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1. The PLATO Mission

Author: Rauer, Heike, Aerts, Conny, Cabrera, Juan, Deleuil, Magali, Erikson, Anders, Gizon, Laurent, Goupil, Mariejo, Heras, Ana, Lorenzo-Alvarez, Jose, Marliani, Filippo, Martin-Garcia, Cesar, Mas-Hesse, J. Miguel, O'Rourke, Laurence, Osborn, Hugh, Pagano, Isabella, Piotto, Giampaolo, Pollacco, Don, Ragazzoni, Roberto, Ramsay, Gavin, Udry, Stéphane, Appourchaux, Thierry, Benz, Willy, Brandeker, Alexis, Güdel, Manuel, Janot-Pacheco, Eduardo, Kabath, Petr, Kjeldsen, Hans, Min, Michiel, Santos, Nuno, Smith, Alan, Suarez, Juan-Carlos, Werner, Stephanie C., Aboudan, Alessio, Abreu, Manuel, Acuña, Lorena, Adams, Moritz, Adibekyan, Vardan, Affer, Laura, Agneray, François, Agnor, Craig, Børsen-Koch, Victor Aguirre, Ahmed, Saad, Aigrain, Suzanne, Al-Bahlawan, Ashraf, Gil, M de los Angeles Alcacera, Alei, Eleonora, Alencar, Silvia, Alexander, Richard, Alfonso-Garzón, Julia, Alibert, Yann, Prieto, Carlos Allende, Almeida, Leonardo, Sobrino, Roi Alonso, Altavilla, Giuseppe, Althaus, Christian, Trujillo, Luis Alonso Alvarez, Amarsi, Anish, Eiff, Matthias Ammler-von, Amôres, Eduardo, Andrade, Laerte, Antoniadis-Karnavas, Alexandros, António, Carlos, del Moral, Beatriz Aparicio, Appolloni, Matteo, Arena, Claudio, Armstrong, David, Aliaga, Jose Aroca, Asplund, Martin, Audenaert, Jeroen, Auricchio, Natalia, Avelino, Pedro, Baeke, Ann, Baillié, Kevin, Balado, Ana, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebastià Barceló, Barker, Adrian, Barklem, Paul, Barnes, Sydney, Navascues, David Barrado, Barragan, Oscar, Baruteau, Clément, Basu, Sarbani, Baudin, Frederic, Baumeister, Philipp, Bayliss, Daniel, Bazot, Michael, Beck, Paul G., Bedding, Tim, Belkacem, Kevin, Bellinger, Earl, Benatti, Serena, Benomar, Othman, Bérard, Diane, Bergemann, Maria, Bergomi, Maria, Bernardo, Pierre, Biazzo, Katia, Bignamini, Andrea, Bigot, Lionel, Billot, Nicolas, Binet, Martin, Biondi, David, Biondi, Federico, Birch, Aaron C., Bitsch, Bertram, Ceballos, Paz Victoria Bluhm, Bódi, Attila, Bognár, Zsófia, Boisse, Isabelle, Bolmont, Emeline, Bonanno, Alfio, Bonavita, Mariangela, Bonfanti, Andrea, Bonfils, Xavier, Bonito, Rosaria, Bonomo, Aldo Stefano, Börner, Anko, Saikia, Sudeshna Boro, Martín, Elisa Borreguero, Borsa, Francesco, Borsato, Luca, Bossini, Diego, Bouchy, Francois, Boué, Gwenaël, Boufleur, Rodrigo, Boumier, Patrick, Bourrier, Vincent, Bowman, Dominic M., Bozzo, Enrico, Bradley, Louisa, Bray, John, Bressan, Alessandro, Breton, Sylvain, Brienza, Daniele, Brito, Ana, Brogi, Matteo, Brown, Beverly, Brown, David, Brun, Allan Sacha, Bruno, Giovanni, Bruns, Michael, Buchhave, Lars A., Bugnet, Lisa, Buldgen, Gaël, Burgess, Patrick, Busatta, Andrea, Busso, Giorgia, Buzasi, Derek, Caballero, José A., Cabral, Alexandre, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, Martins, Bruno Leonardo Canto, Cara, Christophe, Carone, Ludmila, Carrasco, Josep Manel, Casagrande, Luca, Casewell, Sarah L., Cassisi, Santi, Castellani, Marco, Castro, Matthieu, Catala, Claude, Fernández, Irene Catalán, Catelan, Márcio, Cegla, Heather, Cerruti, Chiara, Cessa, Virginie, Chadid, Merieme, Chaplin, William, Charpinet, Stephane, Chiappini, Cristina, Chiarucci, Simone, Chiavassa, Andrea, Chinellato, Simonetta, Chirulli, Giovanni, Christensen-Dalsgaard, Jorgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, Conseil, Simon, Corbard, Thierry, Correia, Alexandre C. M., Corsaro, Enrico, Cosentino, Rosario, Costes, Jean, Cottinelli, Andrea, Covone, Giovanni, Creevey, Orlagh L., Crida, Aurelien, Csizmadia, Szilard, Cunha, Margarida, Curry, Patrick, da Costa, Jefferson, da Silva, Francys, Dalal, Shweta, Damasso, Mario, Damiani, Cilia, Damiani, Francesco, Chagas, Maria Liduina das, Davies, Melvyn, Davies, Guy, Davies, Ben, Davison, Gary, de Almeida, Leandro, de Angeli, Francesca, de Barros, Susana Cristina Cabral, Leão, Izan de Castro, de Freitas, Daniel Brito, de Freitas, Marcia Cristina, De Martino, Domitilla, de Medeiros, José Renan, de Paula, Luiz Alberto, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Degl'Innocenti, Scilla, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, Desidera, Silvano, Dexet, Marc, Di Criscienzo, Marcella, Di Giorgio, Anna Maria, Di Mauro, Maria Pia, Rial, Federico Jose Diaz, Díaz-García, José-Javier, Dima, Marco, Dinuzzi, Giacomo, Dionatos, Odysseas, Distefano, Elisa, Nascimento Jr., Jose-Dias do, Domingo, Albert, D'Orazi, Valentina, Dorn, Caroline, Doyle, Lauren, Duarte, Elena, Ducellier, Florent, Dumaye, Luc, Dumusque, Xavier, Dupret, Marc-Antoine, Eggenberger, Patrick, Ehrenreich, David, Eigmüller, Philipp, Eising, Johannes, Emilio, Marcelo, Eriksson, Kjell, Ermocida, Marco, Giribaldi, Riano Isidoro Escate, Eschen, Yoshi, Estrela, Inês, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, Ferrari, Lorenza, Ferraz-Mello, Sylvio, Fialho, Fabio, Fienga, Agnes, Figueira, Pedro, Fiori, Laura, Flaccomio, Ettore, Focardi, Mauro, Foley, Steve, Fontignie, Jean, Ford, Dominic, Fornazier, Karin, Forveille, Thierry, Fossati, Luca, Franca, Rodrigo de Marca, da Silva, Lucas Franco, Frasca, Antonio, Fridlund, Malcolm, Furlan, Marco, Gabler, Sarah-Maria, Gaido, Marco, Gallagher, Andrew, Galli, Emanuele, Garcia, Rafael A., Hernández, Antonio García, Munoz, Antonio Garcia, García-Vázquez, Hugo, Haba, Rafael Garrido, Gaulme, Patrick, Gauthier, Nicolas, Gehan, Charlotte, Gent, Matthew, Georgieva, Iskra, Ghigo, Mauro, Giana, Edoardo, Gill, Samuel, Girardi, Leo, Winter, Silvia Giuliatti, Giusi, Giovanni, da Silva, João Gomes, Zazo, Luis Jorge Gómez, Gomez-Lopez, Juan Manuel, Hernández, Jonay Isai González, Murillo, Kevin Gonzalez, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, Grießbach, Denis, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Loïc, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, Guiot, Pierre, Guterman, Pascal, Gutiérrez, Antonio, Gutiérrez-Canales, Fernando, Hagelberg, Janis, Haldemann, Jonas, Hall, Cassandra, Handberg, Rasmus, Harrison, Ian, Harrison, Diana L., Hasiba, Johann, Haswell, Carole A., Hatalova, Petra, Hatzes, Artie, Haywood, Raphaelle, Hébrard, Guillaume, Heckes, Frank, Heiter, Ulrike, Hekker, Saskia, Heller, René, Helling, Christiane, Helminiak, Krzysztof, Hemsley, Simon, Heng, Kevin, Hermans, Aline, Hermes, JJ, Torres, Nadia Hidalgo, Hinkel, Natalie, Hobbs, David, Hodgkin, Simon, Hofmann, Karl, Hojjatpanah, Saeed, Houdek, Günter, Huber, Daniel, Huesler, Joseph, Hui-Bon-Hoa, Alain, Huygen, Rik, Huynh, Duc-Dat, Iro, Nicolas, Irwin, Jonathan, Irwin, Mike, Izidoro, André, Jacquinod, Sophie, Jannsen, Nicholas Emborg, Janson, Markus, Jeszenszky, Harald, Jiang, Chen, Mancebo, Antonio José Jimenez, Jofre, Paula, Johansen, Anders, Johnston, Cole, Jones, Geraint, Kallinger, Thomas, Kálmán, Szilárd, Kanitz, Thomas, Karjalainen, Marie, Karjalainen, Raine, Karoff, Christoffer, Kawaler, Steven, Kawata, Daisuke, Keereman, Arnoud, Keiderling, David, Kennedy, Tom, Kenworthy, Matthew, Kerschbaum, Franz, Kidger, Mark, Kiefer, Flavien, Kintziger, Christian, Kislyakova, Kristina, Kiss, László, Klagyivik, Peter, Klahr, Hubert, Klevas, Jonas, Kochukhov, Oleg, Köhler, Ulrich, Kolb, Ulrich, Koncz, Alexander, Korth, Judith, Kostogryz, Nadiia, Kovács, Gábor, Kovács, József, Kozhura, Oleg, Krivova, Natalie, Kučinskas, Arunas, Kuhlemann, Ilyas, Kupka, Friedrich, Laauwen, Wouter, Labiano, Alvaro, Lagarde, Nadege, Laget, Philippe, Laky, Gunter, Lam, Kristine Wai Fun, Lambrechts, Michiel, Lammer, Helmut, Lanza, Antonino Francesco, Lanzafame, Alessandro, Martiz, Mariel Lares, Laskar, Jacques, Latter, Henrik, Lavanant, Tony, Lawrenson, Alastair, Lazzoni, Cecilia, Lebre, Agnes, Lebreton, Yveline, Etangs, Alain Lecavelier des, Leinhardt, Zoe, Leleu, Adrien, Lendl, Monika, Leto, Giuseppe, Levillain, Yves, Libert, Anne-Sophie, Lichtenberg, Tim, Ligi, Roxanne, Lignieres, Francois, Lillo-Box, Jorge, Linsky, Jeffrey, Liu, John Scige, Loidolt, Dominik, Longval, Yuying, Lopes, Ilídio, Lorenzani, Andrea, Ludwig, Hans-Guenter, Lund, Mikkel, Lundkvist, Mia Sloth, Luri, Xavier, Maceroni, Carla, Madden, Sean, Madhusudhan, Nikku, Maggio, Antonio, Magliano, Christian, Magrin, Demetrio, Mahy, Laurent, Maibaum, Olaf, Malac-Allain, LeeRoy, Malapert, Jean-Christophe, Malavolta, Luca, Maldonado, Jesus, Mamonova, Elena, Manchon, Louis, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, Érico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, Figueiredo, Ana Carolina Mattiuci, Maxted, Pierre F. L., Mazeh, Tsevi, Mazevet, Stephane, Mazzei, Francesco, McCormac, James, McMillan, Paul, Menou, Lucas, Merle, Thibault, Meru, Farzana, Mesa, Dino, Messina, Sergio, Mészáros, Szabolcs, Meunier, Nadége, Meunier, Jean-Charles, Micela, Giuseppina, Michaelis, Harald, Michel, Eric, Michielsen, Mathias, Michtchenko, Tatiana, Miglio, Andrea, Miguel, Yamila, Milligan, David, Mirouh, Giovanni, Mitchell, Morgan, Moedas, Nuno, Molendini, Francesca, Molnár, László, Mombarg, Joey, Montalban, Josefina, Montalto, Marco, Monteiro, Mário J. P. F. G., Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Benoît, Mourard, Denis, Mousis, Olivier, Moutou, Claire, Mowlavi, Nami, Moya, Andrés, Muehlmann, Prisca, Muirhead, Philip, Munari, Matteo, Musella, Ilaria, Mustill, Alexander James, Nardetto, Nicolas, Nardiello, Domenico, Narita, Norio, Nascimbeni, Valerio, Nash, Anna, Neiner, Coralie, Nelson, Richard P., Nettelmann, Nadine, Nicolini, Gianalfredo, Nielsen, Martin, Niemi, Sami-Matias, Noack, Lena, Noels-Grotsch, Arlette, Noll, Anthony, Norazman, Azib, Norton, Andrew J., Nsamba, Benard, Ofir, Aviv, Ogilvie, Gordon, Olander, Terese, Olivetto, Christian, Olofsson, Göran, Ong, Joel, Ortolani, Sergio, Oshagh, Mahmoudreza, Ottacher, Harald, Ottensamer, Roland, Ouazzani, Rhita-Maria, Paardekooper, Sijme-Jan, Pace, Emanuele, Pajas, Miriam, Palacios, Ana, Palandri, Gaelle, Palle, Enric, Paproth, Carsten, Parro, Vanderlei, Parviainen, Hannu, Granado, Javier Pascual, Passegger, Vera Maria, Pastor-Morales, Carmen, Pätzold, Martin, Pedersen, May Gade, Hidalgo, David Pena, Pepe, Francesco, Pereira, Filipe, Persson, Carina M., Pertenais, Martin, Peter, Gisbert, Petit, Antoine C., Petit, Pascal, Pezzuto, Stefano, Pichierri, Gabriele, Pietrinferni, Adriano, Pinheiro, Fernando, Pinsonneault, Marc, Plachy, Emese, Plasson, Philippe, Plez, Bertrand, Poppenhaeger, Katja, Poretti, Ennio, Portaluri, Elisa, Portell, Jordi, de Mello, Gustavo Frederico Porto, Poyatos, Julien, Pozuelos, Francisco J., Moroni, Pier Giorgio Prada, Pricopi, Dumitru, Prisinzano, Loredana, Quade, Matthias, Quirrenbach160, ndreas, Reina6, Julio Arturo Rabanal, Soares, Maria Cristina Rabello, Raimondo, Gabriella, Rainer, Monica, Rodón, Jose Ramón, Ramón-Ballesta, Alejandro, Zapata, Gonzalo Ramos, Rätz, Stefanie, Rauterberg, Christoph, Redman, Bob, Redmer, Ronald, Reese, Daniel, Regibo, Sara, Reiners, Ansgar, Reinhold, Timo, Renie, Christian, Ribas, Ignasi, Ribeiro, Sergio, Ricciardi, Thiago Pereira, Rice, Ken, Richard, Olivier, Riello, Marco, Rieutord, Michel, Ripepi, Vincenzo, Rixon, Guy, Rockstein, Steve, Rodríguez, María Teresa Rodrigo, Díaz, Luisa Fernanda Rodríguez, Garcia, Juan Pablo Rodriguez, Rodriguez-Gomez, Julio, Roehlly, Yannick, Roig, Fernando, Rojas-Ayala, Bárbara, Rolf, Tobias, Rørsted, Jakob Lysgaard, Rosado, Hugo, Rosotti, Giovanni, Roth, Olivier, Roth, Markus, Rousseau, Alex, Roxburgh, Ian, Roy, Fabrice, Royer, Pierre, Ruane, Kirk, Mastropasqua, Sergio Rufini, de Galarreta, Claudia Ruiz, Russi, Andrea, Saar, Steven, Saillenfest, Melaine, Salaris, Maurizio, Salmon, Sebastien, Saltas, Ippocratis, Samadi, Réza, Samadi, Aunia, Samra, Dominic, da Silva, Tiago Sanches, Carrasco, Miguel Andrés Sánchez, Santerne, Alexandre, Santoli, Francesco, Santos, Ângela R. G., Mesa, Rosario Sanz, Sarro, Luis Manuel, Scandariato, Gaetano, Schäfer, Martin, Schlafly, Edward, Schmider, François-Xavier, Schneider, Jean, Schou, Jesper, Schunker, Hannah, Schwarzkopf, Gabriel Jörg, Serenelli, Aldo, Seynaeve, Dries, Shan, Yutong, Shapiro, Alexander, Shipman, Russel, Sicilia, Daniela, Sanmartin, Maria Angeles Sierra, Sigot, Axelle, Silliman, Kyle, Silvotti, Roberto, Simon, Attila E., Napoli, Ricardo Simoyama, Skarka, Marek, Smalley, Barry, Smiljanic, Rodolfo, Smit, Samuel, Smith, Alexis, Smith, Leigh, Snellen, Ignas, Sódor, Ádám, Sohl, Frank, Solanki, Sami K., Sortino, Francesca, Sousa, Sérgio, Southworth, John, Souto, Diogo, Sozzetti, Alessandro, Stamatellos, Dimitris, Stassun, Keivan, Steller, Manfred, Stello, Dennis, Stelzer, Beate, Stiebeler, Ulrike, Stokholm, Amalie, Storelvmo, Trude, Strassmeier, Klaus, Strøm, Paul Anthony, Strugarek, Antoine, Sulis, Sophia, Švanda, Michal, Szabados, László, Szabó, Róbert, Szabó, Gyula M., Szuszkiewicz, Ewa, Talens, Geert Jan, Teti, Daniele, Theisen, Tom, Thévenin, Frédéric, Thoul, Anne, Tiphene, Didier, Titz-Weider, Ruth, Tkachenko, Andrew, Tomecki, Daniel, Tonfat, Jorge, Tosi, Nicola, Trampedach, Regner, Traven, Gregor, Triaud, Amaury, Trønnes, Reidar, Tsantaki, Maria, Tschentscher, Matthias, Turin, Arnaud, Tvaruzka, Adam, Ulmer, Bernd, Ulmer-Moll, Solène, Ulusoy, Ceren, Umbriaco, Gabriele, Valencia, Diana, Valentini, Marica, Valio, Adriana, Guijarro, Ángel Luis Valverde, Van Eylen, Vincent, Van Grootel, Valerie, van Kempen, Tim A., Van Reeth, Timothy, Van Zelst, Iris, Vandenbussche, Bart, Vasiliou, Konstantinos, Vasilyev, Valeriy, de Mascarenhas, David Vaz, Vazan, Allona, Nunez, Marina Vela, Velloso, Eduardo Nunes, Ventura, Rita, Ventura, Paolo, Venturini, Julia, Trallero, Isabel Vera, Veras, Dimitri, Verdugo, Eva, Verma, Kuldeep, Vibert, Didier, Martinez, Tobias Vicanek, Vida, Krisztián, Vigan, Arthur, Villacorta, Antonio, Villaver, Eva, Aparicio, Marcos Villaverde, Viotto, Valentina, Vorobyov, Eduard, Vorontsov, Sergey, Wagner, Frank W., Walloschek, Thomas, Walton, Nicholas, Walton, Dave, Wang, Haiyang, Waters, Rens, Watson, Christopher, Wedemeyer, Sven, Weeks, Angharad, Weingril, Jörg, Weiss, Annita, Wendler, Belinda, West, Richard, Westerdorff, Karsten, Westphal, Pierre-Amaury, Wheatley, Peter, White, Tim, Whittaker, Amadou, Wickhusen, Kai, Wilson, Thomas, Windsor, James, Winter, Othon, Winther, Mark Lykke, Winton, Alistair, Witteck, Ulrike, Witzke, Veronika, Woitke, Peter, Wolter, David, Wuchterl, Günther, Wyatt, Mark, Yang, Dan, Yu, Jie, Sanchez, Ricardo Zanmar, Osorio, María Rosa Zapatero, Zechmeister, Mathias, Zhou, Yixiao, Ziemke, Claas, and Zwintz, Konstanze
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.
Published: 2024

