12 results on '"Infravermelho"'
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2. A survey of extended H2 emission from massive YSOs
- Author
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F. Navarete, Robert Blum, Augusto Damineli, and C. L. Barbosa
- Subjects
Physics ,Infrared ,Astrophysics::High Energy Astrophysical Phenomena ,Young stellar object ,Near-infrared spectroscopy ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Galactic plane ,Accretion (astrophysics) ,law.invention ,Telescope ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,law ,INFRAVERMELHO ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics - Abstract
We present the results from a survey, designed to investigate the accretion process of massive young stellar objects (MYSOs) through near infrared narrow band imaging using the H$_2$ $\nu$=1-0 S(1) transition filter. A sample of 353 Massive Young Stellar Object (MYSO) candidates was selected from the Red MSX Source survey using photometric criteria at longer wavelengths (infrared and submillimeter) and chosen with positions throughout the Galactic Plane. Our survey was carried out at the SOAR Telescope in Chile and CFHT in Hawaii covering both hemispheres. The data reveal that extended H$_2$ emission is a good tracer of outflow activity, which is a signpost of accretion process on young massive stars. Almost half of the sample exhibit extended H$_2$ emission and 74 sources (21\%) have polar morphology, suggesting collimated outflows. The polar-like structures are more likely to appear on radio-quiet sources, indicating these structures occur during the pre-UCHII phase. We also found an important fraction of sources associated with fluorescent H$_2$ diffuse emission that could be due to a more evolved phase. The images also indicate only $\sim$23\% (80) of the sample is associated with extant (young) stellar clusters. These results support the scenario in which massive stars are formed by accretion disks, since the merging of low mass stars would not produce outflow structures., Comment: to appear on MNRAS. 18 pages, 86 figures and supplementary data available at CDS
- Published
- 2015
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3. Identifying clouds over the Pierre Auger Observatory using infrared satellite data
- Author
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M. Zavrtanik, N. Nierstenhoefer, R. Dallier, F. Salamida, J. F. Valdés Galicia, K. H. Becker, I. De Mitri, A. Gascon Bravo, A. Saftoiu, D. Garcia-Gamez, S. T. Garcia Roca, B. Gookin, D. Melo, David Walz, D. Pakk Selmi-Dei, R. Sato, M. Niechciol, D. B. Tridapalli, A. Segreto, A.M. van den Berg, Darko Veberič, I. Rodriguez Cabo, B. Sarkar, J. L. Navarro, M. Videla, J. C. Diaz, M. A. Leigui de Oliveira, R. Tcaciuc, F. Montanet, J. C. dos Anjos, Petr Schovanek, D. Maurizio, J. C. Moreno, C. Aramo, Lorenzo Caccianiga, Y. Guardincerri, G. Müller, J.M. Chirinos, B. Rouillé-D'Orfeuil, Bruno Daniel, Pham Ngoc Diep, D. Garcia-Pinto, Radomir Smida, T. Yapici, J. J. Masías Meza, R. Gaior, S. H. Cheng, Heino Falcke, B. Tome, L. Buroker, J. Knapp, R. Bonino, J. Vicha, G. Wieczorek, A. Lopez Agüera, F. Diogo, F. Suarez, Sergio Dasso, T. Niggemann, R. M. de Almeida, P. Allison, A. Tapia, G. Cocciolo, H. Gemmeke, C. Rühle, V. de Souza, M. Unger, H. Wahlberg, L. Nellen, B. Zamorano Garcia, M. Buscemi, N. Scharf, V. Pirronello, F. Guarino, John Matthews, Peter Buchholz, M. S. A. B. Leão, C. Macolino, C. Hojvat, C. Morello, K. D. de Vries, D. Nosek, T. Yamamoto, R. M. Kieckhafer, C. Jarne, M. Tueros, J. Rautenberg, B. Revenu, Jan Ebr, M. Melissas, O. Wainberg, I.M. Brancus, D. Huber, S. Westerhoff, H. Glass, Marco Aglietta, W. C. Brown, A. Nelles, Jaime Alvarez-Muñiz, D. Schuster, M. A. Muller, Lu Lu, G. Marsella, D. Martraire, S. Gambetta, Peter L. Biermann, D. Harari, Alessandro Petrolini, B. Mitrica, M. Ludwig, J. Rosado, A. van Vliet, A. Tonachini, L. Nožka, A. Weindl, N. Hollon, V. Verzi, P. Brogueira, M. Urban, A. C. Rovero, C. Bleve, B. Keilhauer, V. H. Ponce, S. J. Sciutto, J. Schovancova, Paolo Privitera, L. Perrone, Jiri Chudoba, D. Torres Machado, H.O. Klages, G. Torralba Elipe, D. Kruppke-Hansen, B. Wundheiler, R. Krause, Gregory R Snow, Alina Mihaela Badescu, M. Oliveira, M. Ave, E. Trovato, J. Lozano Bahilo, Segev BenZvi, Corbin Covault, Maria-Teresa Dova, M. Gómez Berisso, R. C. Shellard, Azadeh Keivani, A. P. Ferguson, R. Alves Batista, C. Baus, A. Aminaei, Y. Petrov, J. Gitto, P. Hansen, A. Chiavassa, A. E. Herve, Lino Miramonti, Vincenzo Rizi, M. D. Rodríguez-Frías, Paul Sommers, R. Cester, B. J. Whelan, P. Gouffon, W. Rodrigues de Carvalho, M. Risse, D. Martello, M. Ziolkowski, O. Martínez Bravo, P. N. Dong, M. J. Cooper, F. Sánchez, M. Ambrosio, M. De Domenico, Jing Zhou, G. Toma, S. Mićanović, B. M. Baughman, L. R. Wiencke, T. A. Harrison, A. Porcelli, M. Tartare, J. W. Cronin, B. D. Fox, N. T. Thao, G. Parente, A. Gorgi, V. Marin, J. Espadanal, M. Palatka, P. W. Younk, A. Śmiałkowski, P. Pieroni, Peter Schiffer, V. Scherini, Nataliia Borodai, H. R. Marquez Falcon, Alejandro Almela, S. van Velzen, E. Menichetti, G. Matthiae, G. Varner, H. Spinka, Antonio Bueno, Sergio Pastor, I. M. Pepe, J. Oehlschläger, A. F. Barbosa, Maria Rita Coluccia, Miguel Mostafá, Dusan Mandat, Gualberto Avila, Ingomar Allekotte, Angela V. Olinto, M. Monasor, F. Arqueros, P. Necesal, P. Gonçalves, N. Palmieri, Markus Ahlers, J. K. Kulbartz, H. Rivera, E. Varela, N. Griffith, J. A.J. Matthews, Xavier Bertou, R. E. Burton, S. Jiraskova, T. Rossler, J. D. Swain, A. Menshikov, J. C. Marin, H. Schieler, A. Zepeda, R. Ulrich, Karl-Heinz Kampert, Antonella