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1. In-situ observations of resident space objects with the CHEOPS space telescope

Author: Billot, Nicolas, Hellmich, Stephan, Benz, Willy, Fortier, Andrea, Ehrenreich, David, Broeg, Christopher, Heitzmann, Alexis, Bekkelien, Anja, Brandeker, Alexis, Alibert, Yann, Alonso, Roi, Bárczy, Tamas, Navascues, David Barrado, Barros, Susana C. C., Baumjohann, Wolfgang, Biondi, Federico, Borsato, Luca, Cameron, Andrew Collier, van Damme, Carlos Corral, Correia, Alexandre C. M., Csizmadia, Szilard, Cubillos, Patricio E., Davies, Melvyn B., Deleuil, Magali, Deline, Adrien, Demangeon, Olivier D. S., Demory, Brice-Olivier, Derekas, Aliz, Edwards, Billy, Egger, Jo Ann, Erikson, Anders, Fossati, Luca, Fridlund, Malcolm, Gandolfi, Davide, Gazeas, Kosmas, Gillon, Michaël, Güdel, Manuel, Günther, Maximilian N., Helling, Ch., Isaak, Kate G., Kiss, Laszlo L., Korth, Judith, Lam, Kristine W. F., Laskar, Jacques, Etangs, Alain Lecavelier des, Lendl, Monika, Magrin, Demetrio, Maxted, Pierre F. L., Mecina, Marko, Merín, Bruno, Mordasini, Christoph, Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Ribas, Ignasi, Rieder, Martin, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Sousa, Sérgio G., Stalport, Manu, Sulis, Sophia, Szabó, Gyula M., Udry, Stéphane, Ulmer, Bernd, Ulmer-Moll, Solène, Van Grootel, Valérie, Venturini, Julia, Villaver, Eva, Walton, Nicholas A., and Wilson, Thomas G.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Data Analysis, Statistics and Probability, Physics - Space Physics
Abstract: The CHaracterising ExOPlanet Satellite (CHEOPS) is a partnership between the European Space Agency and Switzerland with important contributions by 10 additional ESA member States. It is the first S-class mission in the ESA Science Programme. CHEOPS has been flying on a Sun-synchronous low Earth orbit since December 2019, collecting millions of short-exposure images in the visible domain to study exoplanet properties. A small yet increasing fraction of CHEOPS images show linear trails caused by resident space objects crossing the instrument field of view. To characterize the population of satellites and orbital debris observed by CHEOPS, all and every science images acquired over the past 3 years have been scanned with a Hough transform algorithm to identify the characteristic linear features that these objects cause on the images. Thousands of trails have been detected. This statistically significant sample shows interesting trends and features such as an increased occurrence rate over the past years as well as the fingerprint of the Starlink constellation. The cross-matching of individual trails with catalogued objects is underway as we aim to measure their distance at the time of observation and deduce the apparent magnitude of the detected objects. As space agencies and private companies are developing new space-based surveillance and tracking activities to catalogue and characterize the distribution of small debris, the CHEOPS experience is timely and relevant. With the first CHEOPS mission extension currently running until the end of 2026, and a possible second extension until the end of 2029, the longer time coverage will make our dataset even more valuable to the community, especially for characterizing objects with recurrent crossings., Comment: 9 pages, 8 figures, Special Issue of the Journal of Space Safety Engineering
Published: 2024
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2. Prominent mid-infrared excess of the dwarf planet (136472) Makemake discovered by JWST/MIRI indicates ongoing activity

Author: Kiss, Csaba, Müller, Thomas G., Farkas-Takács, Anikó, Moór, Attila, Protopapa, Silvia, Parker, Alex H., Santos-Sanz, Pablo, Ortiz, Jose Luis, Holler, Bryan J., Wong, Ian, Stansberry, John, Fernández-Valenzuela, Estela, Glein, Christopher R., Lellouch, Emmanuel, Vilenius, Esa, Kalup, Csilla E., Regály, Zsolt, Szakáts, Róbert, Marton, Gábor, Pál, András, and Szabó, Gyula M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report on the discovery of a very prominent mid-infrared (18-25 {\mu}m) excess associated with the trans-Neptunian dwarf planet (136472) Makemake. The excess, detected by the MIRI instrument of the James Webb Space Telescope, along with previous measurements from the Spitzer and Herschel space telescopes, indicates the occurrence of temperatures of about 150 K, much higher than what solid surfaces at Makemake's heliocentric distance could reach by solar irradiation. We identify two potential explanations: a continuously visible, currently active region, powered by subsurface upwelling and possibly cryovolcanic activity, covering <1% of Makemake's surface, or an as yet undetected ring containing very small carbonaceous dust grains, which have not been seen before in trans-Neptunian or Centaur rings. Both scenarios point to unprecedented phenomena among trans-Neptunian objects and could greatly impact our understanding of these distant worlds., Comment: Accepted for publication in The Astrophysical Journal Letters
Published: 2024

3. 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

4. Exocomet models in transit: light curve morphology in the optical -- near infrared wavelength range

Author: Kálmán, Szilárd, Szabó, Gyula M., and Kiss, Csaba
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Following the widespread practice of exoplanetary transit simulations, various presumed components of an extrasolar system can be examined in numerically simulated transits, including exomoons, rings around planets, and the deformation of exoplanets. Template signals can then be used to efficiently search for light curve features that mark specific phenomena in the data, and they also provide a basis for feasibility studies of instruments and search programs. In this paper, we present a method for exocomet transit light curve calculations using arbitrary dust distributions in transit. The calculations, spanning four distinct materials (carbon, graphite, pyroxene, and olivine), dust grain sizes ($100$\,nm -- $300$\,nm, $300$\,nm -- $1000$\,nm, and $1000$\,nm -- $3000$\,nm) encompass light curves in VRJHKL bands. We also investigated the behavior of scattering colors. We show that multicolor photometric observations are highly effective tools in the detection and characterization of exocomet transits. They provide information on the dust distribution of the comet (encoded in the light curve shape), while the color information itself can reveal the particle size change and material composition of the transiting material, in relation to the surrounding environment. We also show that the typical cometary tail can result in the wavelength dependence of the transit timing. We demonstrate that multi-wavelength observations can yield compelling evidence for the presence of exocomets in real observations., Comment: 26 pages, 20 figures. Accepted for publication in Publications of the Astronomical Society of the Pacific
Published: 2024

5. Discovery of two warm mini-Neptunes with contrasting densities orbiting the young K3V star TOI-815

Author: Psaridi, Angelica, Osborn, Hugh, Bouchy, François, Lendl, Monika, Parc, Léna, Billot, Nicolas, Broeg, Christopher, Sousa, Sérgio G., Adibekyan, Vardan, Attia, Omar, Bonfanti, Andrea, Chakraborty, Hritam, Collins, Karen A., Davoult, Jeanne, Delgado-Mena, Elisa, Grieves, Nolan, Guillot, Tristan, Heitzmann, Alexis, Helled, Ravit, Hellier, Coel, Jenkins, Jon M., Knierim, Henrik, Krenn, Andreas, Lissauer, JackJ., Luque, Rafael, Rapetti, David, Santos, Nuno C., Suárez, Olga, Venturini, Julia, Wilkin, Francis P., Wilson, Thomas G., Winn, Joshua N., Ziegler, Carl, Zingales, Tiziano, Alibert, Yann, Brandeker, Alexis, Egger, Jo Ann, Gandolfi, Davide, Hooton, Matthew J., Tuson, Amy, Ulmer-Moll, Solène, Abe, Lyu, Allart, Romain, Alonso, Roi, Anderson, David R., Anglada, Guillem, Bárczy, Tamas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Benz, Willy, Bonfils, Xavier, Borsato, Luca, Bourrier, Vincent, Ciardi, David R., Cameron, Andrew Collier, Charnoz, Sébastien, Cointepas, Marion, Csizmadia, Szilárd, Cubillos, Patricio, Curto, Gaspare Lo, Davies, Melvyn B., Daylan, Tansu, Deleuil, Magali, Deline, Adrien, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dorn, Caroline, Dumusque, Xavier, Ehrenreich, David, Erikson, Anders, Etangs, Alain Lecavelier des, Ferreras, Elena Diana de Miguel, Fortier, Andrea, Fossati, Luca, Frensch, Yolanda G. C., Fridlund, Malcolm, Gillon, Michaël, Güdel, Manuel, Günther, Maximilian N., Hagelberg, Janis, Helling, Christiane, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo L., Lam, Kristine, Laskar, Jacques, Lavie, Baptiste, Lovis, Christophe, Magrin, Demetrio, Marafatto, Luca, Maxted, Pierre, McDermott, Scott, Mékarnia, Djamel, Mordasini, Christoph, Murgas, Felipe, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Ramos, Devin, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Seager, Sara, Ségransan, Damien, Scandariato, Gaetano, Simon, Attila, Smith, Alexis M. S., Stalport, Manu, Steller, Manfred, Szabó, Gyula, Thomas, Nicolas, Pritchard, Tyler A., Udry, Stéphane, Van Damme, Carlos Corral, Van Grootel, Valérie, Villaver, Eva, Walter, Ingo, Walton, Nicholas, Watkins, Cristilyn N., and West, Richard G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery and characterization of two warm mini-Neptunes transiting the K3V star TOI-815 in a K-M binary system. Analysis of the spectra and rotation period reveal it to be a young star with an age of $200^{+400}_{-200}$Myr. TOI-815b has a 11.2-day period and a radius of 2.94$\pm$0.05$\it{R_{\rm\mathrm{\oplus}}}$ with transits observed by TESS, CHEOPS, ASTEP, and LCOGT. The outer planet, TOI-815c, has a radius of 2.62$\pm$0.10$\it{R_{\rm\mathrm{\oplus}}}$, based on observations of three non-consecutive transits with TESS, while targeted CHEOPS photometry and radial velocity follow-up with ESPRESSO were required to confirm the 35-day period. ESPRESSO confirmed the planetary nature of both planets and measured masses of 7.6$\pm$1.5 $\it{M_{\rm \mathrm{\oplus}}}$ ($\rho_\mathrm{P}$=1.64$^{+0.33}_{-0.31}$gcm$^{-3}$) and 23.5$\pm$2.4$\it{M_{\rm\mathrm{\oplus}}}$ ($\rho_\mathrm{P}$=7.2$^{+1.1}_{-1.0}$gcm$^{-3}$) respectively. Thus, the planets have very different masses, unlike the usual similarity of masses in compact multi-planet systems. Moreover, our statistical analysis of mini-Neptunes orbiting FGK stars suggests that weakly irradiated planets tend to have higher bulk densities compared to those suffering strong irradiation. This could be ascribed to their cooler atmospheres, which are more compressed and denser. Internal structure modeling of TOI-815b suggests it likely has a H-He atmosphere constituting a few percent of the total planet mass, or higher if the planet is assumed to have no water. In contrast, the measured mass and radius of TOI-815c can be explained without invoking any atmosphere, challenging planetary formation theories. Finally, we infer from our measurements that the star is viewed close to pole-on, which implies a spin-orbit misalignment at the 3$\sigma$ level., Comment: 24 pages, 27 figures, 6 tables
Published: 2024

6. TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906

Author: Tuson, Amy, Queloz, Didier, Osborn, Hugh P., Wilson, Thomas G., Hooton, Matthew J., Beck, Mathias, Lendl, Monika, Olofsson, Göran, Fortier, Andrea, Bonfanti, Andrea, Brandeker, Alexis, Buchhave, Lars A., Cameron, Andrew Collier, Ciardi, David R., Collins, Karen A., Gandolfi, Davide, Garai, Zoltan, Giacalone, Steven, da Silva, João Gomes, Howell, Steve B., Patel, Jayshil A., Persson, Carina M., Serrano, Luisa M., Sousa, Sérgio G., Ulmer-Moll, Solène, Vanderburg, Andrew, Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Bárczy, Tamas, Navascues, David Barrado, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Borsato, Luca, Broeg, Christopher, Cabrera, Juan, Charnoz, Sébastien, Conti, Dennis M., Csizmadia, Szilard, Cubillos, Patricio E., Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dragomir, Diana, Dressing, Courtney D., Ehrenreich, David, Erikson, Anders, Essack, Zahra, Farinato, Jacopo, Fossati, Luca, Fridlund, Malcolm, Furlan, Elise, Gill, Holden, Gillon, Michaël, Gnilka, Crystal L., Gonzales, Erica, Güdel, Manuel, Günther, Maximilian N., Hoyer, Sergio, Isaak, Kate G., Jenkins, Jon M., Kiss, Laszlo L., Laskar, Jacques, Latham, David W., Law, Nicholas, Etangs, Alain Lecavelier des, Curto, Gaspare Lo, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Mann, Andrew W., Maxted, Pierre F. L., Mayor, Michel, McDermott, Scott, Mecina, Marko, Mordasini, Christoph, Mortier, Annelies, Nascimbeni, Valerio, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Pritchard, Tyler, Ragazzoni, Roberto, Rando, Nicola, Ratti, Francesco, Rauer, Heike, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Savel, Arjun B., Scandariato, Gaetano, Schwarz, Richard P., Seager, Sara, Ségransan, Damien, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula M., Thomas, Nicolas, Torres, Guillermo, Tronsgaard, René, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valérie, Vanderspek, Roland, Venturini, Julia, Walton, Nicholas A., Winn, Joshua N., and Wohler, Bill
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution., Comment: 30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS
Published: 2023
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7. Two Warm Neptunes transiting HIP 9618 revealed by TESS & Cheops

Author: Osborn, Hugh P., Nowak, Grzegorz, Hébrard, Guillaume, Masseron, Thomas, Lillo-Box, J., Pallé, Enric, Bekkelien, Anja, Florén, Hans-Gustav, Guterman, Pascal, Simon, Attila E., Adibekyan, V., Bieryla, Allyson, Borsato, Luca, Brandeker, Alexis, Ciardi, David R., Cameron, Andrew Collier, Collins, Karen A., Egger, Jo A., Gandolfi, Davide, Hooton, Matthew J., Latham, David W., Lendl, Monika, Matthews, Elisabeth C., Tuson, Amy, Ulmer-Moll, Solène, Vanderburg, Andrew, Wilson, Thomas G., Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Arnold, Luc, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Belinski, Alexandr A., Benz, Willy, Biondi, Federico, Boisse, Isabelle, Bonfils, Xavier, Broeg, Christopher, Buchhave, Lars A., Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Guillen, Carlos Cardona, Carleo, Ilaria, Castro-González, Amadeo, Charnoz, Sébastien, Christiansen, Jessie, Cortes-Zuleta, Pia, Csizmadia, Szilard, Dalal, Shweta, Davies, Melvyn B., Deleuil, Magali, Delfosse, Xavier, Delrez, Laetitia, Demory, Brice-Olivier, Dunlavey, Ava B., Ehrenreich, David, Erikson, Anders, Fernandes, Rachel B., Fortier, Andrea, Forveille, Thierry, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Goeke, Robert F., Goliguzova, Maria V., Gonzales, Erica J., Günther, M. N., Güdel, Manuel, Heidari, Neda, Henze, Christopher E., Howell, Steve, Hoyer, Sergio, Frey, Jonas Immanuel, Isaak, Kate G., Jenkins, Jon M., Kiefer, Flavien, Kiss, Laszlo, Korth, Judith, Maxted, Pierre F. L., Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Lund, Michael B., Luque, Rafa, Magrin, Demetrio, Almenara, Jose Manuel, Martioli, Eder, Mecina, Marko, Medina, Jennifer V., Moldovan, Daniel, Morales-Calderón, María, Morello, Giuseppe, Moutou, Claire, Murgas, Felipe, Jensen, Eric L. N., Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Ribas, Ignasi, Ricker, George, Demangeon, Olivier D. S., Smith, Alexis M. S., Santos, Nuno, Scandariato, Gaetano, Seager, Sara, Sousa, Sergio G., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valerie, Vanderspek, Roland, Walton, Nicholas, and Winn, Joshua N.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright ($G=9.0$ mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of $3.9 \pm 0.044$ $R_\oplus$ (HIP 9618 b) and $3.343 \pm 0.039$ $R_\oplus$ (HIP 9618 c). While the 20.77291 day period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-day gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE and CAFE revealed a mass of $10.0 \pm 3.1 M_\oplus$ for HIP 9618 b, which, according to our interior structure models, corresponds to a $6.8\pm1.4\%$ gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of $< 18M_\oplus$. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion ($0.08^{+0.12}_{-0.05} M_\odot$) orbiting at $26^{+19}_{-11}$ au. This detection makes HIP 9618 one of only five bright ($K<8$ mag) transiting multi-planet systems known to host a planet with $P>50$ d, opening the door for the atmospheric characterisation of warm ($T_{\rm eq}<750$ K) sub-Neptunes., Comment: 19 pages, 16 figures, 9 tables. Accepted at MNRAS. CHEOPS, RV and ground-based photometric data is available on CDS at https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/523/3069
Published: 2023
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8. Converting the sub-Jovian desert of exoplanets to a savanna with TESS, PLATO and Ariel