2. Herschel Gould Belt Survey Observations of Dense Cores in the Cepheus Flare Clouds

Author: Di Francesco, James, Keown, Jared, Fallscheer, Cassandra, André, Philippe, Ladjelate, Bilal, Könyves, Vera, Men'shchikov, Alexander, Stephens-Whale, Shaun, Nguyen-Luong, Quang, Martin, Peter, Sadavoy, Sarah, Pezzuto, Stefano, Fiorellino, Eleonora, Benedettini, Milena, Schneider, Nicola, Bontemps, Sylvain, Arzoumanian, Doris, Palmeirim, Pedro, Kirk, Jason M., and Ward-Thompson, Derek
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present Herschel SPIRE and PACS maps of the Cepheus Flare clouds L1157, L1172, L1228, L1241, and L1251, observed by the Herschel Gould Belt Survey (HGBS) of nearby star-forming molecular clouds. Through modified blackbody fits to the SPIRE and PACS data, we determine typical cloud column densities of 0.5-1.0 $\times$ 10$^{21}$ cm$^{-2}$ and typical cloud temperatures of 14-15 K. Using the getsources identification algorithm, we extract 832 dense cores from the SPIRE and PACS data at 160-500 $\mu$m. From placement in a mass vs. size diagram, we consider 303 to be candidate prestellar cores, and 178 of these to be "robust" prestellar cores. From an independent extraction of sources at 70 $\mu$m, we consider 25 of the 832 dense cores to be protostellar. The distribution of background column densities coincident with candidate prestellar cores peaks at 2-4 $\times$ 10$^{21}$ cm$^{-2}$. About half of the candidate prestellar cores in Cepheus may have formed due to the widespread fragmentation expected to occur within filaments of "transcritical" line mass. The lognormal robust prestellar core mass function (CMF) drawn from all five Cepheus clouds peaks at 0.56 M$_{\odot}$ and has a width of $\sim$0.5 dex, similar to that of Aquila's CMF. Indeed, the width of Cepheus' aggregate CMF is similar to the stellar system Initial Mass Function (IMF). The similarity of CMF widths in different clouds and the system IMF suggests a common, possibly turbulent origin for seeding the fluctuations that evolve into prestellar cores and stars., Comment: 36 pages, 21 figures, 2 online text tables (not yet included here), accepted for publication in The Astrophysical Journal
Published: 2020
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3. The Herschel view of the dense core population in the Ophiuchus molecular cloud

Author: Ladjelate, Bilal, André, Philippe, Könyves, Vera, Ward-Thompson, Derek, Men'shchikov, Alexander, Bracco, Andrea, Palmeirim, Pedro, Roy, Arabindo, Shimajiri, Yoshito, Kirk, Jason M., Arzoumanian, Doris, Benedettini, Milena, Di Francesco, James, Fiorellino, Eleonora, Schneider, Nicola, and Pezzuto, Stefano
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Herschel observations of nearby clouds in the Gould Belt support a paradigm for low-mass star formation, starting with the generation of molecular filaments, followed by filament fragmentation, and the concentration of mass into self-gravitating prestellar cores. With the unique far-infrared and submillimeter continuum imaging capabilities of the Herschel Space observatory, the closeby (d = 139 pc) Ophiuchus cloud was mapped at five wavelengths from 70 ${\mu}m$ to 500 ${\mu}m$ with the aim of providing a complete census of dense cores in this region, including unbound starless cores, bound prestellar cores, and protostellar cores. Taking advantage of the high dynamic range and multi-wavelength nature of the Herschel data, we used the multi-scale decomposition algorithms getsources and getfilaments to identify a complete sample of dense cores and filaments in the cloud and study their properties. The densest clouds of the Ophiuchus complex, L1688 and L1689, which thus far are only indirectly described as filamentary regions owing to the spatial distribution of their young stellar objects (YSOs), are confirmed to be dominated by filamentary structures. The tight correlation observed between prestellar cores and filamentary structures in L1688 and L1689 supports the view that solar-type star formation occurs primarily in dense filaments. While the sub clouds of the complex show disparities, L1689 being less efficient than L1688 at forming stars when considering their total mass budgets, both sub clouds share almost the same prestellar core formation efficiency in dense molecular gas. We also find evidence in the Herschel data for a remarkable concentric geometrical configuration in L1688 which is dominated by up to three arc-like compression fronts and presumably created by shockwave events emanating from the Sco OB2 association, including the neighboring massive (O9V) star ${\sigma}$ Sco., Comment: Accepted for publication in A&A
Published: 2020
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4. KFPA Examinations of Young STellar Object Natal Environments (KEYSTONE): Hierarchical Ammonia Structures in Galactic Giant Molecular Clouds

