8,242 results on '"Rodriguez, L."'
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202. Design, Simulation and Fabrication of Highly Sensitive Cooled Silicon Bolometers for Millimeter-Wave Detection
- Author
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Aliane, A., Adami, O-A., Dussopt, L., Rodriguez, L., Rabaud, W., Ouvrier-Buffet, J-L., Goudon, V., Kaya, H., Vialle, C., Sauvageot, J-L., Reveret, V., Becker, S., and Poglitsch, A.
- Published
- 2020
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203. Rare predicted loss-of-function variants of type I IFN immunity genes are associated with life-threatening COVID-19
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Matuozzo, D, Talouarn, E, Marchal, A, Zhang, P, Manry, J, Seeleuthner, Y, Zhang, Y, Bolze, A, Chaldebas, M, Milisavljevic, B, Gervais, A, Bastard, P, Asano, T, Bizien, L, Barzaghi, F, Abolhassani, H, Abou Tayoun, A, Aiuti, A, Alavi Darazam, I, Allende, L, Alonso-Arias, R, Arias, A, Aytekin, G, Bergman, P, Bondesan, S, Bryceson, Y, Bustos, I, Cabrera-Marante, O, Carcel, S, Carrera, P, Casari, G, Chaibi, K, Colobran, R, Condino-Neto, A, Covill, L, Delmonte, O, El Zein, L, Flores, C, Gregersen, P, Gut, M, Haerynck, F, Halwani, R, Hancerli, S, Hammarstrom, L, Hatipoglu, N, Karbuz, A, Keles, S, Kyheng, C, Leon-Lopez, R, Franco, J, Mansouri, D, Martinez-Picado, J, Metin Akcan, O, Migeotte, I, Morange, P, Morelle, G, Martin-Nalda, A, Novelli, G, Novelli, A, Palabiyik, F, Pan-Hammarstrom, Q, de Diego, R, Planas-Serra, L, Pleguezuelo, D, Prando, C, Pujol, A, Reyes, L, Riviere, J, Rodriguez-Gallego, C, Rojas, J, Rovere-Querini, P, Schluter, A, Shahrooei, M, Sobh, A, Soler-Palacin, P, Tandjaoui-Lambiotte, Y, Tipu, I, Tresoldi, C, Troya, J, van de Beek, D, Zatz, M, Zawadzki, P, Al-Muhsen, S, Alosaimi, M, Alsohime, F, Baris-Feldman, H, Butte, M, Constantinescu, S, Cooper, M, Dalgard, C, Fellay, J, Heath, J, Lau, Y, Lifton, R, Maniatis, T, Mogensen, T, von Bernuth, H, Lermine, A, Vidaud, M, Boland, A, Deleuze, J, Nussbaum, R, Kahn-Kirby, A, Mentre, F, Tubiana, S, Gorochov, G, Tubach, F, Hausfater, P, Al-Mulla, F, Anderson, M, Andreakos, E, Feldman, H, Belot, A, Biggs, C, Bogunovic, D, Bondarenko, A, Bousfiha, A, Brodin, P, Bustamante, C, Chakravorty, S, Christodoulou, J, Desai, M, Drolet, B, Baghdadi, J, Espinosa-Padilla, S, Froidure, A, Hagin, D, Henrickson, S, Hsieh, E, Husebye, E, Imai, K, Itan, Y, Jarvis, E, Karamitros, T, Kisand, K, Ku, C, Ling, Y, Lucas, C, Marodi, L, Milner, J, Mironska, K, Morio, T, Ng, L, O'Farrelly, C, Okada, S, Planas, A, Quintana-Murci, L, Renia, L, Resnick, I, Sancho-Shimizu, V, Sediva, A, Seppanen, M, Shcherbina, A, Slaby, O, Snow, A, Spaan, A, Tancevski, I, Tangye, S, Ramaswamy, S, Turvey, S, Uddin, F, Uddin, M, Vinh, D, Casanova, J, Vacher, Y, Gysembergh-Houal, A, Demerville, L, Chachoua, A, Abad, S, Abassi, R, Abdellaoui, A, Abdelmalek, A, Abdoul, H, Abergel, H, Abeud, F, Abgrall, S, Abisror, N, Adechian, M, Aderdour, N, Admane, H, Adnet, F, Afritt, S, Agostini, H, Aguilar, C, Agut, S, Aiello, T, Kaci, M, Oufella, H, Ajeenthiravasan, G, Alauzy, V, Alby-Laurent, F, Allard, L, Alyanakian, M, Borrero, B, Amam, S, Amrouche, L, Andronikof, M, Anglicheau, D, Anguel, N, Annane, D, Aounzou, M, Aparicio, C, Aratus, G, Arlet, J, Arzoine, J, Aslangul, E, Assefi, M, Aubry, A, Audiffred, L, Audureau, E, Auger, C, Auregan, J, Awotar, C, Milla, S, Azan, D, Azemar, L, Azzouguen, B, Elrufaai, M, Badsi, A, Bakouboula, P, Balcerowiak, C, Balde, F, Baldivia, E, Bangamingo, E, Baptiste, A, Baran-Marszak, F, Barau, C, Barget, N, Baronnet, F, Barthelemy, R, Baudel, J, Baudry, C, Baudry, E, Beaugerie, L, Belamri, A, Belaube, N, Belilita, R, Bellassen, P, Belmokhtar, R, Beltran, I, Benainous, R, Benallaoua, M, Benamouzig, R, Benbara, A, Benhida, J, Benkhelouf, A, Benlagha, J, Benmostafa, C, Benothmane, S, Bentifraouine, M, Berard, L, Bernier, Q, Berti, E, Bertier, A, Berton, L, Bessis, S, Beurton, A, Bianco, C, Bianquis, C, Bidar, F, Blanche, P, Blayau, C, Bleibtreu, A, Blin, E, Bloch-Queyrat, C, Boissier, M, Bollens, D, Bolzoni, M, Bompard, R, Bonnet, N, Bonnouvrier, J, Botha, S, Boucenna, W, Bouchama, F, Bouchaud, O, Bouchghoul, H, Boudjebla, T, Boudjema, N, Bouffard, C, Bougle, A, Bouguerra, M, Bouras, L, Bourcier, A, Durand, A, Bourrier, A, Bouscarat, F, Bouvry, D, Bouziri, N, Bouzrara, O, Bribier, S, Brugier, D, Brunel, M, Bui, E, Buisson, A, Bukreyeva, I, Bureau, C, Cadranel, J, Cailhol, J, Calin, R, Vega, C, Canavaggio, P, Cancella, M, Cantin, D, Cao, A, Carbillon, L, Carlier, N, Cassard, C, Castor, G, Cauchy, M, Cha, O, Chaigne, B, Challal, S, Champion, K, Chariot, P, Chas, J, Chauveau, S, Chauvin, A, Chauvin, C, Chavarot, N, Chebbout, K, Cherai, M, Cherubini, I, Chevalier, A, Chiarabini, T, Chinet, T, Chocron, R, Choinier, P, Chommeloux, J, Choquet, C, Choupeaux, L, Chousterman, B, Ciocan, D, Clarke, A, Clavere, G, Clavier, F, Clement, K, Clerc, S, Cohen, Y, Cohen, F, Cohen, A, Coilly, A, Colboc, H, Colin, P, Collet, M, Comarmond, C, Combacon, E, Combes, A, Comparon, C, Constantin, J, Cordel, H, Cordier, A, Costantini, A, Chalumeau, N, Couffignal, C, Coupeau, D, Creange, A, Lamarre, Y, Da Silveira, C, Kayani, S, De Castro, N, De Rycke, Y, Del Pozo, L, Delannoy, Q, Delay, M, Deleris, R, Delforge, J, Delphine, L, Demare, N, Demeret, S, Demoule, A, Deniau, A, Depret, F, Derolez, S, Derradji, O, Derridj, N, Descamps, V, Deschamps, L, Desconclois, C, Desnos, C, Desongins, K, Dhote, R, Diallo, B, Didier, M, Diemer, M, Diez, S, Djadi-Prat, J, Monnory, F, Djebara, S, Djebra, N, Djietcheu, M, Djillali, H, Djouadi, N, Donneger, S, Dos Santos, C, Dournon, N, Dres, M, Droctove, L, Drogrey, M, Dropy, M, Drouet, E, Dubosq, V, Dubreucq, E, Dubus, E, Duchemann, B, Duchenoy, T, Dudoignon, E, Dufau, R, Dumas, F, Duran, C, Duron, E, Durrbach, A, Duvivier, C, Ebstein, N, Khalifa, J, Elabbadi, A, Elie, C, Ernotte, G, Esling, A, Etienne, M, Eyer, X, Fartoukh, M, Fayali, T, Fermaut, M, Fiorentino, A, Fliss, S, Fournier, M, Fournier, B, Francois, H, Freynet, O, Frigout, Y, Fromont, I, Fuentes, A, Furet, T, Galand, J, Garnier, M, Gaubert, A, Gaudry, S, Gaugain, S, Gauthier, D, Gautier, M, Georgin-Lavialle, S, Geromin, D, Ghalayini, M, Ghaleh, B, Ghezal, M, Gibelin, A, Gimeno, L, Girard, B, Leprieur, B, Gomes, D, Gomes-Pires, E, Gouge, A, Gouja, A, Goulet, H, Goupil, S, De Bouille, J, Gras, J, Greffe, S, Grimaldi, L, Guedeney, P, Guidet, B, Guillo, M, Gulczynski, M, Hadjam, T, Haguenauer, D, Hammal, S, Hammoudi, N, Hanon, O, Harrois, A, Hautem, C, Hekimian, G, Heming, N, Hermine, O, Ho, S, Houllier, M, Huot, B, Huscenot, T, Saied, W, Ikherbane, G, Imarazene, M, Ingiliz, P, Iratni, L, Jaureguiberry, S, Jean-Marc, J, Jeyarajasingham, D, Jouany, P, Jouis, V, Jourdaine, C, Kafif, O, Kallala, R, Katsahian, S, Kelesyan, L, Keo, V, Ketz, F, Khamis, W, Khelili, E, Khellaf, M, Youkou, C, Kounis, I, Kpalma, G, Krause, J, Labbe, V, Lacombe, K, Lacorte, J, Lafont, A, Lafont, E, Lagha, L, Lamhaut, L, Lancelot, A, Landman, C, Lanternier, F, Larcheveque, C, Combe, C, Lassel, L, Laverdant, B, Lavergne, C, Lavillegrand, J, Lazureanu, P, Le Guennec, L, Leberre, L, Leblanc, C, Leboyer, M, Lecomte, F, Lecorre, M, Leenhardt, R, Lefebvre, M, Lefebvre, B, Legendre, P, Leger, A, Legros, L, Legrosse, J, Lehuunghia, S, Lemarec, J, Leporrier-Ext, J, Lesein, M, Lesur, H, Levy, V, Levy, A, Lopes, E, Lopes, A, Lopez, V, Lopinto, J, Lortholary, O, Louadah, B, Loze, B, Lucas, M, Lucasamichi, A, Luong, L, Magazimama-Ext, A, Maingret, D, Mameri, L, Manivet, P, Mansouri, C, Marcault, E, Marey, J, Marin, N, Marois, C, Martin, O, Martineau, L, Martinez-Lopez, C, Martyniuck, P, De