Author: Kálmán, Szilárd, Szabó, Gyula M., Borsato, Luca, Bódi, Attila, Pál, András, and Szabó, Róbert
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: There is a lack of exoplanets with sizes similar to Neptune orbiting their host stars with periods $\lesssim 3$ days -- hence the name ``sub-Jovian/Neptune desert''. Recently, several exoplanets have been confirmed to reside in the desert transforming it into a ``savanna'' with several ``giraffe'' planets (such as LTT 9779 b and TOI-674 b). The most prominent scenarios put forward for the explanation of the formation of the desert are related to the stellar irradiation destroying the primary atmosphere of certain specific exoplanets. We aim to present three targets (LTT 9779 b, TOI-674 b and WASP-156 b) which, when observed at wide wavelength ranges in infrared (IR), could prove the presence of these processes, and therefore improve the theories of planetary formation/evolution. We simulate and analyse realistic light curves of the selected exoplanets with PLATO/NCAM and the three narrow-band filters of Ariel (VISPhot, FGS1 and FGS2) based on TESS observations of these targets. We improved the precision of the transit parameters of the three considered planets from the TESS data. We find that the combination of the three narrow-band filters of Ariel can yield inner precision of $\lesssim 1.1\%$ for the planetary radii. Data from the three telescopes together will span decades, allowing the monitoring of changes in the planetary atmosphere through radius measurements. The three selected ``giraffe'' planets can be golden targets for Ariel, whereby the loss of planetary mass due to stellar irradiation could be studied with high precision, multi-wavelength (spectro-)photometry., Comment: Accepted for publication in MNRAS; 16 pages, 17 figures
Published: 2023
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9. Sub-Jovian desert of exoplanets at its boundaries. Parameter dependence along the main sequence

Author: Szabó, Gyula M., Kálmán, Szilárd, Borsato, Luca, Hegedűs, Viola, Mészáros, Szabolcs, and Szabó, Róbert
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Context. The lack of sub-Jovian planets on orbits of $P_{\rm orb} < 3$ days is a puzzling aspect of galaxy formation with regard to the distribution of exoplanets whose origins are currently unresolved. Aims. The possible explanations behind the formation of the sub-Jovian or Neptunian desert include several scenarios that can lead to different shapes for the boundary, predicting various dependencies between the position of the boundary and the stellar parameters. Methods. We explored the exoplanet distribution in various 2D and 3D projections, revealing the stellar-dependent substructures in the $P_{\rm orb}-M_{P}$ and the $P_{\rm orb}-R_{P}$ parameter plane. Results. We demonstrate that the upper boundary includes a range of planets, namely, inflated hot Jupiters and normal hot Jupiters, in the two parameter planes, respectively. We confirm the dependence of the boundary on several stellar parameters and, based on a fuzzy clustering analysis, we provide quantitative formulae for the dependencies in groups of smaller and larger planets. The overall period-radius distribution shows chemical substructures as well, with the boundary being dependent on volatiles and alpha-elements, alongside marginal (to none) dependence found for refractory elements. Conclusions. These findings confirm multiple plausible causes for the formation of the desert, particularly preferring those scenarios related to the irradiation-driven loss of the atmospheres of moderately massive planets as the predominant process in shaping planetary distributions., Comment: Accepted for publication in A&A; 11 pages, 11 figuress
Published: 2023
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10. Human Factors and Use of the Surgical Guide in Dentistry—Real Practice Example

Author: Pavlova, Diana, Dovramadjiev, Tihomir, Peev, Ivan, Daskalov, Dimo, Mirchev, Nikolay, Dimova, Rozalina, Radeva, Julia, Szabo, Gyula, Mrugalska, Beata, Kandioglou, Andromachos, Kacprzyk, Janusz, Series Editor, Gomide, Fernando, Advisory Editor, Kaynak, Okyay, Advisory Editor, Liu, Derong, Advisory Editor, Pedrycz, Witold, Advisory Editor, Polycarpou, Marios M., Advisory Editor, Rudas, Imre J., Advisory Editor, Wang, Jun, Advisory Editor, Kaiser, M. Shamim, editor, Xie, Juanying, editor, and Rathore, Vijay Singh, editor
Published: 2024
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11. Developing Occupational Safety Skills for Safety Engineering Students in an Electronic Learning Environment

Author: Szabó, Gyula, López-Paredes, Adolfo, Series Editor, Prostean, Gabriela I., editor, Lavios, Juan J., editor, Brancu, Laura, editor, and Şahin, Faruk, editor
Published: 2024
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12. 3D Design of a Dental Crown with Artificial Intelligence Based in Cloud Space

Author: Pavlova, Diana, Dovramadjiev, Tihomir, Daskalov, Dimo, Mirchev, Nikolay, Peev, Ivan, Radeva, Julia, Dimova, Rozalina, Kavaldzhieva, Kalina, Mrugalska, Beata, Szabo, Gyula, Kandioglou, Andromachos, Kacprzyk, Janusz, Series Editor, Gomide, Fernando, Advisory Editor, Kaynak, Okyay, Advisory Editor, Liu, Derong, Advisory Editor, Pedrycz, Witold, Advisory Editor, Polycarpou, Marios M., Advisory Editor, Rudas, Imre J., Advisory Editor, Wang, Jun, Advisory Editor, Nagar, Atulya K., editor, Jat, Dharm Singh, editor, Mishra, Durgesh Kumar, editor, and Joshi, Amit, editor
Published: 2024
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13. Light curves of transneptunian objects from the K2 mission of the Kepler Space Telescope

Author: Kecskeméthy, Viktória, Kiss, Csaba, Szakáts, Róbert, Pál, András, Szabó, Gyula M., Molnár, László, Sárneczky, Krisztián, Vinkó, József, Szabó, Róbert, Marton, Gábor, Farkas-Takács, Anikó, Kalup, Csilla E., and Kiss, László L.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The K2 mission of the Kepler Space Telescope allowed the observations of light curves of small solar system bodies throughout the whole Solar system. In this paper we present the results of a collection of K2 transneptunian object observations, between Campaigns C03 (November 2014 -- February 2015) to C19 (August -- September, 2018), which includes 66 targets. Due to the faintness of our targets the detectability rate of a light curve period is $\sim$56%, notably lower than in the case of other small body populations, like Hildas or Jovian trojans. We managed to obtain light curve periods with an acceptable confidence for 37 targets; the majority of these cases are new identifications. We were able to give light curve amplitude upper limits for the other 29 targets. Several of the newly detected light curve periods are longer than $\sim$24 h, in many cases close to $\sim$80 h, i.e., these targets are slow rotators. This relative abundance of slowly rotating objects is similar to that observed among Hildas, Jovian trojans and Centaurs in the K2 mission, and also among main belt asteroids measured with the TESS Space Telescope. Transneptunian objects show notably higher light curve amplitudes at large (D $\gtrsim$ 300 km) sizes than that found among large main belt asteroids, in contrast to the general expectation that due to their lower compressive strength they reach hydrostatic equlibrium at smaller sizes than their inner solar system counterparts., Comment: Accepted for publication in ApJS
Published: 2022
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14. TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

Author: Hawthorn, Faith, Bayliss, Daniel, Wilson, Thomas G., Bonfanti, Andrea, Adibekyan, Vardan, Alibert, Yann, Sousa, Sérgio G., Collins, Karen A., Bryant, Edward M., Osborn, Ares, Armstrong, David J., Abe, Lyu, Acton, Jack S., Addison, Brett C., Agabi, Karim, Alonso, Roi, Alves, Douglas R., Anglada-Escudé, Guillem, Bárczy, Tamas, Barclay, Thomas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Bendjoya, Philippe, Benz, Willy, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brandeker, Alexis, Broeg, Christopher, Brown, David J. A., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Caldwell, Douglas A., Casewell, Sarah L., Charbonneau, David, Charnoz, Sébastian, Cloutier, Ryan, Cameron, Andrew Collier, Collins, Kevin I., Conti, Dennis M., Crouzet, Nicolas, Czismadia, Szilárd, Davies, Melvyn B., Deleuil, Magali, Delgado-Mena, Elisa, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dransfield, Georgina, Dumusque, Xavier, Egger, Jo Ann, Ehrenreich, David, Eigmüller, Philipp, Erickson, Anders, Essack, Zahra, Fortier, Andrea, Fossati, Luca, Fridlund, Malcolm, Günther, Maximilian N., Güdel, Manuel, Gandolfi, Davide, Gillard, Harvey, Gillon, Michaël, Gnilka, Crystal, Goad, Michael R., Goeke, Robert F., Guillot, Tristan, Hadjigeorghiou, Andreas, Hellier, Coel, Henderson, Beth A., Heng, Kevin, Hooton, Matthew J., Horne, Keith, Howell, Steve B., Hoyer, Sergio, Irwin, Jonathan M., Jenkins, James S., Jenkins, Jon M., Jensen, Eric L. N., Kane, Stephen R., Kendall, Alicia, Kielkopf, John F., Kiss, Laszlo L., Lacedelli, Gaia, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavalier des, Leleu, Adrien, Lendl, Monika, Lillo-Box, Jorge, Lovis, Christophe, Mékarnia, Djamel, Massey, Bob, Masters, Tamzin, Maxted, Pierre F. L., Nascimbeni, Valerio, Nielsen, Louise D., O'Brien, Sean M., Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Persson, Carina M., Piotto, Giampaolo, Plavchan, Peter, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rauer, Heike, Ribas, Ignasi, Ricker, George, Ségransan, Damien, Salmon, Sébastien, Santerne, Alexandre, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Seager, Sara, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Srdoc, Gregor, Steller, Manfred, Suarez, Olga, Szabó, Gyula M., Teske, Johanna, Thomas, Nicolas, Tilbrook, Rosanna H., Triaud, Amaury H. M. J., Udry, Stéphane, Van Grootel, Valérie, Walton, Nicholas, Wang, Sharon X., Wheatley, Peter J., Winn, Joshua N., Wittenmyer, Robert A., and Zhang, Hui
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright ($T = 8.5$ mag), high proper motion ($\sim\,200$ mas yr$^{-1}$), low metallicity ([Fe/H]$\approx\,-0.28$) K-dwarf with a mass of $0.68\pm0.05$ M$_{\odot}$ and a radius of $0.67\pm0.01$ R$_{\odot}$. We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a $1.70\pm0.07$ R$_{\oplus}$ super-Earth in a 3.82 day orbit, placing it directly within the so-called 'radius valley'. The outer planet, TOI-836 c, is a $2.59\pm0.09$ R$_{\oplus}$ mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of $4.5\pm0.9$ M$_{\oplus}$ , while TOI-836 c has a mass of $9.6\pm2.6$ M$_{\oplus}$. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet.
Published: 2022
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15. Power of wavelets in analyses of transit and phase curves in the presence of stellar variability and instrumental noise. II. Accuracy of the transit parameters

