@unpublished{AcharyaActisAghajanietal.2013,
  author    = {Acharya, B. S. and Actis, M. and Aghajani, T. and Agnetta, G. and Aguilar, J. and Aharonian, Felix A. and Ajello, M. and Akhperjanian, A. G. and Alcubierre, M. and Aleksic, J. and Alfaro, R. and Aliu, E. and Allafort, A. J. and Allan, D. and Allekotte, I. and Amato, E. and Anderson, J. and Ang{\"u}ner, Ekrem Oǧuzhan and Antonelli, L. A. and Antoranz, P. and Aravantinos, A. and Arlen, T. and Armstrong, T. and Arnaldi, H. and Arrabito, L. and Asano, K. and Ashton, T. and Asorey, H. G. and Awane, Y. and Baba, H. and Babic, A. and Baby, N. and Baehr, J. and Bais, A. and Baixeras, C. and Bajtlik, S. and Balbo, M. and Balis, D. and Balkowski, C. and Bamba, A. and Bandiera, R. and Barber, A. and Barbier, C. and Barcelo, M. and Barnacka, Anna and Barnstedt, J{\"u}rgen and Barres de Almeida, U. and Barrio, J. A. and Basili, A. and Basso, S. and Bastieri, D. and Bauer, C. and Baushev, Anton N. and Becerra Gonzalez, J. and Becherini, Yvonne and Bechtol, K. C. and Tjus, J. Becker and Beckmann, Volker and Bednarek, W. and Behera, B. and Belluso, M. and Benbow, W. and Berdugo, J. and Berger, K. and Bernard, F. and Bernardino, T. and Bernl{\"o}hr, K. and Bhat, N. and Bhattacharyya, S. and Bigongiari, C. and Biland, A. and Billotta, S. and Bird, T. and Birsin, E. and Bissaldi, E. and Biteau, Jonathan and Bitossi, M. and Blake, S. and Blanch Bigas, O. and Blasi, P. and Bobkov, A. A. and Boccone, V. and Boettcher, Markus and Bogacz, L. and Bogart, J. and Bogdan, M. and Boisson, Catherine and Boix Gargallo, J. and Bolmont, J. and Bonanno, G. and Bonardi, A. and Bonev, T. and Bonifacio, P. and Bonnoli, G. and Bordas, Pol and Borgland, A. W. and Borkowski, Janett and Bose, R. and Botner, O. and Bottani, A. and Bouchet, L. and Bourgeat, M. and Boutonnet, C. and Bouvier, A. and Brau-Nogue, S. and Braun, I. and Bretz, T. and Briggs, M. S. and Bringmann, T. and Brook, P. and Brun, Pierre and Brunetti, L. and Buanes, T. and Buckley, J. H. and Buehler, R. and Bugaev, V. and Bulgarelli, A. and Bulik, Tomasz and Busetto, G. and Buson, S. and Byrum, K. and Cailles, M. and Cameron, R. A. and Camprecios, J. and Canestrari, R. and Cantu, S. and Capalbi, M. and Caraveo, P. A. and Carmona, E. and Carosi, A. and Carr, John and Carton, P. H. and Casanova, Sabrina and Casiraghi, M. and Catalano, O. and Cavazzani, S. and Cazaux, S. and Cerruti, M. and Chabanne, E. and Chadwick, Paula M. and Champion, C. and Chen, Andrew and Chiang, J. and Chiappetti, L. and Chikawa, M. and Chitnis, V. R. and Chollet, F. and Chudoba, J. and Cieslar, M. and Cillis, A. N. and Cohen-Tanugi, J. and Colafrancesco, Sergio and Colin, P. and Calome, J. and Colonges, S. and Compin, M. and Conconi, P. and Conforti, V. and Connaughton, V. and Conrad, Jan and Contreras, J. L. and Coppi, P. and Corona, P. and Corti, D. and Cortina, J. and Cossio, L. and Costantini, H. and Cotter, G. and Courty, B. and Couturier, S. and Covino, S. and Crimi, G. and Criswell, S. J. and Croston, J. and Cusumano, G. and Dafonseca, M. and Dale, O. and Daniel, M. and Darling, J. and Davids, I. and Dazzi, F. and De Angelis, A. and De Caprio, V. and De Frondat, F. and de Gouveia Dal Pino, E. M. and de la Calle, I. and De La Vega, G. A. and Lopez, R. de los Reyes and De Lotto, B. and De Luca, A. and de Mello Neto, J. R. T. and de Naurois, M. and de Oliveira, Y. and de Ona Wilhelmi, E. and de Souza, V. and Decerprit, G. and Decock, G. and Deil, C. and Delagnes, E. and Deleglise, G. and Delgado, C. and Della Volpe, D. and Demange, P. and Depaola, G. and Dettlaff, A. and Di Paola, A. and Di Pierro, F. and Diaz, C. and Dick, J. and Dickherber, R. and Dickinson, H. and Diez-Blanco, V. and Digel, S. and Dimitrov, D. and Disset, G. and Djannati-Ata{\"i}, A. and Doert, M. and Dohmke, M. and Domainko, W. and Prester, Dijana Dominis and Donat, A. and Dorner, D. and Doro, M. and Dournaux, J-L. and Drake, G. and Dravins, D. and Drury, L. and Dubois, F. and Dubois, R. and Dubus, G. and Dufour, C. and Dumas, D. and Dumm, J. and Durand, D. and Dyks, J. and Dyrda, M. and Ebr, J. and Edy, E. and Egberts, Kathrin and Eger, P. and Einecke, S. and Eleftheriadis, C. and Elles, S. and Emmanoulopoulos, D. and Engelhaupt, D. and Enomoto, R. and Ernenwein, J-P and Errando, M. and Etchegoyen, A. and Evans, P. and Falcone, A. and Fantinel, D. and Farakos, K. and Farnier, C. and Fasola, G. and Favill, B. and Fede, E. and Federici, S. and Fegan, S. and Feinstein, F. and Ferenc, D. and Ferrando, P. and Fesquet, M. and Fiasson, A. and Fillin-Martino, E. and Fink, D. and Finley, C. and Finley, J. P. and Fiorini, M. and Firpo Curcoll, R. and Flores, H. and Florin, D. and Focke, W. and Foehr, C. and Fokitis, E. and Font, L. and Fontaine, G. and Fornasa, M. and Foerster, A. and Fortson, L. and Fouque, N. and Franckowiak, A. and Fransson, C. and Fraser, G. and Frei, R. and Albuquerque, I. F. M. and Fresnillo, L. and Fruck, C. and Fujita, Y. and Fukazawa, Y. and Fukui, Y. and Funk, S. and Gaebele, W. and Gabici, S. and Gabriele, R. and Gadola, A. and Galante, N. and Gall, D. and Gallant, Y. and Gamez-Garcia, J. and Garcia, B. and Garcia Lopez, R. and Gardiol, D. and Garrido, D. and Garrido, L. and Gascon, D. and Gaug, M. and Gaweda, J. and Gebremedhin, L. and Geffroy, N. and Gerard, L. and Ghedina, A. and Ghigo, M. and Giannakaki, E. and Gianotti, F. and Giarrusso, S. and Giavitto, G. and Giebels, B. and Gika, V. and Giommi, P. and Girard, N. and Giro, E. and Giuliani, A. and Glanzman, T. and Glicenstein, J. -F. and Godinovic, N. and Golev, V. and Gomez Berisso, M. and Gomez-Ortega, J. and Gonzalez, M. M. and Gonzalez, A. and Gonzalez, F. and Gonzalez Munoz, A. and Gothe, K. S. and Gougerot, M. and Graciani, R. and Grandi, P. and Granena, F. and Granot, J. and Grasseau, G. and Gredig, R. and Green, A. and Greenshaw, T. and Gregoire, T. and Grimm, O. and Grube, J. and Grudzinska, M. and Gruev, V. and