Farcy, P, Marzouk, N, Masmoudi, R, Mebazaa, A, Mechai, F, Mecozzi, F, Mediouni, C, Megarbane, B, Meghadecha, M, Mejean, E, Mekinian, A, Abdelhadi, N, Mekni, R, Meliti, T, Lima, B, Meng, P, Merbah, S, Messani, F, Messaoudi, Y, Mewasing, B, Meziane, L, Michelot-Burger, C, Mignot, F, Minka, F, Miyara, M, Moine, P, Molina, J, Montegnies-Boulet, A, Monti, A, Montlahuc, C, Montout, A, Moores, A, Morbieu, C, Mortelette, H, Mouly, S, Muzaffar, R, Nacerddine, C, Nadal, M, Nadif, H, Nassarmadji, K, Natella, P, Ndingamondze, S, Neraal, S, Nguyen, C, N'Guyen, B, Larmurier, I, Nlomenyengue, L, Noel, N, Nunes, H, Omar, E, Ouazene, Z, Ouedraogo, E, Ouelaa, W, Oukhedouma, A, Amara, Y, Oya, H, Oziel, J, Padilla, T, Paillaud, E, Paiva, S, Parfait, B, Parize, P, Parizot, C, Parrot, A, Pavot, A, Peaudecerf, L, Pene, F, Pepin, M, Pernet, J, Pernin, C, Petit, M, Peyrony, O, Pietri, M, Pietri, O, De Chambrun, M, Pinson, M, Pintado, C, Pires, C, Planquette, B, Poirier, S, Pomel, A, Pons, S, Ponscarme, D, Pourcelot, A, Pourcher, V, Pouvaret, A, Prever, F, Previlon, M, Prevost, M, Provoost, M, Quemeneur, C, Rafat, C, Rami, A, Ranque, B, Raphael, M, Raphalen, J, Rastoin, A, Raux, M, Rebai, A, Reby, M, Regent, A, Regrag, A, Resche-Rigon, M, Ressaire, Q, Richard, C, Richard, M, Robert, M, Rohaut, B, Rolland-Debord, C, Ropers, J, Roque-Afonso, A, Rosso, C, Rousseaux, M, Rousseaux, N, Roux, S, Roux, L, Rouzaud, C, Rozes, A, Rubenstein, E, Sabate, J, Sabet, S, Sacleux, S, Kermanach, N, Saliba, F, Salmon, D, Savale, L, Savary, G, Sberro, R, Scemla, A, Schlemmer, F, Schwartz, M, Sedfi, S, Sefir-Kribel, S, Seksik, P, Sellier, P, Selves, A, Sembach, N, Semerano, L, Senat, M, Sene, D, Serris, A, Sese, L, Sghiouar, N, Sigaux, J, Siguier, M, Silvain, J, Simon, N, Simon, T, Skandri, L, Slimani, M, Snauwaert, A, Sokol, H, Soliman, H, Soltani, N, Soyer, B, Steg, G, Suarez, L, Szwebel, T, Taffame, K, Tantet, C, Tateo, M, Theodose, I, Thiebaud, P, Thomas, C, Tiercelet, K, Tisserand, J, Tomczak, C, Torelino, K, Touam-Ext, F, Toumi, L, Toury, G, Toy-Miou, M, Lien, O, Trandinh, A, Treluyer, J, Trinque, B, Truchot, J, Tunesi, S, Turpin, M, Turpin, A, Urbina, T, Narvaez, R, Uzunhan, Y, Vaittinadaayar, P, Valent, A, Valentian, M, Valin, N, Vallet, H, Vaz, M, Vazquezibarra, M, Vedie, B, Velly, L, Verstuyft, C, Viallette, C, Vicaut, E, Vignes, D, Vimpere, D, Virlouvet, M, Voiriot, G, Voisot, L, Weiss, E, Weiss, N, Winchenne, A, Yordanov, Y, Zafrani, L, Zaidan, M, Zaidi, W, Zak, C, Zarhrate-Ghoul, A, Zatout, O, Zeino, S, Zeitouni, M, Zemirli, N, Zerah, L, Zia, O, Ziol, M, Zolario, O, Zuber, J, Andrejak, C, Angoulvant, F, Bachelet, D, Bartoli, M, Basmaci, R, Behilill, S, Beluze, M, Benkerrou, D, Bhavsar, K, Bouadma, L, Bouchez, S, Bouscambert, M, Cervantes-Gonzalez, M, Chair, A, Coelho, A, D'Ortenzio, E, Debray, M, Deconinck, L, Deplanque, D, Descamps, D, Desvallee, M, Diallo, A, Diouf, A, Dorival, C, Dubos, F, Duval, X, Elharrar, B, Eloy, P, Enouf, V, Esperou, H, Esposito-Farese, M, Devouge, E, Gault, N, Gaymard, A, Ghosn, J, Gigante, T, Gilg, M, Guedj, J, Hoctin, A, Hoffmann, I, Houas, I, Hulot, J, Jaafoura, S, Kaguelidou, F, Kali, S, Khalil, A, Khan, C, Laouenan, C, Laribi, S, Le, M, Le Hingrat, Q, Le Mestre, S, Le Nagard, H, Lescure, F, Levy, Y, Lingas, G, Lucet, J, Malvy, D, Mambert, M, Meziane, A, Mouquet, H, Mullaert, J, Neant, N, Nguyen, D, Noret, M, Nseir, S, Papadopoulos, A, Paul, C, Peiffer-Smadja, N, Perpoint, T, Petrov-Sanchez, V, Peytavin, G, Pham, H, Picone, O, Puechal, O, Rabaud, C, Rosa-Calatrava, M, Rossignol, B, Rossignol, P, Roy, C, Schneider, M, Su, R, Tardivon, C, Tellier, M, Teoule, F, Terrier, O, Timsit, J, Tual, C, Van Der Werf, S, Vanel, N, Veislinger, A, Visseaux, B, Wiedemann, A, Yazdanpanah, Y, Alavoine, L, Behillil, S, Burdet, C, Charpentier, C, Dechanet, A, Ecobichon, J, Frezouls, W, Houhou, N, Lehacaut, J, Letrou, S, Lina, B, Manchon, P, Nouroudine, M, Piquard, V, Quintin, C, Thy, M, Vignali, V, Chahine, A, Waucquier, N, Migaud, M, Djossou, F, Mergeay-Fabre, M, Lucarelli, A, Demar, M, Bruneau, L, Gerardin, P, Maillot, A, Payet, C, Laviolle, B, Laine, F, Paris, C, Desille-Dugast, M, Fouchard, J, Pistone, T, Perreau, P, Gissot, V, Goas, C, Montagne, S, Richard, L, Chirouze, C, Bouiller, K, Desmarets, M, Meunier, A, Bourgeon, M, Lefevre, B, Jeulin, H, Legrand, K, Lomazzi, S, Tardy, B, Gagneux-Brunon, A, Bertholon, F, Botelho-Nevers, E, Christelle, K, Nicolas, L, Roufai, L, Amat, K, Couffin-Cadiergues, S, Hendou, S, Foti, G, Bellani, G, Citerio, G, Contro, E, Pesci, A, Valsecchi, M, Cazzaniga, M, Abad, J, Accordino, G, Achille, C, Aguilera-Albesa, S, Aguilo-Cucurull, A, Ozkan, E, Albisures, J, Aldave, J, Ramos, M, Khan, T, Aliberti, A, Nadji, S, Alkan, G, Alkhater, S, Allardet-Servent, J, Alshahrani, M, Alsina, L, Amoura, Z, Antoli, A, Arrestier, R, Aubart, M, Auguet, T, Avramenko, I, Azot, A, Bahram, S, Bajolle, F, Baldanti, F, Baldolli, A, Ballester, M, Barrou, B, Basso, S, Bayhan, G, Bezrodnik, L, Bilbao, A, Blanchard-Rohner, G, Blanco, I, Blandinieres, A, Blazquez-Gamero, D, Bloomfield, M, Bolivar-Prados, M, Borghesi, A, Borie, R, Botdhlo-Nevers, E, Bousquet, A, Boutolleau, D, Bouvattier, C, Boyarchuk, O, Bravais, J, Briones, M, Brunner, M, Bruno, R, Bueno, M, Bukhari, H, Bustamante, J, Agra, J, Capra, R, Carapito, R, Carrabba, M, Casasnovas, C, Caseris, M, Cassaniti, I, Castelle, M, Castelli, F, de Vera, M, Castro, M, Catherinot, E, Celik, J, Ceschi, A, Chalumeau, M, Charbit, B, Cheng, M, Clave, P, Clotet, B, Codina, A, Comoli, P, Corsico, A, Sozeri, B, Coskuner, T, Cvetkovski, A, Cyrus, C, Dalmau, D, Danion, F, Darley, D, Das, V, Dauby, N, Dauger, S, De Munter, P, de Pontual, L, Dehban, A, Delplancq, G, Desguerre, I, Di Sabatino, A, Diehl, J, Dobbelaere, S, Dominguez-Garrido, E, Dubost, C, Ekwall, O, Bozdemir, S, Elnagdy, M, Emiroglu, M, Endo, A, Erdeniz, E, Aytekin, S, Lasa, M, Euvrard, R, Fabio, G, Faivre, L, Falck, A, Faure, M, Arquero, M, Ferrer, R, Ferreres, J, Francois, B, Fumado, V, Fung, K, Fusco, F, Gagro, A, Solis, B, Garcon, P, Gaussem, P, Gayretli, Z, Gil-Herrera, J, Gilardin, L, Gatineau, A, Girona-Alarcon, M, Godinez, K, Goffard, J, Gonzales, N, Gonzalez-Granado, L, Gonzalez-Montelongo, R, Guerder, A, Gulhan, B, Gumucio, V, Hanitsch, L, Gunst, J, Hadjadj, J, Hariyan, T, Heppekcan, D, Hernandez-Brito, E, Ho, P, Holanda-Pena, M, Horcajada, J, Hraiech, S, Humbert, L, Hung, I, Iglesias, A, Inigo-Campos, A, Jamme, M, Arranz, M, Jimeno, M, Jordan, I, Yuksek, S, Kara, Y, Karahan, A, Yasar, K, Kasapcopur, O, Kashimada, K, Demirkol, Y, Kido, Y, Kizil, C, Kilic, A, Klocperk, A, Koutsoukou, A, Krol, Z, Ksouri, H, Kuentz, P, Kwan, A, Kwan, Y, Kwok, J, Lagier, J, Lam, D, Lampropoulou, V, Le Bourgeois, F, Leo, Y, Leung, D, Levin, M, Levy, M, Levy, R, Li, Z, Lilleri, D, Lima, E, Linglart, A, Lopez-Collazo, E, Lorenzo-Salazar, J, Louapre, C, Lubetzki, C, Lung, K, Luyt, C, Lye, D, Magnone, C, Marchioni, E, Marioli, C, Marjani, M, Marques, L, Pereira, J, Pueyo, D, Marzana, I, Mata-Martinez, C, Mathian, 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U., Uzunhan Y., Vaittinadaayar P., Valent A., Valentian M., Valin N., Vallet H., Vaz M., Vazquezibarra M. -A., Vedie B., Velly L., Verstuyft C., Viallette C., Vicaut E., Vignes D., Vimpere D., Virlouvet M., Voiriot G., Voisot L., Weiss E., Weiss N., Winchenne A., Yordanov Y., Zafrani L., Zaidan M., Zaidi W., Zak C., Zarhrate-Ghoul A., Zatout O., Zeino S., Zeitouni M., Zemirli N., Zerah L., Zia O., Ziol M., Zolario O., Zuber J., Andrejak C., Angoulvant F., Bachelet D., Bartoli M., Basmaci R., Behilill S., Beluze M., Benkerrou D., Bhavsar K., Bouadma L., Bouchez S., Bouscambert M., Cervantes-Gonzalez M., Chair A., Coelho A., d'Ortenzio E., Debray M. -P., Deconinck L., Deplanque D., Descamps D., Desvallee M., Diallo A., Diouf A., Dorival C., Dubos F., Duval X., Elharrar B., Eloy P., Enouf V., Esperou H., Esposito-Farese M., Devouge E. F., Gault N., Gaymard A., Ghosn J., Gigante T., Gilg M., Guedj J., Hoctin A., Hoffmann I., Houas I., Hulot J. -S., Jaafoura S., Kaguelidou F., Kali S., Khalil A., Khan C., Laouenan C., Laribi S., Le M., Le Hingrat Q., Le Mestre S., Le Nagard H., Lescure F. -X., Levy Y., Lingas G., Lucet J. C., Malvy D., Mambert M., Meziane