Author: Kálmán, Szilárd, Szabó, Gyula M., and Csizmadia, Szilárd
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Context. Correlated noise in exoplanet light curves, such as noise from stellar activity, convection noise, and instrumental noise, distorts the exoplanet transit light curves and leads to biases in the best-fit transit parameters. An optimal fitting algorithm can provide stability against the presence of correlated noises and lead to statistically consistent results, namely, the actual biases are usually within the error interval. This is not automatically satisfied by most of the algorithms in everyday use and the testing of the algorithms is necessary. Aims. In this paper, we describe a bootstrapping-like test to handle with the general case and we apply it to the wavelet-based Transit and Light Curve Modeller (TLCM) algorithm, testing it for the stability against the correlated noise. We compare and contrast the results with regard to the FITSH algorithm, which is based on an assumption of white noise. Methods. We simulated transit light curves with previously known parameters in the presence of a correlated noise model generated by an Autoregressive Integrated Moving Average (ARIMA) process. Then we solved the simulated observations and examined the resulting parameters and error intervals. Results. We have found that the assumption of FITSH, namely, that only white noise is present, has led to inconsistencies in the results: the distribution of best-fit parameters is then broader than the determined error intervals by a factor of 3-6. On the other hand, the wavelet-based TLCM algorithm handles the correlated noise properly, leading to both properly determined parameter and error intervals that are perfectly consistent with the actual biases, Comment: Accepted for publication in A&A, 11 pages, 8 figures
Published: 2022
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16. Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

Author: Garai, Zoltán, Pribulla, Theodor, Kovács, József, Szabó, Gyula M., Claret, Antonio, Komžík, Richard, and Kundra, Emil
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Rapidly rotating early-type main-sequence stars with transiting planets are interesting in many aspects. Unfortunately, several astrophysical effects in such systems are not well understood yet. Therefore, we performed a photometric mini-survey of three rapidly rotating stars with transiting planets, namely KELT-17b, KELT-19Ab, and KELT-21b, using the Characterising Exoplanets Satellite (CHEOPS), complemented with Transiting Exoplanet Survey Satellite (TESS) data, and spectroscopic data. We aimed at investigating the spin-orbit misalignment and its photometrical signs, therefore the high-quality light curves of the selected objects were tested for transit asymmetry, transit duration variations, and orbital precession. In addition, we performed transit time variation analyses, obtained new stellar parameters, and refined the system parameters. For KELT-17b and KELT-19Ab we obtained significantly smaller planet radius as found before. The gravity-darkening effect is very small compared to the precision of CHEOPS data. We can report only on a tentative detection of the stellar inclination of KELT-21, which is about 60 deg. In KELT-17b and KELT-19Ab we were able to exclude long-term transit duration variations causing orbital precession. The shorter transit duration of KELT-19Ab compared to the discovery paper is probably a consequence of a smaller planet radius. KELT-21b is promising from this viewpoint, but further precise observations are needed. We did not find any convincing evidence for additional objects in the systems., Comment: Accepted for publication in MNRAS
Published: 2022
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17. Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

Author: Osborn, Hugh P., Bonfanti, Andrea, Gandolfi, Davide, Hedges, Christina, Leleu, Adrien, Fortier, Andrea, Futyan, David, Gutermann, Pascal, Maxted, Pierre F. L., Borsato, Luca, Collins, Karen A., da Silva, J. Gomes, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Lendl, Monika, Parviainen, Hannu, Salmon, Sébastien, Schanche, Nicole, Serrano, Luisa M., Sousa, Sergio G., Tuson, Amy, Ulmer-Moll, Solène, Van Grootel, Valerie, Wells, R. D., Wilson, Thomas G., Alibert, Yann, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Biondi, Federico, Bonfils, Xavier, Bouchy, Francois, Brandeker, Alexis, Broeg, Christopher, Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Charnoz, Sébastien, Cameron, Andrew Collier, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demory, Brice-Olivier, Ehrenreich, David, Erikson, Anders, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Gómez-Muñoz, M. A., Güdel, Manuel, Heng, Kevin, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo, Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Magrin, Demetrio, Malavolta, Luca, McCormac, James, Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Demangeon, Olivier D. S., Smith, Alexis M. S., Sabin, L., Santos, Nuno, Scandariato, Gaetano, Schroffenegger, U., Schwarz, Rick P., Shporer, Avi, Simon, Attila E., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Walter, Ingo, and Walton, Nicholas
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Context: TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young ($340\pm80$ Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims: To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods: We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results: CHEOPS observations revealed a clear detection for TOI-2076 c at $P=21.01538^{+0.00084}_{-0.00074}$ d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the $P=35.12537\pm0.00067$ d alias. These observations also improved the radius precision of all three sub-Neptunes to $2.518\pm0.036$, $3.497\pm0.043$, and $3.232\pm0.063$ $R_\oplus$. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST., Comment: 18 pages, 7 figure, 8 tables. Accepted for publication in Astronomy & Astrophysics. Photometry available on CDS/Vizier. Python package presented for modelling duotransiting planet candidates available at https://github.com/hposborn/MonoTools. Modelling & figure-creation code available at https://github.com/hposborn/TOI2076
Published: 2022
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18. Rotation periods and shape asphericity in asteroid families based on TESS S1-S13 observations

Author: Szabó, Gyula M., Pál, András, Szigeti, László, Bognár, Zsófia, Bódi, Attila, Kalup, Csilla, Jäger, Zoltán J., Kiss, László L., Kiss, Csaba, Kovács, József, Marton, Gábor, Molnár, László, Plachy, Emese, Sárneczky, Krisztián, Szakáts, Róbert, and Szabó, Róbert
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Here we present the analysis of the distribution of rotation periods and light curve amplitudes based on 2859 family asteroids in 16 Main Belt families based on 9912 TESS asteroid light curves in the TSSYS-DR1 asteroid light curve database. We found that the distribution of the light curve properties follow a family-specific character in some asteroid families, including the Hungaria, Maria, Juno, Eos, Eucharis, and Alauda families. While in other large families, these distributions are in general very similar to each other. We confirm that older families tend to contain a larger fraction of more spheroidal, low-amplitude asteroids. We found that rotation period distributions are different in the cores and outskirts of the Flora and Maria families, while the Vesta, Eos, and Eunomia families lack this feature. We also confirm that very fast spinning asteroids are close to spherical (or spinning top shapes), and minor planets rotating slower than ~11 hour are also more spherical than asteroids in the 4--8 hour period range and this group is expected to contain the most elongated bodies., Comment: 12 pages, 9 figures, accepted by A&A
Published: 2022
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19. A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Author: Wilson, Thomas G., Goffo, Elisa, Alibert, Yann, Gandolfi, Davide, Bonfanti, Andrea, Persson, Carina M., Cameron, Andrew Collier, Fridlund, Malcolm, Fossati, Luca, Korth, Judith, Benz, Willy, Deline, Adrien, Florén, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sébastien, Sousa, Sérgio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Bárczy, Tamas, Navascues, David Barrado y, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Billot, Nicolas, Bonfils, Xavier, Brandeker, Alexis, Broeg, Christopher, Bryant, Edward M., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Charnoz, Sébastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colón, Knicole D., Crouzet, Nicolas, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier, Demory, Brice-Olivier, Dragomir, Diana, Dransfield, Georgina, Ehrenreich, David, Erikson, Anders, Fortier, Andrea, Gan, Tianjun, Gill, Samuel, Gillon, Michaël, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Güdel, Manuel, Guillot, Tristan, Haldemann, Jonas, Heng, Kevin, Horne, Keith, Howell, Steve B., Isaak, Kate G., Jenkins, Jon M., Jensen, Eric L. N., Kiss, Laszlo, Lacedelli, Gaia, Lam, Kristine, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavelier des, Lendl, Monika, Lester, Kathryn V., Levine, Alan M., Livingston, John, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Marie-Sainte, Wenceslas, Maxted, Pierre F. L., Mayo, Andrew W., McLean, Brian, Mecina, Marko, Mékarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Ségransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stéphane, Van Eylen, Vincent, Van Grootel, Valérie, Vanderspek, Roland K., Viotto, Valentina, Walton, Nicholas, and Winn, Joshua N.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine $T_{\rm eff, \star}=4734\pm67$ K, $R_{\star}=0.726\pm0.007$ $R_{\odot}$, and $M_{\star}=0.748\pm0.032$ $M_{\odot}$. We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of $P_{\rm b}=6.44387\pm0.00003$ d, a radius of $R_{\rm b}=2.59\pm0.04$ $R_{\oplus}$, and a mass of $M_{\rm b}=13.5_{-1.8}^{+1.7}$ $M_{\oplus}$, whilst TOI-1064 c has an orbital period of $P_{\rm c}=12.22657^{+0.00005}_{-0.00004}$ d, a radius of $R_{\rm c}=2.65\pm0.04$ $R_{\oplus}$, and a 3$\sigma$ upper mass limit of 8.5 ${\rm M_{\oplus}}$. From the high-precision photometry we obtain radius uncertainties of $\sim$1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets., Comment: 30 pages, 24 figures, 6 tables including the Appendix; accepted for publication in MNRAS
Published: 2022
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20. Enhanced thermal radiation from a tidally heated exomoon with a single hot spot