Castellina, E. M. Santos, Pedro Assis, A. Etchegoyen, K. Kadija, Carola Dobrigkeit, A. Insolia, M. Kleifges, D. Zavrtanik, I. Katkov, Javier Tiffenberg, J. Allen, E. Mayotte, R. Mussa, J. J. Beatty, P. Wahrlich, K. Louedec, J. Pȩkala, Mariangela Settimo, Iván Sidelnik, Alexey Yushkov, H. Dembinski, N. Fazzini, K. Weidenhaupt, J. Kleinfeller, Jose Chinellato, Alan Watson, M. I. Micheletti, T. Huege, A. Parra, S. J. De Jong, I. Zaw, O. Fratu, H. Cook, Jeffrey Brack, Olaf Scholten, P. Lautridou, M. Avenier, D. Thomas, Bruce R. Dawson, Y. N. Srivastava, Humberto Ibarguen Salazar, T. Hebbeker, Julien Aublin, A. Widom, D. LaHurd, F. Werner, P.O. Mazur, J. Alvarez Castillo, F. Sarazin, Elton J. G. Santos, K. Link, M. Prouza, Piotr Homola, P. Facal San Luis, Rúben Conceição, P. Abreu, M. Josebachuili, D. Ravignani, Miroslav Hrabovský, Daniel Kuempel, Carlos Escobar, R. F. Gamarra, A. Haungs, J. Neuser, J. R. T. de Mello Neto, E. J. Ahn, A. Letessier-Selvon, L. Molina-Bueno, E. Kemp, S. Le Coz, Luis A. Anchordoqui, J. L. Harton, D. Monnier Ragaigne, Lorenzo Cazon, S. Maldera, C. Pfendner, I. A. Minaya, A. Bellétoile, A. Schmidt, H. Martinez, O. Krömer, P. Mantsch, Z. Szadkowski, Ivone F. M. Albuquerque, Ke Fang, N. Pacheco, Lukas Middendorf, M. Platino, G. Navarra, J. Bäuml, C. E. Santo, Francisco J. Blanco, Johannes Schulz, G. Golup, N. Kunka, F. Gomez Albarracin, M. Pimenta, C. A. Moura, Brian Fick, H. Blümer, Balázs Kégl, Moritz Münchmeyer, G. Rodriguez Fernandez, A. D. Supanitsky, Hernán Asorey, Christopher B. Williams, G. C. Hill, M. Zimbres Silva, T. Šuša, I. C. Mariş, Ralph Engel, M. Plum, E. Petermann, D. Nitz, J. Stapleton, Miroslav Pech, J. Ridky, M. L. Díaz Castro, G. Farrar, S. Fliescher, A. Stutz, Pavel Horvath, Kai Daumiller, M. S. Sutherland, Rémi Bardenet, Petr Travnicek, P. Lebrun, L. Tomankova, Trent D. Grubb, Sofia Andringa, R. Meyhandan, M. Ortiz, R. J. Lauer, Juan Manuel Figueira, Roberta Colalillo, P. Ristori, A. G. Mariazzi, S. Jansen, B. García, Mario Scuderi, S. Messina, G. Salina, A. Curutiu, Tobias Winchen, R. López, Karen S. Caballero-Mora, Olivier Deligny, B. Caccianiga, S. Stanič, H. Schoorlemmer, P.F. Gómez Vitale, Martina Bohacova, Martin Erdmann, A. Dorofeev, Guenter Sigl, J. Sorokin, M. Blanco, C. E. Fracchiolla, Roger W Clay, D. D'Urso, L. Latronico, Corinne Berat, M. Giller, S. Navas, G. P. Guedes, K. B. Barber, M. Weber, U. Fröhlich, R. A. Vázquez, L. Valore, P. Karhan, P. A. Kasper, A. Filipčič, M. Straub, D. Maurel, Markus Roth, A. Shadkam, C. Timmermans, S. Petrera, J. R. Vázquez, A. F. Grillo, Juan Carlos D'Olivo, T. Pierog, J. Maller, Rossella Caruso, W. J. M. de Mello, A. Lucero, G. La Rosa, P. L. Ghia, Octavian Sima, J. G. Gonzalez, V. C. Holmes, D. Lebrun, R. Pesce, Jörg R. Hörandel, F. Salesa Greus, G. Cataldi, G. Garilli, D. Heck, L. Villaseñor, L. Martin, I. Lhenry-Yvon, S. Mollerach, E. Roulet, Marco Cilmo, B. Wilczyńska, W. Docters, Peter Gorham, R. Pelayo, L. Collica, S. Querchfeld, J. L. Kelley, E. D. Fraenkel, S. J. Saffi, L. Niemietz, L. del Peral, J. Roberts, O. Ravel, R. Piegaia, J. Rodriguez Martino, H. J. Mathes, G. De La Vega, O. Taşcǎu, J. Rodriguez Rojo, M. Szuba, F.G. Schröder, Enrique Zas, C. Di Giulio, Fernando Contreras, L. Caramete, M. Will, W. Tkaczyk, G. Yuan, S. Riggi, T. Antičić, J. Stasielak, S. Coutu, M. Lauscher, M. Pontz, A. C. Fauth, M. Stephan, H. Lyberis, Carla Bonifazi, Jose A. Bellido, B. Morales, Denise Boncioli, German Ros, B. Vargas Cárdenas, Maria Concetta Maccarone, T. Suomijärvi, J. Pallotta, E. J. Quel, Béatrice Fuchs, Niraj Dhital, I. Valiño, A. Filevich, P. T. Nhung, S. Grebe, R. Squartini, T. Paul, G. Medina-Tanco, G. van Aar, A. Criss, C. J. Todero Peixoto, M. Malacari, Yunrong Zhu, N. Krohm, Christian Glaser, H. Wilczyński, P. Billoir, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), PIERRE AUGER, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Research unit Astroparticle Physics, P., Abreu, M., Aglietta, M., Ahler, E. J., Ahn, I. F. M., Albuquerque, I., Allekotte, J., Allen, P., Allison, A., Almela, J., Alvarez Castillo, J., Alvarez Muñiz, R., Alves Batista, M., Ambrosio, A., Aminaei, L., Anchordoqui, S., Andringa, T., Antičić, C., Aramo, F., Arquero, H., Asorey, P., Assi, J., Aublin, M., Ave, M., Avenier, G., Avila, A. M., Badescu, K. B., Barber, A. F., Barbosa, R., Bardenet, B., Baughman, J., Bäuml, C., Bau, J. J., Beatty, K. H., Becker, A., Bellétoile, J. A., Bellido, S., Benzvi, C., Berat, X., Bertou, P. L., Biermann, P., Billoir, F., Blanco, M., Blanco, Bleve, Carla, H., Blümer, M., Boháčová, D., Boncioli, C., Bonifazi, R., Bonino, N., Borodai, J., Brack, I., Brancu, P., Brogueira, W. C., Brown, P., Buchholz, A., Bueno, L., Buroker, R. E., Burton, M., Buscemi, K. S., Caballero Mora, B., Caccianiga, L., Caccianiga, L., Caramete, R., Caruso, A., Castellina, G., Cataldi, L., Cazon, R., Cester, S. H., Cheng, A., Chiavassa, J. A., Chinellato, J., Chirino, J., Chudoba, M., Cilmo, R. W., Clay, Cocciolo, Giuseppe, R., Colalillo, L., Collica, Coluccia, MARIA RITA, R., Conceição, F., Contrera, H., Cook, M. J., Cooper, S., Coutu, C. E., Covault, A., Cri, J., Cronin, A., Curutiu, R., Dallier, B., Daniel, S., Dasso, K., Daumiller, B. R., Dawson, R. M., de Almeida, M., De Domenico, S. J., de Jong, G., De La Vega, W. J. M., de Mello, J. R. T., de Mello Neto, DE MITRI, Ivan, V., de Souza, K. D., de Vrie, L., del Peral, O., Deligny, H., Dembinski, N., Dhital, C., Di Giulio, J. C., Diaz, M. L., Díaz Castro, P. N., Diep, F., Diogo, C., Dobrigkeit, W., Docter, J. C., D’Olivo, P. N., Dong, A., Dorofeev, J. C., dos