Gruenewald, S. and Grygorczuk, J. and Guarino, V. and Gunji, S. and Gyuk, G. and Hadasch, D. and Hagiwara, R. and Hahn, J. and Hakansson, N. and Hallgren, A. and Hamer Heras, N. and Hara, S. and Hardcastle, M. J. and Harris, J. and Hassan, T. and Hatanaka, K. and Haubold, T. and Haupt, A. and Hayakawa, T. and Hayashida, M. and Heller, R. and Henault, F. and Henri, G. and Hermann, G. and Hermel, R. and Herrero, A. and Hidaka, N. and Hinton, J. and Hoffmann, D. and Hofmann, W. and Hofverberg, P. and Holder, J. and Horns, D. and Horville, D. and Houles, J. and Hrabovsky, M. and Hrupec, D. and Huan, H. and Huber, B. and Huet, J. -M. and Hughes, G. and Humensky, T. B. and Huovelin, J. and Ibarra, A. and Illa, J. M. and Impiombato, D. and Incorvaia, S. and Inoue, S. and Inoue, Y. and Ioka, K. and Ismailova, E. and Jablonski, C. and Jacholkowska, A. and Jamrozy, M. and Janiak, M. and Jean, P. and Jeanney, C. and Jimenez, J. J. and Jogler, T. and Johnson, T. and Journet, L. and Juffroy, C. and Jung, I. and Kaaret, P. and Kabuki, S. and Kagaya, M. and Kakuwa, J. and Kalkuhl, C. and Kankanyan, R. and Karastergiou, A. and Kaercher, K. and Karczewski, M. and Karkar, S. and Kasperek, Aci. and Kastana, D. and Katagiri, H. and Kataoka, J. and Katarzynski, K. and Katz, U. and Kawanaka, N. and Kellner-Leidel, B. and Kelly, H. and Kendziorra, E. and Khelifi, B. and Kieda, D. B. and Kifune, T. and Kihm, T. and Kishimoto, T. and Kitamoto, K. and Kluzniak, W. and Knapic, C. and Knapp, J. w and Knoedlseder, J. and Koeck, F. and Kocot, J. and Kodani, K. and Koehne, J. -H. and Kohri, K. and Kokkotas, K. and Kolitzus, D. and Komin, N. and Kominis, I. and Konno, Y. and Koeppel, H. and Korohoda, P. and Kosack, K. and Koss, G. and Kossakowski, R. and Kostka, P. and Koul, R. and Kowal, G. and Koyama, S. and Koziol, J. and Kraehenbuehl, T. and Krause, J. and Krawzcynski, H. and Krennrich, F. and Krepps, A. and Kretzschmann, A. and Krobot, R. and Krueger, P. and Kubo, H. and Kudryavtsev, V. A. and Kushida, J. and Kuznetsov, A. and La Barbera, A. and La Palombara, N. and La Parola, V. and La Rosa, G. and Lacombe, K. and Lamanna, G. and Lande, J. and Languignon, D. and Lapington, J. and Laporte, P. and Lavalley, C. and Le Flour, T. and Le Padellec, A. and Lee, S. -H. and Lee, W. H. and Leigui de Oliveira, M. A. and Lelas, D. and Lenain, J. -P. and Leopold, D. J. and Lerch, T. and Lessio, L. and Lieunard, B. and Lindfors, E. and Liolios, A. and Lipniacka, A. and Lockart, H. and Lohse, T. and Lombardi, S. and Lopatin, A. and Lopez, M. and Lopez-Coto, R. and Lopez-Oramas, A. and Lorca, A. and Lorenz, E. and Lubinski, P. and Lucarelli, F. and Luedecke, H. and Ludwin, J. and Luque-Escamilla, P. L. and Lustermann, W. and Luz, O. and Lyard, E. and Maccarone, M. C. and Maccarone, T. J. and Madejski, G. M. and Madhavan, A. and Mahabir, M. and Maier, G. and Majumdar, P. and Malaguti, G. and Maltezos, S. and Manalaysay, A. and Mancilla, A. and Mandat, D. and Maneva, G. and Mangano, A. and Manigot, P. and Mannheim, K. and Manthos, I. and Maragos, N. and Marcowith, A. and Mariotti, M. and Marisaldi, M. and Markoff, S. and Marszalek, A. and Martens, C. and Marti, J. and Martin, J-M. and Martin, P. and Martinez, G. and Martinez, F. and Martinez, M. and Masserot, A. and Mastichiadis, A. and Mathieu, A. and Matsumoto, H. and Mattana, F. and Mattiazzo, S. and Maurin, G. and Maxfield, S. and Maya, J. and Mazin, D. and Mc Comb, L. and McCubbin, N. and McHardy, I. and McKay, R. and Medina, C. and Melioli, C. and Melkumyan, D. and Mereghetti, S. and Mertsch, P. and Meucci, M. and Michalowski, J. and Micolon, P. and Mihailidis, A. and Mineo, T. and Minuti, M. and Mirabal, N. and Mirabel, F. and Miranda, J. M. and Mirzoyan, R. and Mizuno, T. and Moal, B. and Moderski, R. and Mognet, I. and Molinari, E. and Molinaro, M. and Montaruli, T. and Monteiro, I. and Moore, P. and Moralejo Olaizola, A. and Mordalska, M. and Morello, C. and Mori, K. and Mottez, F. and Moudden, Y. and Moulin, E. and Mrusek, I. and Mukherjee, R. and Munar-Adrover, P. and Muraishi, H. and Murase, K. and Murphy, A. and Nagataki, S. and Naito, T. and Nakajima, D. and Nakamori, T. and Nakayama, K. and Naumann, C. L. and Naumann, D. and Naumann-Godo, M. and Nayman, P. and Nedbal, D. and Neise, D. and Nellen, L. and Neustroev, V. and Neyroud, N. and Nicastro, L. and Nicolau-Kuklinski, J. and Niedzwiecki, A. and Niemiec, J. and Nieto, D. and Nikolaidis, A. and Nishijima, K. and Nolan, S. and Northrop, R. and Nosek, D. and Nowak, N. and Nozato, A. and O'Brien, P. and Ohira, Y. and Ohishi, M. and Ohm, S. and Ohoka, H. and Okuda, T. and Okumura, A. and Olive, J. -F. and Ong, R. A. and Orito, R. and Orr, M. and Osborne, J. and Ostrowski, M. and Otero, L. A. and Otte, N. and Ovcharov, E. and Oya, I. and Ozieblo, A. and Padilla, L. and Paiano, S. and Paillot, D. and Paizis, A. and Palanque, S. and Palatka, M. and Pallota, J. and Panagiotidis, K. and Panazol, J. -L. and Paneque, D. and Panter, M. and Paoletti, R. and Papayannis, Alexandros and Papyan, G. and Paredes, J. M. and Pareschi, G. and Parks, G. and Parraud, J. -M. and Parsons, D. and Arribas, M. Paz and Pech, M. and Pedaletti, G. and Pelassa, V. and Pelat, D. and Perez, M. D. C. and Persic, M. and Petrucci, P-O and Peyaud, B. and Pichel, A. and Pita, S. and Pizzolato, F. and Platos, L. and Platzer, R. and Pogosyan, L. and Pohl, M. and Pojmanski, G. and Ponz, J. D. and Potter, W. and Poutanen, J. and Prandini, E. and Prast, J. and Preece, R. and Profeti, F. and Prokoph, H. and Prouza, M. and Proyetti, M. and Puerto-Gimenez, I. and Puehlhofer, G. and Puljak, I. and Punch, M. and Pyziol, R. and Quel, E. J. and Quinn, J. and Quirrenbach, A. and Racero, E. and Rajda, P. J. and Ramon, P. and Rando, R. and Rannot, R. C. and Rataj, M. and Raue, M. and Reardon, P. and Reimann, O. and Reimer, A. and Reimer, O. and Reitberger, K. and Renaud, M. and Renner, S. and Reville, B. and