A., Mouquet H., Mullaert J., Neant N., Nguyen D., Noret M., Nseir S., Papadopoulos A., Paul C., Peiffer-Smadja N., Perpoint T., Petrov-Sanchez V., Peytavin G., Pham H., Picone O., Puechal O., Rabaud C., Rosa-Calatrava M., Rossignol B., Rossignol P., Roy C., Schneider M., Su R., Tardivon C., Tellier M. -C., Teoule F., Terrier O., Timsit J. -F., Tual C., Van Der Werf S., Vanel N., Veislinger A., Visseaux B., Wiedemann A., Yazdanpanah Y., Alavoine L., Behillil S., Burdet C., Charpentier C., Dechanet A., Ecobichon J. -L., Frezouls W., Houhou N., Lehacaut J., Letrou S., Lina B., Manchon P., Nouroudine M., Piquard V., Quintin C., Thy M., Vignali V., Chahine A., Waucquier N., Migaud M. -C., Djossou F., Mergeay-Fabre M., Lucarelli A., Demar M., Bruneau L., Gerardin P., Maillot A., Payet C., Laviolle B., Laine F., Paris C., Desille-Dugast M., Fouchard J., Pistone T., Perreau P., Gissot V., Goas C. L. E., Montagne S., Richard L., Chirouze C., Bouiller K., Desmarets M., Meunier A., Bourgeon M., Lefevre B., Jeulin H., Legrand K., Lomazzi S., Tardy B., Gagneux-Brunon A., Bertholon F., Botelho-Nevers E., Christelle K., Nicolas L., Roufai L., Amat K., Couffin-Cadiergues S., Hendou S., Foti G., Bellani G., Citerio G., Contro E., Pesci A., Valsecchi M. G., Cazzaniga M., Abad J., Accordino G., Achille C., Aguilera-Albesa S., Aguilo-Cucurull A., Ozkan E. A., Albisures J. A. R., Aldave J. C., Ramos M. A., Khan T. A., Aliberti A., Nadji S. A., Alkan G., AlKhater S. A., Allardet-Servent J., Alshahrani M. S., Alsina L., Amoura Z., Antoli A., Arrestier R., Aubart M., Auguet T., Avramenko I., Azot A., Bahram S., Bajolle F., Baldanti F., Baldolli A., Ballester M., Barrou B., Basso S., Bayhan G. I., Bezrodnik L., Bilbao A., Blanchard-Rohner G., Blanco I., Blandinieres A., Blazquez-Gamero D., Bloomfield M., Bolivar-Prados M., Borghesi A., Borie R., Botdhlo-Nevers E., Bousquet A., Boutolleau D., Bouvattier C., Boyarchuk O., Bravais J., Briones M. L., Brunner M. -E., Bruno R., Bueno M. R. P., Bukhari H., Bustamante J., Agra J. J. C., Capra R., Carapito R., Carrabba M., Casasnovas C., Caseris M., Cassaniti I., Castelle M., Castelli F., de Vera M. C., Castro M. V., Catherinot E., Celik J. B., Ceschi A., Chalumeau M., Charbit B., Cheng M. P., Clave P., Clotet B., Codina A., Comoli P., Corsico A. G., Sozeri B., Coskuner T., Cvetkovski A., Cyrus C., Dalmau D., Danion F., Darley D. R., Das V., Dauby N., Dauger S., De Munter P., de Pontual L., Dehban A., Delplancq G., Desguerre I., Di Sabatino A., Diehl J. -L., Dobbelaere S., Dominguez-Garrido E., Dubost C., Ekwall O., Bozdemir S. E., Elnagdy M. H., Emiroglu M., Endo A., Erdeniz E. H., Aytekin S. E., Lasa M. P. E., Euvrard R., Fabio G., Faivre L., Falck A., Faure M., Arquero M. F., Ferrer R., Ferreres J., Francois B., Fumado V., Fung K. S. C., Fusco F., Gagro A., Solis B. G., Garcon P., Gaussem P., Gayretli Z., Gil-Herrera J., Gilardin L., Gatineau A. G., Girona-Alarcon M., Godinez K. A. C., Goffard J. -C., Gonzales N., Gonzalez-Granado L. I., Gonzalez-Montelongo R., Guerder A., Gulhan B., Gumucio V. D., Hanitsch L. G., Gunst J., Hadjadj J., Hariyan T., Heppekcan D., Hernandez-Brito E., Ho P. -K., Holanda-Pena M. S., Horcajada J. P., Hraiech S., Humbert L., Hung I. F. N., Iglesias A. D., Inigo-Campos A., Jamme M., Arranz M. J., Jimeno M. -T., Jordan I., Yuksek S. K., Kara Y. B., Karahan A., Yasar K. K., Kasapcopur O., Kashimada K., Demirkol Y. K., Kido Y., Kizil C., Kilic A. O., Klocperk A., Koutsoukou A., Krol Z. J., Ksouri H., Kuentz P., Kwan A. M. C., Kwan Y. W. M., Kwok J. S. Y., Lagier J. -C., Lam D. S. Y., Lampropoulou V., Le Bourgeois F., Leo Y. -S., Leung D., Levin M., Levy M., Levy R., Li Z., Lilleri D., Lima E. J. A. B., Linglart A., Lopez-Collazo E., Lorenzo-Salazar J. M., Louapre C., Lubetzki C., Lung K. -C., Luyt C. -E., Lye D. C., Magnone C., Marchioni E., Marioli C., Marjani M., Marques L., Pereira J. M., Pueyo D. M., Marzana I., Mata-Martinez C., Mathian A., Matos L. R. B., Matthews G. V., Mayaux J., McLaughlin-Garcia R., Meersseman P., Mege J. -L., Mekontso-Dessap A., Melki I., Meloni F., Meritet J. -F., Merlani P., Akcan O. M., Mezidi M., Millereux M., Million M., Mirault T., Mircher C., Mirsaeidi M., Mizoguchi Y., Modi B. P., Mojoli F., Moncomble E., Melian A. M., Martinez A. M., Morandeira F., Mordacq C., Mouly S. J., Munoz-Barrera A., Nafati C., Nagashima S., Nakagama Y., Neven B., Neves J. F., Ng Y. -Y., Nielly H., Medina Y. N., Cuadros E. N., Ocejo-Vinyals J. G., Okamoto K., Oualha M., Ouedrani A., Ozcelik T., Ozkaya-Parlakay A., Pagani M., Papadaki M., Parola P., Pascreau T., Paul S., Paz-Artal E., Pedraza S., Pellecer N. C. G., Pellegrini S., Perez-Fernandez X. L., Philippe A., Philippot Q., Picod A., Piralla A., Ploin D., Poissy J., Poncelet G., Poulakou G., Pouletty M. S., Pourshahnazari P., Qiu-Chen J. L., Quentric P., Rambaud T., Raoult D., Raoult V., Rebillat A. -S., Redin C., Resmini L., Ricart P., Richard J. -C., Rigo-Bonnin R., rivet N., Rocamora-Blanch G., Rodero M. P., Rodrigo C., Rodriguez L. A., Rodriguez-Palmero A., Romero C. S., Rothenbuhler A., Roux D., Rovina N., Rozenberg F., Ruch Y., Ruiz M., del Prado M. Y. R., Ruiz-Rodriguez J. C., Sabater-Riera J., Saks K., Salagianni M., Sanchez O., Sanchez-Montalva A., Sanchez-Ramon S., Schidlowski L., Schmidt J., Schmidt M., Schuetz C., Schweitzer C. E., Scolari F., Seijo L., Seminario A. G., Seng P., Senoglu S., Seppanen M., Llovich A. S., Siguret V., Siouti E., Smadja D. M., Smith N., Solanich X., Sole-Violan J., Soler C., Stella G. M., Stepanovskiy Y., Stoclin A., Taccone F., Taupin J. -L., Tavernier S. J., Tello L. V., Terrier B., Thiery G., Thorball C., Thorn K., Thumerelle C., Tolstrup M., Tomasoni G., Toubiana J., Alvarez J. T., Triantafyllia V., Trouillet-Assant S., Tsang O. T. Y., Tserel L., Tso E. Y. K., Tucci A., Oz S. K. T., Ursini M. V., Utsumi T., Vabres P., Valencia-Ramos J., Van Den Rym A. M., Vandernoot I., Velez-Santamaria V., Veliz S. P. Z., Vidigal M. C., Viel S., Villain C., Vilaire-Meunier M. E., Villar-Garcia J., Vincent A., Volokha A., Vuotto F., Wauters E., Wauters J., Wu A. K. L., Wu T. -C., Yahsi A., Yesilbas O., Yildiz M., Young B. E., Yukselmis U., Zecca M., Zuccaro V., Van Praet J., Lambrecht B. N., Van Braeckel E., Bosteels C., Hoste L., Hoste E., Bauters F., De Clercq J., Heijmans C., Slabbynck H., Naesens L., Florkin B., Boulanger C., Vanderlinden D., Berkell M., Carelli V., Malhotra S., Mattiaccio A., Pippucci T., Seri M., Tacconelli E., van Agtmael M., Algera A. G., Appelman B., van Baarle F., Bax D., Beudel M., Bogaard H. J., Bomers M., Bonta P., Bos L., Botta M., de Brabander J., de Bree G., de Bruin S., Buis D. T. P., Bugiani M., Bulle E., Cloherty O. C. A., Dijkstra M., Dongelmans D. A., Dujardin R. W. G., Elbers P., Fleuren L., Geijtenbeek S. G. T., Girbes A., Goorhuis B., Grobusch M. P., Hafkamp F., Hagens L., Hamann J., Harris V., Hemke R., Heunks S. M. H. L., Hollmann M., Horn J., Hovius J. W., de Jong M. D., Koning R., Lim E. H. T., van Mourik N., Nellen J., Nossent E. J., Paulus F., Peters E., Pina-Fuentes D. A. I., van der Poll T., Preckel B., Prins J. M., Raasveld J., Reijnders T., de Rotte M. C. F. J., Schinkel M., Schultz M. J., Schrauwen F. A. P., Schuurmans A., Schuurmans J., Sigaloff K., Slim M. A., Smeele P., Smit M., Stijnis C. S., Stilma W., Teunissen C., Thoral P., Tsonas A. M., Tuinman P. R., van der Valk M., Veelo D., Volleman C., de Vries H., Vught L. A., van Vugt M., Wouters D., Zwinderman A. H., Brouwer M. C., Wiersinga W. J., Vlaar A. P. J., Tompkins M. F., Alba C., Hupalo D. N., Rosenberger J., Sukumar G., Wilkerson M. D., Zhang X., Lack J., Oler A. J., Dobbs K., Danielson J. J., Biondi A., Bettini L. R., D'Angio' M., Beretta I., Imberti L., Sottini A., Quaresima V., Quiros-Roldan E., Rossi C., Meyts I., Zhang S. -Y., Puel A., Notarangelo L. D., Boisson-Dupuis S., Su H. C., Boisson B., Jouanguy E., Zhang Q., Abel L., and Cobat A.