Author: Keown, Jared, Di Francesco, James, Rosolowsky, Erik, Singh, Ayushi, Figura, Charles, Kirk, Helen, Anderson, L. D., Chen, Michael Chun-Yuan, Elia, Davide, Friesen, Rachel, Ginsburg, Adam, Marston, A., Pezzuto, Stefano, Schisano, Eugenio, Bontemps, Sylvain, Caselli, Paola, Liu, Hong-Li, Longmore, Steven, Motte, Frederique, Myers, Philip C., Offner, Stella S. R., Sanhueza, Patricio, Schneider, Nicola, Stephens, Ian, Urquhart, James, and collaboration, the KEYSTONE
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present initial results from the K-band focal plane array Examinations of Young STellar Object Natal Environments (KEYSTONE) survey, a large project on the 100-m Green Bank Telescope mapping ammonia emission across eleven giant molecular clouds at distances of $0.9-3.0$ kpc (Cygnus X North, Cygnus X South, M16, M17, MonR1, MonR2, NGC2264, NGC7538, Rosette, W3, and W48). This data release includes the NH$_3$ (1,1) and (2,2) maps for each cloud, which are modeled to produce maps of kinetic temperature, centroid velocity, velocity dispersion, and ammonia column density. Median cloud kinetic temperatures range from $11.4\pm2.2$ K in the coldest cloud (MonR1) to $23.0\pm6.5$ K in the warmest cloud (M17). Using dendrograms on the NH$_3$ (1,1) integrated intensity maps, we identify 856 dense gas clumps across the eleven clouds. Depending on the cloud observed, $40-100\%$ of the clumps are aligned spatially with filaments identified in H$_2$ column density maps derived from SED-fitting of dust continuum emission. A virial analysis reveals that 523 of the 835 clumps ($\sim63\%$) with mass estimates are bound by gravity alone. We find no significant difference between the virial parameter distributions for clumps aligned with the dust-continuum filaments and those unaligned with filaments. In some clouds, however, hubs or ridges of dense gas with unusually high mass and low virial parameters are located within a single filament or at the intersection of multiple filaments. These hubs and ridges tend to host water maser emission, multiple 70$\mu$m-detected protostars, and have masses and radii above an empirical threshold for forming massive stars., Comment: Accepted for publication in ApJ
Published: 2019
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5. How the power spectrum of dust continuum images may hide the presence of a characteristic filament width

Author: Roy, Arabindo, André, Philippe, Arzoumanian, Doris, Miville-Deschênes, Marc-Antoine, Könyves, Vera, Schneider, Nicola, Pezzuto, Stefano, Palmeirim, Pedro, and Kirk, Jason M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Herschel observations of interstellar clouds support a paradigm for star formation in which filaments play a central role. One of the foundations of this paradigm is the finding, based on studies of the radial column density profiles, that nearby filaments share a common inner width of ~0.1 pc. The existence of a characteristic filament width has been questioned, however, as it seems inconsistent with the scale-free nature of the power spectrum of cloud images. In an effort to clarify the origin of this apparent discrepancy, we examined the power spectra of the Herschel 250 micron images of the Polaris, Aquila, and Taurus clouds and performed a number of simple numerical experiments by injecting synthetic filaments in both the Herschel images and synthetic background images. We constructed several populations of synthetic filaments of 0.1 pc width with realistic area filling factors ($A_{\rm fil}$) and distributions of column density contrasts ($\delta_c$). After adding synthetic filaments to the Herschel images, we re-computed the image power spectra and compared the results with the original, essentially scale-free power spectra. We used the $\chi^2$ variance of the residuals between the best power-law fit and the output power spectrum as a diagnostic of the presence of a significant departure from a scale-free power spectrum. We found that the $\chi^2$ variance depends primarily on the combined parameter $\delta_c^2\, A_{\rm fil}$. Analysis of the real Herschel data shows that the observed filamentary structure contributes only 1/5 of the power in the power spectra at angular frequencies where an effect of the characteristic filament width is expected. We conclude that the scale-free power spectra of Herschel images remain consistent with the existence of a characteristic filament width ~0.1 pc and do not invalidate the conclusions drawn from studies of the filament profiles., Comment: 14 pages, 18 figures. Accepted for publication in Astronomy and Astrophysics
Published: 2019
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6. Distance biases in the estimation of the physical properties of Hi-GAL compact sources-I. Clump properties and the identification of high-mass star forming candidates

Author: Baldeschi, Adriano, Elia, Davide, Molinari, Sergio, Pezzuto, Stefano, Schisano, Eugenio, Gatti, Marco, Serra, Andrea, Benedettini, Milena, Di Giorgio, Anna Maria, Liu, John Scige, and Merello, Manuel
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The degradation of spatial resolution in star-forming regions observed at large distances ($d\gtrsim1$ kpc) with Herschel,can lead to estimates of the physical parameters of the detected compact sources (clumps) which do not necessarily mirror the properties of the original population of cores. This paper aims at quantifying the bias introduced in the estimation of these parameters by the distance effect. To do so, we consider Herschel maps of nearby star-forming regions taken from the Herschel-Gould-Belt survey, and simulate the effect of increased distance to understand what amount of information is lost when a distant star-forming region is observed with Herschel resolution. In the maps displaced to different distances we extract compact sources, and we derive their physical parameters as if they were original Hi-GAL maps of the extracted source samples. In this way, we are able to discuss how the main physical properties change with distance. In particular, we discuss the ability of clumps to form massive stars: we estimate the fraction of distant sources that are classified as high-mass stars-forming objects due to their position in the mass vs radius diagram, that are only "false positives". We give also a threshold for high-mass star-formation $M>1282 \ \left(\frac{r}{[\mathrm{pc}]}\right)^{1.42} M_{\odot}$. In conclusion, this paper provides the astronomer dealing with Herschel maps of distant star-forming regions with a set of prescriptions to partially recover the character of the core population in unresolved clumps., Comment: 32 pages, 42 figures, accepted for publication in MNRAS
Published: 2017
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7. Source clustering in the Hi-GAL survey determined using a minimum spanning tree method

Author: Beuret, Maxime, Billot, Nicolas, Cambrésy, Laurent, Eden, David J., Elia, Davide, Molinari, Sergio, Pezzuto, Stefano, and Schisano, Eugenio
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The aims are to investigate the clustering of the far-infrared sources from the Herschel infrared Galactic Plane Survey (Hi-GAL) in the Galactic longitude range of -71 to 67 deg. These clumps, and their spatial distribution, are an imprint of the original conditions within a molecular cloud. This will produce a catalogue of over-densities. The minimum spanning tree (MST) method was used to identify the over-densities in two dimensions. The catalogue was further refined by folding in heliocentric distances, resulting in more reliable over-densities, which are cluster candidates. We found 1,633 over-densities with more than ten members. Of these, 496 are defined as cluster candidates because of the reliability of the distances, with a further 1,137 potential cluster candidates. The spatial distributions of the cluster candidates are different in the first and fourth quadrants, with all clusters following the spiral structure of the Milky Way. The cluster candidates are fractal. The clump mass functions of the clustered and isolated are statistically indistinguishable from each other and are consistent with Kroupa's initial mass function., Comment: 24 pages, 27 figures
Published: 2016
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8. The JCMT and Herschel Gould Belt Surveys: A comparison of SCUBA-2 and Herschel data of dense cores in the Taurus dark cloud L1495

Author: Ward-Thompson, Derek, Pattle, Kate, Kirk, Jason, Marsh, Ken, Buckle, Jane, Hatchell, Jennifer, Nutter, David, Griffin, Matt, Di Francesco, James, André, Philippe, Beaulieu, Sylvie, Berry, David, Broekhoven-Fiene, Hannah, Currie, Malcolm, Fich, Michel, Jenness, Timothy, Johnstone, Doug, Kirk, Helen, Mottram, Joseph, Pineda, Jaime, Quinn, Ciera, Sadavoy, Sarah, Salji, Carl, Tisi, Sam, Walker-Smith, Sarah, White, Glenn, Hill, Tracey, Könyves, Vera, Palmeirim, Pedro, and Pezzuto, Stefano
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a comparison of SCUBA-2 850-$\mu$m and Herschel 70--500-$\mu$m observations of the L1495 filament in the Taurus Molecular Cloud with the goal of characterising the SCUBA-2 Gould Belt Survey (GBS) data set. We identify and characterise starless cores in three data sets: SCUBA-2 850-$\mu$m, Herschel 250-$\mu$m, and Herschel 250-$\mu$m spatially filtered to mimic the SCUBA-2 data. SCUBA-2 detects only the highest-surface-brightness sources, principally detecting protostellar sources and starless cores embedded in filaments, while Herschel is sensitive to most of the cloud structure, including extended low-surface-brightness emission. Herschel detects considerably more sources than SCUBA-2 even after spatial filtering. We investigate which properties of a starless core detected by Herschel determine its detectability by SCUBA-2, and find that they are the core's temperature and column density (for given dust properties). For similar-temperature cores, such as those seen in L1495, the surface brightnesses of the cores are determined by their column densities, with the highest-column-density cores being detected by SCUBA-2. For roughly spherical geometries, column density corresponds to volume density, and so SCUBA-2 selects the densest cores from a population at a given temperature. This selection effect, which we quantify as a function of distance, makes SCUBA-2 ideal for identifying those cores in Herschel catalogues that are closest to forming stars. Our results can now be used by anyone wishing to use the SCUBA-2 GBS data set., Comment: MNRAS accepted, 19 pages, 14 figures
Published: 2016
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9. Remarkable analytic relations among greybody parameters

Author: Elia, Davide and Pezzuto, Stefano
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: In this paper we derive and discuss several implications of the analytic form of a modified blackbody, also called greybody, which is widely used in Astrophysics, and in particular in the study of star formation in the far-infrared/sub-millimeter domain. The research in this area has been greatly improved thanks to recent observations taken with the Herschel satellite, so that it became important to clarify the sense of the greybody approximation, to suggest possible further uses, and to delimi its intervals of validity. First, we discuss the position of the greybody peak, making difference between the optically thin and thick regimes. Second, we analyze the behavior of bolometric quantities as a function of the different greybody parameters. The ratio between the bolometric luminosity and the mass of a source, the ratio between the so-called "sub-millimeter luminosity" and the bolometric one, and the bolometric temperature are observables used to characterize the evolutionary stage of a source, and it is of primary importance to have analytic equations describing the dependence of such quantities on the greybody parameters. Here we discuss all these aspects, providing analytic relations, illustrating particular cases and providing graphical examples. Some equations reported here are well-known in Astrophysics, but are often spread over different publications. Some of them, instead, are brand new and represent a novelty in Astrophysics literature. Finally we indicate an alternative way to obtain, under some conditions, the greybody temperature and dust emissivity directly from an observing spectral energy distribution, avoiding a best-fit procedure., Comment: accepted by MNRAS
Published: 2016
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10. Large-scale latitude distortions of the inner Milky Way Disk from the Herschel/Hi-GAL Survey

Author: Molinari, Sergio, Noriega-Crespo, Alberto, Bally, John, Moore, Toby, Elia, Davide, Schisano, Eugenio, Plume, Rene, Swinyard, Bruce, Di Giorgio, Anna Maria, Pezzuto, Stefano, Benedettini, Milena, and Testi, Leonardo
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We use the Herschel Hi-GAL survey data to study the spatial distribution in Galactic longitude and latitude of the interstellar medium and of dense, star-forming clumps in the inner Galaxy. The peak position and width of the latitude distribution of the dust column density as well as of number density of compact sources from the band-merged Hi-GAL photometric catalogues are analysed as a function of longitude. The width of the diffuse dust column density traced by the Hi-GAL 500 micron emission varies across the inner Galaxy, with a mean value of 1{\deg}.2-1{\deg}.3, similar to that of the 250um Hi-GAL sources. 70um Hi-GAL sources define a much thinner disk, with a mean FWHM of 0{\deg}.75, and an average latitude of b=0{\deg}.06, coincident with the results from ATLASGAL. The GLAT distribution as a function of GLON shows modulations, both for the diffuse emission and for the compact sources, with ~0{\deg}.2 displacements mostly toward negative latitudes at l~ +40{\deg}, +12{\deg}, -25{\deg} and -40{\deg}. No such modulations can be found in the MIPSGAL 24 or WISE 22 um data when the entire source samples are considered. The distortions revealed by Herschel are interpreted as large-scale bending modes of the Plane. The lack of similar distortions in tracers of more evolved YSOs or stars rules out gravitational instabilities or satellite-induced perturbations, as they should act on both the diffuse and stellar disk components. We propose that the observed bends are caused by incoming flows of extra-planar gas interacting with the gaseous disk. Stars decouple from the gaseous ISM and relax into the stellar disk potential. The time required for the disappearance of the distortions from the diffuse ISM to the relatively evolved YSO stages are compatible with star-formation timescales., Comment: Astronomy & Astrophysics, accepted. 13 pages, 9 figures
Published: 2015
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11. Machine learning based data mining for Milky Way filamentary structures reconstruction

