, Yu, Weixiang, and Zabludoff, Ann
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) dataset will dramatically alter our understanding of the Universe, from the origins of the Solar System to the nature of dark matter and dark energy. Much of this research will depend on the existence of robust, tested, and scalable algorithms, software, and services. Identifying and developing such tools ahead of time has the potential to significantly accelerate the delivery of early science from LSST. Developing these collaboratively, and making them broadly available, can enable more inclusive and equitable collaboration on LSST science. To facilitate such opportunities, a community workshop entitled "From Data to Software to Science with the Rubin Observatory LSST" was organized by the LSST Interdisciplinary Network for Collaboration and Computing (LINCC) and partners, and held at the Flatiron Institute in New York, March 28-30th 2022. The workshop included over 50 in-person attendees invited from over 300 applications. It identified seven key software areas of need: (i) scalable cross-matching and distributed joining of catalogs, (ii) robust photometric redshift determination, (iii) software for determination of selection functions, (iv) frameworks for scalable time-series analyses, (v) services for image access and reprocessing at scale, (vi) object image access (cutouts) and analysis at scale, and (vii) scalable job execution systems. This white paper summarizes the discussions of this workshop. It considers the motivating science use cases, identified cross-cutting algorithms, software, and services, their high-level technical specifications, and the principles of inclusive collaborations needed to develop them. We provide it as a useful roadmap of needs, as well as to spur action and collaboration between groups and individuals looking to develop reusable software for early LSST science., Comment: White paper from "From Data to Software to Science with the Rubin Observatory LSST" workshop
Published: 2022

8. Give Me a Few Hours: Exploring Short Timescales in Rubin Observatory Cadence Simulations

Author: Bellm, Eric C., Burke, Colin J., Coughlin, Michael W., Andreoni, Igor, Raiteri, Claudia M., and Bonito, Rosaria
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The limiting temporal resolution of a time-domain survey in detecting transient behavior is set by the time between observations of the same sky area. We analyze the distribution of visit separations for a range of Vera C. Rubin Observatory cadence simulations. Current simulations are strongly peaked at the 22 minute visit pair separation and provide effectively no constraint on temporal evolution within the night. This choice will necessarily prevent Rubin from discovering a wide range of astrophysical phenomena in time to trigger rapid followup. We present a science-agnostic metric to supplement detailed simulations of fast-evolving transients and variables and suggest potential approaches for improving the range of timescales explored., Comment: 7 pages, 2 figures. Submitted to the ApJS Rubin Cadence Focus Issue
Published: 2021
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9. Effects of Radiation in Accretion Regions of Classical T Tauri Stars: Pre-heating of accretion column in non-LTE regime

Author: Colombo, Salvatore, Ibgui, Laurent, Orlando, Salvatore, Rodriguez, Rafael, Espinosa, Guadalupe, González, Matthias, Stehlé, Chantal, de Sá, Lionel, Argiroffi, Costanza, Bonito, Rosaria, and Peres, Giovanni
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Models and observations indicate that the impact of matter accreting onto the surface of young stars produces regions at the base of accretion columns, in which optically thin and thick plasma components coexist. Thus an accurate description of these impacts requires to account for the effects of absorption and emission of radiation. We study the effects of radiation emerging from shock-heated plasma in impact regions on the structure of the pre-shock downfalling material. We investigate if a significant absorption of radiation occurs and if it leads to a pre-shock heating of the accreting gas. We developed a radiation hydrodynamics model describing an accretion column impacting onto the surface of a Classical T Tauri Star. The model takes into account the stellar gravity, the thermal conduction, and the effects of both radiative losses and absorption of radiation by matter in the non local thermodynamic equilibrium regime. After the impact, a hot slab of post-shock plasma develops at the base of the accretion column. Part of radiation emerging from the slab is absorbed by the pre-shock accreting material. As a result, the pre-shock accretion column gradually heats up to temperatures of $10^5$ K, forming a radiative precursor of the shock. The precursor has a thermal structure with the hottest part at $T \approx 10^5$ K, with size comparable to that of the hot slab, above the post-shock region. At larger distances the temperature gradually decreases to $T \approx 10^4$ K., Comment: Letter Accepted for publication in A&A
Published: 2019
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10. A new view of the corona of classical T Tauri stars: Effects of flaring activity in circumstellar disks

Author: Colombo, Salvatore, Orlando, Salvatore, Peres, Giovanni, Reale, Fabio, Argiroffi, Costanza, Bonito, Rosaria, Ibgui, Laurent, and Stehlé, Chantal
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Classical T Tauri stars (CTTSs) are young low-mass stellar objects accreting mass from their circumstellar disks. They are characterized by high levels of coronal activity as revealed by X-ray observations. This activity may affect the disk stability and the circumstellar environment. Here we investigate if an intense coronal activity due to flares occurring close to the accretion disk may perturb the inner disk stability, disrupt the inner part of the disk and, possibly, trigger accretion phenomena with rates comparable with those observed. We model a magnetized protostar surrounded by an accretion disk through 3D magnetohydrodinamic simulations. We explore cases characterized by a dipole plus an octupole stellar magnetic field configuration and different density of the disk or by different levels of flaring activity. As a result of the simulated intense flaring activity, we observe the formation of several loops that link the star to the disk; all these loops build up a hot extended corona with an X-ray luminosity comparable with typical values observed in CTTSs. The intense flaring activity close to the disk can strongly perturb the disk stability. The flares trigger overpressure waves which travel through the disk and modify its configuration. Accretion funnels may be triggered by the flaring activity, thus contributing to the mass accretion rate of the star. Accretion rates synthesized from the simulations are in a range between 10^-10 and 10^-9M_sun yr^-1 The accretion columns can be perturbed by the flares and they can interact with each other, possibly merging together in larger streams. As a result, the accretion pattern can be rather complex: the streams are highly inhomogeneous, with a complex density structure, and clumped, Comment: 12 pages, 9 figures
Published: 2019
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11. Young Stars and their Variability with LSST

Author: Bonito, Rosaria, Hartigan, Patrick, Venuti, Laura, Guarcello, Mario, Prisinzano, Loredana, Argiroffi, Costanza, Messina, Sergio, Johns-Krull, Christopher, Feigelson, Eric, Stauffer, John, Giannini, Teresa, Antoniucci, Simone, Sciortino, Salvo, Micela, Giusi, Pillitteri, Ignazio, Fedele, Davide, Podio, Linda, Damiani, Francesco, McGehee, Peregrine, Street, Rachel, Gizis, John, Sacco, Germano, Magrini, Laura, Flaccomio, Ettore, Orlando, Salvatore, Miceli, Marco, Stelzer, Beate, Fuchs, Julien, Chen, Sophia, Pikuz, Sergey, Frasca, Antonio, Biazzo, Katia, Codella, Claudio, Pastorello, Andrea, Alcala', Juan Manuel, Covino, Elvira, Bianchi, Eleonora, and Nisini, Brunella
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Young stars exhibit short-term photometric variability caused by mass accretion events from circumstellar disks, the presence of dusty warps within the inner disks, starspots that rotate across the stellar surfaces, and flares. Long-term variability also occurs owing to starspot longevity and cycles, and from changes in stellar angular momenta and activity as the stars age. We propose to observe the Carina star-forming region in different bands with a cadence of 30 minutes every night for one week per year to clarify the nature of both the short-term and long-term variability of the thousands of young stars in this region. By obtaining well-sampled multicolor lightcurves of this dense young cluster, LSST would acquire the first statistically significant data on how these objects vary on both short and long timescales. This information will allow us to relate the observed variability to stellar properties such as mass, age, binarity, and to environmental properties such as location within or exterior to the H II region, and to the presence or absence of a circumstellar disk., Comment: Contribution in response of the Call for White Papers on LSST Cadence Optimization
Published: 2018