Author: Jäger, Zoltán and Szabó, Gyula M
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: An exomoon on a non perfectly circular orbit experiences tidal heating that is capable to significantly contribute to the thermal brightness of the moon. Here we argue that the thermal heat is unevenly distributed on the moon's surface, the emission of the tidal heat is limited to a few hot spots on the surface. A well-known example is the tidally heated Io. Due to their significantly increased temperature, the hot spots enhance the energy emission in thermal wavelengths. We made simulations using Monte-Carlo method to examine this contribution, and to predict about the possible detectability of such a spotted exomoon. We found that in the case of large, Earth sized companions to jupiters around red dwarf stars exhibit a thermal flux that enables the direct detection of the moon, due to its photometric signal that can exceed $\approx$100 ppm in the most favourable configurations., Comment: Accepted by MNRAS, 16 pages
Published: 2021
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21. Transit detection of the long-period volatile-rich super-Earth $\nu^2$ Lupi d with $CHEOPS$

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

Author: Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Da Peppo, Vania, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Di Giorgio, Anna, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Van Eylen, Vincent, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Van der Swaelmen, Mathieu, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Del Vecchio, Ciro, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, and Zuppella, Paola
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution., Comment: Ariel Definition Study Report, 147 pages. Reviewed by ESA Science Advisory Structure in November 2020. Original document available at: https://www.cosmos.esa.int/documents/1783156/3267291/Ariel_RedBook_Nov2020.pdf/
Published: 2021

23. The Rotation of Selected Globular Clusters and the Differential Rotation of M3 in Multiple Populations from the SDSS-IV APOGEE-2 Survey

Author: Szigeti, László, Mészáros, Szabolcs, Szabó, Gyula M., Fernández-Trincado, José G., Lane, Richard R., and Cohen, Roger E.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: In this paper, we analyze 10 globular clusters in order to measure their rotational properties by using high precision radial velocity data from the SDSS-IV APOGEE-2 survey. Out of the 10 clusters we were able to successfully measure the rotation speed and position angle of the rotation axis for 9 clusters (M2, M3, M5, M12, M13, M15, M53, M92, M107). The comparison between our results and previous ones shows a really good agreement within our uncertainties. For four of the globular clusters, M3, M13, M5 and M15, we separated the sample into two generation of stars using their [Al/Fe] abundances and examined the kinematic features of these generations separately from one another. In case of M3, we found significant difference between the rotational properties of first and second populations, confirming for the first time the predictions of several numerical simulations from the literature. The other three clusters (M5, M13, M15) also show smaller deviation between the two groups of stars, but those deviations are comparable to our errors., Comment: 9 pages, 3 figures, 4 tables. Accepted for publication in MNRAS
Published: 2021
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24. Ancillary science with Ariel: Feasibility and scientific potential of young stellar object observations

Author: Gyűrűs, Boldizsár I., Kiss, Csaba, Morales, Juan Carlos, Nakhjiri, Navid, Marton, Gábor, Ábrahám, Péter, Kóspál, Ágnes, Moór, Attila, Szabó, Gyula M., and Szabó, Róbert
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: To investigate the feasibility of ancillary target observations with ESA's Ariel mission, we compiled a list of potentially interesting young stars: FUors, systems harbouring extreme debris discs and a larger sample of young stellar objects showing strong near/mid-infrared excess. These objects can be observed as additional targets in the waiting times between the scheduled exoplanet transit and occultation observations. After analyzing the schedule for Ariel an algorithm was constructed to find the optimal target to be observed in each gap. The selection was mainly based on the slew and stabilization time needed to observe the selected YSO, but it also incorporated the scientific importance of the targets and whether they have already been sufficiently measured. After acquiring an adequately large sample of simulation data, it was concluded that approximately 99.2% of the available -- at least one hour long -- gaps could be used effectively. With an average slewing and stabilization time of about 16.7 minutes between scheduled exoplanet transits and ancillary targets, this corresponds to an additional $2881 \pm 56$ hours of active data gathering. When this additional time is used to observe our selected 200 ancillary targets, a typical signal-to-noise ratio of $\sim$10$^4$ can be achieved along the whole spectral window covered by Ariel., Comment: Accepted for publication in Experimental Astronomy
Published: 2021
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25. A new sample of warm extreme debris disks from the ALLWISE catalog

Author: Moór, Attila, Ábrahám, Péter, Szabó, Gyula, Vida, Krisztián, Cataldi, Gianni, Derekas, Alíz, Henning, Thomas, Kinemuchi, Karen, Kóspál, Ágnes, Kovács, József, Pál, András, Sarkis, Paula, Seli, Bálint, Szabó, Zsófia M., and Takáts, Katalin
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Extreme debris disks (EDDs) are rare systems with peculiarly large amounts of warm dust that may stem from recent giant impacts between planetary embryos during the final phases of terrestrial planet growth. Here we report on the identification and characterization of six new EDDs. These disks surround F5-G9 type main-sequence stars with ages >100 Myr, have dust temperatures higher than 300K and fractional luminosities between 0.01 and 0.07. Using time-domain photometric data at 3.4 and 4.6$\mu$m from the WISE all sky surveys, we conclude that four of these disks exhibited variable mid-infrared emission between 2010 and 2019. Analyzing the sample of all known EDDs, now expanded to 17 objects, we find that 14 of them showed changes at 3-5$\mu$m over the past decade suggesting that mid-infrared variability is an inherent characteristic of EDDs. We also report that wide-orbit pairs are significantly more common in EDD systems than in the normal stellar population. While current models of rocky planet formation predict that the majority of giant collisions occur in the first 100 Myr, we find that the sample of EDDs is dominated by systems older than this age. This raises the possibility that the era of giant impacts may be longer than we think, or that some other mechanism(s) can also produce EDDs. We examine a scenario where the observed warm dust stems from the disruption and/or collisions of comets delivered from an outer reservoir into the inner regions, and explore what role the wide companions could play in this process., Comment: 39 pages, 11 figures, accepted for publication in ApJ
Published: 2021
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26. 101 Trojans: a tale of period bimodality, binaries, and extremely slow rotators from K2 photometry

Author: Kalup, Csilla E., Molnár, László, Kiss, Csaba, Szabó, Gyula M., Pál, András, Szakáts, Róbert, Sárneczky, Krisztián, Vinkó, József, Szabó, Róbert, Kecskeméthy, Viktória, and Kiss, László L.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Various properties of Jovian trojan asteroids such as composition, rotation periods, and photometric amplitudes, or the rate of binarity in the population can provide information and constraints on the evolution of the group and of the Solar System itself. Here we present new photometric properties of 45 Jovian trojans from the K2 mission of the Kepler space telescope, and present phase-folded light curves for 44 targets, including (11351) Leucus, one of the targets of the Lucy mission. We extend our sample to 101 asteroids with previous K2 Trojan measurements, then compare their combined amplitude- and frequency distributions to other ground-based and space data. We show that there is a dichotomy in the periods of Trojans with a separation at $\sim 100$ hr. We find that 25% of the sample are slow rotators (P$\geq$30 hr), which excess can be attributed to binary objects. We also show that 32 systems can be classified as potential detached binary systems. Finally, we calculate density and rotation constraints for the asteroids. Both the spin barrier and fits to strengthless ellipsoid models indicate low densities and thus compositions similar to cometary and TNO populations throughout the sample. This supports the scenario of outer Solar System origin for Jovian trojans., Comment: 25 pages, 19 figures, accepted for publication in ApJS
Published: 2021
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27. Qualitative Assessment of the Occupational Health and Safety Knowledge Management Practices of Hungarian Companies