Rhode, W. and Ribo, M. and Ribordy, M. and Richer, M. G. and Rico, J. and Ridky, J. and Rieger, F. and Ringegni, P. and Ripken, J. and Ristori, P. R. and Riviere, A. and Rivoire, S. and Rob, L. and Roeser, U. and Rohlfs, R. and Rojas, G. and Romano, Patrizia and Romaszkan, W. and Romero, G. E. and Rosen, S. and Lees, S. Rosier and Ross, D. and Rouaix, G. and Rousselle, J. and Rousselle, S. and Rovero, A. C. and Roy, F. and Royer, S. and Rudak, B. and Rulten, C. and Rupinski, M. and Russo, F. and Ryde, F. and Sacco, B. and Saemann, E. O. and Saggion, A. and Safiakian, V. and Saito, K. and Saito, T. and Saito, Y. and Sakaki, N. and Sakonaka, R. and Salini, A. and Sanchez, F. and Sanchez-Conde, M. and Sandoval, A. and Sandaker, H. and Sant'Ambrogio, E. and Santangelo, A. and Santos, E. M. and Sanuy, A. and Sapozhnikov, L. and Sarkar, S. and Sartore, N. and Sasaki, H. and Satalecka, K. and Sawada, M. and Scalzotto, V. and Scapin, V. and Scarcioffolo, M. and Schafer, J. and Schanz, T. and Schlenstedt, S. and Schlickeiser, R. and Schmidt, T. and Schmoll, J. and Schovanek, P. and Schroedter, M. and Schultz, C. and Schultze, J. and Schulz, A. and Schure, K. and Schwab, T. and Schwanke, U. and Schwarz, J. and Schwarzburg, S. and Schweizer, T. and Schwemmer, S. and Segreto, A. and Seiradakis, J. -H. and Sembroski, G. H. and Seweryn, K. and Sharma, M. and Shayduk, M. and Shellard, R. C. and Shi, J. and Shibata, T. and Shibuya, A. and Shum, E. and Sidoli, L. and Sidz, M. and Sieiro, J. and Sikora, M. and Silk, J. and Sillanpaa, A. and Singh, B. B. and Sitarek, J. and Skole, C. and Smareglia, R. and Smith, A. and Smith, D. and Smith, J. and Smith, N. and Sobczynska, D. and Sol, H. and Sottile, G. and Sowinski, M. and Spanier, F. and Spiga, D. and Spyrou, S. and Stamatescu, V. and Stamerra, A. and Starling, R. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steiner, S. and Stergioulas, N. and Sternberger, R. and Sterzel, M. and Stinzing, F. and Stodulski, M. and Straumann, U. and Strazzeri, E. and Stringhetti, L. and Suarez, A. and Suchenek, M. and Sugawara, R. and Sulanke, K. -H. and Sun, S. and Supanitsky, A. D. and Suric, T. and Sutcliffe, P. and Sykes, J. and Szanecki, M. and Szepieniec, T. and Szostek, A. and Tagliaferri, G. and Tajima, H. and Takahashi, H. and Takahashi, K. and Takalo, L. and Takami, H. and Talbot, C. and Tammi, J. and Tanaka, M. and Tanaka, S. and Tasan, J. and Tavani, M. and Tavernet, J. -P. and Tejedor, L. A. and Telezhinsky, Igor O. and Temnikov, P. and Tenzer, C. and Terada, Y. and Terrier, R. and Teshima, M. and Testa, V. and Tezier, D. and Thuermann, D. and Tibaldo, L. and Tibolla, O. and Tiengo, A. and Tluczykont, M. and Todero Peixoto, C. J. and Tokanai, F. and Tokarz, M. and Toma, K. and Torii, K. and Tornikoski, M. and Torres, D. F. and Torres, M. and Tosti, G. and Totani, T. and Toussenel, C. and Tovmassian, G. and Travnicek, P. and Trifoglio, M. and Troyano, I. and Tsinganos, K. and Ueno, H. and Umehara, K. and Upadhya, S. S. and Usher, T. and Uslenghi, M. and Valdes-Galicia, J. F. and Vallania, P. and Vallejo, G. and van Driel, W. and van Eldik, C. and Vandenbrouke, J. and Vanderwalt, J. and Vankov, H. and Vasileiadis, G. and Vassiliev, V. and Veberic, D. and Vegas, I. and Vercellone, S. and Vergani, S. and Veyssiere, C. and Vialle, J. P. and Viana, A. and Videla, M. and Vincent, P. and Vincent, S. and Vink, J. and Vlahakis, N. and Vlahos, L. and Vogler, P. and Vollhardt, A. and von Gunten, H. P. and Vorobiov, S. and Vuerli, C. and Waegebaert, V. and Wagner, R. and Wagner, R. G. and Wagner, S. and Wakely, S. P. and Walter, R. and Walther, T. and Warda, K. and Warwick, R. and Wawer, P. and Wawrzaszek, R. and Webb, N. and Wegner, P. and Weinstein, A. and Weitzel, Q. and Welsing, R. and Werner, M. and Wetteskind, H. and White, R. and Wierzcholska, A. and Wiesand, S. and Wilkinson, M. and Williams, D. A. and Willingale, R. and Winiarski, K. and Wischnewski, R. and Wisniewski, L. and Wood, M. and Woernlein, A. and Xiong, Q. and Yadav, K. K. and Yamamoto, H. and Yamamoto, T. and Yamazaki, R. and Yanagita, S. and Yebras, J. M. and Yelos, D. and Yoshida, A. and Yoshida, T. and Yoshikoshi, T. and Zabalza, V. and Zacharias, M. and Zajczyk, A. and Zanin, R. and Zdziarski, A. and Zech, Alraune and Zhao, A. and Zhou, X. and Zietara, K. and Ziolkowski, J. and Ziolkowski, P. and Zitelli, V. and Zurbach, C. and Zychowski, P.},
  title     = {Introducing the CTA concept},
  series = {Astroparticle physics},
  volume    = {43},
  journal   = {Astroparticle physics},
  number    = {2},
  publisher = {Elsevier},
  address   = {Amsterdam},
  organization    = {CTA Consortium},
  issn      = {0927-6505},
  doi       = {10.1016/j.astropartphys.2013.01.007},
  pages     = {3 -- 18},
  year      = {2013},
  abstract  = {The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project.},
  language  = {en}
}
@article{DeAngelisTatischeffGrenieretal.2018,
  author    = {De Angelis, A. and Tatischeff, V. and Grenier, I. A. and McEnery, J. and Mallamaci, Manuela and Tavani, M. and Oberlack, U. and Hanlon, L. and Walter, R. and Argan, A. and Von Ballmoos, P. and Bulgarelli, A. and Bykov, A. and Hernanz, M. and Kanbach, G. and Kuvvetli, I. and Pearce, M. and Zdziarski, A. and Conrad, J. and Ghisellini, G. and Harding, A. and Isern, J. and Leising, M. and Longo, F. and Madejski, G. and Martinez, M. and Mazziotta, Mario Nicola and Paredes, J. M. and Pohl, Martin and Rando, R. and Razzano, M. and Aboudan, A. and Ackermann, M. and Addazi, A. and Ajello, M. and Albertus, C. and Alvarez, J. M. and Ambrosi, G. and Anton, S. and Antonelli, L. A. and Babic, A. and Baibussinov, B. and Balbom, M. and Baldini, L. and Balman, S. and Bambi, C. and Barres de Almeida, U. and Barrio, J. A. and Bartels, R. and Bastieri, D. and Bednarek, W. and Bernard, D. and Bernardini, E. and Bernasconi, T. and Bertucci, B. and Biland, A. and Bissaldi, E. and Boettcher, M. and