Author: Riccio, Giuseppe, Cavuoti, Stefano, Schisano, Eugenio, Brescia, Massimo, Mercurio, Amata, Elia, Davide, Benedettini, Milena, Pezzuto, Stefano, Molinari, Sergio, and Di Giorgio, Anna Maria
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Computer Science - Computer Vision and Pattern Recognition
Abstract: We present an innovative method called FilExSeC (Filaments Extraction, Selection and Classification), a data mining tool developed to investigate the possibility to refine and optimize the shape reconstruction of filamentary structures detected with a consolidated method based on the flux derivative analysis, through the column-density maps computed from Herschel infrared Galactic Plane Survey (Hi-GAL) observations of the Galactic plane. The present methodology is based on a feature extraction module followed by a machine learning model (Random Forest) dedicated to select features and to classify the pixels of the input images. From tests on both simulations and real observations the method appears reliable and robust with respect to the variability of shape and distribution of filaments. In the cases of highly defined filament structures, the presented method is able to bridge the gaps among the detected fragments, thus improving their shape reconstruction. From a preliminary "a posteriori" analysis of derived filament physical parameters, the method appears potentially able to add a sufficient contribution to complete and refine the filament reconstruction., Comment: Proceeding of WIRN 2015 Conference, May 20-22, Vietri sul Mare, Salerno, Italy. Published in Smart Innovation, Systems and Technology, Springer, ISSN 2190-3018, 9 pages, 4 figures
Published: 2015
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12. The Kinematic and Chemical Properties of a Potential Core-Forming Clump: Perseus B1-E

Author: Sadavoy, Sarah I., Shirley, Yancy, Di Francesco, James, Henning, Thomas, Currie, Malcolm J., Andre, Philippe, and Pezzuto, Stefano
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present 13CO and C18O (1-0), (2-1), and (3-2) maps towards the core-forming Perseus B1-E clump using observations from the James Clerk Maxwell Telescope (JCMT), Submillimeter Telescope (SMT) of the Arizona Radio Observatory, and IRAM 30 m telescope. We find that the 13CO and C18O line emission both have very complex velocity structures, indicative of multiple velocity components within the ambient gas. The (1-0) transitions reveal a radial velocity gradient across B1-E of 1 km/s/pc that increases from north-west to south-east, whereas the majority of the Perseus cloud has a radial velocity gradient increasing from south-west to north-east. In contrast, we see no evidence of a velocity gradient associated with the denser Herschel-identified substructures in B1-E. Additionally, the denser substructures have much lower systemic motions than the ambient clump material, which indicates that they are likely decoupled from the large-scale gas. Nevertheless, these substructures themselves have broad line widths (0.4 km/s) similar to that of the C18O gas in the clump, which suggests they inherited their kinematic properties from the larger-scale, moderately dense gas. Finally, we find evidence of C18O depletion only toward one substructure, B1-E2, which is also the only object with narrow (transonic) line widths. We suggest that as prestellar cores form, their chemical and kinematic properties are linked in evolution, such that these objects must first dissipate their turbulence before they deplete in CO., Comment: Accepted by ApJ, 34 pages, 12 figures
Published: 2015
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13. Changes Of Dust Opacity With Density in the Orion A Molecular Cloud

Author: Roy, Arabindo, Martin, Peter G., Polychroni, Danae, Bontemps, Sylvain, Abergel, Alain, Andre, Philippe, Arzoumanian, Doris, Di Francesco, James, Hill, Tracey, Konyves, Vera, Nguyen-Luong, Quang, Pezzuto, Stefano, Schneider, Nicola, Testi, Leonardo, and White, Glenn
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have studied the opacity of dust grains at submillimeter wavelengths by estimating the optical depth from imaging at 160, 250, 350, and 500 um from the Herschel Gould Belt Survey and comparing this to a column density obtained from the 2MASS-derived color excess E(J-Ks). Our main goal was to investigate the spatial variations of the opacity due to "big" grains over a variety of environmental conditions and thereby quantify how emission properties of the dust change with column (and volume) density. The central and southern areas of the Orion A molecular cloud examined here, with NH ranging from 1.5X10^21 cm^-2 to 50X10^21 cm^-2, are well suited to this approach. We fit the multi-frequency Herschel spectral energy distributions (SEDs) of each pixel with a modified blackbody to obtain the temperature, T, and optical depth, \tau(1200), at a fiducial frequency of 1200 GHz (250 um). Using a calibration of NH/E(J-Ks)for the interstellar medium (ISM) we obtained the opacity (dust emission cross-section per H nucleon), \sigma_e(1200), for every pixel. From a value of ~ 1X10^-25 cm^2 H^-1 at the lowest column densities that is typical of the high latitude diffuse ISM, \sigma_e(1200) increases as NH^0.28 over the range studied. This is suggestive of grain evolution. Integrating the SEDs over frequency, we also calculated the specific power P (emission power per H) for the big grains. In low column density regions where dust clouds are optically thin to the interstellar radiation field (ISRF), P is typically 3.7 X 10^-31 W H^-1, again close to that in the high latitude diffuse ISM. However, we find evidence for a decrease of P in high column density regions, which would be a natural outcome of attenuation of the ISRF that heats the grains, and for localized increases for dust illuminated by nearby stars or embedded protostars., Comment: 13 pages, 11 Figures, To appear in the Astrophysical Journal
Published: 2012
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14. Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud

Author: Pezzuto, Stefano, Elia, D., Schisano, E., Strafella, F., Di Francesco, J., Sadavoy, S., André, P., Benedettini, M., Bernard, J. P., di Giorgio, A. M., Facchini, A., Hennemann, M., Hill, T., Könyves, V., Molinari, S., Motte, F., Nguyen-Luong, Q., Peretto, N., Pestalozzi, M., Polychroni, D., Rygl, K. L. J., Saraceno, P., Schneider, N., Spinoglio, L., Testi, L., Ward-Thompson, D., and White, G. J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report far-IR Herschel observations obtained between 70 $\mu$m and 500 $\mu$m of two star-forming dusty condensations, B1-bS and B1-bN, in the B1 region of the Perseus star-forming cloud. In the Western part of the Perseus cloud, B1-bS is the only source detected in all of the 6 PACS and SPIRE photometric bands without being visible in the Spitzer map at 24 $\mu$m. B1-bN is clearly detected between 100 $\mu$m and 250 $\mu$m. We have fitted the spectral energy distributions of these sources to derive their physical properties, and find that a simple greybody model fails to reproduce the observed SEDs. At least a two-component model, consisting of a central source surrounded by a dusty envelope is required. The properties derived from the fit, however, suggest that the central source is not a Class 0 object. We then conclude that while B1-bS and B1-bN appear to be more evolved than a pre-stellar core, the best-fit models suggest that their central objects are younger than a Class 0 source. Hence, they may be good candidates to be examples of the first hydrostatic core phase. The projected distance between B1-bS and B1-bN is a few Jeans lengths. If their physical separation is close to this value, this pair would allow the mutual interactions between two forming stars at a very early stage of their evolution to be studied., Comment: 14 pages, 4 figures. Accepted for publication in A&A, main journal
Published: 2012
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15. Multi-line spectral imaging of dense cores in the Lupus molecular cloud

Author: Benedettini, Milena, Pezzuto, Stefano, Burton, Micheal G., Viti, Serena, Molinari, Sergio, Caselli, Paola, and Testi, Leonardo
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The molecular clouds Lupus 1, 3 and 4 were mapped with the Mopra telescope at 3 and 12 mm. Emission lines from high density molecular tracers were detected, i.e. NH$_3$ (1,1), NH$_3$ (2,2), N$_2$H$^+$ (1-0), HC$_3$N (3-2), HC$_3$N (10-9), CS (2-1), CH$_3$OH (2$_0-1_0$)A$^+$ and CH$_3$OH (2$_{-1}-1_{-1}$)E. Velocity gradients of more than 1 km s$^{-1}$ are present in Lupus 1 and 3 and multiple gas components are present in these clouds along some lines of sight. Lupus 1 is the cloud richest in high density cores, 8 cores were detected in it, 5 cores were detected in Lupus 3 and only 2 in Lupus 4. The intensity of the three species HC$_3$N, NH$_3$ and N$_2$H$^+$ changes significantly in the various cores: cores that are brighter in HC$_3$N are fainter or undetected in NH$_3$ and N$_2$H$^+$ and vice versa. We found that the column density ratios HC$_3$N/N$_2$H$^+$ and HC$_3$N/NH$_3$ change by one order of magnitude between the cores, indicating that also the chemical abundance of these species is different. The time dependent chemical code that we used to model our cores shows that the HC$_3$N/N$_2$H$^+$ and HC$_3$N/NH$_3$ ratios decrease with time therefore the observed column density of these species can be used as an indicator of the chemical evolution of dense cores. On this base we classified 5 out of 8 cores in Lupus 1 and 1 out of 5 cores in Lupus 3 as very young protostars or prestellar cores. Comparing the millimetre cores population with the population of the more evolved young stellar objects identified in the Spitzer surveys, we conclude that in Lupus 3 the bulk of the star formation activity has already passed and only a moderate number of stars are still forming. On the contrary, in Lupus 1 star formation is on-going and several dense cores are still in the pre--/proto--stellar phase. Lupus 4 is at an intermediate stage, with a smaller number of individual objects., Comment: 27 pages, 11 figures
Published: 2011
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16. Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites

Author: Hill, Tracey, Motte, Frederique, Didelon, Pierre, Bontemps, Sylvain, Minier, Vincent, Hennemann, Martin, Schneider, Nicola, Andre, Philippe, Men'shchikov, Alexander, Anderson, Loren D., Arzoumanian, Doris, Bernard, Jean-Philippe, di Francesco, James, Elia, Davide, Giannini, Teresa, Griffin, Matt J., Kirk, Jason, Konyves, Vera, Marston, Anthony P., Martin, Peter, Molinari, Sergio, Luong, Quang Nguyen, Peretto, Nicolas, Pezzuto, Stefano, Roussel, Helene, Sauvage, Marc, Sousbie, Thierry, Testi, Leonardo, Ward-Thompson, Derek, White, Glenn J., Wilson, Christine D., and Zavagno, Annie
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present the first Herschel PACS and SPIRE results of the Vela C molecular complex in the far-infrared and submillimetre regimes at 70, 160, 250, 350, and 500 um, spanning the peak of emission of cold prestellar or protostellar cores. Column density and multi-resolution analysis (MRA) differentiates the Vela C complex into five distinct sub-regions. Each sub-region displays differences in their column density and temperature probability distribution functions (PDFs), in particular, the PDFs of the `Centre-Ridge' and `South-Nest' sub-regions appear in stark contrast to each other. The Centre-Ridge displays a bimodal temperature PDF representative of hot gas surrounding the HII region RCW 36 and the cold neighbouring filaments, whilst the South-Nest is dominated by cold filamentary structure. The column density PDF of the Centre-Ridge is flatter than the South-Nest, with a high column density tail, consistent with formation through large-scale flows, and regulation by self-gravity. At small to intermediate scales MRA indicates the Centre-Ridge to be twice as concentrated as the South-Nest, whilst on larger scales, a greater portion of the gas in the South-Nest is dominated by turbulence than in the Centre-Ridge. In Vela C, high-mass stars appear to be preferentially forming in ridges, i.e., dominant high column density filaments., Comment: 7 pages + 2 page figure appendix, 8 Figures (one in the appendix). Accepted by A&A
Published: 2011
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17. Search for massive protostar candidates in the southern hemisphere: II. Dust continuum emission

Author: Beltran, Maria T., Brand, Jan, Cesaroni, Riccardo, Fontani, Francesco, Pezzuto, Stefano, Testi, Leonardo, and Molinari, Sergio
Subjects: Astrophysics
Abstract: In an ongoing effort to identify and study high-mass protostellar candidates we have observed in various tracers a sample of 235 sources selected from the IRAS Point Source Catalog, mostly with dec < -30 deg, with the SEST antenna at millimeter wavelengths. The sample contains 142 Low sources and 93 High, which are believed to be in different evolutionary stages. Both sub-samples have been studied in detail by comparing their physical properties and morphologies. Massive dust clumps have been detected in all but 8 regions, with usually more than one clump per region. The dust emission shows a variety of complex morphologies, sometimes with multiple clumps forming filaments or clusters. The mean clump has a linear size of ~0.5 pc, a mass of ~320 Msolar for a dust temperature Td=30 K, an H_2 density of 9.5E5 cm-3, and a surface density of 0.4 g cm-2. The median values are 0.4 pc, 102 Msolar, 4E4 cm-3, and 0.14 g cm-2, respectively. The mean value of the luminosity-to-mass ratio, L/M ~99 Lsolar/Msolar, suggests that the sources are in a young, pre-ultracompact HII phase. We have compared the millimeter continuum maps with images of the mid-IR MSX emission, and have discovered 95 massive millimeter clumps non-MSX emitters, either diffuse or point-like, that are potential prestellar or precluster cores. The physical properties of these clumps are similar to those of the others, apart from the mass that is ~3 times lower than for clumps with MSX counterpart. Such a difference could be due to the potential prestellar clumps having a lower dust temperature. The mass spectrum of the clumps with masses above M ~100 Msolar is best fitted with a power-law dN/dM proportional to M-alpha with alpha=2.1, consistent with the Salpeter (1955) stellar IMF, with alpha=2.35., Comment: 83 pages, 10 figures, 3 tables. Accepted for publication by A&A. The full paper, including Fig.2 with the maps of all the individual regions, complete Tables 1 and 2 can be found at http://www.arcetri.astro.it/~starform/publ2005.htm
Published: 2005
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18. The ISO-LWS far-infrared spectra of pre-Main Sequence objects