- Abstract
Background: We previously reported that impaired type I IFN activity, due to inborn errors of TLR3- and TLR7-dependent type I interferon (IFN) immunity or to autoantibodies against type I IFN, account for 15–20% of cases of life-threatening COVID-19 in unvaccinated patients. Therefore, the determinants of life-threatening COVID-19 remain to be identified in ~ 80% of cases. Methods: We report here a genome-wide rare variant burden association analysis in 3269 unvaccinated patients with life-threatening COVID-19, and 1373 unvaccinated SARS-CoV-2-infected individuals without pneumonia. Among the 928 patients tested for autoantibodies against type I IFN, a quarter (234) were positive and were excluded. Results: No gene reached genome-wide significance. Under a recessive model, the most significant gene with at-risk variants was TLR7, with an OR of 27.68 (95%CI 1.5–528.7, P = 1.1 × 10−4) for biochemically loss-of-function (bLOF) variants. We replicated the enrichment in rare predicted LOF (pLOF) variants at 13 influenza susceptibility loci involved in TLR3-dependent type I IFN immunity (OR = 3.70[95%CI 1.3–8.2], P = 2.1 × 10−4). This enrichment was further strengthened by (1) adding the recently reported TYK2 and TLR7 COVID-19 loci, particularly under a recessive model (OR = 19.65[95%CI 2.1–2635.4], P = 3.4 × 10−3), and (2) considering as pLOF branchpoint variants with potentially strong impacts on splicing among the 15 loci (OR = 4.40[9%CI 2.3–8.4], P = 7.7 × 10−8). Finally, the patients with pLOF/bLOF variants at these 15 loci were significantly younger (mean age [SD] = 43.3 [20.3] years) than the other patients (56.0 [17.3] years; P = 1.68 × 10−5). Conclusions: Rare variants of TLR3- and TLR7-dependent type I IFN immunity genes can underlie life-threatening COVID-19, particularly with recessive inheritance, in patients under 60 years old.
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- 2023
204. Obesity and survival among women with ovarian cancer: results from the Ovarian Cancer Association Consortium
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Nagle, CM, Dixon, SC, Jensen, A, Kjaer, SK, Modugno, F, deFazio, A, Fereday, S, Hung, J, Johnatty, SE, Fasching, PA, Beckmann, MW, Lambrechts, D, Vergote, I, Van Nieuwenhuysen, E, Lambrechts, S, Risch, HA, Rossing, MA, Doherty, JA, Wicklund, KG, Chang-Claude, J, Goodman, MT, Ness, RB, Moysich, K, Heitz, F, du Bois, A, Harter, P, Schwaab, I, Matsuo, K, Hosono, S, Goode, EL, Vierkant, RA, Larson, MC, Fridley, BL, Høgdall, C, Schildkraut, JM, Weber, RP, Cramer, DW, Terry, KL, Bandera, EV, Paddock, L, Rodriguez-Rodriguez, L, Wentzensen, N, Yang, HP, Brinton, LA, Lissowska, J, Høgdall, E, Lundvall, L, Whittemore, A, McGuire, V, Sieh, W, Rothstein, J, Sutphen, R, Anton-Culver, H, Ziogas, A, Pearce, CL, Wu, AH, and Webb, PM
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Biomedical and Clinical Sciences ,Oncology and Carcinogenesis ,Prevention ,Nutrition ,Ovarian Cancer ,Obesity ,Rare Diseases ,Cancer ,Body Mass Index ,Carcinoma ,Ovarian Epithelial ,Disease-Free Survival ,Female ,Humans ,Kaplan-Meier Estimate ,Neoplasms ,Glandular and Epithelial ,Ovarian Neoplasms ,ovarian cancer ,obesity ,overall survival ,progression-free survival ,ovarian cancer-specific survival ,Australian Ovarian Cancer Study Group ,Ovarian Cancer Association Consortium ,Public Health and Health Services ,Oncology & Carcinogenesis ,Oncology and carcinogenesis - Abstract
BackgroundObservational studies have reported a modest association between obesity and risk of ovarian cancer; however, whether it is also associated with survival and whether this association varies for the different histologic subtypes are not clear. We undertook an international collaborative analysis to assess the association between body mass index (BMI), assessed shortly before diagnosis, progression-free survival (PFS), ovarian cancer-specific survival and overall survival (OS) among women with invasive ovarian cancer.MethodsWe used original data from 21 studies, which included 12 390 women with ovarian carcinoma. We combined study-specific adjusted hazard ratios (HRs) using random-effects models to estimate pooled HRs (pHR). We further explored associations by histologic subtype.ResultsOverall, 6715 (54%) deaths occurred during follow-up. A significant OS disadvantage was observed for women who were obese (BMI: 30-34.9, pHR: 1.10 (95% confidence intervals (CIs): 0.99-1.23); BMI: ⩾35, pHR: 1.12 (95% CI: 1.01-1.25)). Results were similar for PFS and ovarian cancer-specific survival. In analyses stratified by histologic subtype, associations were strongest for women with low-grade serous (pHR: 1.12 per 5 kg m(-2)) and endometrioid subtypes (pHR: 1.08 per 5 kg m(-2)), and more modest for the high-grade serous (pHR: 1.04 per 5 kg m(-2)) subtype, but only the association with high-grade serous cancers was significant.ConclusionsHigher BMI is associated with adverse survival among the majority of women with ovarian cancer.
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- 2015
205. A Phase II Randomized, Controlled Trial of S-Adenosylmethionine in Reducing Serum  -Fetoprotein in Patients with Hepatitis C Cirrhosis and Elevated AFP
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Morgan, T. R, Osann, K., Bottiglieri, T., Pimstone, N., Hoefs, J. C, Hu, K.-Q., Hassanein, T., Boyer, T. D, Kong, L., Chen, W.-P., Richmond, E., Gonzalez, R., Rodriguez, L. M, and Meyskens, F. L
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- 2015
206. Signatures of infall motions in the images of the molecular emission of G31 HMC
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Mayen-Gijon, J. M., Anglada, G., Osorio, M., Rodriguez, L. F., Lizano, S., Gomez, J. F., and Carrasco-Gonzalez, C.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Although gravitational collapse is supposed to play an essential role in the star formation process, infall motions have been always elusive to detect. So far, only a few observational signatures have been commonly used to claim for the presence of infall. Often these features consist in either "blue-asymmetries" or absorption at red-shifted velocities (e.g., inverse P-Cygni profiles). Both signatures are based only on the shape of the line profile and they do not guarantee by themselves the presence of dominant infall motions. More robust "mapping signatures" can be obtained from images that angularly resolve the infalling gas. Here we present VLA observations of the ammonia inversion transitions (2,2), (3,3), (4,4), (5,5), and (6,6) towards the hot molecular core (HMC) near G31.41+0.31 that show the signatures of protostellar infall theoretically predicted by Anglada et al. (1991). The intensity of the ammonia emission is compact and sharply increases towards the centre in the blue-shifted velocity channel maps, while it shows a more flattened distribution in the red-shifted velocity channels. Additionally, the emission becomes more compact with increasing (relative) velocity for both red and blue-shifted channels. We introduce a new infall signature, the "central blue spot", easily identifiable in the first-order moment maps. We show that rotation produces an additional, independent signature, making the distribution of the emission in the channel maps asymmetric with respect to the central position, but without masking the infall signatures. All these mapping signatures, which are identified here for the first time, are present in the observed ammonia transitions of G31 HMC., Comment: Too appear in MNRAS
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- 2013
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207. Multi-epoch VLBA H$_2$O maser observations toward the massive YSOs AFGL 2591 VLA 2 and VLA 3
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Torrelles, J. M., Trinidad, M. A., Curiel, S., Estalella, R., Patel, N. A., Gómez, J. F., Anglada, G., Carrasco-González, C., Cantó, J., Raga, A., and Rodríguez, L. F.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present multi-epoch Very Long Baseline Array (VLBA) H$_2$O maser observations toward the massive young stellar objects (YSOs) VLA 2 and VLA 3 in the star-forming region AFGL 2591. Through these observations, we have extended the study of the evolution of the masers towards these objects up to a time span of $\sim$ 10 yrs, measuring their radial velocities and proper motions. The H$_2$O masers in VLA 3, the most massive YSO in AFGL 2591 ($\sim$ 30--40~M$_{\odot}$), are grouped within projected distances of $\lesssim$ 40 mas ($\lesssim$ 130 AU) from VLA 3. In contrast to other H$_2$O masers in AFGL 2591, the masers associated with VLA 3 are significantly blueshifted (up to $\sim$ 30 km s$^{-1}$) with respect to the velocity of the ambient molecular cloud. We find that the H$_2$O maser cluster as a whole, has moved westwards of VLA~3 between the 2001 and 2009 observations, with a proper motion of $\sim$ 1.2 mas yr$^{-1}$ ($\sim$ 20 km s$^{-1}$). We conclude that these masers are tracing blueshifted outflowing material, shock excited at the inner parts of a cavity seen previously in ammonia molecular lines and infrared images, and proposed to be evacuated by the outflow associated with the massive VLA 3 source. The masers in the region of VLA 2 are located at projected distances of $\sim$ 0.7$''$ ($\sim$ 2300 AU) north from this source, with their kinematics suggesting that they are excited by a YSO other than VLA 2. This driving source has not yet been identified.