Anjo, M. T., Dova, D., D’Urso, J., Ebr, R., Engel, M., Erdmann, C. O., Escobar, J., Espadanal, A., Etchegoyen, P., Facal San Lui, H., Falcke, K., Fang, G., Farrar, A. C., Fauth, N., Fazzini, A. P., Ferguson, B., Fick, J. M., Figueira, A., Filevich, A., Filipčič, S., Fliescher, B. D., Fox, C. E., Fracchiolla, E. D., Fraenkel, O., Fratu, U., Fröhlich, B., Fuch, R., Gaior, R. F., Gamarra, S., Gambetta, B., García, S. T., Garcia Roca, D., Garcia Gamez, D., Garcia Pinto, G., Garilli, A., Gascon Bravo, H., Gemmeke, P. L., Ghia, M., Giller, J., Gitto, C., Glaser, H., Gla, G., Golup, F., Gomez Albarracin, M., Gómez Berisso, P. F., Gómez Vitale, P., Gonçalve, J. G., Gonzalez, B., Gookin, A., Gorgi, P., Gorham, P., Gouffon, S., Grebe, N., Griffith, A. F., Grillo, T. D., Grubb, Y., Guardincerri, F., Guarino, G. P., Guede, P., Hansen, D., Harari, T. A., Harrison, J. L., Harton, A., Haung, T., Hebbeker, D., Heck, A. E., Herve, G. C., Hill, C., Hojvat, N., Hollon, V. C., Holme, P., Homola, J. R., Hörandel, P., Horvath, M., Hrabovský, D., Huber, T., Huege, A., Insolia, S., Jansen, C., Jarne, S., Jiraskova, M., Josebachuili, K., Kadija, K. H., Kampert, P., Karhan, P., Kasper, I., Katkov, B., Kégl, B., Keilhauer, A., Keivani, J. L., Kelley, E., Kemp, R. M., Kieckhafer, H. O., Klage, M., Kleifge, J., Kleinfeller, J., Knapp, R., Krause, N., Krohm, O., Krömer, D., Kruppke Hansen, D., Kuempel, J. K., Kulbartz, N., Kunka, G., La Rosa, D., Lahurd, L., Latronico, R., Lauer, M., Lauscher, P., Lautridou, S., Le Coz, M. S. A. B., Leão, D., Lebrun, P., Lebrun, M. A., Leigui de Oliveira, A., Letessier Selvon, I., Lhenry Yvon, K., Link, R., López, A., Lopez Agüera, K., Louedec, J., Lozano Bahilo, L., Lu, A., Lucero, M., Ludwig, H., Lyberi, M. C., Maccarone, C., Macolino, M., Malacari, S., Maldera, J., Maller, D., Mandat, P., Mantsch, A. G., Mariazzi, J., Marin, V., Marin, I. C., Mariş, H. R., Marquez Falcon, Marsella, Giovanni, Martello, Daniele, L., Martin, H., Martinez, O., Martínez Bravo, D., Martraire, J. J., Masías Meza, H. J., Mathe, J., Matthew, J. A. J., Matthew, G., Matthiae, D., Maurel, D., Maurizio, E., Mayotte, P. O., Mazur, G., Medina Tanco, M., Melissa, D., Melo, E., Menichetti, A., Menshikov, S., Messina, R., Meyhandan, S., Mićanović, M. I., Micheletti, L., Middendorf, I. A., Minaya, L., Miramonti, B., Mitrica, L., Molina Bueno, S., Mollerach, M., Monasor, D., Monnier Ragaigne, F., Montanet, B., Morale, C., Morello, J. C., Moreno, M., Mostafá, C. A., Moura, M. A., Muller, G., Müller, M., Münchmeyer, R., Mussa, G., Navarra, J. L., Navarro, S., Nava, P., Necesal, L., Nellen, A., Nelle, J., Neuser, P. T., Nhung, M., Niechciol, L., Niemietz, N., Nierstenhoefer, T., Niggemann, D., Nitz, D., Nosek, L., Nožka, J., Oehlschläger, A., Olinto, M., Oliveira, M., Ortiz, N., Pacheco, D., Pakk Selmi Dei, M., Palatka, J., Pallotta, N., Palmieri, G., Parente, A., Parra, S., Pastor, T., Paul, M., Pech, J., Pe¸kala, R., Pelayo, I. M., Pepe, Perrone, Lorenzo, R., Pesce, E., Petermann, S., Petrera, A., Petrolini, Y., Petrov, C., Pfendner, R., Piegaia, T., Pierog, P., Pieroni, M., Pimenta, V., Pirronello, M., Platino, M., Plum, V. H., Ponce, M., Pontz, A., Porcelli, P., Privitera, M., Prouza, E. J., Quel, S., Querchfeld, J., Rautenberg, O., Ravel, D., Ravignani, B., Revenu, J., Ridky, S., Riggi, M., Risse, P., Ristori, H., Rivera, V., Rizi, J., Robert, W., Rodrigues de Carvalho, I., Rodriguez Cabo, G., Rodriguez Fernandez, J., Rodriguez Martino, J., Rodriguez Rojo, M. D., Rodríguez Fría, G., Ro, J., Rosado, T., Rossler, M., Roth, B., Rouillé d’Orfeuil, E., Roulet, A. C., Rovero, C., Rühle, S. J., Saffi, A., Saftoiu, F., Salamida, H., Salazar, F., Salesa Greu, G., Salina, F., Sánchez, C. E., Santo, E., Santo, E. M., Santo, F., Sarazin, B., Sarkar, R., Sato, N., Scharf, Scherini, Viviana, H., Schieler, P., Schiffer, A., Schmidt, O., Scholten, H., Schoorlemmer, J., Schovancova, P., Schovánek, F. G., Schröder, J., Schulz, D., Schuster, S. J., Sciutto, M., Scuderi, A., Segreto, M., Settimo, A., Shadkam, R. C., Shellard, I., Sidelnik, G., Sigl, O., Sima, A., Śmiałkowski, R., Šmída, G. R., Snow, P., Sommer, J., Sorokin, H., Spinka, R., Squartini, Y. N., Srivastava, S., Stanič, J., Stapleton, J., Stasielak, M., Stephan, M., Straub, A., Stutz, F., Suarez, T., Suomijärvi, A. D., Supanitsky, T., Šuša, M. S., Sutherland, J., Swain, Z., Szadkowski, M., Szuba, A., Tapia, M., Tartare, O., Taşcău, R., Tcaciuc, N. T., Thao, D., Thoma, J., Tiffenberg, C., Timmerman, W., Tkaczyk, C. J., Todero Peixoto, G., Toma, L., Tomankova, B., Tomé, A., Tonachini, G., Torralba Elipe, D., Torres Machado, P., Travnicek, D. B., Tridapalli, E., Trovato, M., Tuero, R., Ulrich, M., Unger, M., Urban, J. F., Valdés Galicia, I., Valiño, L., Valore, G., van Aar, A. M., van den Berg, S., van Velzen, A., van Vliet, E., Varela, B., Vargas Cárdena, G., Varner, J. R., Vázquez, R. A., Vázquez, D., Veberič, V., Verzi, J., Vicha, M., Videla, L., Villaseñor, H., Wahlberg, P., Wahrlich, O., Wainberg, D., Walz, A. A., Watson, M., Weber, K., Weidenhaupt, A., Weindl, F., Werner, S., Westerhoff, B. J., Whelan, A., Widom, G., Wieczorek, L., Wiencke, B., Wilczyńska, H., Wilczyński, M., Will, C., William, T., Winchen, B., Wundheiler, T., Yamamoto, T., Yapici, P., Younk, G., Yuan, A., Yushkov, B., Zamorano Garcia, E., Za, D., Zavrtanik, M., Zavrtanik, I., Zaw, A., Zepeda, J., Zhou, Y., Zhu, M., Zimbres Silva, M., Ziolkowski, P. Abreu, M. Aglietta, M. Ahler, E.J. Ahn, I.F.M. Albuquerque, I. Allekotte, J. Allen, P. Allison, A. Almela, J. Alvarez Castillo, J. Alvarez-Muñiz, R. Alves Batista, M. Ambrosio, A. Aminaei, L. Anchordoqui, S. Andringa, T. Antičić, C. Aramo, F. Arquero, H. Asorey, P. Assi, J. Aublin, M. Ave, M. Avenier, G. Avila, A.M. Badescu, K.B. Barber, A.F. Barbosa, R. Bardenet, B. Baughman, J. Bäuml, C. Bau, J.J. Beatty, K.H. Becker, A. Bellétoile, J.A. Bellido, S. BenZvi, C. Berat, X. Bertou, P.L. Biermann, P. Billoir, F. Blanco, M. Blanco, C. Bleve, H. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, R. Bonino, N. Borodai, J. Brack, I. Brancu, P. Brogueira, W.C. Brown, P. Buchholz, A. Bueno, L. Buroker, R.E. Burton, M. Buscemi, K.S. Caballero-Mora, B. Caccianiga, L. Caccianiga, L. Caramete, R. Caruso, A. Castellina, G. Cataldi, L. Cazon, R. Cester, S.H. Cheng, A. Chiavassa, J.A. Chinellato, J. Chirino, J. Chudoba, M. Cilmo, R.W. Clay, G. Cocciolo, R. Colalillo, L. Collica, M.R. Coluccia, R. Conceição, F. Contrera, H. Cook, M.J. Cooper, S. Coutu, C.E. Covault, A. Cri, J. Cronin, A. Curutiu, R. Dallier, B. Daniel, S. Dasso, K. Daumiller, B.R. Dawson, R.M. de Almeida, M. De Domenico, S.J. de Jong, G. De La Vega, W.J.M. de Mello, J.R.T. de Mello Neto, I. De Mitri, V. de Souza, K.D. de Vrie, L. del Peral, O. Deligny, H. Dembinski, N. Dhital, C. Di Giulio, J.C. Diaz, M.L. Díaz Castro, P.N. Diep, F. Diogo, C. Dobrigkeit, W. Docter, J.C. D’Olivo, P.N. Dong, A. Dorofeev, J.C. dos Anjo, M.T. Dova, D. D’Urso, J. Ebr, R. Engel, M. Erdmann, C.O. Escobar, J. Espadanal, A. Etchegoyen, P. Facal San Lui, H. Falcke, K. Fang, G. Farrar, A.C. Fauth, N. Fazzini, A.P. Ferguson, B. Fick, J.M. Figueira, A. Filevich, A. Filipčič, S. Fliescher, B.D. Fox, C.E. Fracchiolla, E.D. Fraenkel, O. Fratu, U. Fröhlich, B. Fuch, R. Gaior, R.F. Gamarra, S. Gambetta, B. García, S.T. Garcia Roca, D. Garcia-Gamez, D. Garcia-Pinto, G. Garilli, A. Gascon Bravo, H. Gemmeke, P.L. Ghia, M. Giller, J. Gitto, C. Glaser, H. Gla, G. Golup, F. Gomez Albarracin, M. Gómez Berisso, P.F. Gómez Vitale, P. Gonçalve, J.G. Gonzalez, B. Gookin, A. Gorgi, P. Gorham, P. Gouffon, S. Grebe, N. Griffith, A.F. Grillo, T.D. Grubb, Y. Guardincerri, F. Guarino, G.P. Guede, P. Hansen, D. Harari, T.A. Harrison, J.L. Harton, A. Haung, T. Hebbeker, D. Heck, A.E. Herve, G.C. Hill, C. Hojvat, N. Hollon, V.C. Holme, P. Homola, J.R. Hörandel, P. Horvath, M. Hrabovský, D. Huber, T. Huege, A. Insolia, S. Jansen, C. Jarne, S. Jiraskova, M. Josebachuili, K. Kadija, K.H. Kampert, P. Karhan, P. Kasper, I. Katkov, B. Kégl, B. Keilhauer, A. Keivani, J.L. Kelley, E. Kemp, R.M. Kieckhafer, H.O. Klage, M. Kleifge, J. Kleinfeller, J. Knapp, R. Krause, N. Krohm, O. Krömer, D. Kruppke-Hansen, D. Kuempel, J.K. Kulbartz, N. Kunka, G. La Rosa, D. LaHurd, L. Latronico, R. Lauer, M. Lauscher, P. Lautridou, S. Le Coz, M.S.A.B. Leão, D. Lebrun, P. Lebrun, M.A. Leigui de Oliveira, A. Letessier-Selvon, I. Lhenry-Yvon, K. Link, R. López, A. Lopez Agüera, K. Louedec, J. Lozano Bahilo, L. Lu, A. Lucero, M. Ludwig, H. Lyberi, M.C. Maccarone, C. Macolino, M. Malacari, S. Maldera, J. Maller, D. Mandat, P. Mantsch, A.G. Mariazzi, J. Marin, V. Marin, I.C. Mariş, H.R. Marquez Falcon, G. Marsella, D. Martello, L. Martin, H. Martinez, O. Martínez Bravo, D. Martraire, J.J. Masías Meza, H.J. Mathe, J. Matthew, J.A.J. Matthew, G. Matthiae, D. Maurel, D. Maurizio, E. Mayotte, P.O. Mazur, G. Medina-Tanco, M. Melissa, D. Melo, E. Menichetti, A. Menshikov, S. Messina, R. Meyhandan, S. Mićanović, M.I. Micheletti, L. Middendorf, I.A. Minaya, L. Miramonti, B. Mitrica, L. Molina-Bueno, S. Mollerach, M. Monasor, D. Monnier Ragaigne, F. Montanet, B. Morale, C. Morello, J.C. Moreno, M. Mostafá, C.A. Moura, M.A. Muller, G. Müller, M. Münchmeyer, R. Mussa, G. Navarra, J.L. Navarro, S. Nava, P. Necesal, L. Nellen, A. Nelle, J. Neuser, P.T. Nhung, M. Niechciol, L. Niemietz, N. Nierstenhoefer, T. Niggemann, D. Nitz, D. Nosek, L. Nožka, J. Oehlschläger, A. Olinto, M. Oliveira, M. Ortiz, N. Pacheco, D. Pakk Selmi-Dei, M. Palatka, J. Pallotta, N. Palmieri, G. Parente, A. Parra, S. Pastor, T. Paul, M. Pech, J. Pe¸kala, R. Pelayo, I.M. Pepe, L. Perrone, R. Pesce, E. Petermann, S. Petrera, A. Petrolini, Y. Petrov, C. Pfendner, R. Piegaia, T. Pierog, P. Pieroni, M. Pimenta, V. Pirronello, M. Platino, M. Plum, V.H. Ponce, M. Pontz, A. Porcelli, P. Privitera, M. Prouza, E.J. Quel, S. Querchfeld, J. Rautenberg, O. Ravel, D. Ravignani, B. Revenu, J. Ridky, S. Riggi, M. Risse, P. Ristori, H. Rivera, V. Rizi, J. Robert, W. Rodrigues de Carvalho, I. Rodriguez Cabo, G. Rodriguez Fernandez, J. Rodriguez Martino, J. Rodriguez Rojo, M.D. Rodríguez-Fría, G. Ro, J. Rosado, T. Rossler, M. Roth, B. Rouillé-d’Orfeuil, E. Roulet, A.C. Rovero, C. Rühle, S.J. Saffi, A. Saftoiu, F. Salamida, H. Salazar, F. Salesa Greu, G. Salina, F. Sánchez, C.E. Santo, E. Santo, E.M. Santo, F. Sarazin, B. Sarkar, R. Sato, N. Scharf, V. Scherini, H. Schieler, P. Schiffer, A. Schmidt, O. Scholten, H. Schoorlemmer, J. Schovancova, P. Schovánek, F.G. Schröder, J. Schulz, D. Schuster, S.J. Sciutto, M. Scuderi, A. Segreto, M. Settimo, A. Shadkam, R.C. Shellard, I. Sidelnik, G. Sigl, O. Sima, A. Śmiałkowski, R. Šmída, G.R. Snow, P. Sommer, J. Sorokin, H. Spinka, R. Squartini, Y.N. Srivastava, S. Stanič, J. Stapleton, J. Stasielak, M. Stephan, M. Straub, A. Stutz, F. Suarez, T. Suomijärvi, A.D. Supanitsky, T. Šuša, M.S. Sutherland, J. Swain, Z. Szadkowski, M. Szuba, A. Tapia, M. Tartare, O. Taşcău, R. Tcaciuc, N.T. Thao, D. Thoma, J. Tiffenberg, C. Timmerman, W. Tkaczyk, C.J. Todero Peixoto, G. Toma, L. Tomankova, B. Tomé, A. Tonachini, G. Torralba Elipe, D. Torres Machado, P. Travnicek, D.B. Tridapalli, E. Trovato, M. Tuero, R. Ulrich, M. Unger, M. Urban, J.F. Valdés Galicia, I. Valiño, L. Valore, G. van Aar, A.M. van den Berg, S. van Velzen, A. van Vliet, E. Varela, B. Vargas