Bonvicini, V. and Bosch-Ramon, V. and Bottacini, E. and Bozhilov, V. and Bretz, T. and Branchesi, M. and Brdar, V. and Bringmann, T. and Brogna, A. and Jorgensen, C. Budtz and Busetto, G. and Buson, S. and Busso, M. and Caccianiga, A. and Camera, S. and Campana, R. and Caraveo, P. and Cardillo, M. and Carlson, P. and Celestin, S. and Cermeno, M. and Chen, A. and Cheung, C. C. and Churazov, E. and Ciprini, S. and Coc, A. and Colafrancesco, S. and Coleiro, A. and Collmar, W. and Coppi, P. and Curado da Silva, R. and Cutini, S. and De Lotto, B. and de Martino, D. and De Rosa, A. and Del Santo, M. and Delgado, L. and Diehl, R. and Dietrich, S. and Dolgov, A. D. and Dominguez, A. and Prester, D. Dominis and Donnarumma, I. and Dorner, D. and Doro, M. and Dutra, M. and Elsaesser, D. and Fabrizio, M. and Fernandez-Barral, A. and Fioretti, V. and Foffano, L. and Formato, V. and Fornengo, N. and Foschini, L. and Franceschini, A. and Franckowiak, A. and Funk, S. and Fuschino, F. and Gaggero, D. and Galanti, G. and Gargano, F. and Gasparrini, D. and Gehrz, R. and Giammaria, P. and Giglietto, N. and Giommi, P. and Giordano, F. and Giroletti, M. and Ghirlanda, G. and Godinovic, N. and Gouiffes, C. and Grove, J. E. and Hamadache, C. and Hartmann, D. H. and Hayashida, M. and Hryczuk, A. and Jean, P. and Johnson, T. and Jose, J. and Kaufmann, S. and Khelifi, B. and Kiener, J. and Knodlseder, J. and Kolem, M. and Kopp, J. and Kozhuharov, V. and Labanti, C. and Lalkovski, S. and Laurent, P. and Limousin, O. and Linares, M. and Lindfors, E. and Lindner, M. and Liu, J. and Lombardi, S. and Loparco, F. and Lopez-Coto, R. and Lopez Moya, M. and Lott, B. and Lubrano, P. and Malyshev, D. and Mankuzhiyil, N. and Mannheim, K. and Marcha, M. J. and Marciano, A. and Marcote, B. and Mariotti, M. and Marisaldi, M. and McBreen, S. and Mereghetti, S. and Merle, A. and Mignani, R. and Minervini, G. and Moiseev, A. and Morselli, A. and Moura, F. and Nakazawa, K. and Nava, L. and Nieto, D. and Orienti, M. and Orio, M. and Orlando, E. and Orleanski, P. and Paiano, S. and Paoletti, R. and Papitto, A. and Pasquato, M. and Patricelli, B. and Perez-Garcia, M. A. and Persic, M. and Piano, G. and Pichel, A. and Pimenta, M. and Pittori, C. and Porter, T. and Poutanen, J. and Prandini, E. and Prantzos, N. and Produit, N. and Profumo, S. and Queiroz, F. S. and Raino, S. and Raklev, A. and Regis, M. and Reichardt, I. and Rephaeli, Y. and Rico, J. and Rodejohann, W. and Fernandez, G. Rodriguez and Roncadelli, M. and Roso, L. and Rovero, A. and Ruffini, R. and Sala, G. and Sanchez-Conde, M. A. and Santangelo, A. and Parkinson, P. Saz and Sbarrato, T. and Shearer, A. and Shellard, R. and Short, K. and Siegert, T. and Siqueira, C. and Spinelli, P. and Stamerra, A. and Starrfield, S. and Strong, A. and Strumke, I. and Tavecchio, F. and Taverna, R. and Terzic, T. and Thompson, D. J. and Tibolla, O. and Torres, D. F. and Turolla, R. and Ulyanov, A. and Ursi, A. and Vacchi, A. and Van den Abeele, J. and Vankova-Kirilovai, G. and Venter, C. and Verrecchia, F. and Vincent, P. and Wang, X. and Weniger, C. and Wu, X. and Zaharijas, G. and Zampieri, L. and Zane, S. and Zimmer, S. and Zoglauer, A.},
  title     = {Science with e-ASTROGAM A space mission for MeV-GeV gamma-ray astrophysics},
  series = {Journal of High Energy Astrophysics},
  volume    = {19},
  journal   = {Journal of High Energy Astrophysics},
  publisher = {Elsevier},
  address   = {Amsterdam},
  organization    = {e-ASTROGAM Collaboration},
  issn      = {2214-4048},
  doi       = {10.1016/j.jheap.2018.07.001},
  pages     = {1 -- 106},
  year      = {2018},
  language  = {en}
}
@inproceedings{TatischeffDeAngelisTavanietal.2018,
  author    = {Tatischeff, V. and De Angelis, A. and Tavani, M. and Grenier, I. and Oberlack, U. and Hanlon, L. and Walter, R. and Argan, A. and von Ballmoos, P. and Bulgarelli, A. and Donnarumma, I. and Hernanz, Margarita and Kuvvetli, I. and Mallamaci, M. and Pearce, M. and Zdziarski, A. and Aboudan, A. and Ajello, M. and Ambrosi, G. and Bernard, D. and Bernardini, E. and Bonvicini, V. and Brogna, A. and Branchesi, M. and Budtz-Jorgensen, C. and Bykov, A. and Campana, R. and Cardillo, M. and Ciprini, S. and Coppi, P. and Cumani, P. and da Silva, R. M. Curado and De Martino, D. and Diehl, R. and Doro, M. and Fioretti, V. and Funk, S. and Ghisellini, G. and Giordano, F. and Grove, J. E. and Hamadache, C. and Hartmann, D. H. and Hayashida, M. and Isern, J. and Kanbach, G. and Kiener, J. and Knodlseder, J. and Labanti, C. and Laurent, P. and Leising, M. and Limousin, O. and Longo, F. and Mannheim, K. and Marisaldi, M. and Martinez, M. and Mazziotta, M. N. and McEnery, J. E. and Mereghetti, S. and Minervini, G. and Moiseev, A. and Morselli, A. and Nakazawa, K. and Orleanski, P. and Paredes, J. M. and Patricelli, B. and Peyre, J. and Piano, G. and Pohl, Martin and Rando, R. and Roncadelli, M. and Tavecchio, F. and Thompson, D. J. and Turolla, R. and Ulyanov, A. and Vacchi, A. and Wu, X. and Zoglauer, A.},
  title     = {The e-ASTROGAM gamma-ray space observatory for the multimessenger astronomy of the 2030s},
  series = {Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray},
  volume    = {10699},
  booktitle = {Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray},
  editor    = {DenHerder, JWA Nikzad},
  publisher = {SPIE - The International Society for Optical Engineering},
  address   = {Bellingham},
  isbn      = {978-1-5106-1952-4},
  issn      = {0277-786X},
  doi       = {10.1117/12.2315151},
  pages     = {15},
  year      = {2018},