12. Modeling the shock-cloud interaction in SN 1006: unveiling the origin of nonthermal X-ray and gamma-ray emission

Author: Miceli, Marco, Orlando, Salvatore, Pereira, Victor, Acero, Fabio, Katsuda, Satoru, Decourchelle, Anne, Winkler, Frank P., Bonito, Rosaria, Reale, Fabio, Peres, Giovanni, Li, Jiangtao, and Dubner, Gloria
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The supernova remnant SN 1006 is a source of high-energy particles and its southwestern limb is interacting with a dense ambient cloud, thus being a promising region for gamma-ray hadronic emission. We aim at describing the physics and the nonthermal emission associated with the shock-cloud interaction to derive the physical parameters of the cloud (poorly constrained by the data analysis), to ascertain the origin of the observed spatial variations in the spectral properties of the X-ray synchrotron emission, and to predict spectral and morphological features of the resulting gamma-ray emission. We performed 3-D magnetohydrodynamic simulations modeling the evolution of SN 1006 and its interaction with the ambient cloud, and explored different model setups. By applying the REMLIGHT code on the model results, we synthesized the synchrotron X-ray emission, and compared it with actual observations, to constrain the parameters of the model. We also synthesized the leptonic and hadronic gamma-ray emission from the models, deriving constraints on the energy content of the hadrons accelerated at the southwestern limb. We found that the impact of the SN 1006 shock front with a uniform cloud with density 0.5 cm^-3 can explain the observed morphology, the azimuthal variations of the cutoff frequency of the X-ray synchrotron emission, and the shock proper motion in the interaction region. Our results show that the current upper limit for the total hadronic energy in the southwestern limb is 2.5e49 erg., Comment: Accepted for publication in A&A
Published: 2016
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13. The Gaia-ESO Survey: Catalogue of H$\alpha$ emission stars

Author: Traven, Gregor, Zwitter, Tomaž, Van Eck, Sophie, Klutsch, Alexis, Bonito, Rosaria, Lanzafame, Alessandro C., Alfaro, Emilio J., Bayo, Amelia, Bragaglia, Angela, Costado, María Teresa, Damiani, Francesco, Flaccomio, Ettore, Frasca, Antonio, Hourihane, Anna, Jimenez-Esteban, Fran, Lardo, Carmela, Morbidelli, Lorenzo, Pancino, Elena, Prisinzano, Loredana, Sacco, Germano G., and Worley, Clare C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We discuss the properties of H$\alpha$ emission stars across the sample of 22035 spectra from the Gaia-ESO Survey internal data release, observed with the GIRAFFE instrument and largely belonging to stars in young open clusters. Automated fits using two independent Gaussian profiles and a third component that accounts for the nebular emission allow us to discern distinct morphological types of H$\alpha$ line profiles with the introduction of a simplified classification scheme. All in all we find 3765 stars with intrinsic emission and sort their spectra into eight distinct morphological categories: single--component emission, emission blend, sharp emission peaks, double emission, P-Cygni, inverted P-Cygni, self--absorption, and emission in absorption. We have more than one observation for 1430 stars in our sample, thus allowing a quantitative discussion of the degree of variability of H$\alpha$ emission profiles, which is expected for young, active objects. We present a catalogue of stars with properties of their H$\alpha$ emission line profiles, morphological classification, analysis of variability with time and the supplementary information from the SIMBAD, VizieR, and ADS databases. The records in SIMBAD indicate the presence of H$\alpha$ emission for roughly 25% of all stars in our catalogue, while at least 305 of them have already been more thoroughly investigated according to the references in ADS. The most frequently identified morphological categories in our sample of spectra are emission blend (23%), emission in absorption (22%), and self--absorption (16%). Objects with repeated observations demonstrate that our classification into discrete categories is generally stable through time, but categories P-Cygni and self--absorption seem less stable, which is the consequence of discrete classification rules, as well as of the fundamental change in profile shape.
Published: 2015
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14. X-ray emission from stellar jets by collision against high-density molecular clouds: an application to HH 248

Author: Lopez-Santiago, Javier, Bonito, Rosaria, Orellana, Mariana, Miceli, Marco, Orlando, Salvatore, Ustamujic, Sabina, Albacete-Colombo, Juan Facundo, de Castro, Elisa, and de Castro, Ana Ines Gomez
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We investigate the plausibility of detecting X-ray emission from a stellar jet that impacts against a dense molecular cloud. This scenario may be usual for classical T Tauri stars with jets in dense star-forming complexes. We first model the impact of a jet against a dense cloud by 2D axisymmetric hydrodynamic simulations, exploring different configurations of the ambient environment. Then, we compare our results with XMM-Newton observations of the Herbig-Haro object HH 248, where extended X-ray emission aligned with the optical knots is detected at the edge of the nearby IC 434 cloud. Our simulations show that a jet can produce plasma with temperatures up to 10 MK, consistent with production of X-ray emission, after impacting a dense cloud. We find that jets denser than the ambient medium but less dense than the cloud produce detectable X-ray emission only at the impact onto the cloud. From the exploration of the model parameter space, we constrain the physical conditions (jet density and velocity, cloud density) that reproduce well the intrinsic luminosity and emission measure of the X-ray source possibly associated with HH 248. Thus, we suggest that the extended X-ray source close to HH 248 corresponds to the jet impacting on a dense cloud., Comment: Accepted for publication in ApJ. (12 pages, 12 figures)
Published: 2015
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15. High Energy Emission from Shocks Due to Jets and Accretion in Young Stars with Disks: Combining Observations, Numerical Models, and Laboratory Experiments

Author: Bonito, Rosaria, Argiroffi, Costanza, Orlando, Salvatore, Miceli, Marco, Fuchs, Julien, Ciardi, Andrea, and Sauty, Christophe, editor
Published: 2019
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16. Pre-main sequence stars older than 8 Myr in the Eagle Nebula

Author: De Marchi, Guido, Panagia, Nino, Guarcello, M. G., and Bonito, Rosaria
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Attention is given to a population of 110 stars in the NGC 6611 cluster of the Eagle Nebula that have prominent near-infrared (NIR) excess and optical colours typical of pre-main sequence (PMS) stars older than 8 Myr. At least half of those for which spectroscopy exists have a Halpha emission line profile revealing active accretion. In principle, the V-I colours of all these stars would be consistent with those of young PMS objects (< 1 Myr) whose radiation is heavily obscured by a circumstellar disc seen at high inclination and in small part scattered towards the observer by the back side of the disc. However, using theoretical models it is shown here that objects of this type can only account for a few percent of this population. In fact, the spatial distribution of these objects, their X-ray luminosities, their optical brightness, their positions in the colour-magnitude diagram and the weak Li absorption lines of the stars studied spectroscopically suggest that most of them are at least 8 times older than the ~1 Myr-old PMS stars already known in this cluster and could be as old as ~30 Myr. This is the largest homogeneous sample to date of Galactic PMS stars considerably older than 8 Myr that are still actively accreting from a circumstellar disc and it allows us to set a lower limit of 7% to the disc frequency at ~16 Myr in NGC 6611. These values imply a characteristic exponential lifetime of ~6 Myr for disc dissipation., Comment: 12 pages, 5 figures, accepted for publication in Monthly Notices of the Astronomical Society
Published: 2013
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17. Generation of radiative knots in a randomly pulsed protostellar jet I. Dynamics and energetics