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- 2013
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208. First observation of the thermal Sunyaev-Zel'dovich effect with kinetic inductance detectors
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Adam, R., Comis, B., Macías-Pérez, J. F., Adane, A., Ade, P., André, P., Beelen, A., Belier, B., Benoît, A., Bideaud, A., Billot, N., Boudou, N., Bourrion, O., Calvo, M., Catalano, A., Coiffard, G., D'Addabbo, A., Désert, F. -X., Doyle, S., Goupy, J., Kramer, C., Leclercq, S., Martino, J., Mauskopf, P., Mayet, F., Monfardini, A., Pajot, F., Pascale, E., Perotto, L., Pointecouteau, E., Ponthieu, N., Revéret, V., Rodriguez, L., Savini, G., Schuster, K., Sievers, A., Tucker, C., and Zylka, R.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Clusters of galaxies provide valuable information on the evolution of the Universe and large scale structures. Recent cluster observations via the thermal Sunyaev-Zel'dovich (tSZ) effect have proven to be a powerful tool to detect and study them. In this context, high resolution tSZ observations (~ tens of arcsec) are of particular interest to probe intermediate and high redshift clusters. Observations of the tSZ effect will be carried out with the millimeter dual-band NIKA2 camera, based on Kinetic Inductance Detectors (KIDs) to be installed at the IRAM 30-meter telescope in 2015. To demonstrate the potential of such an instrument, we present tSZ observations with the NIKA camera prototype, consisting of two arrays of 132 and 224 detectors that observe at 140 and 240 GHz with a 18.5 and 12.5 arcsec angular resolution, respectively. The cluster RX J1347.5-1145 was observed simultaneously at 140 and 240 GHz. We used a spectral decorrelation technique to remove the atmospheric noise and obtain a map of the cluster at 140 GHz. The efficiency of this procedure has been characterized through realistic simulations of the observations. The observed 140 GHz map presents a decrement at the cluster position consistent with the tSZ nature of the signal. We used this map to study the pressure distribution of the cluster by fitting a gNFW model to the data. Subtracting this model from the map, we confirm that RX J1347.5-1145 is an ongoing merger, which confirms and complements previous tSZ and X-ray observations. For the first time, we demonstrate the tSZ capability of KID based instruments. The NIKA2 camera with ~ 5000 detectors and a 6.5 arcmin field of view will be well-suited for in-depth studies of the intra cluster medium in intermediate to high redshifts, which enables the characterization of recently detected clusters by the Planck satellite., Comment: Accepted by A&A
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- 2013
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209. Latest NIKA results and the NIKA-2 project
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Monfardini, A., Adam, R., Adane, A., Ade, P., André, P., Beelen, A., Belier, B., Benoit, A., Bideaud, A., Billot, N., Bourrion, O., Calvo, M., Catalano, A., Coiffard, G., Comis, B., D'Addabbo, A., Désert, F. -X., Doyle, S., Goupy, J., Kramer, C., Leclercq, S., Macias-Perez, J., Martino, J., Mauskopf, P., Mayet, F., Pajot, F., Pascale, E., Ponthieu, N., Revéret, V., Rodriguez, L., Savini, G., Schuster, K., Sievers, A., Tucker, C., and Zylka, R.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
NIKA (New IRAM KID Arrays) is a dual-band imaging instrument installed at the IRAM (Institut de RadioAstronomie Millimetrique) 30-meter telescope at Pico Veleta (Spain). Two distinct Kinetic Inductance Detectors (KID) focal planes allow the camera to simultaneously image a field-of-view of about 2 arc-min in the bands 125 to 175 GHz (150 GHz) and 200 to 280 GHz (240 GHz). The sensitivity and stability achieved during the last commissioning Run in June 2013 allows opening the instrument to general observers. We report here the latest results, in particular in terms of sensitivity, now comparable to the state-of-the-art Transition Edge Sensors (TES) bolometers, relative and absolute photometry. We describe briefly the next generation NIKA-2 instrument, selected by IRAM to occupy, from 2015, the continuum imager/polarimeter slot at the 30-m telescope., Comment: Proceedings of Low Temperature Detectors 15 (LTD-15), Pasadena, June 2013
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- 2013
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210. Quantized Faraday effect in (3+1)-dimensional and (2+1)-dimensional systems
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Rodriguez, L. Cruz, Martinez, A. Perez, Rojas, H. Perez, and Querts, E. Rodriguez
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High Energy Physics - Phenomenology ,Condensed Matter - Mesoscale and Nanoscale Physics - Abstract
We study Faraday rotation in the quantum relativistic limit. Starting from the photon self-energy in the presence of a constant magnetic field the rotation of the polarization vector of a plane electromagnetic wave which travel along the fermion-antifermion gas is studied. The connection between Faraday Effect and Quantum Hall Effect (QHE) is discussed. The Faraday Effect is also investigated for a massless relativistic (2D+1)-dimensional fermion system which is derived by using the compactification along the dimension parallel to the magnetic field. The Faraday angle shows a quantized behavior as Hall conductivity in two and three dimensions., Comment: 15 pages, 5 figures
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- 2013
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211. MUSCLE W49 : A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. I. Data and The Mass Structure of the Giant Molecular Cloud
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Galván-Madrid, R., Liu, H. B., Zhang, Z. -Y., Pineda, J. E., Peng, T. -C., Zhang, Q., Keto, E. R., Ho, P. T. P., Rodríguez, L. F., Zapata, L., Peters, T., and De Pree, C. G.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The Multi-Scale Continuum and Line Exploration of W49 (MUSCLE W49) is a comprehensive gas and dust survey of the giant molecular cloud (GMC) of W49A, the most luminous star-formation region in the Milky Way. It covers the entire GMC at different scales and angular resolutions. In this paper we present: 1) an all-configuration SMA mosaic in the 230-GHz band covering the central 3 arcmin (10 pc, known as W49N), with most of the embedded massive stars; and 2) PMO 14m telescope observations in the 90-GHz band, covering the entire GMC with maps up to 35 arcmin in size, or 113 pc. We also make use of archival data from the VLA, JCMT-SCUBA, IRAM 30m, and the CSO BOLOCAM GPS. Our main findings are: 1) The W49 GMC is one of the most massive in the Galaxy, with a total mass ~1.1x10^6 Msun within a radius of 60 pc. Within a radius of 6 pc, the total gas mass is ~2x10^5 Msun. At these scales only 1% of the material is photoionized. The mass reservoir is sufficient to form several young massive clusters (YMCs) as massive as a globular cluster. 2) The mass of the GMC is distributed in a hierarchical network of filaments. At scales <10 pc, a triple, centrally condensed structure peaks toward the ring of HC HII regions in W49N. This structure extends to scales from ~10 to 100 pc. The W49A starburst most likely formed from global gravitational contraction with localized collapse in a "hub-filament" geometry. 3) Currently, feedback from the central YMCs (with a present mass Mcl > 5x10^4 Msun) is still not enough to entirely disrupt the GMC, but further stellar mass growth could be enough to allow radiation pressure to clear the cloud and halt star formation. 4) The resulting stellar content will probably remain as a gravitationally bound massive star cluster, or a small system of bound clusters. (ABRIDGED), Comment: Author version of paper published in ApJ. For high-quality figures please see the Journal version
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- 2013
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212. Point-form dynamics of quasistable states
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Gadella, M., Gómez-Cubillo, F., Rodriguez, L., and Wickramasekara, S.
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Mathematical Physics ,Nuclear Theory - Abstract
We present a field theoretical model of point-form dynamics which exhibits resonance scattering. In particular, we construct point-form Poincar\'e generators explicitly from field operators and show that in the vector spaces for the in-states and out-states (endowed with certain analyticity and topological properties suggested by the structure of the $S$-matrix) these operators integrate to furnish differentiable representations of the causal Poincar\'e semigroup, the semidirect product of the semigroup of spacetime translations into the forward lightcone and the group of Lorentz transformations. We also show that there exists a class of \emph{irreducible} representations of the Poincar\'e semigroup defined by a complex mass and a half-integer spin. The complex mass characterizing the representation naturally appears in the construction as the square root of the pole position of the propagator. These representations provide a description of resonances in the same vein as Wigner's unitary irreducible representations of the Poincar\'e group provide a description of stable particles., Comment: 68 pages
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- 2013
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213. Star formation in the massive 'starless' infrared dark cloud G0.253$+$0.016
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Rodriguez, L. F. and Zapata, L.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
G0.253+0.016 is a remarkable massive infrared dark cloud located within $\sim$100 pc of the galactic center. With a high mass of $1.3 \times 10^5 M_\odot$, a compact average radius of $\sim$2.8 pc and a low dust temperature of 23 K, it has been believed to be a yet starless precursor to a massive Arches-like stellar cluster. We present sensitive JVLA 1.3 and 5.6 cm radio continuum observations that reveal the presence on three compact thermal radio sources projected against this cloud. These radio sources are interpreted as HII regions powered by $\sim$B0.5 ZAMS stars. We conclude that although G0.253+0.016 does not show evidence of O-type star formation, there are certainly early B-type stars embedded in it. We detect three more sources in the periphery of G0.253+0.016 with non-thermal spectral indices. We suggest that these sources may be related to the galactic center region and deserve further study., Comment: 10 pages, 1 figure
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- 2013
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214. Inflight performance of the PILOT balloon-borne experiment
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Mangilli, A., Foënard, G., Aumont, J., Hughes, A., Mot, B., Bernard, J-Ph., Lacourt, A., Ristorcelli, I., Montier, L., Longval, Y., Ade, P., André, Y., Bautista, L., deBernardis, P., Boulade, O., Bousqet, F., Bouzit, M., Bray, N., Buttice, V., Charra, M., Chaigneau, M., Crane, B., Doumayrou, E., Dubois, J. P., Dupac, X., Engel, C., Etcheto, P., Gelot, Ph., Griffin, M., Grabarnik, S., Hargrave, P., Lepennec, Y., Laureijs, R., Leriche, B., Maestre, S., Maffei, B., Martignac, J., Marty, C., Marty, W., Masi, S., Mirc, F., Misawa, R., Nicot, J. M., Montel, J., Narbonne, J., Pajot, F., Pérot, E., Parot, G., Pimentao, J., Pisano, G., Ponthieu, N., Rodriguez, L., Roudil, G., Roussel, H., Salatino, M., Savini, G., Simonella, O., Saccoccio, M., Stever, S., Tapie, P., Tauber, J., Tibbs, C., and Tucker, C.