  abstract  = {e-ASTROGAM is a concept for a breakthrough observatory space mission carrying a gamma-ray telescope dedicated to the study of the non-thermal Universe in the photon energy range from 0.15 MeV to 3 GeV. The lower energy limit can be pushed down to energies as low as 30 keV for gamma-ray burst detection with the calorimeter. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with remarkable polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous and current generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will be a major player of the multiwavelength, multimessenger time-domain astronomy of the 2030s, and provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LISA, LIGO, Virgo, KAGRA, the Einstein Telescope and the Cosmic Explorer, IceCube-Gen2 and KM3NeT, SKA, ALMA, JWST, E-ELT, LSST, Athena, and the Cherenkov Telescope Array.},
  language  = {en}
}
@article{TosiCapaccioniCapriaetal.2019,
  author    = {Tosi, Federico and Capaccioni, F. and Capria, M. T. and Mottola, Stefano and Zinzi, A. and Ciarniello, M. and Filacchione, G. and Hofstadter, M. and Fonti, S. and Formisano, M. and Kappel, David and K{\"u}hrt, E. and Leyrat, C. and Vincent, J-B and Arnold, G. and De Sanctis, M. C. and Longobardo, Andrea and Palomba, E. and Raponi, A. and Rousseau, Batiste and Schmitt, Bernard and Barucci, Maria Antonietta and Bellucci, Giancarlo and Benkhoff, Johannes and Bockelee-Morvan, D. and Cerroni, P. and Combe, J-Ph and Despan, D. and Erard, St{\´e}phane and Mancarella, F. and McCord, T. B. and Migliorini, Alessandra and Orofino, V and Piccioni, G.},
  title     = {The changing temperature of the nucleus of comet 67P induced by morphological and seasonal effects},
  series = {Nature astronomy},
  volume    = {3},
  journal   = {Nature astronomy},
  number    = {7},
  publisher = {Nature Publ. Group},
  address   = {London},
  issn      = {2397-3366},
  doi       = {10.1038/s41550-019-0740-0},
  pages     = {649 -- 658},
  year      = {2019},
  abstract  = {Knowledge of the surface temperature distribution on a comet's nucleus and its temporal evolution at different timescales is key to constraining its thermophysical properties and understanding the physical processes that take place at and below the surface. Here we report on time-resolved maps of comet 67P/Churyumov-Gerasimenko retrieved on the basis of infrared data acquired by the Visible InfraRed and Thermal Imaging Spectrometer (VIRTIS) onboard the Rosetta orbiter in 2014, over a roughly two-month period in the pre-perihelion phase at heliocentric distances between 3.62 and 3.31 au from the Sun. We find that at a spatial resolution ≤15 m per pixel, the measured temperatures point out the major effect that self-heating, due to the complex shape of the nucleus, has on the diurnal temperature variation. The bilobate nucleus of comet 67P also induces daytime shadowing effects, which result in large thermal gradients. Over longer periods, VIRTIS-derived temperature values reveal seasonal changes driven by decreasing heliocentric distance combined with an increasing abundance of ice within the uppermost centimetre-thick layer, which implies the possibility of having a largely pristine nucleus interior already in the shallow subsurface},
  language  = {en}
}
@article{NideverOlsenWalkeretal.2017,
  author    = {Nidever, David L. and Olsen, Knut and Walker, Alistair R. and Katherina Vivas, A. and Blum, Robert D. and Kaleida, Catherine and Choi, Yumi and Conn, Blair C. and Gruendl, Robert A. and Bell, Eric F. and Besla, Gurtina and Munoz, Ricardo R. and Gallart, Carme and Martin, Nicolas F. and Olszewski, Edward W. and Saha, Abhijit and Monachesi, Antonela and Monelli, Matteo and de Boer, Thomas J. L. and Johnson, L. Clifton and Zaritsky, Dennis and Stringfellow, Guy S. and van der Marel, Roeland P. and Cioni, Maria-Rosa L. and Jin, Shoko and Majewski, Steven R. and Martinez-Delgado, David and Monteagudo, Lara and Noel, Noelia E. D. and Bernard, Edouard J. and Kunder, Andrea and Chu, You-Hua and Bell, Cameron P. M. and Santana, Felipe and Frechem, Joshua and Medina, Gustavo E. and Parkash, Vaishali and Seron Navarrete, J. C. and Hayes, Christian},
  title     = {SMASH: Survey of the MAgellanic Stellar History},
  series = {The astronomical journal},
  volume    = {154},
  journal   = {The astronomical journal},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {0004-6256},
  doi       = {10.3847/1538-3881/aa8d1c},
  pages     = {310 -- 326},
  year      = {2017},
  abstract  = {The Large and Small Magellanic Clouds are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community Dark Energy Camera (DECam) survey of the Clouds mapping 480 deg2 (distributed over similar to 2400 square degrees at similar to 20\% filling factor) to similar to 24th. mag in ugriz. The primary goals of SMASH are to identify low surface brightness stellar populations associated with the stellar halos and tidal debris of the Clouds, and to derive spatially resolved star formation histories. Here, we present a summary of the survey, its data reduction, and a description of the first public Data Release (DR1). The SMASH DECam data have been reduced with a combination of the NOAO Community Pipeline, the PHOTRED automated point-spread-function photometry pipeline, and custom calibration software. The astrometric precision is similar to 15 mas and the accuracy is similar to 2 mas with respect to the Gaia reference frame. The photometric precision is similar to 0.5\%-0.7\% in griz and similar to 1\% in u with a calibration accuracy of similar to 1.3\% in all bands. The median 5s point source depths in ugriz are 23.9, 24.8, 24.5, 24.2, and 23.5 mag. The SMASH data have already been used to discover the Hydra II Milky Way satellite, the SMASH 1 old globular cluster likely associated with the LMC, and extended stellar populations around the LMC out to R. similar to. 18.4 kpc. SMASH DR1 contains measurements of similar to 100 million objects distributed in 61 fields. A prototype version of the NOAO Data Lab provides data access and exploration tools.},
  language  = {en}
}
@article{DeAngelisTatischeffTavanietal.2017,