Author: Bonito, Rosaria, Orlando, Salvatore, Peres, Giovanni, Eislöffel, Jochen, Miceli, Marco, and Favata, Fabio
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: HH objects are characterized by a complex knotty morphology detected mainly along the axis of protostellar jets in a wide range of bands. Evidence of interactions between knots formed in different epochs have been found, suggesting that jets may result from the ejection of plasma blobs from the source. We aim at investigating the physical mechanism leading to the irregular knotty structure observed in jets in different bands and the complex interactions occurring among blobs of plasma ejected from the stellar source. We perform 2D axisymmetric HD simulations of a randomly ejected pulsed jet. The jet consists of a train of blobs which ram with supersonic speed into the ambient medium. The initial random velocity of each blob follows an exponential distribution. We explore the ejection rate parameter to derive constraints on the physical properties of protostellar jets by comparison of model results with observations. Our model takes into account radiative losses and thermal conduction. We find that the mutual interactions of blobs ejected at different epochs and with different speed lead to a variety of plasma components not described by current models. The main features characterizing the random pulsed jet scenario are: single high speed knots, showing a measurable proper motion in nice agreement with observations; irregular chains of knots aligned along the jet axis and possibly interacting with each other; reverse shocks interacting with outgoing knots; oblique shocks produced by the reflection of shocks at the jet cocoon. All these structures concur to determine the morphology of the jet in different bands. We also find that the thermal conduction plays a crucial role in damping out HD instabilities that would develop within the cocoon and that contribute to the jet breaking., Comment: 10 pages, 10 figures, accepted for publication in A&A
Published: 2009
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18. Rubin Observatory LSST Transients and Variable Stars Roadmap

Author: Hambleton, Kelly M., primary, Bianco, Federica B., additional, Street, Rachel, additional, Bell, Keaton, additional, Buckley, David, additional, Graham, Melissa, additional, Hernitschek, Nina, additional, Lund, Michael B., additional, Mason, Elena, additional, Pepper, Joshua, additional, Prša, Andrej, additional, Rabus, Markus, additional, Raiteri, Claudia M., additional, Szabó, Róbert, additional, Szkody, Paula, additional, Andreoni, Igor, additional, Antoniucci, Simone, additional, Balmaverde, Barbara, additional, Bellm, Eric, additional, Bonito, Rosaria, additional, Bono, Giuseppe, additional, Botticella, Maria Teresa, additional, Brocato, Enzo, additional, Bučar Bricman, Katja, additional, Cappellaro, Enrico, additional, Carnerero, Maria Isabel, additional, Chornock, Ryan, additional, Clarke, Riley, additional, Cowperthwaite, Phil, additional, Cucchiara, Antonino, additional, D’Ammando, Filippo, additional, Dage, Kristen C., additional, Dall’Ora, Massimo, additional, Davenport, James R. A., additional, de Martino, Domitilla, additional, de Somma, Giulia, additional, Di Criscienzo, Marcella, additional, Di Stefano, Rosanne, additional, Drout, Maria, additional, Fabrizio, Michele, additional, Fiorentino, Giuliana, additional, Gandhi, Poshak, additional, Garofalo, Alessia, additional, Giannini, Teresa, additional, Gomboc, Andreja, additional, Greggio, Laura, additional, Hartigan, Patrick, additional, Hundertmark, Markus, additional, Johnson, Elizabeth, additional, Johnson, Michael, additional, Jurkic, Tomislav, additional, Khakpash, Somayeh, additional, Leccia, Silvio, additional, Li, Xiaolong, additional, Magurno, Davide, additional, Malanchev, Konstantin, additional, Marconi, Marcella, additional, Margutti, Raffaella, additional, Marinoni, Silvia, additional, Mauron, Nicolas, additional, Molinaro, Roberto, additional, Möller, Anais, additional, Moniez, Marc, additional, Muraveva, Tatiana, additional, Musella, Ilaria, additional, Ngeow, Chow-Choong, additional, Pastorello, Andrea, additional, Petrecca, Vincenzo, additional, Piranomonte, Silvia, additional, Ragosta, Fabio, additional, Reguitti, Andrea, additional, Righi, Chiara, additional, Ripepi, Vincenzo, additional, Rivera Sandoval, Liliana, additional, Stassun, Keivan G., additional, Stroh, Michael, additional, Terreran, Giacomo, additional, Trimble, Virginia, additional, Tsapras, Yiannis, additional, van Velzen, Sjoert, additional, Venuti, Laura, additional, and Vink, Jorick S., additional
Published: 2023
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19. 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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20. An Evenly Spaced LSST Cadence for Rapidly Variable Stars

Author: Feigelson, Eric D., primary, Bianco, Federica B., additional, and Bonito, Rosaria, additional
Published: 2023
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21. Stellar Clusters in 4MOST

Author: Lucatello, Sara, Bragaglia, Angela, Vallenari, Antonella, Cantat-Gaudin, Tristan, Kuzma, Pete, Guarcello, Mario G., Spina, Lorenzo, Aguado, David, Carrera, Ricardo, Castro-Ginard, Alfred, Damiani, Francesco, D’Orazi, Valentina, Prisinzano, Loredana, Valenti, Elena, Alfaro, Emilio, Balaguer-Nuñez, Lola, Balbinot, Eduardo, Barrado, David, Baumgardt, Holger, Bellazzini, Michele, Bonito, Rosaria, Bossini, Diego, Carraro, Giovanni, Carretta, Eugenio, Catanzaro, Giovanni, Casamiquela, Laia, Cassisi, Santi, Dalessandro, Emanuele, De Silva, Gayandhi M., Ferguson, Annette, Ferraro, Francesco R., Frasca, Antonio, Galli, Phillip, Gieles, Mark, Gran, Felipe, Gratton, Raffaele, Hilker, Michael, Jeffries, Rob, Jordi, Carme, Korn, Anreas J., Lanzoni, Barbara, Larsen, Søren, Lattanzio, John, Lugaro, Maria, Mapelli, Michela, Massari, Davide, Miglio, Andrea, Miret-Roig, Nuria, Momany, Yazan, Mucciarelli, Alessio, Olivares, Javier, Pasquato, Mario, Roccatagliata, Veronica, Salaris, Maurizio, Schiavon, Ricardo, Smiljanic, Rodolfo, Sollima, Antonio, Tautvaišienė, Gražina, Varri, Anna Lisa, and Wright, Nicholas
Subjects: Astronomy
Abstract: The 4MOST Stellar Clusters Survey will target essentially all the Galactic globular and open clusters and star-forming regions accessible to 4MOST (about 120 globulars, 1800 open clusters and 80 star-forming regions). This will: shed light on how clusters form, evolve, dissolve, and populate the Milky Way; calibrate complex physics that affects stellar evolution, on which our ability to measure accurate ages ultimately rests; and evaluate the contribution of star clusters to the formation and evolution of the individual Galactic components with unparalleled statistics., Published in The Messenger vol. 190, pp. 13-16, March 2023.
Published: 2023