Author: Faragó, Ferenc, Szabó, Gyula, Kacprzyk, Janusz, Series Editor, Gomide, Fernando, Advisory Editor, Kaynak, Okyay, Advisory Editor, Liu, Derong, Advisory Editor, Pedrycz, Witold, Advisory Editor, Polycarpou, Marios M., Advisory Editor, Rudas, Imre J., Advisory Editor, Wang, Jun, Advisory Editor, Salopek Čubrić, Ivana, editor, Čubrić, Goran, editor, Jambrošić, Kristian, editor, Jurčević Lulić, Tanja, editor, and Sumpor, Davor, editor
Published: 2023
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28. In vivo estrogenicity of glyphosate, its formulations, and AMPA on transgenic zebrafish (Danio rerio) embryos

Author: Tóth, Gergő, Háhn, Judit, Szabó, Gyula, Bakos, Katalin, Volner, Cintia, Liang, Xinyue, Göbölös, Balázs, Bock, Illés, Szoboszlay, Sándor, Urbányi, Béla, Kriszt, Balázs, Kaszab, Edit, Szabó, István, and Csenki, Zsolt
Published: 2024
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29. Long-term study of the bacterial colonization of polypropylene microplastics in a freshwater lake by optical and molecular methods

Author: Szabó, István, Al-Omari, Jafar, Dąbrowska, Agnieszka, Gábor Szerdahelyi, Soma, Sebők, Rózsa, Szabó, Gyula, Micsinai, Adrienn, Kaszab, Edit, Szoboszlay, Sándor, and Kriszt, Balázs
Published: 2024
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30. The CHEOPS mission

Author: Benz, Willy, Broeg, Christopher, Fortier, Andrea, Rando, Nicola, Beck, Thomas, Beck, Mathias, Queloz, Didier, Ehrenreich, David, Maxted, Pierre, Isaak, Kate, Billot, Nicolas, Alibert, Yann, Alonso, Roi, António, Carlos, Asquier, Joel, Bandy, Timothy, Bárczy, Tamas, Barrado, David, Barros, Susana, Baumjohann, Wolfgang, Bekkelien, Anja, Bergomi, Maria, Biondi, Federico, Bonfils, Xavier, Borsato, Luca, Brandeker, Alexis, Busch, Martin-Diego, Cabrera, Juan, Cessa, Virginie, Charnoz, Sébastien, Chazelas, Bruno, Cameron, Andrew Collier, Van Damme, Carlos Corral, Cortes, David, Davies, Melvyn, Deleuil, Magali, Deline, Adrien, Delrez, Laetitia, Demangeon, Olivier, Demory, Brice-Olivier, Erikson, Anders, Farinato, Jacopo, Fossati, Luca, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Munoz, Antonio Garcia, Gillon, Michaël, Guterman, Pascal, Gutierrez, Antonio, Hasiba, Johann, Heng, Kevin, Hernandez, Eduardo, Hoyer, Sergio, Kiss, Laszlo, Kovacs, Zsolt, Kuntzer, Thibault, Laskar, Jacques, Etangs, Alain Lecavelier des, Lendl, Monika, López, Amador, Lora, Ivan, Lovis, Christophe, Lüftinger, Theresa, Magrin, Demetrio, Malvasio, Luca, Marafatto, Luca, Michaelis, Harald, de Miguel, Diana, Modrego, David, Munari, Matteo, Nascimbeni, Valerio, Olofsson, Göran, Ottacher, Harald, Ottensamer, Roland, Pagano, Isabella, Palacios, Roberto, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pizarro, Alberto, Pollaco, Don, Ragazzoni, Roberto, Ratti, Francesco, Rauer, Heike, Ribas, Ignasi, Rieder, Martin, Rohlfs, Reiner, Safa, Frederic, Salatti, Mario, Santos, Nuno, Scandariato, Gaetano, Ségransan, Damien, Simon, Attila, Smith, Alexis, Sordet, Michael, Sousa, Sergio, Steller, Manfred, Szabó, Gyula, Szoke, Janos, Thomas, Nicolas, Tschentscher, Matthias, Udry, Stéphane, Van Grootel, Valérie, Viotto, Valentina, Walter, Ingo, Walton, Nicholas, Wildi, François, and Wolter, David
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The CHaracterising ExOPlanet Satellite (CHEOPS) was selected in 2012, as the first small mission in the ESA Science Programme and successfully launched in December 2019. CHEOPS is a partnership between ESA and Switzerland with important contributions by ten additional ESA Member States. CHEOPS is the first mission dedicated to search for transits of exoplanets using ultrahigh precision photometry on bright stars already known to host planets. As a follow-up mission, CHEOPS is mainly dedicated to improving, whenever possible, existing radii measurements or provide first accurate measurements for a subset of those planets for which the mass has already been estimated from ground-based spectroscopic surveys and to following phase curves. CHEOPS will provide prime targets for future spectroscopic atmospheric characterisation. Requirements on the photometric precision and stability have been derived for stars with magnitudes ranging from 6 to 12 in the V band. In particular, CHEOPS shall be able to detect Earth-size planets transiting G5 dwarf stars in the magnitude range between 6 and 9 by achieving a photometric precision of 20 ppm in 6 hours of integration. For K stars in the magnitude range between 9 and 12, CHEOPS shall be able to detect transiting Neptune-size planets achieving a photometric precision of 85 ppm in 3 hours of integration. This is achieved by using a single, frame-transfer, back-illuminated CCD detector at the focal plane assembly of a 33.5 cm diameter telescope. The 280 kg spacecraft has a pointing accuracy of about 1 arcsec rms and orbits on a sun-synchronous dusk-dawn orbit at 700 km altitude. The nominal mission lifetime is 3.5 years. During this period, 20% of the observing time is available to the community through a yearly call and a discretionary time programme managed by ESA., Comment: Submitted to Experimental Astronomy
Published: 2020
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31. Origin of large meteoritic SiC stardust grains in metal-rich AGB stars

Author: Lugaro, Maria, Cseh, Borbála, Világos, Blanka, Karakas, Amanda I., Ventura, Paolo, Dell'Agli, Flavia, Trappitsch, Reto, Hampel, Melanie, D'Orazi, Valentina, Pereira, Claudio B., Tagliente, Giuseppe, Szabó, Gyula M., Pignatari, Marco, Battino, Umberto, Tattersall, Ashley, Ek, Mattias, Schönbächler, Maria, Hron, Josef, and Nittler, Larry R.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Stardust grains that originated in ancient stars and supernovae are recovered from meteorites and carry the detailed composition of their astronomical sites of origin. We present evidence that the majority of large ($\mu$m-sized) meteoritic silicon carbide (SiC) grains formed in C-rich asymptotic giant branch (AGB) stars that were more metal-rich than the Sun. In the framework of the slow neutron-captures (the s process) that occurs in AGB stars the lower-than-solar 88Sr/86Sr isotopic ratios measured in the large SiC grains can only be accompanied by Ce/Y elemental ratios that are also lower than solar, and predominately observed in metal-rich barium stars - the binary companions of AGB stars. Such an origin suggests that these large grains represent the material from high-metallicity AGB stars needed to explain the s-process nucleosynthesis variations observed in bulk meteorites (Ek et al. 2020). In the outflows of metal-rich, C-rich AGB stars SiC grains are predicted to be small ($\simeq$ 0.2 $\mu$m-sized); large ($\simeq$ $\mu$m-sized) SiC grains can grow if the number of dust seeds is two to three orders of magnitude lower than the standard value of $10^{-13}$ times the number of H atoms. We therefore predict that with increasing metallicity the number of dust seeds might decrease, resulting in the production of larger SiC grains., Comment: accepted for publication in The Astrophysical Journal
Published: 2020
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32. Propagation and mitigation of epidemics in a scale-free network

Author: Szabó, Gyula M.
Subjects: Quantitative Biology - Populations and Evolution, Physics - Physics and Society
Abstract: The epidemic curve and the final extent of the COVID-19 pandemic are usually predicted from the rate of early exponential raising using the SIR model. These predictions implicitly assume a full social mixing, which is not plausible generally. Here I am showing a counterexample to the these predictions, based on random propagation of an epidemic in Barab\'asi--Albert scale-free network models. The start of the epidemic suggests $R_0=2.6$, but unlike $\Omega\approx 70\%{}$ predicted by the SIR model, they reach a final extent of only $\Omega\approx 4\%{}$ without external mitigation and $\Omega\approx 0.5$--$1.5\%{}$ with mitigation. Daily infection rate at the top is also 1--1.5 orders of magnitude less than in SIR models. Quarantining only the 1.5\%{} most active superspreaders has similar effect on extent and top infection rate as blind quarantining a random 50\%{} of the full community., Comment: 8 pages, 5 figures. Currently submitted to ArXiv only and waiting for comments
Published: 2020