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- 2019
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215. Precursor superconducting diamagnetism in YBa2Cu3O7-d with in-plane or intercalated magnetic impurities
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Soto, F., Cotón, N., Dancausa, J. D., Doval, J. M., Ramos-Álvarez, A., Rey, R. I., Rodríguez, L., Carballeira, C., Mosqueira, J., Ramallo, M. V., and Vidal, F.
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Condensed Matter - Superconductivity - Abstract
The magnetization around the superconducting transition was measured in YBa2Cu3O7-d with magnetic impurities in the CuO2 layers (Cu substituted by Zn or Ni) or between them (Y substituted by Gd or Pr). While some of these impurities have an important effect on the superconducting transition temperature (Tc), the precursor diamagnetism observed above Tc is not appreciably affected. This result contrasts with recent observations in a conventional BCS superconductor (La), in which the precursor diamagnetism was found to increase several orders of magnitude with the addition of a small amount (a few atomic percent) of Gd or Pr magnetic impurities., Comment: 14 pages including 5 figures and 1 table
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- 2013
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216. Formation and evolution of the water maser outflow event in AFGL 2591 VLA 3-N
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Trinidad, M. A., Curiel, S., Estalella, R., Cantó, J., Raga, A., Torrelles, J. M., Patel, N. A., Gómez, J. F., Anglada, G., Carrasco-González, C., and Rodríguez, L. F.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
In this paper we analyze multi-epoch Very Long Baseline Interferometry (VLBI) water maser observations carried out with the Very Long Baseline Array (VLBA) toward the high-mass star-forming region AFGL 2591. We detected maser emission associated with the radio continuum sources VLA 2 and VLA 3. In addition, a water maser cluster, VLA 3-N, was detected ~ 0.5" north of VLA 3. We concentrate the discussion of this paper on the spatio-kinematical distribution of the water masers towards VLA 3-N. The water maser emission toward the region VLA 3-N shows two bow shock-like structures, Northern and Southern, separated from each other by ~ 100 mas (~ 330 AU). The spatial distribution and kinematics of the water masers in this cluster have persisted over a time span of seven years. The Northern bow shock has a somewhat irregular morphology, while the Southern one has a remarkably smooth morphology. We measured the proper motions of 33 water maser features, which have an average proper motion velocity of ~ 1.3 mas/yr (~ 20 km/s). The morphology and the proper motions of this cluster of water masers show systematic expanding motions that could imply one or two different centers of star formation activity. We made a detailed model for the Southern structure, proposing two different kinematic models to explain the 3-dimensional spatio-kinematical distribution of the water masers: (1) a static central source driving the two bow-shock structures; (2) two independent driving sources, one of them exciting the Northern bow-shock structure, and the other one, a young runaway star moving in the local molecular medium exciting and molding the remarkably smoother Southern bow-shock structure. Future observations will be necessary to discriminate between the two scenarios, in particular by identifying the still unseen driving source(s).
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- 2012
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217. Linking two consecutive nonmerging magnetic clouds with their solar sources
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Dasso, S., Mandrini, C. H., Schmieder, B., Cremades, H., Cid, C., Cerrato, Y., Saiz, E., Démoulin, P., Zhukov, A. N., Rodriguez, L., Aran, A., Menvielle, M., and Poedts, S.
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Astrophysics - Solar and Stellar Astrophysics ,Physics - Space Physics - Abstract
On 15 May 2005, a huge interplanetary coronal mass ejection (ICME) was observed near Earth. It triggered one of the most intense geomagnetic storms of solar cycle 23 (Dst peak = -263 nT). This structure has been associated with the two-ribbon flare, filament eruption, and coronal mass ejection originating in active region 10759 (NOAA number). We analyze here the sequence of events, from solar wind measurements (at 1 AU) and back to the Sun, to understand the origin and evolution of this geoeffective ICME. From a detailed observational study of in situ magnetic field observations and plasma parameters in the interplanetary (IP) medium and the use of appropriate models we propose an alternative interpretation of the IP observations, different to those discussed in previous studies. In our view, the IP structure is formed by two extremely close consecutive magnetic clouds (MCs) that preserve their identity during their propagation through the interplanetary medium. Consequently, we identify two solar events in H{\alpha} and EUV which occurred in the source region of the MCs. The timing between solar and IP events, as well as the orientation of the MC axes and their associated solar arcades are in good agreement. Additionally, interplanetary radio type II observations allow the tracking of the multiple structures through inner heliosphere and pin down the interaction region to be located midway between the Sun and the Earth. The chain of observations from the photosphere to interplanetary space is in agreement with this scenario. Our analysis allows the detection of the solar sources of the transients and explains the extremely fast changes of the solar wind due to the transport of two attached (though nonmerging) MCs which affect the magnetosphere.
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- 2012
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218. Regional differences in subduction ground motions
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Beauval, Céline, Cotton, F., Abrahamson, N., Theodulidis, N., Delavaud, E., Rodriguez, L., Scherbaum, F., and Haendel, A.
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Physics - Geophysics - Abstract
A few ground-motion prediction models have been published in the last years, for predicting ground motions produced by interface and intraslab earthquakes. When one must carry out a probabilistic seismic hazard analysis in a region including a subduction zone, GMPEs must be selected to feed a logic tree. In the present study, the aim is to identify which models provide the best fit to the dataset M6+, global or local models. The subduction regions considered are Japan, Taiwan, Central and South America, and Greece. Most of the data comes from the database built to develop the new BCHydro subduction global GMPE (Abrahamson et al., submitted). We show that this model is among best-fitting models in all cases, followed closely by Zhao et al. (2006), whereas the local Lin and Lee (2008) is well predicting the data in Taiwan and also in Greece. The Scherbaum et al. (2009) LLH method prove to be efficient in providing one number quantifying the overall fit, but additional analysis on the between-event and within-event variabilities are mandatory, to control if median prediction per event and/or variability within an event is within the scatter predicted by the model., Comment: 10 pages
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- 2012
219. A one-sided knot ejection at the core of the HH 111 outflow
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Gomez, L., Rodriguez, L. F., and Loinard, L.
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Astrophysics - Galaxy Astrophysics - Abstract
We present an astrometry study of the radio source VLA 1 at the core of the HH 111 outflow using new data (2007) as well as archival observations (1992-1996). All data were taken at 3.6 cm with the Very Large Array in its most extended (A) configuration. The source VLA 1 has undergone a dramatic morphological change, showing a one-sided knot ejection in the 2007 epoch. We also report on the detection of a 3.6 cm compact continuum source (VLA 3) located at (-10.6",98.7") from VLA 1. No significant absolute proper motions were found for VLA 1 and VLA 3 and the upper limits are consistent with those found for (embedded) radio sources in the Orion Nebula. We favor the interpretation that in the continuum at 3.6 cm we are observing two nearly perpendicular jets. HH 111 presents a new case of one-sided jet ejection in a young stellar object. The Galactic (or extragalactic) nature of VLA 3 remains unclear., Comment: Accepted for publication in RevMexAA
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- 2012
220. The majority of cells in so-called “mesenchymal stem cell” population are neither stem cells nor progenitors
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Loncaric, D., Labat, V., Debeissat, C., Brunet de la Grange, P., Rodriguez, L., Vlaski-Lafarge, M., and Ivanovic, Z.
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- 2019
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221. Prediction of multicomponent ION exchange equilibria by using the e-NRTL model for computing the activity coefficients in solution
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García, E., Rodriguez, L., Ferro, V., and Valverde, J.L.
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- 2019
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222. Mechanical modeling and characterization of suspended cooled silicon bolometers for sub-millimeter and millimeter waves polarization detection
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Aliane, A., Ouvrier-Buffet, J-L., Dussopt, L., Goudon, V., Rabaud, W., Kaya, H., Torrecillas, R., Agnèse, P., Adami, O., Rodriguez, L., Reveret, V., and Poglitsch, A.
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- 2019
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223. Imaging findings for mucinous tumors tumortumorof the abdomen and pelvis
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Raposo Rodríguez, L., Fernández García, N., Tovar Salazar, D.J., Gómez Illán, R., and Díaz Sánchez, T.B.
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- 2019
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224. Hallazgos en imagen en los tumores mucinosos de abdomen y pelvis
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Raposo Rodríguez, L., Fernández García, N., Tovar Salazar, D.J., Gómez Illán, R., and Díaz Sánchez, T.B.
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- 2019
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225. Influence of purification on physicochemical and emulsifying properties of tamarind (Tamarindus indica L.) seed gum
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Crispín-Isidro, G., Hernández-Rodríguez, L., Ramírez-Santiago, C., Sandoval-Castilla, O., Lobato-Calleros, C., and Vernon-Carter, E.J.
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- 2019
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226. Is fibromyalgia a cause of arthroscopic subacromial decompression failure?
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Lopiz, Y., Marcelo, H., Arvinius, C., Rodriguez-Rodriguez, L., García-Fernández, C., and Marco, F.
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- 2019
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227. ¿Es la fibromialgia causa de fracaso de una descompresión subacromial artroscópica?
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Lopiz, Y., Marcelo, H., Arvinius, C., Rodriguez-Rodriguez, L., García-Fernández, C., and Marco, F.
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- 2019
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228. Changes in the prevalence of asthma and related risk factors in adolescents: Three surveys between 1994 and 2015
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Mallol, J., Aguirre, V., Mallol-Simmonds, M., Matamala- Bezmalinovic, A., Calderón-Rodriguez, L., and Osses-Vergara, F.
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- 2019
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229. Late Quaternary glacial phases in the Iberian Peninsula
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Oliva, M., Palacios, D., Fernández-Fernández, J.M., Rodríguez-Rodríguez, L., García-Ruiz, J.M., Andrés, N., Carrasco, R.M., Pedraza, J., Pérez-Alberti, A., Valcárcel, M., and Hughes, P.D.
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- 2019
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230. Characteristics and longer-term outcomes of paravalvular leak after aortic and mitral valve surgery
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Shah, Shailee, Alashi, Alaa, Pettersson, Gosta B., Rodriguez, L. Leonardo, Gillinov, A. Marc, Grimm, Richard A., Navia, Jose, Kapadia, Samir R., Svensson, Lars G., Griffin, Brian P., and Desai, Milind Y.
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- 2019
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231. On the number of PV modules in series for large-power irrigation systems
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Narvarte, L., Almeida, R.H., Carrêlo, I.B., Rodríguez, L., Carrasco, L.M., and Martinez-Moreno, F.