22. Rubin LSST Observing Strategies to Maximize Volume and Uniformity Coverage of Star-forming Regions in the Galactic Plane

Author: Prisinzano, Loredana, primary, Bonito, Rosaria, additional, Mazzi, Alessandro, additional, Damiani, Francesco, additional, Ustamujic, Sabina, additional, Yoachim, Peter, additional, Street, Rachel, additional, Guarcello, Mario Giuseppe, additional, Venuti, Laura, additional, Clarkson, William, additional, Jones, Lynne, additional, and Girardi, Leo, additional
Published: 2023
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23. The Complex Morphology of the X-ray and Optical Emission from HH 154: The Pulsed Jet Scenario

Author: Bonito, Rosaria, Orlando, Salvatore, Peres, Giovanni, Favata, Fabio, Eislöffel, Jochen, Tsinganos, Kanaris, editor, Ray, Tom, editor, and Stute, Matthias, editor
Published: 2009
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24. Give Me a Few Hours: Exploring Short Timescales in Rubin Observatory Cadence Simulations

Author: Bellm, Eric C., primary, Burke, Colin J., additional, Coughlin, Michael W., additional, Andreoni, Igor, additional, Raiteri, Claudia M., additional, and Bonito, Rosaria, additional
Published: 2022
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25. Accretion/ejection diagnostic in young stellar objects: a multi-band and interdisciplinary approach

Author: Bonito, Rosaria, Orlando, Salvatore, Argiroffi, Costanza, Prisinzano, Loredana, Revet, Guilhem, Burdonov, Konstantin, Fuchs, Julien, and Wolk, Scott
Subjects: Young stars, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the investigation of accretion/ejection properties of young stellar objects (YSOs), combining multi-band observations, numerical simulations, and laboratory experiments: from the Gaia-ESO Survey (GES) spectroscopic optical data of the NGC 2264 cluster (Bonito et al. 2020), to the laser experiments of stellar jets and accretion shocks young stars (e.g. Burdonov et al. 2020, 2021; Revet et al. 2021), to numerical simulations in the UV and X-ray band of accretion shocks, also in the context of next generation telescopes as Athena X-ray Observatory (Bonito et al. in preparation). The analysis of the Hα emission line profile in the GES context, provides us with information on the accretion/ejection activity of young stars, even when the nebular contribution is strong. We have developed a tool, the OHaNA method, to handle the strong nebular contribution and spectra with spurious profiles of the Hα and forbidden emission lines (e.g. [SII] and [NII] doublets). In this case, the mass accretion rate can be related to the full width at zero intensity (FWZI) of the emission line, whose measurement is more robust with respect to any value derived from the peak (e.g. Hα10%) possibly altered by the nebular contribution. The laser experiments of jets and accretion shocks in YSOs will be discussed, focusing on the effect of the local absorption on the detectability of their emission and on the role of the magnetic field on the collimation of jets. For the high energy emission, we will present the new simulations comparing the UV and X-ray shock emission from the models and the observations, taking into account also the local absorption effect and investigating the detectability of the Doppler shift in the line profiles. Future perspectives with next generation instruments, as the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) and the implication on the study of young stellar objects and their variability will be also discussed., {"references":["Rigliaco, E. et al. (2009). Discovery of an old photoevaporating disk in σ Orionis","Reipurth et al. (1996). Hα emission in pre-main sequence stars. I. an atlas of line profiles.","Bonito, R. et al. (2020). The Gaia-ESO Survey: A new diagnostic for accretion and outflow activity in the young cluster NGC 2264","Bonito, R. et al. (2013). Spectroscopic observations of blue stars with infrared excesses in NGC 6611","Prisinzano, L. et al. (2019). The Gaia-ESO Survey: Age spread in the star forming region NGC 6530 from the HR diagram and gravity indicators","Bonito, R. et al. (2008). The nearest X-ray emitting protostellar jet (HH 154) observed with Hubble","Bonito, R. et al. (2010). Generation of radiative knots in a randomly pulsed protostellar jet. I. Dynamics and energetics","Bonito, R. et al. (2011). X-Ray Emission from Protostellar Jet HH 154: The First Evidence of a Diamond Shock?","Argiroffi, C. et al. (2017). Redshifted X-rays from the material accreting onto TW Hydrae: Evidence of a low-latitude accretion spot","Albertazzi, B. et al. (2014). Laboratory formation of a scaled protostellar jet by coaligned poloidal magnetic field","Revet, G. et al. (2017). Laboratory unravelling of matter accretion in young stars","Burdonov, K. et al. (2020). Laboratory evidence for an asymmetric accretion structure upon slanted matter impact in young stars","Burdonov, K. et al. (2021). Inferring possible magnetic field strength of accreting inflows in EXor-type objects from scaled laboratory experiments","Revet, G. et al. (2021). Laboratory disruption of scaled astrophysical outflows by a misaligned magnetic field","Orlando, S. et al. (2013). Radiative accretion shocks along nonuniform stellar magnetic fields in classical T Tauri stars","Bonito, R. et al. (2014). Magnetohydrodynamic Modeling of the Accretion Shocks in Classical T Tauri Stars: The Role of Local Absorption in the X-Ray Emission","Mignone, A. et al. (2007). PLUTO: A Numerical Code for Computational Astrophysics","Romanova, M. et al. (2004).","Bonito, R. & Hartigan, P. et al. (2018). Young Stars and their Variability with LSST","Bonito, R. & Venuti, L. et al. (2021)."]}
Published: 2021
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26. The Complex Morphology of the X-ray and Optical Emission from HH 154: The Pulsed Jet Scenario

Author: Bonito, Rosaria, primary, Orlando, Salvatore, additional, Peres, Giovanni, additional, Favata, Fabio, additional, and Eislöffel, Jochen, additional
Published: 2009
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27. Laboratory unraveling of matter accretion in young stars