Cárdena, G. Varner, J.R. Vázquez, R.A. Vázquez, D. Veberič, V. Verzi, J. Vicha, M. Videla, L. Villaseñor, H. Wahlberg, P. Wahrlich, O. Wainberg, D. Walz, A.A. Watson, M. Weber, K. Weidenhaupt, A. Weindl, F. Werner, S. Westerhoff, B.J. Whelan, A. Widom, G. Wieczorek, L. Wiencke, B. Wilczyńska, H. Wilczyński, M. Will, C. William, T. Winchen, B. Wundheiler, T. Yamamoto, T. Yapici, P. Younk, G. Yuan, A. Yushkov, B. Zamorano Garcia, E. Za, D. Zavrtanik, M. Zavrtanik, I. Zaw, A. Zepeda, J. Zhou, Y. Zhu, M. Zimbres Silva, M. Ziolkowski, J., Alvarez Mu?iz, T., Anti?i?, Aramo, Carla, J., B?uml, A., Bell?toile, C., Bleve, H., Bl?mer, M., Boh??ov?, Buscemi, Mario, Cilmo, Marco, G., Cocciolo, Colalillo, Roberta, M. R., Coluccia, R., Concei??o, I., De Mitri, M. L., D?az Castro, J. C., D?olivo, D., D'Urso, A., Filip?i?, U., Fr?hlich, B., Garc?a, M., G?mez Berisso, P. F., G?mez Vitale, P., Gon?alve, Guarino, Fausto, J. R., H?randel, M., Hrabovsk?, B., K?gl, O., Kr?mer, M. S. A. B., Le?o, R., L?pez, A., Lopez Ag?era, I. C., Mari?, G., Marsella, D., Martello, O., Mart?nez Bravo, J. J., Mas?as Meza, S., Mi?anovi?, M., Mostaf?, G., M?ller, M., M?nchmeyer, L., No?ka, J., Oehlschl?ger, J., Pe?kala, L., Perrone, M. D., Rodr?guez Fr?a, B., Rouill? d?Orfeuil, C., R?hle, F., S?nchez, V., Scherini, P., Schov?nek, F. G., Schr?der, A., ?mia?kowski, R., ?m?da, S., Stani?, T., Suomij?rvi, T., ?u?a, O., Ta?c?u, B., Tom?, J. F., Vald?s Galicia, I., Vali?o, Valore, Laura, B., Vargas C?rdena, J. R., V?zquez, R. A., V?zquez, D., Veberi?, L., Villase?or, B., Wilczy?ska, and H., Wilczy?ski
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[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Atmospheric Monitoring ,Satellites ,Infrared ,Astronomy ,Cloud cover ,FOS: Physical sciences ,Atmospheric monitoring ,01 natural sciences ,Ciencias de la Tierra y relacionadas con el Medio Ambiente ,Auger ,purl.org/becyt/ford/1 [https] ,purl.org/becyt/ford/1.5 [https] ,Observatory ,Clouds ,0103 physical sciences ,Extensive air showers ,010306 general physics ,DETECTOR ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Image resolution ,Ciencias Exactas ,Physics ,Pierre Auger Observatory ,UHE Cosmic Rays, atmosphere ,010308 nuclear & particles physics ,[SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Física ,Astronomy and Astrophysics ,Ultra-high energy cosmic rays ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,INFRAVERMELHO ,Experimental High Energy Physics ,ComputingMethodologies_DOCUMENTANDTEXTPROCESSING ,Pierre Auger observatory ,ultra-high energy cosmic rays ,extensive air showers ,atmospheric monitoring ,clouds ,satellites ,Física nuclear ,Satellite ,Central Laser Facility ,Extensive Air Showers ,Astrophysics - Instrumentation and Methods for Astrophysics ,Meteorología y Ciencias Atmosféricas ,SYSTEM ,CIENCIAS NATURALES Y EXACTAS - Abstract
We describe a new method of identifying night-time clouds over the Pierre Auger Observatory using infrared data from the Imager instruments on the GOES-12 and GOES-13 satellites. We compare cloud. identifications resulting from our method to those obtained by the Central Laser Facility of the Auger Observatory. Using our new method we can now develop cloud probability maps for the 3000 km(2) of the Pierre Auger Observatory twice per hour with a spatial resolution of similar to 2.4 km by similar to 5.5 km. Our method could also be applied to monitor cloud cover for other ground-based observatories and for space-based observatories. (C) 2013 Elsevier B.V. All rights reserved., The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and adminis- trative staff in Malargüe. We are very grateful to the following agencies and organiza- tions for financial support: Comisión Nacional de Energía Atómica, Fundación Antorchas, Gobierno De La Provincia de Mendoza, Municipalidad de Malargüe, NDM Holdings and Valle Las Leñas, in gratitude for their continuing cooperation over land access, Argentina; the Australian Research Council; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Financiadora de Estudos e Projetos (FINEP), Fundação de Amparo à Pesquisa do Estado de Rio de Janeiro (FAPERJ), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Ministério de Ciência e Tecnolo- gia (MCT), Brazil; AVCR AV0Z10100502 and AV0Z10100522, GAAV KJB100100904, MSMT-CR LA08016, LG11044, MEB111003, MSM0021620859, LA08015, TACR TA01010517 and GA UK 119810, Czech Republic; Centre de Calcul IN2P3/CNRS, Centre Na- tional de la Recherche Scientifique (CNRS), Conseil Régional Ile-de- France, Département Physique Nucléaire et Corpusculaire (PNC- IN2P3/CNRS), Département Sciences de l’Univers (SDU-INSU/ CNRS), France; Bundesministerium für Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Finanzministeri- um Baden-Württemberg, Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF), Ministerium für Wissenschaft und Forschung, Nordrhein-Westfalen, Ministerium für Wissenschaft, Forschung und Kunst, Baden-Württemberg, Germany; Istituto Nazionale di Fisica Nucleare (INFN), Ministero dell’Istruzione, dell’Università e della Ricerca (MIUR), Italy; Consejo Nacional de Ciencia y Tecnología (CONACYT), Mexico; Ministerie van Ond- erwijs, Cultuur en Wetenschap, Nederlandse Organisatie voor Wet- enschappelijk Onderzoek (NWO), Stichting voor Fundamenteel Onderzoek der Materie (FOM), Netherlands; Ministry of Science and Higher Education, Grant Nos. N N202 200239 and N N202 207238, Poland; Portuguese national funds and FEDER funds with- in COMPETE - Programa Operacional Factores de Competitividade through Fundação para a Ciência e a Tecnologia, Portugal; Roma- nian Authority for Scientific Research