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- 2019
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232. Guidelines for seizure management in palliative care: proposal for an updated clinical practice model based on a systematic literature review
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León Ruiz, M., Rodríguez Sarasa, M.L., Sanjuán Rodríguez, L., Pérez Nieves, M.T., Ibáñez Estéllez, F., Arce Arce, S., García-Albea Ristol, E., and Benito-León, J.
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- 2019
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233. Guía para el manejo de las crisis epilépticas en cuidados paliativos: propuesta de un modelo actualizado de práctica clínica basado en una revisión sistemática de la literatura
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León Ruiz, M., Rodríguez Sarasa, M.L., Sanjuán Rodríguez, L., Pérez Nieves, M.T., Ibáñez Estéllez, F., Arce Arce, S., García-Albea Ristol, E., and Benito-León, J.
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- 2019
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234. The perspective of different age groups regarding old age and aging in highly aged contexts
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Faílde Garrido, J.M., Dapía Conde, M.D., Vázquez Vázquez, M.A., Ruíz Soriano, L., and Vázquez Rodríguez, L.
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- 2019
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235. Quantum trajectory study of laser-driven atomic ionization
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Cruz-Rodríguez, L., Uranga-Piña, L., Martínez-Mesa, A., and Meier, C.
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- 2019
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236. Resolving the Vela C ridge with P-ArTeMiS and Herschel
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Hill, T., Andre, Ph., Arzoumanian, D., Motte, F., Minier, V., Menshchikov, A., Didelon, P., Hennemann, M., Konyves, V., Nguyen-Luong, Q., Palmeirim, P., Peretto, N., Schneider, N., Bontemps, S., Louvet, F., Elia, D., Giannini, T., Reveret, V., Pennec, J. Le, Rodriguez, L., Boulade, O., Doumayrou, E., Dubreuil, D., Gallais, P., Lortholary, M., Martignac, J., Talvard, M., and De Breuck, C.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
We present APEX/P-ArT\'eMiS 450\mu m continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel's SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArT\'eMiS. We extract the radial density profile of the Vela C ridge which with a ~ 0.1pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. Despite likely different formation mechanisms and histories, the Vela C ridge and Serpens South filament share common characteristics, including their filament central widths., Comment: Accepted by A&A Letters; 4 pages with an appendix; 6 figures - 2 online, 1 in an appendix
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- 2012
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237. Study of a Prominence Eruption using PROBA2/SWAP and STEREO/EUVI Data
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Mierla, M., Seaton, D. B., Berghmans, D., Chifu, I., De Groof, A., Inhester, B., Rodriguez, L., Stenborg, G., and Zhukov, A. N.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Observations of the early rise and propagation phases of solar eruptive prominences can provide clues about the forces acting on them through the behavior of their acceleration with height. We have analyzed such an event, observed on 13 April 2010 by SWAP on PROBA2 and EUVI on STEREO. A feature at the top of the erupting prominence was identified and tracked in images from the three spacecraft. The triangulation technique was used to derive the true direction of propagation of this feature. The reconstructed points were fitted with two mathematical models: i) a power-law polynomial function and ii) a cubic smoothing spline, in order to derive the accelerations. The first model is characterized by five degrees of freedom while the second one is characterized by ten degrees of freedom. The results show that the acceleration increases smoothly and it is continuously increasing with height. We conclude that the prominence is not accelerated immediately by local reconnection but rather is swept away as part of a large-scale relaxation of the coronal magnetic field., Comment: 15 Pages, Accepted for publication in Solar Physics, PROBA2 Topical Issue
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- 2012
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238. Premières expériences d’élevage et d’ensemencement de Paracentrotus lividus, Lamarck, en Galice (Espagne)
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Catoira Gomez, J. L., primary, Talion, J.G. Mosquera, additional, and Rodriguez, L. J. Miguez, additional
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- 2020
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239. VLBA determination of the distance to nearby star-forming regions V. Dynamical mass, distance and radio structure of V773 Tau A
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Torres, R. M., Loinard, L., Mioduszewski, A. J., Boden, A. F., Franco-Hernandez, R., Vlemmings, W. H. T., and Rodriguez, L. R.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
(ABRIDGED) We present multi-epoch Very Long Baseline Array (VLBA) observations of V773 Tau A, the 51-day binary subsystem in the multiple young stellar system V773 Tau. Combined with previous interferometric and radial velocity measurements, these new data enable us to improve the characterization of the physical orbit of the A subsystem. In particular, we infer updated dynamical masses for the primary and the secondary components of 1.55 pm 0.11 Msun, and 1.293 pm 0.068 Msun, respectively, and an updated orbital parallax distance to the system of 135.7 pm 3.2 pc, all consistent with previous estimates. Using the improved orbit, we can calculate the absolute coordinates of the barycenter of V773 Tau A at each epoch of our VLBA observations, and fit for its trigonometric parallax and proper motion. This provides a direct measurement of the distance to the system almost entirely independent of the orbit modeling. The best fit yields a distance of 129.9 pm 3.2 pc, in good agreement (i.e. within 1 sigma) with the distance estimate based on the orbital fit. Taking the mean value of the orbital and trigonometric parallaxes, we conclude that V773 Tau is located at d =132.8 pm 2.3 pc. The accuracy of this determination is nearly one order of magnitude better than that of previous estimates. In projection, V773 Tau and two other young stars (Hubble 4 and HDE 283572) recently observed with the VLBA are located toward the dark cloud Lynds 1495, in the central region of Taurus. These three stars appear to have similar trigonometric parallaxes, radial velocities, and proper motions, and we argue that the weighted mean and dispersion of their distances (d = 131.4 pc and sigma_d = 2.4 pc) provide a good estimate of the distance to and depth of Lynds 1495 and its associated stellar population., Comment: Accepted for publication in The Astrophysical Journal
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- 2011
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240. Extended Non-Thermal Emission Possibly Associated with Cyg OB2 #5
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Ortiz-Leon, G. N., Rodriguez, L. F., and Tapia, M.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Cyg OB2 #5 is a contact binary system (O6.5-7+O5.5-6) with associated radio continuum emission. Two compact ($\leq 0\rlap.{"}3$) radio continuum components have been reported previously: the primary one is associated with the contact binary and the secondary one is an arc-like source $\sim 0\rlap.{"}8$ to the NE of the primary. This arc-like source results from the interaction of the winds of the contact binary and a B-type star in the region. In this paper we report the detection of an extended ($\sim 30"$), non-thermal component to the NE of the compact components. We propose that this extended emission could be an unresolved background source (i. e. a radio galaxy), extended galactic emission, or non-thermal emission related with relativistic electrons that are produced in the shock between the contact binary and the B-type star and that are carried away to large distances by the wind from the contact binary., Comment: 11 pages, 4 figures, to appear in Revista Mexicana de Astronomia y Astrofisica
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- 2011
241. Multiplicity, Disks and Jets in the NGC 2071 Star-Forming Region
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Carrasco-Gonzalez, C., Osorio, M., Anglada, G., D'Alessio, P., Rodriguez, L. F., Gomez, J. F., and Torrelles, J. M.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present centimeter and millimeter observations of the NGC 2071 star-forming region performed with the VLA and CARMA. We detected counterparts at 3.6 cm and 3 mm for the previously known sources IRS 1, IRS 2, IRS 3, and VLA 1. All these sources show SEDs dominated by free-free thermal emission at cm wavelengths, and thermal dust emission at mm wavelengths, suggesting that all of them are associated with YSOs. IRS 1 shows a complex morphology at 3.6 cm, with changes in the direction of its elongation. We discuss two possible explanations to this morphology: the result of changes in the direction of a jet due to interactions with a dense ambient medium, or that we are actually observing the superposition of two jets arising from two components of a binary system. Higher angular resolution observations at 1.3 cm support the second possibility, since a double source is inferred at this wavelength. IRS 3 shows a clear jet-like morphology at 3.6 cm. Over a time-span of four years, we observed changes in the morphology of this source that we interpret as due to ejection of ionized material in a jet. The emission at 3 mm of IRS 3 is angularly resolved, with a deconvolved size (FWHM) of ~120 AU, and seems to be tracing a dusty circumstellar disk perpendicular to the radio jet. An irradiated accretion disk model around an intermediate-mass YSO can account for the observed SED and spatial intensity profile at 3 mm, supporting this interpretation., Comment: Accepted by The Astrophysical Journal
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- 2011
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242. Radio continuum emission from knots in the DG Tau jet
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Rodriguez, L. F., Gonzalez, R. F., Raga, A. C., Canto, J., Riera, A., Loinard, L., Dzib, S. A., and Zapata, L. A.
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Astrophysics - Astrophysics of Galaxies - Abstract
Context: HH 158, the jet from the young star DG Tau, is one of the few sources of its type where jet knots have been detected at optical and X-ray wavelengths. Aims: To search, using Very Large Array observations of this source, radio knots and if detected, compare them with the optical and X-ray knots. To model the emission from the radio knots. Methods: We analyzed archive data and also obtained new Very Large Array observations of this source, as well as an optical image, to measure the present position of the knots. We also modeled the radio emission from the knots in terms of shocks in a jet with intrinsically time-dependent ejection velocities. Results: We detected radio knots in the 1996.98 and 2009.62 VLA data. These radio knots are,within error, coincident with optical knots. We also modeled satisfactorily the observed radio flux densities as shock features from a jet with intrinsic variability. All the observed radio, optical, and X-ray knot positions can be intepreted as four successive knots, ejected with a period of 4.80 years and traveling away from the source with a velocity of 198 km s$^{-1}$ in the plane of the sky. Conclusions: The radio and optical knots are spatially correlated and our model can explain the observed radio flux densities. However, the X-ray knots do not appear to have optical or radio counterparts and their nature remains poorly understood., Comment: 8 pages, 8 figures, to appear in Astronomy & Astrophysics
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- 2011
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243. The Magnetic Field of the H~II Region NGC 6334A
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Rodriguez, L. F., Gomez, Y., and Tafoya, D.