Author: Revet, Guilhem, Chen, Sophia N., Bonito, Rosaria, Khiar, Benjamin, Filippov, Evgeny, Argiroffi, Costanza, Higginson, Drew P., Orlando, Salvatore, Béard, Jérôme, Blecher, Marius, Borghesi, Marco, Burdonov, Konstantin, Khaghani, Dimitri, Naughton, Kealan, Pépin, Henri, Portugall, Oliver, Riquier, Raphael, Rodriguez, Rafael, Ryazantsev, Sergei N., Yu. Skobelev, Igor, Soloviev, Alexander, Willi, Oswald, Pikuz, Sergey, Ciardi, Andrea, Fuchs, Julien, Laboratoire pour l'utilisation des lasers intenses (LULI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Applied Physics (IAP, Nizhny Novgorod), Istituto Nazionale di Astrofisica (INAF), Dipartimento di Fisica e Chimica [Palermo] (DiFC), Università degli studi di Palermo - University of Palermo, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), The National Research Nuclear University MEPhI (Moscow Engineering Physics Institute) [Moscow, Russia], Joint Institute for High Temperatures of the RAS (JIHT), Russian Academy of Sciences [Moscow] (RAS), Lawrence Livermore National Laboratory (LLNL), Laboratoire national des champs magnétiques intenses - Toulouse (LNCMI-T), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut für Laser und Plasmaphysik, Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf], Queen's University [Belfast] (QUB), Gesellschaft für Schwerionenforschung, Helmholtz zentrum für Schwerionenforschung GmbH (GSI), Énergie Matériaux Télécommunications - INRS (EMT-INRS), Institut National de la Recherche Scientifique [Québec] (INRS)-Université du Québec à Montréal = University of Québec in Montréal (UQAM), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Las Palmas de Gran Canaria (ULPGC), ANR-12-BS09-0025,SILAMPA,Simuler en laboratoire des écoulements de plasmas magnétisés pour l'astrophysique(2012), ANR-11-IDEX-0004,SUPER,Sorbonne Universités à Paris pour l'Enseignement et la Recherche(2011), ITA, USA, GBR, FRA, DEU, ESP, CAN, RUS, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Revet, Guilhem, Chen, Sophia N., Bonito, Rosaria, Khiar, Benjamin, Filippov, Evgeny, Argiroffi, Costanza, Higginson, Drew P., Orlando, Salvatore, Béard, Jérôme, Blecher, Mariu, Borghesi, Marco, Burdonov, Konstantin, Khaghani, Dimitri, Naughton, Kealan, Pépin, Henri, Portugall, Oliver, Riquier, Raphael, Rodriguez, Rafael, Ryazantsev, Sergei N., Skobelev, Igor Yu., Soloviev, Alexander, Willi, Oswald, Pikuz, Sergey, Ciardi, Andrea, and Fuchs, Julien
Subjects: HOT, ELECTRON THERMAL CONDUCTION, PLASMA, T-TAURI STARS, Astrophysics::High Energy Astrophysical Phenomena, MAGNETIC-FIELD, CLOUDS, SciAdv r-articles, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, SIMULATIONS, X-RAY-EMISSION, Settore FIS/05 - Astronomia E Astrofisica, GAS, Physical Sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Research Articles, Astrophysics::Galaxy Astrophysics, Research Article, RADIATIVE SHOCKS
Abstract: When matter accretes onto a young star, a shell of dense material can form around the impact, reducing its x-ray emission., Accretion dynamics in the formation of young stars is still a matter of debate because of limitations in observations and modeling. Through scaled laboratory experiments of collimated plasma accretion onto a solid in the presence of a magnetic field, we open a first window on this phenomenon by tracking, with spatial and temporal resolution, the dynamics of the system and simultaneously measuring multiband emissions. We observe in these experiments that matter, upon impact, is ejected laterally from the solid surface and then refocused by the magnetic field toward the incoming stream. This ejected matter forms a plasma shell that envelops the shocked core, reducing escaped x-ray emission. This finding demonstrates one possible structure reconciling current discrepancies between mass accretion rates derived from x-ray and optical observations, respectively.
Published: 2017
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28. Multi-wavelength and multi-disciplinary approach to the study of the emission from accretion/ejection processes in young stars with disks: combining observations, numerical models, and laboratory experiments

Author: Bonito, Rosaria
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: A multi-band investigation of the emission from young stars with disks allows us to obtain a complete characterization of these complex systems, accounting for their accretion and outflow activity. All the components contributing to the emission can strongly influence also the evolution of their disks and possibly the formation of exo-planetary systems. Combining multi-wavelength observations, magnetohydrodynamical models, and laboratory experiments following a multi-disciplinary approach, we aim at a more complete characterization of young stars with accretion/ejection processes at work. We present X-ray and optical analysis of line profiles and Doppler shift for specific objects (e.g. TW Hya) as well as in statistical samples (NGC 2264) and discuss future perspectives with next generation instruments: Athena and LSST. In particular, LSST main characteristics will be presented in the context of the investigation of young stars as this survey will allow us to increase the number of young stars whose accretion/outflow activities can be fully characterized exploiting also the variability of these processes. A science case for the Mini Survey and Deep Drilling Field proposals in LSST in the context of young stars will be discussed.
Published: 2018
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29. Laboratory unraveling of matter accretion in young stars

Author: Revet, G., Chen, S. N., Bonito, Rosaria, Khiar, Benjamin, Filippov, E., argiroffi, costanza, Higginson, D.P., orlando, salvatore, Beard, J., Blecher, marius, Borghesi, Marco, Naughton, Kealan, Chen, Shenchang, Burdonov, Konstantin, Khaghani, D., Pépin, H., Portugall, O., Riquier, R., Rodriguez, Rafael, Ryazantsev, Sergey, Skobelev, I. Yu., Soloviev, A., Willi, Oswald, Pikuz, S. A., Ciardi, A., and Fuchs, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Accretion dynamics in the formation of young stars is still a matter of debate because of limitations in observations and modeling. Through scaled laboratory experiments of collimated plasma accretion onto a solid in the presence of a magnetic field, we open a first windowon this phenomenon by tracking, with spatial and temporal resolution, the dynamics of the system and simultaneously measuring multiband emissions. We observe in these experiments that matter, upon impact, is ejected laterally from the solid surface and then refocused by the magnetic field toward theincoming stream. This ejected matter forms a plasma shell that envelops the shocked core, reducing escaped x-ray emission. This finding demonstrates one possible structure reconciling current discrepancies between mass accretionrates derived from x-ray and optical observations, respectively.
Published: 2017
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30. X-ray emission in protostellar jets: comparison between model predictions and observations

Author: BONITO, Rosaria, PERES, Giovanni, Favata, Fabio, Fridlund, Malcolm, Micela, Giuseppina, Orlando, Salvatore, Rosner, Robert, Sciortino, Salvatore, Bonito, Rosaria, Favata, Fabio, Fridlund, Malcolm, Micela, Giuseppina, Orlando, Salvatore, Peres, Giovanni, Rosner, Robert, and Sciortino, Salvatore
Subjects: hydrodynamics – Herbig-Haro objects – ISM: jets and outﬂows – X-rays: ISM
Published: 2007

31. X-ray and optical emission in protostellar jets: model predictions and comparison with observations

Author: BONITO, Rosaria, PERES, Giovanni, Favata, Fabio, Fridlund, Malcolm, Liseau, Rene, Micela, Giuseppina, Orlando, Salvatore, Rosner, Robert, Sciortino, Salvatore, Bonito, Rosaria, Favata, Fabio, Fridlund, Malcolm, Liseau, Rene, Micela, Giuseppina, Orlando, Salvatore, Peres, Giovanni, Rosner, Robert, and Sciortino, Salvatore
Subjects: hydrodynamics – Herbig-Haro objects – ISM: jets and outﬂows – X-rays: ISM
Published: 2007

32. Herbig-Haro objects: model prediction and comparison with X-ray and optical observations

Author: BONITO, Rosaria, PERES, Giovanni, Favata, Fabio, Fridlund, Malcolm, Micela, Giuseppina, Orlando, Salvatore, Rosner, Robert, Sciortino, Salvatore, Bonito, Rosaria, Favata, Fabio, Fridlund, Malcolm, Micela, Giuseppina, Orlando, Salvatore, Peres, Giovanni, Rosner, Robert, and Sciortino, Salvatore
Subjects: hydrodynamics – Herbig-Haro objects – ISM: jets and outﬂows – X-rays: ISM
Published: 2007