ANCS, CNDI-UEFISCDI part- nership projects nr.20/2012 and nr.194/2012, project nr.1/ ASPERA2/2012 ERA-NET and PN-II-RU-PD-2011-3-0145-17, Roma- nia; Ministry for Higher Education, Science, and Technology, Slove- nian Research Agency, Slovenia; Comunidad de Madrid, FEDER funds, Ministerio de Ciencia e Innovación and Consolider-Ingenio 2010 (CPAN), Xunta de Galicia, Spain; The Leverhulme Foundation, Science and Technology Facilities Council, United Kingdom; Department of Energy, Contract Nos. DE-AC02-07CH11359, DE- FR02-04ER41300, DE-FG02-99ER41107, National Science Founda- tion, Grant No. 0450696, The Grainger Foundation USA; NAFO- STED, Vietnam; Marie Curie-IRSES/EPLANET, European Particle Physics Latin American Network, European Union 7th Framework Program, Grant No. PIRSES-2009-GA-246806; and UNESCO. We would like to thank the former Michigan Tech students: Nathan Kelley-Hoskins, Kyle Luck and Arin Nelson for their impor- tant contribution to the development of this paper. We would like to thank NOAA for the GOES satellite data that we freely down- loaded from their website. Also, we would like to mention in these acknowledgments Dr. Steve Ackerman and Dr. Tony Schreiner for very valuable conversations
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- 2013
- Full Text
- View/download PDF
4. First detection of the 448 GHz H2O transition in space
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F. Rico, Dimitra Rigopoulou, Sara Cazzoli, Jesús Martín-Pintado, Luis Colina, Miguel Pereira-Santaella, T. Storchi Bergmann, Santiago García-Burillo, Santiago Arribas, Almudena Alonso-Herrero, Eduardo González-Alfonso, Antonio Usero, Ministerio de Educación y Ciencia (España), European Commission, and National Aeronautics and Space Administration (US)
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Infrared ,FOS: Physical sciences ,Flux ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Submillimeter Array ,law.invention ,galaxies [Infrared] ,law ,Infravermelho ,0103 physical sciences ,ISM [Galaxies] ,Maser ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,molecules [ISM] ,Galaxies: nuclei ,Line (formation) ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Infrared: galaxies ,Meio interestelar ,Astrophysics - Astrophysics of Galaxies ,ISM: molecules ,Galaxy ,Água ,Galaxies: ISM ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Excited state ,nuclei [Galaxies] ,Millimeter ,Astrophysics::Earth and Planetary Astrophysics ,Nucleo galatico - Abstract
Pereira-Santaella, M. et. al., We present the first detection of the ortho-H2O 423 - 330 transition at 448 GHz in space. We observed this transition in the local (z = 0.010) luminous infrared (IR) galaxy ESO 320-G030 (IRAS F11506-3851) using the Atacama Large Millimeter/submillimeter Array (ALMA). The water 423 - 330 emission, which originates in the highly obscured nucleus of this galaxy, is spatially resolved over a region of ~65 pc in diameter and shows a regular rotation pattern compatible with the global molecular and ionized gas kinematics. The line profile is symmetric and well fitted by a Gaussian with an integrated flux of 37.0 ± 0.7 Jy km s-1. Models predict this water transition as a potential collisionally excited maser transition. On the contrary, in this galaxy, we find that the 423 - 330 emission is primarily excited by the intense far-IR radiation field present in its nucleus. According to our modeling, this transition is a probe of deeply buried galaxy nuclei thanks to the high dust optical depths (τ100μm> 1, NH> 1024 cm-2) required to efficiently excite it. © ESO, 2017., M.P.S. acknowledges support from STFC through grant ST/N000919/1, the John Fell Oxford University Press (OUP) Research Fund and the University of Oxford. E.G.S., A.U., S.G.B., J.M.P., L.C., A.A.H., S.A., S.C., and F.R.V. acknowledge financial support by the Spanish MEC under grants ESP2015-65597-C4-1-R, AYA2012-32295, ESP2015-68694, AYA2013-42227-P and AYA2015-64346-C2-1-P, which is partly funded by the FEDER programme. E.G.A. a Research Associate at the Harvard-Smithsonian CfA and acknowledges support by NASA grant ADAP NNX15AE56G.
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- 2017
5. The AKARI far-infrared all-sky survey maps
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Masahiro Tanaka, Makoto Hattori, Norio Ikeda, S. Komugi, Takao Nakagawa, Yasuo Doi, Yoshimi Kitamura, Takahiro Morishima, Takafumi Ootsubo, Satoshi Takita, Shuji Matsuura, Yuji Chinone, M. Etxaluze, Ko Arimatsu, Elysandra F. Cypriano, Mitsunobu Kawada, Daisuke Kato, and Glenn J. White
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Point source ,media_common.quotation_subject ,Interstellar cloud ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,infrared: galaxies ,Far infrared ,surveys ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Image resolution ,Galaxy: general ,Astrophysics::Galaxy Astrophysics ,media_common ,ISM: general ,Physics ,Luminous infrared galaxy ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Interstellar medium ,atlases ,Space and Planetary Science ,Sky ,Astrophysics of Galaxies (astro-ph.GA) ,INFRAVERMELHO ,Cirrus ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
著者人数: 18名, Accepted: 2015-03-20, 資料番号: SA1150116000
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- 2015
6. Planck intermediate results: XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization
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Ade, P. A. R., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Zotti, G., Delabrouille, J., Désert, F. -X., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, Guilaine, Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J.F., Maffei, B., Magalhães, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Pietrobon, D., Plaszczynski, Stéphane, Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Salerno, E., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, Radek, Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wandelt, B. D., Zacchei, A., Zonca, A., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), PLANCK, European Space Agency, European Research Council, Centre National de la Recherche Scientifique (France), Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Fundação para a Ciência e a Tecnologia (Portugal), Science Foundation Ireland, Research Council of Norway, DTU Space (Denmark), Federal Ministry of Education and Research (Germany), Academy of Finland, Center for Science (Finland), Junta de Andalucía, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), Science and Technology Facilities Council (UK), UK Space Agency, Consiglio Nazionale delle Ricerche, National Aeronautics and Space Administration (US), Department of Energy (US), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Helsinki Institute of Physics, Ade, P, Alves, M, Aniano, G, Armitage-Caplan, C, Arnaud, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bock, J, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Burigana, C, Cardoso, J, Catalano, A, Chamballu, A, Chiang, H, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Zotti, G, Delabrouille, J, Desert, F, Dickinson, C, Diego, J, Donzelli, S, Dore, O, Douspis, M, Dunkley, J, Dupac, X, Ensslin, T, Eriksen, H, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Harrison, D, Helou, G, Hernandez-Monteagudo, C, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Jaffe, A, Jaffe, T, Jones, W, Keihanen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lawrence, C, Leahy, J, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maffei, B, Magalhaes, A, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Noviello, F, Novikov, D, Novikov, I, Oppermann, N, Oxborrow, C, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Popa, L, Pratt, G, Rachen, J, Reach, W, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rubino-Martin, J, Rusholme, B, Salerno, E, Sandri, M, Savini, G, Scott, D, Spencer, L, Stolyarov, V, Stompor, R, Sudiwala, R, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wandelt, B, Zacchei, A, Zonca, A, Ade, P. A. R., Alves, M. I. R., Aniano, G., Armitage Caplan, C., Arnaud, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Zotti, G., Delabrouille, J., Désert, F. X., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Magalhães, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Salerno, E., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wandelt, B. D., Zacchei, A., Zonca, A., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)
- Subjects
Astronomy ,WMAP OBSERVATIONS ,Astrophysics ,7. Clean energy ,law.invention ,law ,Polarization ,Astrophysics::Solar and Stellar Astrophysics ,general [radiation mechanisms] ,QB ,Physics ,Infrared: ISM ,general [ISM] ,FOREGROUND EMISSION ,general [mechanisms] ,ISM [infrared] ,Polarization (waves) ,DMR SKY MAPS ,CMB cold spot ,Synchrotron ,INFRAVERMELHO ,ComputingMethodologies_DOCUMENTANDTEXTPROCESSING ,symbols ,Spectral energy distribution ,[SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,Astrophysics::Earth and Planetary Astrophysics ,INTERSTELLAR DUST ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,COMPONENT SEPARATION ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galaxy: general ,ISM: general ,Radiation mechanisms: general ,Submillimeter: ISM ,NO ,symbols.namesake ,Settore FIS/05 - Astronomia e Astrofisica ,Planck ,ISM [submillimeter] ,general [Galaxy] ,Astrophysics::Galaxy Astrophysics ,Cosmic dust ,SUBMILLIMETER POLARIZATION ,MAGNETIC NANOPARTICLES ,polarization ,SPINNING DUST ,Astronomy and Astrophysics ,Astronomy and Astrophysic ,115 Astronomy, Space science ,Astrophysics - Astrophysics of Galaxies ,MICROWAVE-ANISOTROPY-PROBE ,Interstellar medium ,radiation ,polarization / ISM: general / Galaxy: general / radiation mechanisms: general / submillimeter: ISM / infrared: ISM ,[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,Space and Planetary Science ,13. Climate action ,Astrophysics of Galaxies (astro-ph.GA) ,H-ALPHA EMISSION ,Microwave - Abstract
Interstellar and circumstellar matter.-- et al., Planck has mapped the intensity and polarization of the sky at microwave frequencies with unprecedented sensitivity. We use these data to characterize the frequency dependence of dust emission. We make use of the Planck 353 GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the Planck and WMAP data at 12 frequencies from 23 to 353 GHz, over circular patches with 10° radius. The cross-correlation analysis is performed for both intensity and polarization data in a consistent manner. The results are corrected for the chance correlation between the templates and the anisotropies of the cosmic microwave background. We use a mask that focuses our analysis on the diffuse interstellar medium at intermediate Galactic latitudes. We determine the spectral indices of dust emission in intensity and polarization between 100 and 353 GHz, for each sky patch. Both indices are found to be remarkably constant over the sky. The mean values, 1.59 ± 0.02 for polarization and 1.51 ± 0.01 for intensity, for a mean dust temperature of 19.6 K, are close, but significantly different (3.6σ). We determine the mean spectral energy distribution (SED) of the microwave emission, correlated with the 353 GHz dust templates, by