Author: Benedettini, Milena, Pezzuto, Stefano, Spinoglio, Luigi, Saraceno, Paolo, and di Giorgio, Anna Maria
Subjects: Astrophysics
Abstract: The Long Wavelength Spectrometer (LWS) on board the Infrared Space Observatory (ISO) satellite has allowed for the first time to investigate the whole far infrared (FIR) part of the spectrum (from 43 to 197 um), inaccessible from the ground. The FIR spectrum is crucial for the study of the early phases of protostellar evolution since the peak of the continuum emission of the protostars falls around 100 um and many molecular species emit in this range. In this paper we review the main results of the spectroscopic observations carried out with the LWS on a sample of pre-Main Sequence objects in different evolutionary stages. The FIR spectra are characterized by a strong continuum with superimposed atomic and molecular emission lines. The fine structure lines emitted by the OI and CII atoms are present in all the objects of our sample while emission from molecular species (CO, H_2O and OH) dominate the spectrum of the younger and more embedded objects; lines of highly ionized atoms (OIII, NIII, NII) are present only in high luminosity sources. We will show how both the FIR continuum and the emission lines are powerful indicators of the evolutionary status of young embedded objects. The analysis of the LWS spectra has allowed to study only the average properties of the young stellar objects, due to the large field of view (~ 80 arcsec), the limited sensitivity and the poor spectral resolution (~ 200) of the instrument in its grating mode. The higher spatial and spectral resolutions of the instruments on board the Herschel satellite will allow to address in deeper detail the scientific problems highlighted by the ISO results., Comment: 21 pages, 7 figures
Published: 2003

19. A chemical survey of exoplanets with ARIEL

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

Author: Riccio, Giuseppe, Cavuoti, Stefano, Schisano, Eugenio, Brescia, Massimo, Mercurio, Amata, Elia, Davide, Benedettini, Milena, Pezzuto, Stefano, Molinari, Sergio, Di Giorgio, Anna Maria, Howlett, Robert James, Series editor, Jain, Lakhmi C., Series editor, Bassis, Simone, editor, Esposito, Anna, editor, Morabito, Francesco Carlo, editor, and Pasero, Eros, editor
Published: 2016
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21. The PLATO instrument control unit software: a model based SW architecture

Author: Galli, Emanuele, primary, Giusi, Giovanni, additional, Russi, Andrea, additional, De Angelis, Fabrizio, additional, Farina, Maria, additional, Liù, Scigè, additional, Di Giorgio, Anna Maria, additional, Pezzuto, Stefano, additional, Focardi, Mauro, additional, vela nunez, marina, additional, and Cosentino, Rosario, additional
Published: 2022
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22. PLATO: the status of the instrument control unit following its critical design review

Author: Cosentino, Rosario, primary, Focardi, Mauro, additional, Galli, Emanuele, additional, Steller, Manfred, additional, Del Vecchio Blanco, Carlo, additional, Pezzuto, Stefano, additional, Giusi, Giovanni, additional, Di Giorgio, Anna Maria, additional, Biondi, David, additional, Jeszenszky, Harald, additional, Ottacher, Harald, additional, Laky, Gunter, additional, Serafini, Luca, additional, Loidolt, Dominik, additional, Ottensamer, Roland, additional, Russi, Andrea, additional, Vela Nunez, Marina, additional, Luntzer, Armin, additional, and Kerschbaum, Franz, additional
Published: 2022
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23. Machine Learning Based Data Mining for Milky Way Filamentary Structures Reconstruction

Author: Riccio, Giuseppe, primary, Cavuoti, Stefano, additional, Schisano, Eugenio, additional, Brescia, Massimo, additional, Mercurio, Amata, additional, Elia, Davide, additional, Benedettini, Milena, additional, Pezzuto, Stefano, additional, Molinari, Sergio, additional, and Di Giorgio, Anna Maria, additional
Published: 2016
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24. An alternative approach to the relation between accretion luminosity and mass accretion rate

Author: Pezzuto, Stefano, primary
Published: 2021
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25. The instrument control unit of the PLATO payload: design consolidation following the preliminary design review by ESA

Author: Cosentino, Rosario, primary, Focardi, Mauro, additional, Pezzuto, Stefano, additional, Giusi, Giovanni, additional, Galli, Emanuele, additional, Di Giorgio, Anna Maria, additional, Liù, Scigè, additional, Traficante, Alessio, additional, Biondi, David, additional, Hasiba, Johan, additional, Hofmann, Karl, additional, Jeszenszky, Harald, additional, Laky, Gunter, additional, Ottacher, Harald, additional, Steinberger, Michael, additional, Steller, Manfred, additional, Tonfat, Jorge, additional, Wallner, Robert, additional, Neukirchner, Sonja, additional, Leichtfried, Mario, additional, Del Vecchio Blanco, Carlo, additional, Serafini, Luca, additional, Dini, Devitt, additional, Pilato, Luca, additional, Toscano, Luca, additional, Zolesi, Valfredo, additional, Guedel, Manuel, additional, Kerschbaum, Franz, additional, Ottensamer, Roland, additional, Luntzer, Armin, additional, and Loidolt, Dominik, additional
Published: 2020
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26. Design and validation of the boot software for the instrument control unit of the PLATO mission

Author: Baldacci, Stefano, primary, Granata, Francesco, additional, Serafini, Luca, additional, Pannocchia, Alessio, additional, Azzali, Matteo, additional, Del Vecchio Blanco, Carlo, additional, Zolesi, Valfredo, additional, Focardi, Mauro, additional, Cosentino, Rosario, additional, Giusi, Giovanni, additional, Galli, Emanuele, additional, and Pezzuto, Stefano, additional
Published: 2020
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27. A combined software and hardware data compression approach in PLATO

Author: Loidolt, Dominik, primary, Ottensamer, Roland, additional, Luntzer, Armin, additional, Kerschbaum, Franz, additional, Ottacher, Harald, additional, Tonfat, Jorge, additional, Steller, Manfred, additional, Pezzuto, Stefano, additional, Focardi, Mauro, additional, and Cosentino, Rosario, additional
Published: 2020
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28. Herschel Gould Belt Survey Observations of Dense Cores in the Cepheus Flare Clouds

Author: Di Francesco, James, primary, Keown, Jared, additional, Fallscheer, Cassandra, additional, André, Philippe, additional, Ladjelate, Bilal, additional, Könyves, Vera, additional, Men’shchikov, Alexander, additional, Stephens-Whale, Shaun, additional, Nguyen-Luong, Quang, additional, Martin, Peter, additional, Sadavoy, Sarah, additional, Pezzuto, Stefano, additional, Fiorellino, Eleonora, additional, Benedettini, Milena, additional, Schneider, Nicola, additional, Bontemps, Sylvain, additional, Arzoumanian, Doris, additional, Palmeirim, Pedro, additional, Kirk, Jason M., additional, and Ward-Thompson, Derek, additional
Published: 2020
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29. The PLATO instrument control unit software: a model based SW architecture

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Galli, Emanuele, Giusi, Giovanni, Russi, Andrea, De Angelis, Fabrizio, Farina, Maria, Liu, Scige, Di Giorgio, Anna Maria, Pezzuto, Stefano, Focardi, Mauro, Vela Nuñez, Marina, and Cosentino, Rosario
Published: 2022
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30. PLATO: the status of the instrument control unit following its critical design review

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Cosentino, Rosario, Focardi, Mauro, Galli, Emanuele, Steller, Manfred, Del Vecchio Blanco, Carlo, Pezzuto, Stefano, Giusi, Giovanni, Di Giorgio, Anna Maria, Biondi, David, Jeszenszky, Harald, Ottacher, Harald, Laky, Gunter, Serafini, Luca, Loidolt, Dominik, Ottensamer, Roland, Russi, Andrea, Vela Nuñez, Marina, Luntzer, Armin, and Kerschbaum, Franz
Published: 2022
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31. KFPA Examinations of Young STellar Object Natal Environments (KEYSTONE): Hierarchical Ammonia Structures in Galactic Giant Molecular Clouds

Author: Keown, Jared, primary, Francesco, James Di, additional, Rosolowsky, Erik, additional, Singh, Ayushi, additional, Figura, Charles, additional, Kirk, Helen, additional, Anderson, L. D., additional, Chen, Michael Chun-Yuan, additional, Elia, Davide, additional, Friesen, Rachel, additional, Ginsburg, Adam, additional, Marston, A., additional, Pezzuto, Stefano, additional, Schisano, Eugenio, additional, Bontemps, Sylvain, additional, Caselli, Paola, additional, Liu, Hong-Li, additional, Longmore, Steven, additional, Motte, Frédérique, additional, Myers, Philip C., additional, Offner, Stella S. R., additional, Sanhueza, Patricio, additional, Schneider, Nicola, additional, Stephens, Ian, additional, and Urquhart, James, additional
Published: 2019
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32. Multifractal analysis of the interstellar medium: first application to Hi-GAL observations

Author: Elia, Davide, Strafella, Francesco, Dib, Sami, Schneider, Nicola, Hennebelle, Patrick, Pezzuto, Stefano, Molinari, Sergio, Schisano, Eugenio, Jaffa, Sarah E., Elia, Davide, Strafella, Francesco, Dib, Sami, Schneider, Nicola, Hennebelle, Patrick, Pezzuto, Stefano, Molinari, Sergio, Schisano, Eugenio, and Jaffa, Sarah E.
Abstract: The multifractal geometry remains an underexploited approach to describe and quantify the large-scale structure of interstellar clouds. In this paper, the typical tools of multifractal analysis are applied to Herschel far-infrared (70-500 mu m) dust continuum maps, which represent an ideal case of study. This dust component is a relatively optically thin tracer at these wavelengths and the size in pixel of the maps is well suitable for this statistical analysis. We investigate the so-called multifractal spectrum and generalized fractal dimension of six Hi-GAL regions in the third Galactic quadrant. We measure systematic variations of the spectrum at increasing wavelength, which generally correspond to an increasing complexity of the image, and we observe peculiar behaviours of the investigated fields, strictly related to the presence of high-emission regions, which in turn are connected to star formation activity. The same analysis is applied to synthetic column density maps, generated from numerical turbulent molecular cloud models and from fractal Brownian motion (fBm), allowing for the confrontation of the observations with models with well controlled physical parameters. This comparison shows that, in terms of multifractal descriptors of the structure, fBm images exhibit a very different, quite unrealistic behaviour when compared with Hi-GAL observations, whereas the numerical simulations appear in some cases (depending on the specific model) more similar to the observations. Finally, the link between mono-fractal parameters (commonly found in the literature) and multifractal indicators is investigated: the former appear to be only partially connected with the latter, with the multifractal analysis offering a more extended and complete characterization of the cloud structure..
Published: 2018

33. Multifractal analysis of the interstellar medium:first application to Hi-GAL observations

Author: Elia, Davide, Strafella, Francesco, Dib, Sami, Schneider, Nicola, Hennebelle, Patrick, Pezzuto, Stefano, Molinari, Sergio, Schisano, Eugenio, Jaffa, Sarah E., Elia, Davide, Strafella, Francesco, Dib, Sami, Schneider, Nicola, Hennebelle, Patrick, Pezzuto, Stefano, Molinari, Sergio, Schisano, Eugenio, and Jaffa, Sarah E.
Published: 2018

34. Herschel Gould Belt Survey Observations of Dense Cores in the Cepheus Flare Clouds.

Author: Francesco, James Di, Keown, Jared, Fallscheer, Cassandra, André, Philippe, Ladjelate, Bilal, Könyves, Vera, Men'shchikov, Alexander, Stephens-Whale, Shaun, Nguyen-Luong, Quang, Martin, Peter, Sadavoy, Sarah, Pezzuto, Stefano, Fiorellino, Eleonora, Benedettini, Milena, Schneider, Nicola, Bontemps, Sylvain, Arzoumanian, Doris, Palmeirim, Pedro, Kirk, Jason M., and Ward-Thompson, Derek
Subjects: STELLAR initial mass function, RAIN-making, MOLECULAR clouds, SOLAR flares
Abstract: We present Herschel SPIRE and PACS maps of the Cepheus Flare clouds L1157, L1172, L1228, L1241, and L1251, observed by the Herschel Gould Belt Survey of nearby star-forming molecular clouds. Through modified blackbody fits to the SPIRE and PACS data, we determine typical cloud column densities of (0.5–1.0) × 1021 cm−2 and typical cloud temperatures of 14–15 K. Using the getsources identification algorithm, we extract 832 dense cores from the SPIRE and PACS data at 160–500 μm. From placement in a mass versus size diagram, we consider 303 to be candidate prestellar cores, and 178 of these to be "robust" prestellar cores. From an independent extraction of sources at 70 μm, we consider 25 of the 832 dense cores to be protostellar. The distribution of background column densities coincident with candidate prestellar cores peaks at (2–4) × 1021 cm−2. About half of the candidate prestellar cores in Cepheus may have formed as a result of the widespread fragmentation expected to occur within filaments of "transcritical" line mass. The lognormal robust prestellar core mass function (CMF) drawn from all five Cepheus clouds peaks at 0.56 M⊙ and has a width of ∼0.5 dex, similar to that of Aquila's CMF. Indeed, the width of Cepheus's aggregate CMF is similar to the stellar system initial mass function (IMF). The similarity of CMF widths in different clouds and the system IMF suggests a common, possibly turbulent origin for seeding the fluctuations that evolve into prestellar cores and stars. [ABSTRACT FROM AUTHOR]
Published: 2020
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35. A study of the cold cores population in the Perseus star-forming regions