33. Modeling the non-thermal emission from bowshocks produced by runaway stars

Author: Pereira, V, López Santiago, J, De Castro, E., MICELI, Marco, BONITO, Rosaria, Pereira, V, Miceli, M, Bonito, R, López-Santiago, J, and De Castro, E
Subjects: N/A
Published: 2014

34. Pre-main-sequence stars older than 8 Myr in the Eagle nebula

Author: De Marchi, G, Panagia, N, Guarcello, MG, BONITO, Rosaria, De Marchi, G, Panagia, N, Guarcello, MG, and Bonito, R
Subjects: accretion, accretion discs, scattering, protoplanetary discs, circumstellar matter, Hertzsprung-Russell and colour-magnitude diagrams, stars: pre-main-sequence, pre-main-sequence [accretion, accretion discs, scattering, protoplanetary discs, circumstellar matter, Hertzsprung-Russell and colour-magnitude diagrams, stars]
Published: 2013

35. X-ray structures from outflowing Young Stellar Objects interacting with the Interstellar Medium

Author: Orellana, M., López Santiago, J., Albacete Colombo, J. F., BONITO, Rosaria, MICELI, Marco, Orellana, M., Bonito, R., López-Santiago, J., Albacete Colombo, J. F., and Miceli, M.
Subjects: N/A
Published: 2012

36. Discovery of 15 Myr Old pre-Main Sequence Stars with Active Accretion and Sizeable Discs in NGC 6611

Author: De Marchi, G, Panagia, N, Guarcello, MG, BONITO, Rosaria, De Marchi, G, Panagia, N, Guarcello, MG, and Bonito, R
Subjects: N/A
Published: 2012

37. Modeling the X-ray emission from the nearest jets: HH 154 and DG Tau

Author: BONITO, Rosaria, PERES, Giovanni, Orlando, S, Eislöffel, J., Bonito, R, Orlando, S, Peres, G, and Eislöffel, J
Subjects: hydrodynamics – Herbig-Haro objects – ISM: jets and outﬂows – X-rays: ISM
Published: 2010

38. Modeling the X-ray emission from jets observed with Chandra

Author: Bonito, Rosaria, Salvatore Orlando, Peres, G., Favata, F., Miceli, M., Eisloffel, J., Bonito, R, Orlando, S, Peres, G, Favata, F, Miceli, M, and Eisloffel, J
Subjects: Stars and Star Formation
Published: 2009

39. High Performance Computing on the COMETA Grid Infrastructure

Author: Orlando, S., Bocchino, F., Sacco, G. G., Yelenina, T., PERES, Giovanni, REALE, Fabio, MICELI, Marco, BONITO, Rosaria, PAGANO, Paolo, ARGIROFFI, Costanza, Orlando, S., Peres, G., Reale, F., Bocchino, F., Sacco, G. G., Miceli, M., Bonito, R., Pagano, P., Argiroffi, C., and Yelenina, T.
Subjects: Magnetohydrodynamics, Settore FIS/05 - Astronomia E Astrofisica, High Performance Computing, Hydrodynamics, Astrophysics
Abstract: We present the High Performance Computing (HPC) projects jointly developed at the INAF - Osservatorio Astronomico di Palermo and at the DSFA - Universita` di Palermo which benefits of the Grid infrastructure of COMETA. We have contributed to setup the infrastructure in order to run HPC applications on the Grid. We report on our experience regarding to porting HPC applications to the Grid and to the first HPC simulations performed. The most demanding simulations describe the interaction of a magnetized supernova shock wave with an interstellar gas cloud. We discuss the resources required for the simulations, the performance and the scalability of our code on the Grid, and present first results.
Published: 2008

40. X-ray Emission from Protostellar Jets

Author: BONITO, Rosaria, PERES, Giovanni, Orlando, S., Favata, F., Bonito, R., Orlando, S., Favata, F., and Peres, G
Subjects: Shock wave, ISM: Herbig-Haro object, ISM: jets and outflow, X-rays: ISM
Published: 2008

41. X-ray Emission in protostellar jets

Author: BONITO, Rosaria, Orlando, S., PERES, Giovanni, Favata, F., Rosner, R., Bonito, R., Orlando, S., Peres, G., Favata, F., and Rosner, R
Subjects: hydrodynamics – Herbig-Haro objects – ISM: jets and outﬂows – X-rays: ISM
Abstract: Prompted by the recent detection of X-ray emission from Herbig-Haro objects, we studied the interaction between a supersonic jet originating from a young stellar object and the ambient medium; our aim is to investigate the mechanisms causing the X-ray emission. Our model takes into account the radiative losses from optically in plasmas and Spitzer's thermal conduction including saturation effects. We explored the parameter space defined by the density contrast between the ambient medium and the jet and by the Mach number, to infer the configurations which can give rise to X-ray emission. From the models, we derived the X-ray emission as it would be observed with Chandra/ACIS-I and XMM-Newton/EPIC-pn, using the MEKAL spectral code and including the absorption of interstellar medium. Here we discuss a representative case which produces, without any ad hoc assumption, Xray emission with characteristics very similar to those observed in the protostellar jet, HH 154. We find that the X-ray emission originates from a blob localized just behind the bow shock, moving with velocity 500 km/s. We predict, therefore, among other features, a detectable proper motion of the X-ray blob, which is interesting for future observations.
Published: 2005

42. Pre-main-sequence stars older than 8 Myr in the Eagle nebula

Author: De Marchi, Guido, primary, Panagia, Nino, additional, Guarcello, M. G., additional, and Bonito, Rosaria, additional
Published: 2013
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43. NUMERICAL SIMULATIONS AND DIAGNOSTICS IN ASTROPHYSICS: A FEW MAGNETOHYDRODYNAMICS EXAMPLES

Author: PERES, GIOVANNI, primary, BONITO, ROSARIA, additional, ORLANDO, SALVATORE, additional, and REALE, FABIO, additional
Published: 2007
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44. The diagnostic capability of iron limes

Author: Giannini, Teresa, Nisini, Brunella, Simone Antoniucci, Alcala, Juan, Bacciotti, Francesca, Bonito, Rosaria, Podio, Linda, Stelzer, Beate, Whelan, Emma, Giannini, Teresa, Nisini, Brunella, Antoniucci, Simone, Alcala, Juan, Bacciotti, Francesca, Bonito, Rosaria, Podio, Linda, Stelzer, Beate, and Whelan, Emma
Subjects: N/A

45. Accretion in young stars: measure of the stream velocity of TW Hya from the X-ray Doppler shift

Author: Argiroffi, Costanza, Bonito, Rosaria, Salvatore Orlando, Miceli, Marco, Peres, Giovanni, and ITA
Subjects: Settore FIS/05 - Astronomia E Astrofisica, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Accretion, accretion disks, Stars: pre-main sequence, Stars: variables: T Tauri, Herbig Ae/Be, Techniques: spectroscopic, X-rays: stars, Astrophysics::Galaxy Astrophysics
Abstract: High-resolution X-ray spectra are a unique tool to investigate the accretion process in young stars. In fact X-rays allow to investigate the accretion-shock region, where the infalling material is heated by strong shocks due to the impact with the denser stellar atmosphere. Here we show for the first time that it is possible to constrain the velocity of the accretion stream by measuring the Doppler shift of the emitted X-rays. To this aim we analyzed the deep Chandra/HETGS observation of the accreting young star TW Hya. We selected a sample of emission lines free from significant blends, fitted them with gaussian profiles, computed the radial velocity corresponding to each line, and averaged these velocities to obtain an accurate estimate of the global velocity of the X-ray emitting plasma. After correcting for Earth's motion, we compared this observed velocity with the photospheric radial velocity. In order to check this procedure we applied the same technique to other Chandra/HETGS spectra of single stars, whose X-rays are due only to coronal plasma. While spectra of pure coronal sources provide Doppler shifts in agreement with the known stellar radial velocity, we found that the X-ray spectrum of TW Hya is red-shifted by ~30-40 km/s with respect to the stellar photosphere. This proves that the X-ray emitting plasma on TW Hya is moving with respect to the stellar surface, definitively confirming that it originates in the accretion-shock region. The observed velocity suggests that the base of the accretion region is located at low latitudes of the stellar surface.