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Astrophysics - Astrophysics of Galaxies - Abstract
We have studied the polarization characteristics and Faraday rotation of the extragalactic radio source J17204$-$3554, that appears projected on the north lobe of the galactic H II region NGC 6334A. From observations made with the Very Large Array at 6.0 and 3.6 cm in three different epochs (1994, 1997, and 2006), we estimate a rotation measure of +5100$\pm$900 rad m$^{-2}$ for the extragalactic source. This large rotation measure implies a line-of-sight average magnetic field of $B_\parallel \simeq +36\pm6$ $\mu$G, the largest obtained by this method for an H II region. NGC 6334A is significantly denser than other H II regions studied and this larger magnetic field is expected on the grounds of magnetic flux conservation. The ratio of thermal to magnetic pressure is $\sim$5, in the range of values determined for more diffuse H II regions., Comment: 5 pages, 0 figures
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- 2011
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244. Radio Continuum Emission from FS CMa Stars
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Rodriguez, L. F., Baez-Rubio, A., and Miroshnichenko, A. S.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
The FS CMa stars exhibit bright optical emission-line spectra and strong IR excesses. Very little is known of their radio characteristics. We analyzed archive Very Large Array data to search for radio continuum emission in a sample of them. There are good quality data for seven of the $\sim$40 known FS CMa stars. Of these seven stars, five turn out to have associated radio emission. Two of these stars, CI Cam and MWC 300, have been previously reported in the literature as radio emitters. We present and briefly discuss the radio detection of the other three sources: FS CMa (the prototype of the class), AS 381, and MWC 922. The radio emission is most probably of a free-free nature but additional observations are required to better characterize it., Comment: 7 pages, 5 figures
- Published
- 2011
245. Low polarized emission from the core of coronal mass ejections
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Mierla, M., Chifu, I., Inhester, B., Rodriguez, L., and Zhukov, A.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
In white-light coronagraph images, cool prominence material is sometimes observed as bright patches in the core of coronal mass ejections (CMEs). If, as generally assumed, this emission is caused by Thomson-scattered light from the solar surface, it should be strongly polarised tangentially to the solar limb. However, the observations of a CME made with the SECCHI/STEREO coronagraphs on 31 August 2007 show that the emission from these bright core patches is exceptionally low polarised. We used the polarisation ratio method of Moran and Davila (2004) to localise the barycentre of the CME cloud. By analysing the data from both STEREO spacecraft we could resolve the plane-of-the-sky ambiguity this method usually suffers from. Stereoscopic triangulation was used to independently localise the low-polarisation patch relative to the cloud. We demonstrated for the first time that the bright core material is located close to the centre of the CME cloud. We show that the major part of the CME core emission, more than 85% in our case, is H$\alpha$ radiation and only a small fraction is Thomson-scattered light. Recent calculations also imply that the plasma density in the patch is 8 10$^8$ cm$^{-3}$ or more compared to 2.6 10$^6$ cm$^{-3}$ for the Thomson-scattering CME environment surrounding the core material., Comment: 5 pages, 3 figures
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- 2011
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246. The Gould's Belt distance survey
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Loinard, L., Mioduszewski, A. J., Torres, R. M., Dzib, S., Rodriguez, L. F., and Boden, A. F.
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Astrophysics - Galaxy Astrophysics - Abstract
Very Long Baseline Interferometry (VLBI) observations can provide the position of compact radio sources with an accuracy of order 50 micro-arcseconds. This is sufficient to measure the trigonometric parallax and proper motions of any object within 500 pc of the Sun to better than a few percent. Because they are magnetically active, young stars are often associated with compact radio emission detectable using VLBI techniques. Here we will show how VLBI observations have already constrained the distance to the most often studied nearby regions of star-formation (Taurus, Ophiuchus, Orion, etc.) and have started to provide information on their internal structure and kinematics. We will then briefly describe a large project (called The Gould's Belt Distance Survey) designed to provide a detailed view of star-formation in the Solar neighborhood using VLBI observations., Comment: To be published in the Revista Mexicana de Astronomia y Astrofisica (Serie de Conferencias)
- Published
- 2011
247. Lucky Imaging Adaptive Optics of the brown dwarf binary GJ569Bab
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Femenía, B., Rebolo, R., Pérez-Prieto, J. A., Hildebrandt, S. R., Labadie, L., Pérez-Garrido, A., Béjar, V. J. S., Díaz-Sánchez, A., Villó, I., Oscoz, A., López, R., Rodríguez, L. F., and Piqueras, J.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The potential of combining Adaptive Optics (AO) and Lucky Imaging (LI) to achieve high precision astrometry and differential photometry in the optical is investigated by conducting observations of the close 0\farcs1 brown dwarf binary GJ569Bab. We took 50000 $I$-band images with our LI instrument FastCam attached to NAOMI, the 4.2-m William Herschel Telescope (WHT) AO facility. In order to extract the most of the astrometry and photometry of the GJ569Bab system we have resorted to a PSF fitting technique using the primary star GJ569A as a suitable PSF reference which exhibits an $I$-band magnitude of $7.78\pm0.03$. The AO+LI observations at WHT were able to resolve the binary system GJ569Bab located at $4\farcs 92 \pm 0\farcs05$ from GJ569A. We measure a separation of $98.4 \pm 1.1$ mas and $I$-band magnitudes of $13.86 \pm 0.03$ and $14.48 \pm 0.03$ and $I-J$ colors of 2.72$\pm$0.08 and 2.83$\pm$0.08 for the Ba and Bb components, respectively. Our study rules out the presence of any other companion to GJ569A down to magnitude I$\sim$ 17 at distances larger than 1\arcsec. The $I-J$ colors measured are consistent with M8.5-M9 spectral types for the Ba and Bb components. The available dynamical, photometric and spectroscopic data are consistent with a binary system with Ba being slightly (10-20%) more massive than Bb. We obtain new orbital parameters which are in good agreement with those in the literature., Comment: 13 pages, 9 figures, 7 tables, in press in MNRAS
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- 2010
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248. High contrast optical imaging of companions: the case of the brown dwarf binary HD-130948BC
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Labadie, L., Rebolo, R., Villo, I., Perez-Prieto, J. A., Perez-Garrido, A., Hildebrandt, S. R., Femenia, B., Diaz-Sanchez, A., Bejar, V. J. S., Oscoz, A., Lopez, R., Piqueras, J., and Rodriguez, L. F.
- Subjects
Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
High contrast imaging at optical wavelengths is limited by the modest correction of conventional near-IR optimized AO systems.We take advantage of new fast and low-readout-noise detectors to explore the potential of fast imaging coupled to post-processing techniques to detect faint companions to stars at small separations. We have focused on I-band direct imaging of the previously detected brown dwarf binary HD130948BC,attempting to spatially resolve the L2+L2 benchmark system. We used the Lucky-Imaging instrument FastCam at the 2.5-m Nordic Telescope to obtain quasi diffraction-limited images of HD130948 with ~0.1" resolution.In order to improve the detectability of the faint binary in the vicinity of a bright (I=5.19 \pm 0.03) solar-type star,we implemented a post-processing technique based on wavelet transform filtering of the image which allows us to strongly enhance the presence of point-like sources in regions where the primary halo dominates. We detect for the first time the BD binary HD130948BC in the optical band I with a SNR~9 at 2.561"\pm 0.007" (46.5 AU) from HD130948A and confirm in two independent dataset that the object is real,as opposed to time-varying residual speckles.We do not resolve the binary, which can be explained by astrometric results posterior to our observations that predict a separation below the NOT resolution.We reach at this distance a contrast of dI = 11.30 \pm 0.11, and estimate a combined magnitude for this binary to I = 16.49 \pm 0.11 and a I-J colour 3.29 \pm 0.13. At 1", we reach a detectability 10.5 mag fainter than the primary after image post-processing. We obtain on-sky validation of a technique based on speckle imaging and wavelet-transform processing,which improves the high contrast capabilities of speckle imaging.The I-J colour measured for the BD companion is slightly bluer, but still consistent with what typically found for L2 dwarfs(~3.4-3.6)., Comment: accepted in A\&A
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- 2010
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249. High spatial resolution and high contrast optical speckle imaging with FASTCAM at the ORM
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Labadie, L., Rebolo, R., Femenia, B., Villo, Isidro, Diaz-Sanchez, A., Oscoz, A., Lopez, R., Perez-Prieto, J., Perez-Garrido, A., Hildebrandt, S. R., Bejar-Sanchez, V., Piqueras, J., and Rodriguez, L. F.
- Subjects
Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
In this paper, we present an original observational approach, which combines, for the first time, traditional speckle imaging with image post-processing to obtain in the optical domain diffraction-limited images with high contrast (1e-5) within 0.5 to 2 arcseconds around a bright star. The post-processing step is based on wavelet filtering an has analogy with edge enhancement and high-pass filtering. Our I-band on-sky results with the 2.5-m Nordic Telescope (NOT) and the lucky imaging instrument FASTCAM show that we are able to detect L-type brown dwarf companions around a solar-type star with a contrast DI~12 at 2" and with no use of any coronographic capability, which greatly simplifies the instrumental and hardware approach. This object has been detected from the ground in J and H bands so far only with AO-assisted 8-10 m class telescopes (Gemini, Keck), although more recently detected with small-class telescopes in the K band. Discussing the advantage and disadvantage of the optical regime for the detection of faint intrinsic fluxes close to bright stars, we develop some perspectives for other fields, including the study of dense cores in globular clusters. To the best of our knowledge this is the first time that high contrast considerations are included in optical speckle imaging approach., Comment: Proceedings of SPIE conference - Ground-based and Airborne Instrumentation for Astronomy III (Conference 7735), San Diego 2010
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- 2010
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250. A wide-angle outflow with the simultaneous presence of a high-velocity jet in the high-mass Cepheus A HW2 system
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Torrelles, J. M., Patel, N. A., Curiel, S., Estalella, R., Gomez, J. F., Rodriguez, L. F., Canto, J., Anglada, G., Vlemmings, W., Garay, G., Raga, A., and Ho, P. T. P.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
We present five epochs of VLBI water maser observations around the massive protostar Cepheus A HW2 with 0.4 mas (0.3 AU) resolution. The main goal of these observations was to follow the evolution of the remarkable water maser linear/arcuate structures found in earlier VLBI observations. Comparing the data of our new epochs of observation with those observed five years before, we find that at "large" scales of > 1" (700 AU) the main regions of maser emission persist, implying that both the surrounding medium and the exciting sources of the masers have been relatively stable during that time span. However, at smaller scales of < 0.1" (70 AU) we see large changes in the maser structures, particularly in the expanding arcuate structures R4 and R5. R4 traces a nearly elliptical patchy ring of ~ 70 mas size (50 AU) with expanding motions of ~ 5 mas/yr (15 km/s). This structure is probably driven by the wind of a still unidentified YSO located at the centre of the ring (~ 0.18" south of HW2). On the other hand, the R5 expanding bubble structure (driven by the wind of a previously identified YSO located ~ 0.6" south of HW2) is currently dissipating in the circumstellar medium and losing its previous degree of symmetry, indicating a very short-lived event. In addition, our results reveal, at scales of ~ 1" (700 AU), the simultaneous presence of a relatively slow (~ 10-70 km/s) wide-angle outflow (opening angle of ~ 102 deg, traced by the masers, and the fast (~ 500~km/s) highly collimated radio jet associated with HW2 (opening angle of ~ 18 deg, previously observed with the VLA. This simultaneous presence of a wide-angle outflow and a highly collimated jet associated with a massive protostar is similar to what is found in some low-mass YSOs. The implications of these results in the study of the formation of high-mass stars are discussed., Comment: 28 pages, 7 figures. Animations will be included as supporting material online (MNRAS web page)
- Published
- 2010
- Full Text
- View/download PDF
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