33. Rotational properties of Hilda asteroids observed by the K2 mission

Author: Szabó, Gyula M., Kiss, Csaba, Szakáts, Róbert, Pál, András, Molnár, László, Sárneczky, Krisztián, Vinkó, József, Szabó, Róbert, Marton, Gábor, and Kiss, László L.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Hilda asteroids orbit at the outer edge, or just outside of the Main Belt, occupying the 2:3 mean motion resonance with Jupiter. It is known that the group shows a mixed taxonomy that suggests the mixed origin of Hilda members, having migrated to the current orbit both from the outer Main Belt and from the Trojans swarms. But there are still few observations for comparative studies that help in understanding the Hilda group in deeper details. We identified 125 individual light curves of Hilda asteroids observed by the K2 mission. We found that despite of the mixed taxonomies, the Hilda group highly resembles to the Trojans in the distribution of rotation periods and amplitudes, and even the LR group (mostly C and X-type) Hildas follow this rule. Contrary to the Main Belt, Hilda group lacks the very fast rotators. The ratio of extremely slow rotators (P>100 h) is a surprising 18%, which is unique in the Solar System. The occurrence rate of asteroids with multiple periods (4%) and asteroids with three maxima in the light curves (5%) can be signs of high rate of binarity, which we can estimate as 25% within the Hilda group., Comment: ApJS, in press, 28 pages
Published: 2020
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34. Solar System objects observed with TESS -- First data release: bright main-belt and Trojan asteroids from the Southern Survey

Author: Pál, András, Szakáts, Róbert, Kiss, Csaba, Bódi, Attila, Bognár, Zsófia, Kalup, Csilla, Kiss, László L., Marton, Gábor, Molnár, László, Plachy, Emese, Sárneczky, Krisztián, Szabó, Gyula M., and Szabó, Róbert
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Compared with previous space-borne surveys, the Transiting Exoplanet Survey Satellite (TESS) provides a unique and new approach to observe Solar System objects. While its primary mission avoids the vicinity of the ecliptic plane by approximately six degrees, the scale height of the Solar System debris disk is large enough to place various small body populations in the field-of-view. In this paper we present the first data release of photometric analysis of TESS observations of small Solar System Bodies, focusing on the bright end of the observed main-belt asteroid and Jovian Trojan populations. This data release, named TSSYS-DR1, contains 9912 light curves obtained and extracted in a homogeneous manner, and triples the number of bodies with unambiguous fundamental rotation characteristics, namely where accurate periods and amplitudes are both reported. Our catalogue clearly shows that the number of bodies with long rotation periods are definitely underestimated by all previous ground-based surveys, by at least an order of magnitude., Comment: ApJS, in press. Data are available from https://archive.konkoly.hu/pub/tssys/dr1/ (6.36G, in total)
Published: 2020
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35. Plumage color degradation indicates reproductive effort: an experiment

Author: Hegyi, Gergely, Laczi, Miklós, Szabó, Gyula, Sarkadi, Fanni, and Török, János
Published: 2023
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36. Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

Author: Garai, Zoltán, Pribulla, Theodor, Komžík, Richard, Kundra, Emil, Hambálek, Ľubomír, and Szabó, Gyula M.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Only a few exoplanets are known to orbit around fast rotating stars. One of them is XO-6b, which orbits an F5V-type star. Shortly after the discovery, we started multicolor photometric and radial-velocity follow-up observations of XO-6b, using the telescopes of Astronomical Institute of the Slovak Academy of Sciences. Our main scientific goals were to better characterize the planetary system and to search for transit timing variations. We refined several planetary and orbital parameters. Based on our measurements, the planet XO-6b seems to be about 10% larger, which is, however, only about $2\sigma$ difference, but its orbit inclination angle, with respect to the plane of the sky, seems to be significantly smaller, than it was determined originally by the discoverers. In this case we found about $9.5\sigma$ difference. Moreover, we observed periodic transit timing variations of XO-6b with a semi-amplitude of about 14 min and with a period of about 450 days. There are two plausible explanations of such transit timing variations: (1) a third object in the system XO-6 causing light-time effect, or (2) resonant perturbations between the transiting planet XO-6b and another unknown low-mass planet in this system. From the O-C diagram we derived that the assumed third object in the system should have a stellar mass, therefore significant variations are expected in the radial-velocity measurements of XO-6. Since this is not the case, and since all attempts to fit radial velocities and O-C data simultaneously failed to provide a consistent solution, more realistic is the second explanation., Comment: Accepted for publication in MNRAS
Published: 2019
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37. The Detailed Science Case for the Maunakea Spectroscopic Explorer, 2019 edition

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

38. The sub-Jovian desert of exoplanets: parameter dependent boundaries and implications on planet formation

Author: Szabó, Gyula M. and Kálmán, Szilárd
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The period-mass and period-radius distribution of exoplanets is known to exhibit a desert. Unlike the existence of very hot ($P_{\rm orb}<3$d) super-Earths and hot Jupiters, no planets are known between a super Earths and sub-Jupiters with as short orbital periods as a day or two. In this Letter, we show that the period boundary of this desert is dependent on stellar parameters ($T_{\rm eff}$, $[M/H]$, $\log g$ in the order of significance), there is a conclusive dependence on the incident stellar irradiation, and a dependence on the stellar mass acting only on planets around $T_{\rm eff}<5600$K host stars. We found a significant lack of very inflated planets on closest orbits to the host star. There is no significant dependence on tidal forces currently acting on the planet, planet's surface gravity, or current filling factor of Roche lobe. These distributions are most compatible with the dominant role of photoevaporation in forming the desert., Comment: 5 pages, 4 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society Letters
Published: 2019
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39. Stellar Astrophysics and Exoplanet Science with the Maunakea Spectroscopic Explorer (MSE)

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

40. Qualitative Assessment of the Occupational Health and Safety Knowledge Management Practices of Hungarian Companies

Author: Faragó, Ferenc, primary and Szabó, Gyula, additional
Published: 2023
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41. Arguments for Emerging Technologies Applications to Improve Manufacturing Warehouse Ergonomics

Author: Mocan, Anca, Gaureanu, Alin, Szabó, Gyula, Mrugalska, Beata, Howlett, Robert J., Series Editor, Littlewood, John, Series Editor, Jain, Lakhmi C., Series Editor, Draghici, Anca, editor, and Ivascu, Larisa, editor
Published: 2022
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42. The First Post-Kepler Brightness Dips of KIC 8462852