46. 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
Subjects: 13. Climate action, 530 Physics, 520 Astronomy, Astrophysics::Earth and Planetary Astrophysics, 500 Science, 7. Clean energy
Abstract: Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet’s birth, and evolution. ARIEL was conceived to observe a large number (~1000) of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25–7.8 μm spectral range and multiple narrow-band photometry in the optical. ARIEL will focus on warm and hot planets to take advantage of their well-mixed atmospheres which should show minimal condensation and sequestration of high-Z materials compared to their colder Solar System siblings. Said warm and hot atmospheres are expected to be more representative of the planetary bulk composition. Observations of these warm/hot exoplanets, and in particular of their elemental composition (especially C, O, N, S, Si), will allow the understanding of the early stages of planetary and atmospheric formation during the nebular phase and the following few million years. ARIEL will thus provide a representative picture of the chemical nature of the exoplanets and relate this directly to the type and chemical environment of the host star. ARIEL is designed as a dedicated survey mission for combined-light spectroscopy, capable of observing a large and well-defined planet sample within its 4-year mission lifetime. Transit, eclipse and phase-curve spectroscopy methods, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allow us to measure atmospheric signals from the planet at levels of 10–100 part per million (ppm) relative to the star and, given the bright nature of targets, also allows more sophisticated techniques, such as eclipse mapping, to give a deeper insight into the nature of the atmosphere. These types of observations require a stable payload and satellite platform with broad, instantaneous wavelength coverage to detect many molecular species, probe the thermal structure, identify clouds and monitor the stellar activity. The wavelength range proposed covers all the expected major atmospheric gases from e.g. H₂O, CO₂, CH₄ NH₃, HCN, H₂S through to the more exotic metallic compounds, such as TiO, VO, and condensed species. Simulations of ARIEL performance in conducting exoplanet surveys have been performed – using conservative estimates of mission performance and a full model of all significant noise sources in the measurement – using a list of potential ARIEL targets that incorporates the latest available exoplanet statistics. The conclusion at the end of the Phase A study, is that ARIEL – in line with the stated mission objectives – will be able to observe about 1000 exoplanets depending on the details of the adopted survey strategy, thus confirming the feasibility of the main science objectives.

47. X-ray emission from protostellar jet HH 154: first evidence of a diamond shock?

Author: Bonito, Rosaria, Salvatore Orlando, Miceli, Marco, Peres, Giovanni, Micela, Giusi, Favata, Fabio, Bonito, R, Orlando, S, Miceli, M, Peres, G, Micela, G, and Favata, F
Subjects: N/A

48. The Gaia-ESO Survey: Catalogue of H alpha emission stars

Author: Traven, Gregor, Zwitter, Tomaž, Van Eck, Sophie, Klutsch, Alexis, Bonito, Rosaria, Lanzafame, Alessandro C., Alfaro, Emilio J., Bayo, Amelia, Bragaglia, Angela, Costado, María Teresa, Damiani, Francesco, Flaccomio, Ettore, Frasca, Antonio, Hourihane, Anna, Jimenez-Esteban, Fran, Lardo, Carmela, Morbidelli, Lorenzo, Pancino, Elena, Prisinzano, Loredana, Sacco, Germano G., and Worley, Clare C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, stars: emission-line, Be, stars: peculiar, open clusters and associations: general, Astrophysics::High Energy Astrophysical Phenomena, stars: emission-line, Astrophysics::Solar and Stellar Astrophysics, Be, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract: We discuss the properties of Hα emission stars across the sample of 22035 spectra from the Gaia-ESO Survey internal data release, observed with the GIRAFFE instrument and largely belonging to stars in young open clusters. Automated fits using two independent Gaussian profiles and a third component that accounts for the nebular emission allow us to discern distinct morphological types of Hα line profiles with the introduction of a simplified classification scheme. All in all, we find 3765 stars with intrinsic emission and sort their spectra into eight distinct morphological categories: single–component emission, emission blend, sharp emission peaks, double emission, P-Cygni, inverted P-Cygni, self–absorption, and emission in absorption. We have more than one observation for 1430 stars in our sample, thus allowing a quantitative discussion of the degree of variability of Hα emission profiles, which is expected for young, active objects. We present a catalogue of stars with properties of their Hα emission line profiles, morphological classification, analysis of variability with time and the supplementary information from the SIMBAD, VizieR, and ADS databases. The records in SIMBAD indicate the presence of Hα emission for roughly 25% of all stars in our catalogue, while at least 305 of them have already been more thoroughly investigated according to the references in ADS. The most frequently identified morphological categories in our sample of spectra are emission blend (23%), emission in absorption (22%), and self–absorption (16%). Objects with repeated observations demonstrate that our classification into discrete categories is generally stable through time, but categories P-Cygni and self–absorption seem less stable, which is the consequence of discrete classification rules, as well as of the fundamental change in profile shape. Such records of emission stars can be valuable for automatic pipelines in large surveys, where it may prove very useful for pinpointing outliers when calculating general stellar properties and elemental abundances. They can be used in studies of star formation processes, interacting binaries, and other fields of stellar physics.

49. The Gaia -ESO Survey: Calibrating the lithium-age relation with open clusters and associations: I. Cluster age range and initial membership selections