Author: PEZZUTO, Stefano, Fiorellino, E., BENEDETTINI, Milena, SCHISANO, EUGENIO, ELIA, Davide Quintino, André, P., Könyves, V., Ladjelate, B., Di Francesco, J., Piccotti, L., and Herschel Gould Belt Survey Consortium
Abstract: As part of the Herschel Gould Belt survey, the Perseus star-forming cloud was observed with the Herschel PACS and SPIRE instruments. Source catalogs are preliminary, as well as the here presented core mass function.
Published: 2017

36. The Hi-GAL compact source catalogue - I. The physical properties of the clumps in the inner Galaxy (-71.0° < ℓ < 67.0°)

Author: ELIA, Davide Quintino, MOLINARI, Sergio, SCHISANO, EUGENIO, Pestalozzi, M., PEZZUTO, Stefano, Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., BENEDETTINI, Milena, Bernard, J. P., DI GIORGIO, Anna Maria, Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., OLMI, LUCA, Schneider, N., TESTI, Leonardo, Wyrowski, F., Zavagno, A., Calzoletti, L., FAUSTINI, Fabiana, Natoli, P., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., CESARONI, Riccardo, García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., LIU, Scige' John, Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., RYGL, Kazi Lucie Jessica, Schilke, P., Thompson, M. A., TRAFICANTE, ALESSIO, UMANA, Grazia Maria Gloria, Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., BECCIANI, Ugo, BRESCIA, Massimo, BUEMI, CARLA SIMONA, BUFANO, FILOMENA, Butora, Robert, CAVUOTI, STEFANO, COSTA, Alessandro, Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., LETO, PAOLO, LI CAUSI, Gianluca, MARCHILI, Nicola, Martinavarro-Armengol, S., MERCURIO, AMATA, MOLINARO, Marco, RICCIO, GIUSEPPE, Sano, H., SCIACCA, Eva, Tachihara, K., Torii, K., TRIGILIO, CORRADO, VITELLO, FABIO ROBERTO, Yamamoto, H., ITA, GBR, FRA, DEU, BEL, and HUN
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: https://www.media.inaf.it/2017/07/27/herschel-la-carica-dei-101mila/ Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane -71.0° < ℓ < 67.0°. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between 'on-arm' and 'interarm' positions.
Published: 2017

37. A study of the cold cores population in the Serpens star-forming region

Author: Fiorellino, E., PEZZUTO, Stefano, LIU, Scige' John, BENEDETTINI, Milena, SCHISANO, EUGENIO, ELIA, Davide Quintino, André, P., Könyves, V., Ladjelate, B., and Herschel Gould Belt Survey Consortium
Abstract: As part of the Herschel Gould Belt survey, the Serpens star-forming region was observed with the Herschel PACS and SPIRE instruments. Data analysis is ongoing and a first version of the source catalog is ready; here we show some preliminary results.
Published: 2017

38. The PLATO Payload and Data Processing System Space Wire Network

Author: Focardi, Mauro, primary, Cosentino, Rosario, additional, Pezzuto, Stefano, additional, Biondi, David, additional, Giusi, Giovanni, additional, Serafini, Luca, additional, Del Vecchio Blanco, Carlo, additional, Vangelista, Donatella, additional, Rotundo, Matteo, additional, Fanucci, Luca, additional, Davalle, Daniele, additional, and Dps, Plato, additional
Published: 2018
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39. Multifractal analysis of the interstellar medium: first application to Hi-GAL observations

Author: Elia, Davide, primary, Strafella, Francesco, additional, Dib, Sami, additional, Schneider, Nicola, additional, Hennebelle, Patrick, additional, Pezzuto, Stefano, additional, Molinari, Sergio, additional, Schisano, Eugenio, additional, and Jaffa, Sarah E, additional
Published: 2018
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40. Design of the instrument and telescope control units integrated subsystem of the ESA-ARIEL payload

Author: Focardi, Mauro, primary, Pace, Emanuele, primary, Farina, Maria, primary, Sierra-Roig, Carles, primary, Colomè Ferrer, Joseph, primary, Gesa Bote, Lluis, primary, Ribas, Ignasi, primary, Di Giorgio, Anna Maria, primary, Da Deppo, Vania, primary, Ottensamer, Roland, primary, Pancrazzi, Maurizio, primary, Noce, Vladimiro, primary, Pezzuto, Stefano, primary, Morgante, Gianluca, primary, Eccleston, Paul, primary, Micela, Giuseppina, primary, Terenzi, Luca, primary, Tommasi, Elisabetta, primary, Pascale, Enzo, primary, Amiaux, Jerome, primary, Cara, Christophe, primary, and Malaguti, Giuseppe, primary
Published: 2018
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41. The design of the instrument control unit and its role within the data processing system of the ESA PLATO Mission

Author: Focardi, Mauro, primary, Pezzuto, Stefano, primary, Cosentino, Rosario, primary, Giusi, Giovanni, primary, Di Giorgio, Anna Maria, primary, Biondi, David, primary, Steller, Manfred, primary, del Vecchio Blanco, Carlo, primary, Serafini, Luca, primary, Plasson, Philippe, primary, Jeszenszky, Harald, primary, Ottacher, Harald, primary, Ottensamer, Roland, primary, Pancrazzi, Maurizio, primary, Noce, Vladimiro, primary, Pace, Emanuele, primary, Westerdorff, Karsten, primary, Peter, Gisbert, primary, Ulmer, Bernd, primary, Pagano, Isabella, primary, Berlin, Rainer, primary, Tommasi, Elisabetta, primary, Natalucci, Silvia, primary, Laky, Gunter, primary, Vangelista, Donatella, primary, Kerschbaum, Franz, primary, and Guedel, Manuel, primary
Published: 2018
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42. A census of dense cores in the Taurus L1495 cloud from the Herschel

Author: Marsh, K. A., Kirk, J. M., André, Ph., Griffin, M. J., Könyves, V., Palmeirim, P., Men'shchikov, A., Ward-Thompson, D., BENEDETTINI, Milena, Bresnahan, D. W., di Francesco, J., ELIA, Davide Quintino, Motte, F., Peretto, N., PEZZUTO, Stefano, Roy, A., Sadavoy, S., Schneider, N., SPINOGLIO, Luigi Giuseppe Maria, and White, G. J.
Abstract: We present a catalogue of dense cores in a ∼4° × 2° field of the Taurus star-forming region, inclusive of the L1495 cloud, derived from Herschel SPIRE and PACS observations in the 70 μm, 160 μm, 250 μm, 350 μm, and 500 μm continuum bands. Estimates of mean dust temperature and total mass are derived using modified blackbody fits to the spectral energy distributions. We detect 525 starless cores of which ∼10-20 per cent are gravitationally bound and therefore presumably prestellar. Our census of unbound objects is ∼85 per cent complete for M > 0.015 M☉ in low-density regions (AV ≲ 5 mag), while the bound (prestellar) subset is ∼85 per cent complete for M > 0.1 M☉ overall. The prestellar core mass function (CMF) is consistent with lognormal form, resembling the stellar system initial mass function, as has been reported previously. All of the inferred prestellar cores lie on filamentary structures whose column densities exceed the expected threshold for filamentary collapse, in agreement with previous reports. Unlike the prestellar CMF, the unbound starless CMF is not lognormal, but instead is consistent with a power-law form below 0.3 M☉ and shows no evidence for a low-mass turnover. It resembles previously reported mass distributions for CO clumps at low masses (M ≲ 0.3 M☉). The volume density PDF, however, is accurately lognormal except at high densities. It is consistent with the effects of self-gravity on magnetized supersonic turbulence. The only significant deviation from lognormality is a high-density tail which can be attributed unambiguously to prestellar cores.
Published: 2016

43. The instrument control unit of the PLATO payload: design consolidation following the preliminary design review by ESA

Author: Lystrup, Makenzie, Perrin, Marshall D., Cosentino, Rosario, Focardi, Mauro, Pezzuto, Stefano, Giusi, Giovanni, Galli, Emanuele, Di Giorgio, Anna Maria, Liu, Scige, Traficante, Alessio, Biondi, David, Hasiba, Johan, Hofmann, Karl, Jeszenszky, Harald, Laky, Gunter, Ottacher, Harald, Steinberger, Michael, Steller, Manfred, Tonfat, Jorge, Wallner, Robert, Neukirchner, Sonja, Leichtfried, Mario, Del Vecchio Blanco, Carlo, Serafini, Luca, Dini, Devitt, Pilato, Luca, Toscano, Luca, Zolesi, Valfredo, Guedel, Manuel, Kerschbaum, Franz, Ottensamer, Roland, Luntzer, Armin, and Loidolt, Dominik
Published: 2020
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44. A combined software and hardware data compression approach in PLATO

Author: Lystrup, Makenzie, Perrin, Marshall D., Loidolt, Dominik, Ottensamer, Roland, Luntzer, Armin, Kerschbaum, Franz, Ottacher, Harald, Tonfat, Jorge, Steller, Manfred, Pezzuto, Stefano, Focardi, Mauro, and Cosentino, Rosario
Published: 2020
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45. Progress in the Critical Assessment for a Far-Infrared Space Interferometer with Double Fourier Modulation (FP7-FISICA)

Author: Savini, G., Ade, P.A.R., Baccichet, Nicola, Bracken, Colm, Dohlen, Kjetil, Donohoe, Anthony, Gom, Brad, Griffin, Matthew J., Holland, Wayne, Iafolla, Valerio, Ivison, Rob, Jones, Martyn, Juanola-Parramon, Roser, Lightfoot, John, Liu, Scige, McMillan, Alison, Murphy, J.Anthony, Naylor, David A., O'Sullivan, Créidhe, Pascale, Enzo, Pezzuto, Stefano, Rakotonimbahy, Eddy, Schito, Daniele, Spencer, Locke D., Spinoglio, Luigi, Swinyard, Bruce, Veenendaal, Ian, Vives, Sebastien, Walker, David, Leisawitz, David T., Shi, Sheng-Cai, Matsuo, Hiroshi, Savini, G., Ade, P.A.R., Baccichet, Nicola, Bracken, Colm, Dohlen, Kjetil, Donohoe, Anthony, Gom, Brad, Griffin, Matthew J., Holland, Wayne, Iafolla, Valerio, Ivison, Rob, Jones, Martyn, Juanola-Parramon, Roser, Lightfoot, John, Liu, Scige, McMillan, Alison, Murphy, J.Anthony, Naylor, David A., O'Sullivan, Créidhe, Pascale, Enzo, Pezzuto, Stefano, Rakotonimbahy, Eddy, Schito, Daniele, Spencer, Locke D., Spinoglio, Luigi, Swinyard, Bruce, Veenendaal, Ian, Vives, Sebastien, Walker, David, Leisawitz, David T., Shi, Sheng-Cai, and Matsuo, Hiroshi
Abstract: The progress and results of the ongoing FP7-FISICA programme to re-asses the scientific goals of a Far-Infrared Space Interfereometer and push the development of some of its key technology elements are reported.
Published: 2015

46. Two mass distributions in the L1641 molecular clouds: the Herschel connection of dense cores and filaments in Orion A

Author: Polychroni, Danae, Schisano, Eugenio, Elia, Davide, Roy, Arabindo, Molinari, Sergio, Martin, Peter, Andre, Philippe, Turrini, Diego, Rygl, Kazi, Busquet, Gemma, di Giorgio, Anna Maria, Pestalozzi, Michele, Pezzuto, Stefano, Arzoumanian, Doris, Bontemps, Silvain, Di Francesco, James, Hennemann, Martin, Hill, Tracy, Konyves, Vera, Men'shchikov, Alexander, Motte, Frederique, Nguyen-Luong, Quang, Peretto, Nicolas, Schneider, Nicola, and White, Glenn
Subjects: macromolecular substances
Abstract: We present the Herschel Gould Belt survey maps of the L 1641 molecular clouds in Orion A. We extracted both the filaments and dense cores in the region. We identified which of dense sources are proto- or pre-stellar, and studied their association with the identified filaments. We find that although most (71%) of the pre-stellar sources are located on filaments there is still a significant fraction of sources not associated with such structures. We find that these two populations (on and off the identified filaments) have distinctly different mass distributions. The mass distribution of the sources on the filaments is found to peak at 4 Solar Masses and drives the shape of the CMF at higher masses, which we fit with a power law of the form dN /dlogM ∝ M -1.4±0.4 . The mass distribution of the sources off the filaments, on the other hand, peaks at 0.8⊙ and leads to a flattening of the CMF at masses lower than ˜4⊙. We postulate that this difference between the mass distributions is due to the higher proportion of gas that is available in the filaments, rather than in the diffuse cloud.
Published: 2013