  author    = {De Angelis, A. and Tatischeff, V. and Tavani, M. and Oberlack, U. and Grenier, I. and Hanloni, L. and Walter, R. and Argan, A. and Von Ballmoos, P. and Bulgarelli, A. and Donnarumma, I. and Hernanz, M. and Kuvvetli, I. and Pearce, M. and Zdziarski, A. and Aboudan, A. and Ajello, M. and Ambrosi, G. and Bernard, D. and Bernardini, E. and Bonvicini, V. and Brogna, A. and Branchesi, M. and Budtz-Jorgensen, C. and Bykov, A. M. and Campana, R. and Cardillo, M. and Coppi, P. and De Martino, D. and Diehl, R. and Doro, M. and Fioretti, V. and Funk, S. and Ghisellini, G. and Grove, E. and Hamadache, C. and Hartmann, D. H. and Hayashida, M. and Isern, J. and Kanbach, G. and Kiener, J. and Knodlseder, J. and Labanti, C. and Laurent, P. and Limousin, O. and Longo, F. and Mannheim, K. and Marisaldi, M. and Martinez, M. and Mazziotta, Mario Nicola and McEnery, J. and Mereghetti, S. and Minervini, G. and Moiseev, A. and Morselli, A. and Nakazawa, K. and Orleanski, P. and Paredes, J. M. and Patricelli, B. and Pevre, J. and Piano, G. and Pohl, Martin and Ramarijaona, H. and Rando, R. and Reichardt, I. and Roncadelli, M. and Silva, R. and Tavecchio, F. and Thompson, D. J. and Turolla, R. and Ulyanov, A. and Vacchi, A. and Wu, X. and Zoglauer, A.},
  title     = {The e-ASTROGAM mission Exploring the extreme Universe with gamma rays in the MeV - GeV range},
  series = {Experimental astronomy : an international journal on astronomical instrumentation and data analysis},
  volume    = {44},
  journal   = {Experimental astronomy : an international journal on astronomical instrumentation and data analysis},
  publisher = {Springer},
  address   = {Dordrecht},
  organization    = {The e-ASTROGAM Collaboration},
  issn      = {0922-6435},
  doi       = {10.1007/s10686-017-9533-6},
  pages     = {25 -- 82},
  year      = {2017},
  abstract  = {e-ASTROGAM ('enhanced ASTROGAM') is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV - the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.},
  language  = {en}
}
@article{StarkenburgMartinYouakimetal.2017,
  author    = {Starkenburg, Else and Martin, Nicolas and Youakim, Kris and Aguado, David S. and Allende Prieto, Carlos and Arentsen, Anke and Bernard, Edouard J. and Bonifacio, Piercarlo and Caffau, Elisabetta and Carlberg, Raymond G. and Cote, Patrick and Fouesneau, Morgan and Francois, Patrick and Franke, Oliver and Gonzalez Hernandez, Jonay I. and Gwyn, Stephen D. J. and Hill, Vanessa and Ibata, Rodrigo A. and Jablonka, Pascale and Longeard, Nicolas and McConnachie, Alan W. and Navarro, Julio F. and Sanchez-Janssen, Ruben and Tolstoy, Eline and Venn, Kim A.},
  title     = {The Pristine survey - I. Mining the Galaxy for the most metal-poor stars},
  series = {Monthly notices of the Royal Astronomical Society},
  volume    = {471},
  journal   = {Monthly notices of the Royal Astronomical Society},
  publisher = {Oxford Univ. Press},
  address   = {Oxford},
  issn      = {0035-8711},
  doi       = {10.1093/mnras/stx1068},
  pages     = {2587 -- 2604},
  year      = {2017},
  abstract  = {We present the Pristine survey, a new narrow-band photometric survey focused on the metallicity-sensitive Ca H\&K lines and conducted in the Northern hemisphere with the wide-field imager MegaCam on the Canada-France-Hawaii Telescope. This paper reviews our overall survey strategy and discusses the data processing and metallicity calibration. Additionally we review the application of these data to the main aims of the survey, which are to gather a large sample of the most metal-poor stars in the Galaxy, to further characterize the faintest Milky Way satellites, and to map the (metal-poor) substructure in the Galactic halo. The current Pristine footprint comprises over 1000 deg(2) in the Galactic halo ranging from b similar to 30 degrees to similar to 78 degrees and covers many known stellar substructures. We demonstrate that, for Sloan Digital Sky Survey (SDSS) stellar objects, we can calibrate the photometry at the 0.02-mag level. The comparison with existing spectroscopic metallicities from SDSS/Sloan Extension for Galactic Understanding and Exploration (SEGUE) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope shows that, when combined with SDSS broad-band g and i photometry, we can use the CaHK photometry to infer photometric metallicities with an accuracy of similar to 0.2 dex from [Fe/H] = -0.5 down to the extremely metal-poor regime ([Fe/H] < -3.0). After the removal of various contaminants, we can efficiently select metal-poor stars and build a very complete sample with high purity. The success rate of uncovering [Fe/H](SEGUE) < -3.0 stars among [Fe/H](Pristine) < -3.0 selected stars is 24 per cent, and 85 per cent of the remaining candidates are still very metal poor ([Fe/H]<-2.0). We further demonstrate that Pristine is well suited to identify the very rare and pristine Galactic stars with [Fe/H] < -4.0, which can teach us valuable lessons about the early Universe.},
  language  = {en}
}
@article{BoydSpenceHuangetal.2016,
  author    = {Boyd, A. J. and Spence, Harlan E. and Huang, Chia-Lin and Reeves, Geoffrey D. and Baker, Daniel N. and Turner, D. L. and Claudepierre, Seth G. and Fennell, Joseph F. and Blake, J. Bernard and Shprits, Yuri Y.},
  title     = {Statistical properties of the radiation belt seed population},
  series = {Journal of geophysical research : Space physics},
  volume    = {121},
  journal   = {Journal of geophysical research : Space physics},
  publisher = {American Geophysical Union},
  address   = {Washington},
  issn      = {2169-9380},
  doi       = {10.1002/2016JA022652},
  pages     = {7636 -- 7646},
  year      = {2016},