Author: E. Delgado Mena, Paula Jofre, Andreas J. Korn, Gerard Gilmore, Rosaria Bonito, Lorenzo Monaco, Giovanni Carraro, Clare Worley, Sofia Randich, Ulrike Heiter, Sofia Feltzing, Simone Zaggia, D. Montes, Hugo M. Tabernero, F. Jiménez Esteban, Thomas Bensby, A. Hourihane, S. G. Sousa, Rodolfo Smiljanic, L. Prisinzano, L. Morbidelli, Antonio Frasca, V. Roccatagliata, Emilio J. Alfaro, A. Klutsch, M. L. Gutiérrez Albarrán, M. Gómez Garrido, A. C. Lanzafame, Emilio Marfil, Amelia Bayo, M. Van der Swaelmen, E. Franciosini, J. I. González Hernández, Anais Gonneau, Thomas Masseron, M. Baratella, Ministerio de Economía y Competitividad (España), European Commission, Istituto Nazionale di Astrofisica, Ministero dell'Istruzione, dell'Università e della Ricerca, Knut and Alice Wallenberg Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Swedish National Space Agency, Fundação para a Ciência e a Tecnologia (Portugal), Science and Technology Facilities Council (UK), Leverhulme Trust, European Science Foundation, Ministerio de Economía y Competitividad (MINECO), European Commission (EC), Istituto Nazionale di Astrofisica (INAF), Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR), Agencia Estatal de Investigación (AEI), Fundacao para a Ciencia e a Tecnologia (FCT), Gutiérrez Albarrán, Marta Lúthien https://orcid.org/0000-0002-7569-3513, Montes, David https://orcid.org/0000-0002-7779-238X, Tabernero, Hugo https://orcid.org/0000-0002-8087-4298, González Hernández, Jonay I https://orcid.org/0000-0002-0264-7356, Marfil, Emilio https://orcid.org/0000-0001-8907-4775, Frasca, Antonio https://orcid.org/0000-0002-0474-0896, Klutsch, Alexis https://orcid.org/0000-0001-7869-3888, Franciosini, Elena https://orcid.org/0000-0003-3969-0232, Randichi, Sofia https://orcid.org/0000-0003-2438-0899, Smiljanic, R. https://orcid.org/0000-0003-0942-7855, Bensby, Thomas https://orcid.org/0000-0003-3978-1409, Bonito, Rosaria https://orcid.org/0000-0001-9297-7748, Carraro, Giovanni https://orcid.org/0000-0002-0155-9434, Monaco, Lorenzo https://orcid.org/0000-0002-3148-9836, Knut och Alice Wallenbergs Stiftelse, Swedish National Space Agency (SNSA), Fundação para a Ciência e a Tecnologia (FCT), Science and Technology Facilities Council (STFC), European Science Foundation (ESF), Ministerio de Ciencia e Innovación (MICINN), Guitiérrez Albarrán, M. L. [0000-0002-7569-3513], Montes, D. [0000-0002-7779-238X], Tabernero, H. M. [0000-0002-8087-4298], González Hernández, J. I. [0000-0002-0264-7356], Marfil, E. [0000-0001-8907-4775], Frasca, A. [000-0002-0474-0896], Klutsch, A. [0000-0001-7869-3888], Franciosini, E. [0000-0003-3969-0232], Randichi, S. [0000-0003-2438-0899], Smiljanic, R. [0000-0003-0942-7855], Korn, A. J. [0000-0002-3881-6756], Gilmore, G. [0000-0003-4632-0213], Bayo, A. [000-0001-7868-7031], Bensby, T. [0000-0003-3978-1409], Bonito, R. [0000-0001-9297-7748], Carraro, G. [0000-0002-0155-9434], Ministero dell'Istruzione dell'Università e della Ricerca, Ministerio de Ciencia Innovación y Universidades, España, ITA, GBR, DEU, ESP, CHL, POL, PRT, and SWE
Subjects: Astrofísica, astro-ph.SR, Field (physics), Metallicity, FOS: Physical sciences, Techniques: spectroscopic, Context (language use), Astrophysics, Stars: late-type, 01 natural sciences, spectroscopic [Techniques], Astronomi, astrofysik och kosmologi, 0103 physical sciences, Cluster (physics), Range (statistics), Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, general [Open clusters and associations], 010308 nuclear & particles physics, Stars: abundances, Astronomy and Astrophysics, Open clusters and associations: general, Radial velocity, Astronomía, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, late-type [Stars], abundances [Stars], Open cluster
Abstract: Full list of authors: Gutiérrez Albarrán, M. L.; Montes, D.; Gómez Garrido, M.; Tabernero, H. M.; González Hernández, J. I.; Marfil, E.; Frasca, A.; Lanzafame, A. C.; Klutsch, A.; Franciosini, E.; Randich, S.; Smiljanic, R.; Korn, A. J.; Gilmore, G.; Alfaro, E. J.; Baratella, M.; Bayo, A.; Bensby, T.; Bonito, R.; Carraro, G. Delgado Mena, E.; Feltzing, S.; Gonneau, A.; Heiter, U.; Hourihane, A.; Jiménez Esteban, F.; Jofre, P.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Roccatagliata, V.; Sousa, S.; Van der Swaelmen, M.; Worley, C. C.; Zaggia, S., Context. Previous studies of open clusters have shown that lithium depletion is not only strongly age dependent but also shows a complex pattern with other parameters that is not yet understood. For pre- and main-sequence late-type stars, these parameters include metallicity, mixing mechanisms, convection structure, rotation, and magnetic activity. Aims. We perform a thorough membership analysis for a large number of stars observed within the Gaia-ESO survey (GES) in the field of 20 open clusters, ranging in age from young clusters and associations, to intermediate-age and old open clusters. Methods. Based on the parameters derived from the GES spectroscopic observations, we obtained lists of candidate members for each of the clusters in the sample by deriving radial velocity distributions and studying the position of the kinematic selections in the EW(Li)-versus-Teff plane to obtain lithium members. We used gravity indicators to discard field contaminants and studied [Fe/H] metallicity to further confirm the membership of the candidates. We also made use of studies using recent data from the Gaia DR1 and DR2 releases to assess our member selections. Results. We identified likely member candidates for the sample of 20 clusters observed in GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that allowed us to characterize the properties of these members as well as identify field contaminant stars, both lithium-rich giants and non-giant outliers. Conclusions. This work is the first step towards the calibration of the lithium-age relation and its dependence on other GES parameters. During this project we aim to use this relation to infer the ages of GES field stars, and identify their potential membership to young associations and stellar kinematic groups of different ages. © ESO 2020., Financial support was provided by the Universidad Complutense de Madrid and by the Spanish Ministry of Economy and Competitiveness (MINECO) from project AYA2016-79425-C3-1-P. We acknowledge the support from INAF and Ministero dell' Istruzione, dell' Universita' e della Ricerca (MIUR) in the form of the grant "Premiale VLT 2012". T.B. was funded by the project grant "The New Milky Way" from the Knut and Alice Wallenberg Foundation. J.I.G.H. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2003 Ramon y Cajal program RYC-2013-14875, and also from the Spanish Ministry project MICIU AYA2017-86389-P. E.M. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion through fellowship FPU15/01476. A.G. acknowledges support from the European Union FP7 programme from the UK space agency. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). F.J.E. acknowledges financial support from the Spanish MINECO/FEDER through the grant AyA2017-84089. S.G.S acknowledges the support of Fundacao para a Ciencia e Tecnologia (FCT) through national funds and research grant (project ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S also acknowledges the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividad" - COMPETE MT also acknowledges support from the FCT - Fundacao para a Ciencia e a Tecnologia through national funds (PTDC/FIS-AST/28953/2017) and by FEDER -Fundo Europeu de Desenvolvimento Regional through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao (POCI-01-0145-FEDER-028953). TM acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-88254-P Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme focusID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF-Osservatorio Astrofisico di Arcetri. These data have been obtained from the GES Data Archive, prepared and hosted by theWide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. The results presented here benefit from discussions held during GES workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This work was also supported by Fundacao para a Ciencia e Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of the VizieR database (Ochsenbein et al. 2000) and the SIMBAD database (Wenger et al. 2000), both operated at CDS, Centre de Donnees astronomiques de Strasbourg, France. This research also made use of the WEBDA database, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University, and the interactive graphical viewer and editor for tabular data TOPCAT (Taylor 2005). For the analysis of the distributions of RV and metallicity we used RStudio Team (2015). Integrated Development for R. RStudio, Inc., Boston, MA (http://www.rstudio.com/).Finally, we would like to thank the anonymous referee for helpful comments and suggestions.
Published: 2020

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