47. From Clouds to Young Stellar Objects and back again: the all-in-one view from the Herschel infrared Galactic Plane Survey

Author: Molinari, Sergio, Abergel, Alain, Rivera-Ingraham, Alana, Noriega-Crespo, Alberto, Traficante, Alessio, Di Giorgio, Anna, Zavagno, Annie, Chrysostomou, Antonio, Roy, Arabino, Babar, Ali, Maiolo, Berlinda, Schulz, Bernhard, Jiang, Biwei, Sibthorpe, Bruce, Swinyard, Bruce, Battersby, Cara, Burigana, Carlo, Brunt, Chris, Davis, Chris, Joblin, Christine, Waelkens, Christoffel, Meny, Claude, Codella, Claudio, Popescu, Cristina, Polychroni, Danae, Eden, David, Ikhenaode, David, Elia, Davide, Paradis, Deborah, Shepherd, Debra, Russeil, Delphine, Ward-Thompson, D., Stamatellos, Dimitris, Marshall, Douglas, Sturm, Eckhard, Rosolowsky, Erik, Schisano, Eugenio, Faustini, Fabiana, Agostini, Fabio, Massi, Fabrizio, La Morgia, Federico, Piacentini, Francesco, Strafella, Francesco, Boulanger, Francois, Schuller, Frederic, Motte, Frederique, Wyrowski, Friedrich, Fuller, Gary, de Gasperis, Giancarlo, Joncas, Gilles, Giardino, Giovanna, White, Glenn, Umana, Grazia, Lagache, Guilaine, Rivest, Guillaume, Stringfellow, Guy, Yorke, Harold, Ristorcelli, Isabelle, Difrancesco, James, Brand, Jan, Glenn, Jason, Kirk, Jason, Rodon, Javier, Baluteau, Jean-Paul, Bernard, Jean-Philippe, Li, Jinzeng, Neves, Joao, Mottram, Joe, Fischera, Joerg, Bally, John, Richer, John, Blommaert, Joris, Cernicharo, Jose, Ganga, K., Morgan, Larry, Testi, Leonardo, Anderson, Loren, Piazzo, Lorenzo, Campeggio, Loretta, Conversi, Luca, Olmi, Luca, Valenziano, Luca, Montier, Ludovic, Spinoglio, Luigi, Beltran, Maite, Huang, Maohai, Miville-Deschenes, Marc-Antoine, Sauvage, Marc, Veneziani, Marcella, Thompson, Mark, Cohen, Martin, Giard, Martin, Marengo, Massimo, Compiegne, Mathieu, Griffin, Matt, Pomares, Melanie, Hoare, Melvin, Barlow, Michael, Burton, Michael, Reid, Michael, Smith, Michael, Pestalozzi, Michele, Juvela, Mika, Matsuura, Mikako, Benedettini, Milena, Schneider, N., Billot, Nicolas, Peretto, Nicolas, Berne, Olivier, Caselli, Paola, Debernardis, Paolo, Natoli, Paolo, Saraceno, Paolo, Goldsmith, Paul, Garcia Lario, Pedro, Martin, Peter, Schilke, Peter, Lucas, Phil, Andre, Philippe, Royer, Pierre, Zhang, Qizhou, Plume, Rene, Cesaroni, Riccardo, Tuffs, Richard, Paladini, Roberta, Vavrek, Roland, Taylor, Russ, Carey, Sean, Viti, Serena, Masi, Silvia, Pezzuto, Stefano, Lord, Steve, Chakrabarti, Sukanya, Bontemps, Sylvain, Lim, Tanya, Mueller, Thomas, Robitaille, Thomas, Troost, Tobias, Moore, Toby, Minier, Vincent, Reach, William, Fukui, Yasuo, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Service de Neurologie [CHU Pitié-Salpêtrière], IFR70-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Neurologie et thérapeutique expérimentale, Université Pierre et Marie Curie - Paris 6 (UPMC)-IFR70-Institut National de la Santé et de la Recherche Médicale (INSERM), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique des Lasers (LPL), Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), SLAC National Accelerator Laboratory (SLAC), Stanford University, Istituto di Radioastronomia [Bologna] (IRA), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Mechanical and Aerospace Engineering [Victoria]], Monash University [Clayton], Istituto Nazionale di Geofisica e Vulcanologia – Sezione di Pisa (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Department of Physics and Astronomy, University of Canterbury [Christchurch], University of Manchester [Manchester], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), I. Physikalisches Institut [Köln], Universität zu Köln, Recherche en épidémiologie et biostatistique, Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM), Laboratoire de Nanotechnologie et d'Instrumentation Optique (LNIO), Institut Charles Delaunay (ICD), Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS), Institute of Atomic Physics, Université de Roumanie, Department of Physics and Astronomy [Calgary], University of Calgary, FORMATION STELLAIRE 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Service de neurologie 1 [CHU Pitié-Salpétrière], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Institut National de la Santé et de la Recherche Médicale (INSERM)-IFR70-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), California Institute of Technology (CALTECH)-NASA, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Université Sorbonne Paris Cité (USPC)-Institut Galilée-Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), Stanford Linear Accelerator Center (SLAC), Stanford University [Stanford], Istituto di Radioastronomia (IRA), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universität zu Köln = University of Cologne, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)
Subjects: [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::Galaxy Astrophysics
Abstract: Symposium E, session 14, paper number E14-0026-10 (Oral); From diffuse interstellar cirrus to dense atomic and molecular clouds, from protostellar to post-AGB envelopes, from super-shells to supernovae remnants, the Herschel Hi-GAL survey offer an unprecedented snapshot of all the different phases of the Galactic ISM, its evolution and interactions. I will present early results on a variety of topics including the lifetime of massive pre-stellar phases, the fragmentation and collapse of extended structures, the timeline for massive star formation, dust properties in cirrus and molecular clouds.
Published: 2010

48. The science of EChO

Author: Tinetti , Giovanna, Cho , James Y.-K., Griffith , Caitlin A., Grasset , Olivier, Grenfell , Lee, Guillot , Tristan, Koskinen , Tommi T., Moses , Julianne I., Pinfield , David, Tennyson , Jonathan, Tessenyi , Marcell, Wordsworth , Robin, Aylward , Alan, Van Boekel , Roy, Coradini , Angioletta, Encrenaz , Therese, Snellen , Ignas, Zapatero-Osorio , Maria R., Bouwman , Jeroen, Du Foresto , Vincent Coudé, Lopez-Morales , Mercedes, Mueller-Wodarg , Ingo, Pallé , Enric, Selsis , Franck, Sozzetti , Alessandro, Beaulieu , Jean-Philippe, Henning , Thomas, Meyer , Michael, Micela , Giuseppina, Ribas , Ignasi, Stam , Daphne, Swain , Mark, Krause , Oliver, Ollivier , Marc, Pace , Emanuele, Swinyard , Bruce, Ade , Peter A. R., Achilleos , Nick, Adriani , Alberto, Agnor , Craig B., Afonso , Cristina, Prieto , Carlos Allende, Bakos , Gaspar, Barber , Robert J., Barlow , Michael, Bernath , Peter, Bézard , Bruno, Bordé , Pascal, Brown , Linda R., Cassan , Arnaud, Cavarroc , Céline, Ciaravella , Angela, Cockell , Charles, Coustenis , Athéna, Danielski , Camilla, Decin , Leen, De Kok , Remco, Demangeon , Olivier, Deroo , Pieter, Doel , Peter, Drossart , Pierre, Fletcher , Leigh N., Focardi , Matteo, Forget , Francois, Fossey , Steve, Fouqué , Pascal, Frith , James, Galand , Marina, Gaulme , Patrick, Hernández , Jonay I. González, Grassi , Davide, Griffin , Matt J., Grözinger , Ulrich, Guedel , Manuel, Guio , Pactrick, Hainaut , Olivier, Hargreaves , Robert, Hauschildt , Peter H., Heng , Kevin, Heyrovsky , David, Hueso , Ricardo, Irwin , Pat, Kaltenegger , Lisa, Kervella , Patrick, Kipping , David, Kovacs , Geza, Barbera , Antonino La, Lammer , Helmut, Lellouch , Emmanuel, Leto , Giuseppe, Morales , Mercedes Lopez, Valverde , Miguel A. Lopez, Lopez-Puertas , Manuel, Lovi , Christophe, Maggio , Antonio, Maillard , Jean-Pierre, Prado , Jesus Maldonado, Marquette , Jean-Baptiste, Martin-Torres , Francisco J., Maxted , Pierre, Miller , Steve, Molinari , Sergio, Montes , David, Moro-Martin , Amaya, Mousis , Olivier, Tuong , Napoléon Nguyen, Nelson , Richard, Orton , Glenn S., Pantin , Eric, Pascale , Enzo, Pezzuto , Stefano, Poretti , Ennio, Prinja , Raman, Prisinzano , Loredana, Réess , Jean-Michel, Reiners , Ansgar, Samuel , Benjamin, Forcada , Jorge Sanz, Sasselov , Dimitar, Savini , Giorgio, Sicardy , Bruno, Smith , Alan, Stixrude , Lars, Strazzulla , Giovanni, Vasisht , Gautam, Vinatier , Sandrine, Viti , Serena, Waldmann , Ingo, White , Glenn J., Widemann , Thomas, Yelle , Roger, Yung , Yuk, Yurchenko , Sergey, University College of London [London] ( UCL ), Lunar and Planetary Laboratory [Tucson], University of Arizona, Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides ( CASSIOPEE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [UCL London], Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Istituto di Fisica dello Spazio Interplanetario ( INAF ), Consiglio Nazionale delle Ricerche [Roma] ( CNR ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Département d'Astrophysique (ex SAP) ( DAP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Astronomie ( MPIA ), Liquides Ioniques et Interfaces Chargées ( LI2C ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -ESPCI ParisTech-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astronomico di Palermo ( OAPa ), Istituto Nazionale di Astrofisica ( INAF ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), SRON Netherlands Institute for Space Research ( SRON ), University of Calgary, Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), School of Physics and Astronomy [London], Queen Mary University of London ( QMUL ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Astronomische Rechen-Institut [Heidelberg] ( ARI ), Universität Heidelberg [Heidelberg]-Zentrum für Astronomie der Universität Heidelberg, Planetary and Space Sciences Research Institute [Milton Keynes] ( PSSRI ), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] ( CEPSAR ), The Open University [Milton Keynes] ( OU ) -The Open University [Milton Keynes] ( OU ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of Oxford [Oxford], Institut Pierre-Simon-Laplace ( IPSL ), École normale supérieure - Paris ( ENS Paris ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National d'Etudes Spatiales ( CNES ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Astrophysique de Toulouse-Tarbes ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Blackett Laboratory, Imperial College London, Istituto di Fisica dello Spazio Interplanetaro ( IFSI ), Escuela Superior de Ingenieria, Universidad del País Vasco, Harvard-Smithsonian Center for Astrophysics ( CfA ), Harvard University [Cambridge]-Smithsonian Institution, Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Department of Science and Technology Studies [London] ( STS ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Imperial College Healthcare NHS Trust, STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Department of Physics and Astronomy [Milton Keynes], and The Open University [Milton Keynes] ( OU )
Subjects: [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Instrumentation and Methods for Astrophysics, planets and satellites: formation, planets and satellites: general, Astrophysics::Earth and Planetary Astrophysics, planetary systems, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], planetary systems: formation
Abstract: International audience; The science of extra-solar planets is one of the most rapidly changing areas of astrophysics and since 1995 the number of planets known has increased by almost two orders of magnitude. A combination of ground-based surveys and dedicated space missions has resulted in 560-plus planets being detected, and over 1200 that await confirmation. NASA's Kepler mission has opened up the possibility of discovering Earth-like planets in the habitable zone around some of the 100,000 stars it is surveying during its 3 to 4-year lifetime. The new ESA's Gaia mission is expected to discover thousands of new planets around stars within 200 parsecs of the Sun. The key challenge now is moving on from discovery, important though that remains, to characterisation: what are these planets actually like, and why are they as they are? In the past ten years, we have learned how to obtain the first spectra of exoplanets using transit transmission and emission spectroscopy. With the high stability of Spitzer, Hubble, and large ground-based telescopes the spectra of bright close-in massive planets can be obtained and species like water vapour, methane, carbon monoxide and dioxide have been detected. With transit science came the first tangible remote sensing of these planetary bodies and so one can start to extrapolate from what has been learnt from Solar System probes to what one might plan to learn about their faraway siblings. As we learn more about the atmospheres, surfaces and near-surfaces of these remote bodies, we will begin to build up a clearer picture of their construction, history and suitability for life. The Exoplanet Characterisation Observatory, EChO, will be the first dedicated mission to investigate the physics and chemistry of Exoplanetary Atmospheres. By characterising spectroscopically more bodies in different environments we will take detailed planetology out of the Solar System and into the Galaxy as a whole. EChO has now been selected by the European Space Agency to be assessed as one of four M3 mission candidates.
Published: 2010