  abstract  = {We present a statistical analysis of phase space density data from the first 26 months of the Van Allen Probes mission. In particular, we investigate the relationship between the tens and hundreds of keV seed electrons and >1 MeV core radiation belt electron population. Using a cross-correlation analysis, we find that the seed and core populations are well correlated with a coefficient of approximate to 0.73 with a time lag of 10-15 h. We present evidence of a seed population threshold that is necessary for subsequent acceleration. The depth of penetration of the seed population determines the inner boundary of the acceleration process. However, we show that an enhanced seed population alone is not enough to produce acceleration in the higher energies, implying that the seed population of hundreds of keV electrons is only one of several conditions required for MeV electron radiation belt acceleration.},
  language  = {en}
}
@article{RamiaramanantsoaMoffatHarmonetal.2018,
  author    = {Ramiaramanantsoa, Tahina and Moffat, Anthony F. J. and Harmon, Robert and Ignace, R. and St-Louis, Nicole and Vanbeveren, Dany and Shenar, Tomer and Pablo, Herbert and Richardson, Noel D. and Howarth, Ian D. and Stevens, Ian R. and Piaulet, Caroline and St-Jean, Lucas and Eversberg, Thomas and Pigulski, Andrzej and Popowicz, Adam and Kuschnig, Rainer and Zoclonska, Elzbieta and Buysschaert, Bram and Handler, Gerald and Weiss, Werner W. and Wade, Gregg A. and Rucinski, Slavek M. and Zwintz, Konstanze and Luckas, Paul and Heathcote, Bernard and Cacella, Paulo and Powles, Jonathan and Locke, Malcolm and Bohlsen, Terry and Chen{\´e}, Andr{\´e}-Nicolas and Miszalski, Brent and Waldron, Wayne L. and Kotze, Marissa M. and Kotze, Enrico J. and B{\"o}hm, Torsten},
  title     = {BRITE-Constellation high-precision time-dependent photometry of the early O-type supergiant zeta Puppis unveils the photospheric drivers of its small- and large-scale wind structures},
  series = {Monthly notices of the Royal Astronomical Society},
  volume    = {473},
  journal   = {Monthly notices of the Royal Astronomical Society},
  number    = {4},
  publisher = {Oxford Univ. Press},
  address   = {Oxford},
  issn      = {0035-8711},
  doi       = {10.1093/mnras/stx2671},
  pages     = {5532 -- 5569},
  year      = {2018},
  abstract  = {From 5.5 months of dual-band optical photometric monitoring at the 1 mmag level, BRITE-Constellation has revealed two simultaneous types of variability in the O4I(n)fp star ζ Puppis: one single periodic non-sinusoidal component superimposed on a stochastic component. The monoperiodic component is the 1.78-d signal previously detected by Coriolis/Solar Mass Ejection Imager, but this time along with a prominent first harmonic. The shape of this signal changes over time, a behaviour that is incompatible with stellar oscillations but consistent with rotational modulation arising from evolving bright surface inhomogeneities. By means of a constrained non-linear light-curve inversion algorithm, we mapped the locations of the bright surface spots and traced their evolution. Our simultaneous ground-based multisite spectroscopic monitoring of the star unveiled cyclical modulation of its He ii λ4686 wind emission line with the 1.78-d rotation period, showing signatures of corotating interaction regions that turn out to be driven by the bright photospheric spots observed by BRITE. Traces of wind clumps are also observed in the He ii λ4686 line and are correlated with the amplitudes of the stochastic component of the light variations probed by BRITE at the photosphere, suggesting that the BRITE observations additionally unveiled the photospheric drivers of wind clumps in ζ Pup and that the clumping phenomenon starts at the very base of the wind. The origins of both the bright surface inhomogeneities and the stochastic light variations remain unknown, but a subsurface convective zone might play an important role in the generation of these two types of photospheric variability.},
  language  = {en}
}
@article{NexerAuthemayouSchildgenetal.2015,
  author    = {Nexer, Maelle and Authemayou, Christine and Schildgen, Taylor F. and Hantoro, Wahyoe S. and Molliex, Stephane and Delcaillau, Bernard and Pedoja, Kevin and Husson, Laurent and Regard, Vincent},
  title     = {Evaluation of morphometric proxies for uplift on sequences of coral reef terraces: A case study from Sumba Island (Indonesia)},
  series = {Geomorphology : an international journal on pure and applied geomorphology},
  volume    = {241},
  journal   = {Geomorphology : an international journal on pure and applied geomorphology},
  publisher = {Elsevier},
  address   = {Amsterdam},
  issn      = {0169-555X},
  doi       = {10.1016/j.geomorph.2015.03.036},
  pages     = {145 -- 159},
  year      = {2015},
  abstract  = {Sequences of coral reef terraces characterized by staircase morphologies and a homogeneous lithology make them appropriate to isolate the influence of uplift on drainage morphology. Along the northern coast of Sumba Island, Indonesia, we investigated the correlations between landscape morphology and uplift rates, which range from 0.02 to 0.6 mm.yr(-1). We studied eight morphometric indices at two scales: whole island (similar to 11,000 km(2)) and within sequences of reefal terraces (similar to 3000 km(2)). At the latter scale, we extracted morphometric indices for 15 individual catchments draining mostly the reefal terraces and for 30 areas undergoing specific ranges of uplift rates draining only the reefal terraces. Indices extracted from digital elevation models include residual relief, incision, stream gradient indices (SL and k(sn)), the hypsometric integral, drainage area, mean relief, and the shape factor. We find that SL, the hypsometric integral, mean relief and the shape factor of catchments positively correlate with uplift rates, whereas incision, residual relief, and k(sn) do not. More precisely, we find that only the areas that are uplifting at a rate faster than 03 mm.yr(-1) can yield the extreme values for these indices, implying that these extreme values are indicative of fast uplifting areas. However, the relationship is not bivalent because any uplift rate can be associated with low values of the same indices. For all indices, the transient conditions of the drainage influence the correlation with Pleistocene mean uplift rates, illustrating the necessity to extract morphometric indices with an appropriate choice of catchment scale. This type of analysis helps to identify the morphometric indices that are most useful for tectonic analysis in areas of unknown uplift, allowing for easy identification of short spatial variations of uplift rate and detection of areas with relatively fast uplift rates in unstudied coastal zones. (C) 2015 Elsevier B.V. All rights reserved.},