Author: Boyajian, Tabetha S., Alonso, Roi, Ammerman, Alex, Armstrong, David, Ramos, A. Asensio, Barkaoui, K., Beatty, Thomas G., Benkhaldoun, Z., Benni, Paul, Bentley, Rory, Berdyugin, Andrei, Berdyugina, Svetlana, Bergeron, Serge, Bieryla, Allyson, Blain, Michaela G., Blanco, Alicia Capetillo, Bodman, Eva H. L., Boucher, Anne, Bradley, Mark, Brincat, Stephen M., Brink, Thomas G., Briol, John, Brown, David J. A., Budaj, J., Burdanov, A., Cale, B., Carbo, Miguel Aznar, Garcia, R. Castillo, Clark, Wendy J, Clayton, Geoffrey C., Clem, James L., Coker, Phillip H, Cook, Evan M., Copperwheat, Chris M., Curtis, J., Cutri, R. M., Cseh, B., Cynamon, C. H., Daniels, Alex J., Davenport, James R. A., Deeg, Hans J., De Lorenzo, Roberto, De Jaeger, Thomas, Desrosiers, Jean-Bruno, Dolan, John, Dowhos, D. J., Dubois, Franky, Durkee, R., Dvorak, Shawn, Easley, Lynn, Edwards, N., Ellis, Tyler G., Erdelyi, Emery, Ertel, Steve, Farfán, Rafael. G., Farihi, J., Filippenko, Alexei V., Foxell, Emma, Gandolfi, Davide, Garcia, Faustino, Giddens, F., Gillon, M., González-Carballo, Juan-Luis, González-Fernández, C., Hernández, J. I. González, Graham, Keith A., Greene, Kenton A., Gregorio, J., Hallakoun, Na'ama, Hanyecz, Ottó, Harp, G. R., Henry, Gregory W., Herrero, E., Hildbold, Caleb F., Hinzel, D., Holgado, G., Ignácz, Bernadett, Ivanov, Valentin D., Jehin, E., Jermak, Helen E., Johnston, Steve, Kafka, S., Kalup, Csilla, Kardasis, Emmanuel, Kaspi, Shai, Kennedy, Grant M., Kiefer, F., Kielty, C. L., Kessler, Dennis, Kiiskinen, H., Killestein, T. L., King, Ronald A., Kollar, V., Korhonen, H., Kotnik, C., Könyves-Tóth, Réka, Kriskovics, Levente, Krumm, Nathan, Krushinsky, Vadim, Kundra, E., Lachapelle, Francois-Rene, Lacourse, D., Lake, P., Lam, Kristine, Lamb, Gavin P., Lane, Dave, Lau, Marie Wingyee, Lewin, Pablo, Lintott, Chris, Lisse, Carey, Logie, Ludwig, Longeard, Nicolas, Villanueva, M. Lopez, Ludington, E. Whit, Mainzer, A., Malo, Lison, Maloney, Chris, Mann, A., Mantero, A., Marengo, Massimo, Marchant, Jon, González, M. J. Martinez, Masiero, Joseph R., Mauerhan, Jon C., Mccormac, James, Mcneely, Aaron, Meng, Huan Y. A., Miller, Mike, Molnar, Lawrence A., Morales, J. C., Morris, Brett M., Muterspaugh, Matthew W., Nespral, David, Nugent, C. R., Nugent, Katherine M., Odasso, A., O'keeffe, Derek, Oksanen, A., O'meara, John M., Ordasi, András, Osborn, Hugh, Ott, John J., Parks, J. R., Perez, Diego Rodriguez, Petriew, Vance, Pickard, R., Pál, András, Plavchan, P., Plaza, C. Westendorp, Pollacco, Don, Nuñez, F. Pozo, Pozuelos, F. J., Rau, Steve, Redfield, Seth, Relles, Howard, Ribas, I., Richards, Jon, Saario, Joonas L. O., Safron, Emily J., Sallai, J. Martin, Sárneczky, Krisztián, Schaefer, Bradley E., Schumer, Clea F., Schwartzendruber, Madison, Siegel, Michael H., Siemion, Andrew P. V., Simmons, Brooke D., Simon, Joshua D., Simón-Diaz, S., Sitko, Michael L., Socas-Navarro, Hector, Sódor, Á., Starkey, Donn, Steele, Iain A., Stone, Geoff, Street, R. A., Sullivan, Tricia, Suomela, J., Swift, J. J., Szabó, Gyula M., Szabó, Róbert, Szakáts, Róbert, Szalai, Tamás, Tanner, Angelle M., Toledo-Padrón, B., Tordai, Tamás, Triaud, Amaury H. M. J., Turner, Jake D., Ulowetz, Joseph H., Urbanik, Marian, Vanaverbeke, Siegfried, Vanderburg, Andrew, Vida, Krisztián, Vietje, Brad P., Vinkó, József, Von Braun, K., Waagen, Elizabeth O., Walsh, Dan, Watson, Christopher A., Weir, R. C., Wenzel, Klaus, Williamson, Michael W., Wright, Jason T., Wyatt, M. C., Zheng, Weikang, and Zsidi, Gabriella
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present a photometric detection of the first brightness dips of the unique variable star KIC 8462852 since the end of the Kepler space mission in 2013 May. Our regular photometric surveillance started in October 2015, and a sequence of dipping began in 2017 May continuing on through the end of 2017, when the star was no longer visible from Earth. We distinguish four main 1-2.5% dips, named "Elsie," "Celeste," "Skara Brae," and "Angkor", which persist on timescales from several days to weeks. Our main results so far are: (i) there are no apparent changes of the stellar spectrum or polarization during the dips; (ii) the multiband photometry of the dips shows differential reddening favoring non-grey extinction. Therefore, our data are inconsistent with dip models that invoke optically thick material, but rather they are in-line with predictions for an occulter consisting primarily of ordinary dust, where much of the material must be optically thin with a size scale <<1um, and may also be consistent with models invoking variations intrinsic to the stellar photosphere. Notably, our data do not place constraints on the color of the longer-term "secular" dimming, which may be caused by independent processes, or probe different regimes of a single process., Comment: 19 pages, 8 figures, accepted for publication in ApJL
Published: 2018
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43. Exploiting the transit timing capabilities of Ariel

Author: Borsato, Luca, Nascimbeni, Valerio, Piotto, Giampaolo, and Szabó, Gyula
Published: 2022
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44. High-precision photometry with Ariel

Author: Szabó, Gyula M., Kálmán, Szilárd, Pribulla, Theodor, Claret, Antonio, Mugnai, Lorenzo V., Pascale, Enzo, Waltham, Dave, Borsato, Luca, Garai, Zoltán, and Szabó, Róbert
Published: 2022
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45. Explaining the elongated shape of 'Oumuamua by the Eikonal abrasion model

Author: Domokos, Gábor, Sipos, András A., Szabó, Gyula M., and Várkonyi, Péter L.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The photometry of the minor body with extrasolar origin (1I/2017 U1) 'Oumuamua revealed an unprecedented shape: Meech et al. (2017) reported a shape elongation b/a close to 1/10, which calls for theoretical explanation. Here we show that the abrasion of a primordial asteroid by a huge number of tiny particles ultimately leads to such elongated shape. The model (called the Eikonal equation) predicting this outcome was already suggested in Domokos et al. (2009) to play an important role in the evolution of asteroid shapes., Comment: Accepted by the Research Notes of the AAS
Published: 2017
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46. The European Machinery Directive: A Challenge for Manufacturers and Users

Author: Etienne, Pascal, Zunjic, Aleksandar, Ferreira, Pedro, Michez, Bernard, Szabó, Gyula, Kacprzyk, Janusz, Series Editor, Gomide, Fernando, Advisory Editor, Kaynak, Okyay, Advisory Editor, Liu, Derong, Advisory Editor, Pedrycz, Witold, Advisory Editor, Polycarpou, Marios M., Advisory Editor, Rudas, Imre J., Advisory Editor, Wang, Jun, Advisory Editor, Black, Nancy L., editor, Neumann, W. Patrick, editor, and Noy, Ian, editor
Published: 2021
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47. Modified NIOSH Lifting Equation with MATLAB

Author: Szabó, Gyula, Kacprzyk, Janusz, Series Editor, Pal, Nikhil R., Advisory Editor, Bello Perez, Rafael, Advisory Editor, Corchado, Emilio S., Advisory Editor, Hagras, Hani, Advisory Editor, Kóczy, László T., Advisory Editor, Kreinovich, Vladik, Advisory Editor, Lin, Chin-Teng, Advisory Editor, Lu, Jie, Advisory Editor, Melin, Patricia, Advisory Editor, Nedjah, Nadia, Advisory Editor, Nguyen, Ngoc Thanh, Advisory Editor, Wang, Jun, Advisory Editor, Sumpor, Davor, editor, Jambrošić, Kristian, editor, Jurčević Lulić, Tanja, editor, Milčić, Diana, editor, Salopek Čubrić, Ivana, editor, and Šabarić, Irena, editor
Published: 2021
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48. Evolution of a Work-Related Musculoskeletal Disorder Risk Assessment Tool. The Case of CERA

Author: Szabó, Gyula, Kacprzyk, Janusz, Series Editor, Pal, Nikhil R., Advisory Editor, Bello Perez, Rafael, Advisory Editor, Corchado, Emilio S., Advisory Editor, Hagras, Hani, Advisory Editor, Kóczy, László T., Advisory Editor, Kreinovich, Vladik, Advisory Editor, Lin, Chin-Teng, Advisory Editor, Lu, Jie, Advisory Editor, Melin, Patricia, Advisory Editor, Nedjah, Nadia, Advisory Editor, Nguyen, Ngoc Thanh, Advisory Editor, Wang, Jun, Advisory Editor, Karwowski, Waldemar, editor, Goonetilleke, Ravindra S., editor, Xiong, Shuping, editor, Goossens, Richard H. M., editor, and Murata, Atsuo, editor
Published: 2020
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49. The Characteristics of Industrial Safety Risk Management

Author: Szabó, Gyula, Kacprzyk, Janusz, Series Editor, Pal, Nikhil R., Advisory Editor, Bello Perez, Rafael, Advisory Editor, Corchado, Emilio S., Advisory Editor, Hagras, Hani, Advisory Editor, Kóczy, László T., Advisory Editor, Kreinovich, Vladik, Advisory Editor, Lin, Chin-Teng, Advisory Editor, Lu, Jie, Advisory Editor, Melin, Patricia, Advisory Editor, Nedjah, Nadia, Advisory Editor, Nguyen, Ngoc Thanh, Advisory Editor, Wang, Jun, Advisory Editor, Arezes, Pedro M., editor, and Boring, Ronald L., editor
Published: 2020
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50. Applicability of diatom metabarcoding in the ecological status assessment of Hungarian lotic and soda pan habitats

Author: Duleba, Mónika, Földi, Angéla, Micsinai, Adrienn, Várbíró, Gábor, Mohr, Anita, Sipos, Rita, Szabó, Gyula, Buczkó, Krisztina, Trábert, Zsuzsa, Kiss, Keve T., Bíró, Tibor, Vadkerti, Edit, and Ács, Éva
Published: 2021
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