49. unimap: a generalized least-squares map maker for Herschel data

Author: Piazzo, Lorenzo, primary, Calzoletti, Luca, additional, Faustini, Fabiana, additional, Pestalozzi, Michele, additional, Pezzuto, Stefano, additional, Elia, Davide, additional, di Giorgio, Anna, additional, and Molinari, Sergio, additional
Published: 2014
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50. The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

Author: SWINYARD, Bruce, NAKAGAWA, Takao, MERKEN, Patrick, ROYER, Pierre, SOUVERIJNS, Tim, VANDENBUSSCHE, Bart, WAELKENS, Christoffel, DAVIS, Peter, DI FRANCESCO, James, HALPERN, Mark, HOUDE, Martin, JOHNSTONE, Doug, JONCAS, Gilles, NAYLOR, David, PLUME, Rene, SCOTT, Douglas, ABERGEL, A., BENSAMMAR, S., BRAINE, J., BUAT, V., BURGARELLA, D., CAIS, Ph., DOLE, H., DUBAND, L., ELBAZ, D., GERIN, M., GIARD, M., GOICOECHEA, J., JOBLIN, C., JONES, A., KNEIB, J. P., LAGACHE, Guilaine, MADDEN, S., PONS, R., PAJOT, F., RAMBAUD, D., RAVERA, L., RISTORCELLI, I., RODRIGUEZ, L., VIVES, S., ZAVAGNO, Annie, GEIS, Norbert, KRAUSE, Oliver, LUTZ, Dieter, POGLITSCH, Albrecht, RAAB, Walfried, STEGMAIER, Jutta, STURM, Eckhard, TUFFS, Richard, LEE, Hyung Mok, KOO, Bon-Chul, IM, Myungshin, PAK, Soojong, HAN, Wonyong, PARK, Jang-Hyun, NAM, Uk-Won, JIN, Ho, LEE, Dae-Hee, YUK, In-Soo, LEE, Sungho, AIKAWA, Yuri, ARIMOTO, Nobuo, DOI, Yasuo, ENYA, Keigo, FUKAGAWA, Misato, FURUSHO, Reiko, HASEGAWA, Sunao, HAYASHI, Masahiko, HONDA KANAGAWA, Mitsuhiko, IDA, Shigeru, IMANISHI, MASATOSHI, INUTSUKA, Shu-Ichiro, IZUMIURA, Hideyuki, KAMAYA, Hideyuki, KANEDA, Hidehiro, KASUGA, Toshihiro, KATAZA, Hirokazu, KAWABATA, Koji, KAWADA, Mitsunobu, KAWAKITA, Hideyo, KII, Tsuneo, KODA, Jin, KODAMA, Tadayuki, KOKUBO, Eiichiro, KOMATSU, Keiji, MATSUHARA, Hideo, MATSUMOTO, Toshio, MATSUURA, Shuji, MIYATA, Takashi, MIYATA, Murakam, NAGATA, Hirohisa, NAGATA, Tetsuya, NAKAJIMA, Tadashi, NAOTO, Kobayashi, NISHI, Ryoichi, NODA, Atsushi, OKAMOTO, Atsushi, OKAMOTO, Yoshiko K., OMUKAI, Kazuyuki, ONAKA, Takashi, OOTSUBO, Takafumi, OUCHI, Masami, SAITO, Hirobumi, SATO, Yoichi, SAKO, Shigeyuki, SEKIGUCHI, Tomohiko, SHIBAI, Hiroshi, SUGITA, Hiroyuki, SUGITANI, Koji, SUSA, Hajime, PYO, Tae-Soo, TAMURA, Motohide, UEDA, Yoshihiro, UENO, Munetaka, WADA, Takehiko, WATANABE, Jun'Ichi, YAMADA, Toru, YAMAMURA, Issei, YOSHIDA, Naoki, YOSHIMI, Kitamura, YUI, Yukari, BENEDETTINI, Milena, CERULLI, Riccardo, DI GIORGIO, Anna, MOLINARI, Sergio, ORFEI, Renato, PEZZUTO, Stefano, PIAZZO, Lorenzo, SARACENO, Paolo, SPINOGLIO, Luigi, DE GRAAUW, Thijs, DE KORTE, Piet, HELMICH, Frank, HOEVERS, Henk, HUISMAN, Robert, SHIPMAN, Russell, VAN DER TAK, Floris, VAN DER WERF, Paul, WILD, Wolfgang, ACOSTA-PULIDO, Jose, CERNICHARO, Jose, HERREROS, Jose, MARTIN-PINTADO, Jesus, NAJARRO, Francisco, PEREZ-FOURMON, Ismael, RAMON PARDO, Juan, GOMEZ, Francisca, CASTRO RODRIGUEZ, Nieves, ADE, Peter, BARLOW, Mike, CLEMENTS, David, FERLET, Marc, FRASER, Helen, GRIFFIN, Douglas, GRIFFIN, Matthew, HARGRAVE, Peter, ISAAK, Kate, IVISON, Robert, MANSOUR, Malik, LANIESSE, Jonathan, MAUSKOPF, Phillip, MOROZOV, Dmitry, OLIVER, Seb, ORLANDO, Angiola, PAGE, Mathew, POPESCU, Cristina, SERJEANT, Stephen, SUDIWALA, Rashmi, RIGOPOULOU, Dimitra, WALKER, Ian, WHITE, Glenn, VITI, Serena, WINTER, Berend, BOCK, Jamie, BRADFORD, Matt, HARWIT, Martin, HOLMES, Warren, Institut Méditerranéen d'Ecologie et de Paléoécologie (IMEP), Université Paul Cézanne - Aix-Marseille 3-Centre National de la Recherche Scientifique (CNRS)-Avignon Université (AU)-Université de Provence - Aix-Marseille 1, Institute of Atomic Physics, Université de Roumanie, Groundwater Tracing Unit, Department of Geological Sciences, School of Environmental Sciences [Norwich], University of East Anglia [Norwich] (UEA), Institut de Recherche en Immunologie et en Cancérologie [UdeM-Montréal] (IRIC), Université de Montréal (UdeM), Department of Zoology, University of Otago [Dunedin, Nouvelle-Zélande], Transplantation Biology Group, Imperial College London, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), FORMATION STELLAIRE 2009, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Processus mentaux et activation cérébrale, Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-IFR19-Institut National de la Santé et de la Recherche Médicale (INSERM), IFR des neurosciences de Lyon (IFNL), Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre Hospitalier le Vinatier [Bron]-Hospices Civils de Lyon (HCL)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Department of Radio and Space Science [Göteborg], Chalmers University of Technology [Göteborg], Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Solar Influences Data Analysis Center [Brussels] (SIDC), Royal Observatory of Belgium [Brussels] (ROB), Propriétés Optiques des Matériaux et Applications (POMA), Centre National de la Recherche Scientifique (CNRS)-Université d'Angers (UA), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physiology, The University of Hong Kong (HKU), School of Environmental Systems Engineering (SESE), The University of Western Australia (UWA), Centre for Water Research (CWR), Macaulay Institute, Centre Science des Matériaux et des Structures (SMS-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Département Mécanique et Procédés d'Elaboration (MPE-ENSMSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-SMS, Department of Obstetrics and Gynecology [Stanford], Stanford Medicine, Stanford University-Stanford University, Korea Astronomy and Space Science Institute (KASI), Okayama University, Jack Baskin School of Engineering (UCSC), University of California [Santa Cruz] (UCSC), University of California-University of California, Adobe Systems Inc. (Adobe Advanced Technology Labs), Adobe Systems Inc., Defence Evaluation and Research Agency (DERA), Ministry of Defence (UK) (MOD)-Propulsion and Performance Department, Centre for Air Transport and the Environment (CATE), Manchester Metropolitan University (MMU), Department of Chemistry, Williams Hall-Kent State University, School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Department of Earth and Planetary Sciences [Kobe], Kobe University, National Institute of Agro-Environmental Sciences (NIAES), Department of Earth System Science and Technology [Fukuoka] (ESST), Kyushu University [Fukuoka], Tokyo Institute of Technology [Tokyo] (TITECH), Department of Information and Communication Engineering, Graduate School of Information Science and Technology-The University of Tokyo (UTokyo), Department of Physics and Earth Sciences, University of the Ryukyus [Okinawa], Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Center for Climate System Research [Kashiwa] (CCSR), The University of Tokyo (UTokyo), School of Humanities [Univ of Toyama], University of Toyama, Department of Mechanical System (Hiroshima University), Hiroshima University, High Temperature Plasma Center [Tokyo], Discrete Optimization Laboratory, Toyohashi University of Technology, Hatakeyama Laboratory, University of Electro-Communications [Tokyo] (UEC)-Tohoku University [Sendai], Institute of Industrial Science (IIS), Institut de génétique et biologie moléculaire et cellulaire (IGBMC), Université Louis Pasteur - Strasbourg I-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Research Center (MCC), Mitsubishi Chemical Corporation, Institute for Solid State Physics [Tokyo] (ISSP), University of Electro-Communications [Tokyo] (UEC), Faculty of Science and Engineering [Waseda], Waseda University, Department of Civil Engineering, Chuo University (Chuo University), Frontier Collaborative Research Center (FCRC), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Antarctic Research a European Network for Astrophysics (ARENA), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), Max-Planck-Institut für Radioastronomie (MPIFR), Departamento de Astrofísica Molecular e Infrarroja (DAMIR), Instituto de Estructura de la Materia (IEM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'océanographie et de biogéochimie (LOB), Université de la Méditerranée - Aix-Marseille 2-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecosystèmes Littoraux et Cotiers, Université de Lille, Sciences et Technologies-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Processus d'Activation Sélective par Transfert d'Energie Uni-électronique ou Radiatif (UMR 8640) (PASTEUR), Université Pierre et Marie Curie - Paris 6 (UPMC)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Ecole Supérieure des Affaires (ESA), Université Pierre Mendès France - Grenoble 2 (UPMF), Service de Neurologie [CHU Pitié-Salpêtrière], IFR70-CHU Pitié-Salpêtrière [AP-HP], Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Neurologie et thérapeutique expérimentale, Institut National de la Santé et de la Recherche Médicale (INSERM)-IFR70-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Physics, University of Wales, Engineering Department, University of Cambridge [UK] (CAM), SLAC National Accelerator Laboratory (SLAC), Stanford University, Université Paul Cézanne - Aix-Marseille 3-Université de Provence - Aix-Marseille 1-Avignon Université (AU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université de Lyon-Université de Lyon-Hospices Civils de Lyon (HCL)-Centre Hospitalier le Vinatier [Bron]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université d'Angers (UA)-Centre National de la Recherche Scientifique (CNRS), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Kyushu University, Waseda University [Tokyo, Japan], National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - 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Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Service de neurologie 1 [CHU Pitié-Salpétrière], Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Stanford Linear Accelerator Center (SLAC), Astronomy, Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), The University of Tokyo (UTokyo)-Graduate School of Information Science and Technology, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], and Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Infrared telescope, UNIVERSE, Astrophysics, Spica, Astrophysics::Cosmology and Extragalactic Astrophysics, POLYCYCLIC AROMATIC-HYDROCARBON, 7. Clean energy, 01 natural sciences, Space missions, Cosmology, Space exploration, law.invention, STAR-FORMATION, 010309 optics, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Infrared astronomy, SPECTRUM, Spacecraft, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], SUBMILLIMETER GALAXIES, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, MODEL, SPITZER, PAHS, Space and Planetary Science, Infrared, Physics::Space Physics, IR, Astrophysics::Earth and Planetary Astrophysics, business, EMISSION
Abstract: International audience; The Space Infrared telescope for Cosmology and Astrophysics (SPICA) is planned to be the next space astronomy mission observing in the infrared. The mission is planned to be launched in 2017 and will feature a 3.5 m telescope cooled to 30 microns wavelength). We describe the scientific advances that will be made possible by this large increase in sensitivity and give details of the mission, spacecraft and focal plane conceptual design.
Published: 2009

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