  language  = {en}
}
@article{RichardsonRussellStJeanetal.2017,
  author    = {Richardson, Noel D. and Russell, Christopher M. P. and St-Jean, Lucas and Moffat, Anthony F. J. and St-Louis, Nicole and Shenar, Tomer and Pablo, Herbert and Hill, Grant M. and Ramiaramanantsoa, Tahina and Corcoran, Michael and Hamuguchi, Kenji and Eversberg, Thomas and Miszalski, Brent and Chene, Andre-Nicolas and Waldron, Wayne and Kotze, Enrico J. and Kotze, Marissa M. and Luckas, Paul and Cacella, Paulo and Heathcote, Bernard and Powles, Jonathan and Bohlsen, Terry and Locke, Malcolm and Handler, Gerald and Kuschnig, Rainer and Pigulski, Andrzej and Popowicz, Adam and Wade, Gregg A. and Weiss, Werner W.},
  title     = {The variability of the BRITE-est Wolf-Rayet binary, gamma(2) Velorum-I. Photometric and spectroscopic evidence for colliding winds},
  series = {Monthly notices of the Royal Astronomical Society},
  volume    = {471},
  journal   = {Monthly notices of the Royal Astronomical Society},
  publisher = {Oxford Univ. Press},
  address   = {Oxford},
  issn      = {0035-8711},
  doi       = {10.1093/mnras/stx1731},
  pages     = {2715 -- 2729},
  year      = {2017},
  abstract  = {We report on the first multi-colour precision light curve of the bright Wolf-Rayet binary gamma(2) Velorum, obtained over six months with the nanosatellites in the BRITE-Constellation fleet. In parallel, we obtained 488 high-resolution optical spectra of the system. In this first report on the data sets, we revise the spectroscopic orbit and report on the bulk properties of the colliding winds. We find a dependence of both the light curve and excess emission properties that scales with the inverse of the binary separation. When analysing the spectroscopic properties in combination with the photometry, we find that the phase dependence is caused only by excess emission in the lines, and not from a changing continuum. We also detect a narrow, high-velocity absorption component from the He perpendicular to lambda 5876 transition, which appears twice in the orbit. We calculate smoothed-particle hydrodynamical simulations of the colliding winds and can accurately associate the absorption from He perpendicular to to the leading and trailing arms of the wind shock cone passing tangentially through our line of sight. The simulations also explain the general strength and kinematics of the emission excess observed in wind lines such as C III lambda 5696 of the system. These results represent the first in a series of investigations into the winds and properties of gamma(2) Velorum through multi-technique and multi-wavelength observational campaigns.},
  language  = {en}
}
@article{PabloRichardsonMoffatetal.2015,
  author    = {Pablo, Herbert and Richardson, Noel D. and Moffat, Anthony F. J. and Corcoran, Michael and Shenar, Tomer and Benvenuto, Omar and Fuller, Jim and Naze, Yael and Hoffman, Jennifer L. and Miroshnichenko, Anatoly and Apellaniz, Jesus Maiz and Evans, Nancy and Eversberg, Thomas and Gayley, Ken and Gull, Ted and Hamaguchi, Kenji and Hamann, Wolf-Rainer and Henrichs, Huib and Hole, Tabetha and Ignace, Richard and Iping, Rosina and Lauer, Jennifer and Leutenegger, Maurice and Lomax, Jamie and Nichols, Joy and Oskinova, Lida and Owocki, Stan and Pollock, Andy and Russell, Christopher M. P. and Waldron, Wayne and Buil, Christian and Garrel, Thierry and Graham, Keith and Heathcote, Bernard and Lemoult, Thierry and Li, Dong and Mauclaire, Benjamin and Potter, Mike and Ribeiro, Jose and Matthews, Jaymie and Cameron, Chris and Guenther, David and Kuschnig, Rainer and Rowe, Jason and Rucinski, Slavek and Sasselov, Dimitar and Weiss, Werner},
  title     = {A coordinated X-Ray and optical campaign of the nearest massive eclipsing binary, delta ORIONIS Aa. III. Analysis of optical photometric (most) and spectroscopic (ground based) variations},
  series = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
  volume    = {809},
  journal   = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
  number    = {2},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {0004-637X},
  doi       = {10.1088/0004-637X/809/2/134},
  pages     = {11},
  year      = {2015},
  abstract  = {We report on both high-precision photometry from the Microvariability and Oscillations of Stars (MOST) space telescope and ground-based spectroscopy of the triple system delta Ori A, consisting of a binary O9.5II+early-B (Aa1 and Aa2) with P = 5.7 days, and a more distant tertiary (O9 IV P > 400 years). This data was collected in concert with X-ray spectroscopy from the Chandra X-ray Observatory. Thanks to continuous coverage for three weeks, the MOST light curve reveals clear eclipses between Aa1 and Aa2 for the first time in non-phased data. From the spectroscopy, we have a well-constrained radial velocity (RV) curve of Aa1. While we are unable to recover RV variations of the secondary star, we are able to constrain several fundamental parameters of this system and determine an approximate mass of the primary using apsidal motion. We also detected second order modulations at 12 separate frequencies with spacings indicative of tidally influenced oscillations. These spacings have never been seen in a massive binary, making this system one of only a handful of such binaries that show evidence for tidally induced pulsations.},
  language  = {en}
}