averaging the results of the correlation over all sky patches. We find that the mean SED increases for decreasing frequencies at ν< 60 GHz for both intensity and polarization. The rise of the polarization SED towards low frequencies may be accounted for by a synchrotron component correlated with dust, with no need for any polarization of the anomalous microwave emission. We use a spectral model to separate the synchrotron and dust polarization and to characterize the spectral dependence of the dust polarization fraction. The polarization fraction (p) of the dust emission decreases by (21 ± 6)% from 353 to 70 GHz. We discuss this result within the context of existing dust models. The decrease in p could indicate differences in polarization efficiency among components of interstellar dust (e.g., carbon versus silicate grains). Our observational results provide inputs to quantify and optimize the separation between Galactic and cosmological polarization., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and J.A. (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.
- Published
- 2015
- Full Text
- View/download PDF
7. A Spectral Atlas of HII Galaxies in the Near-Infrared
- Author
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Ruth Gruenwald, Alberto Rodríguez-Ardila, Suzi Diniz, Lucimara P. Martins, and Ronaldo Eustáquio de Souza
- Subjects
Luminous infrared galaxy ,Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar population ,Radio galaxy ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Disc galaxy ,Galaxy ,Space and Planetary Science ,INFRAVERMELHO ,Elliptical galaxy ,Spectral atlas ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Recent models show that TP-AGB stars should dominate the NIR spectra of populations 0.3 to 2 Gyr old, leaving unique signatures that can be used to detect young/intermediate stellar population in galaxies. However, no homogeneous database of star-forming galaxies is available in the NIR to fully explore these results. With this in mind, we study the NIR spectra of a sample of 23 HII and starburst galaxies, aimed at characterizing the most prominent spectral features and continuum shape in the 0.8-2.4 micron region of these objects. Spectral indices are derived for the relevant absorption lines/bands and a comparison with optical indices of the same sample available in the literature is made. We found no correlation between the optical and the NIR indexes. This is probably due to the differences in aperture between these two sets of data. That result is further supported by the absence or weakness of emission lines in the NIR for a subsample galaxies, while in the optical the emission lines are strong and clear, which means that the ionisation source in many of these galaxies is not nuclear, but circumnuclear or located in hot spots. We detected important signatures predicted for a stellar population dominated by the TP-AGBs, like CN 1.1 micron and CO 2.3 micron. In at least one galaxy (NGC 4102) the CN band at 1.4 micron was detected for the first time. We also detect TiO and ZrO bands that have never been reported before in extragalactic sources. The shape of the continuum emission is found to be strongly correlated to the presence/lack of emission lines. An observational template for the star-forming galaxies is derived to be used as a benchmark of stellar population(s) in starburst galaxies against which to compare near-IR spectroscopy of different types of galaxies, especially those with AGN activity and/or those at high-redshift., 21 pages (main) + 28 pages (appendix), 6 figures + 28 figures (appendix), accepted by MNRAS
- Published
- 2013
8. Aplicação da espectroscopia no infravermelho e difração de raio-X na determinação de sacarina em adoçantes líquidos artificiais pelo método volumétrico com Ag+
- Author
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Jhonatas de Souza Lima, Mauro Cesar Dias, and Tulio Matencio
- Subjects
Physics ,raio-X ,saccharin ,General Physics and Astronomy ,General Chemistry ,sacarina ,X-ray ,lcsh:Chemistry ,lcsh:QD1-999 ,adoçantes ,infravermelho ,infrared ,sweeteners ,Nuclear chemistry - Abstract
O uso de adoçantes líquidos com sacarina sódica é uma questão de saúde pública pela relação com obesidade e fonte de sódio. Os níveis de sacarina foram avaliados em quatro marcas de diferentes fabricantes em amostras adquiridas no comércio de Vitória/ES, entre os anos de 2006 e 2008. Foram encontrados níveis com valores entre 260 e 505 vezes acima da Resolução-RDC N0 8, 25/03/2008 (ANVISA), que é de 0,015 g/100 mL para sacarina e seus sais derivados. O perfil das amostras cristalizadas dos adoçantes foram avaliados por espectroscopia na região do infravermelho e por difração de raio-X de pó. A seletividade do método clássico de precipitação com AgNO3 também foi verificada por essas técnicas aplicadas nos precipitados de sacarinato de prata. The use of sweeteners liquid from saccharin sodium is a public health issue by the relationship with obesity and a source of sodium. The levels of saccharin were studied in four different manufacturers in samples from trade in Vitória / ES, between years 2006 and 2008. Levels were found with values between 260 and 505 above of Resolution RDC N0-8, 25/03/2008 from ANVISA, which is 0,015 g/100 mL for saccharin and its salts. The profile of the crystallized sweeteners samples were evaluated by infrared spectroscopy and powder X-ray diffraction. The selectivity of the classic method of precipitation with AgNO3 was also verified by the techniques applied in silver saccharinate precipitates.
- Published
- 2010
9. Comparing pure Yang-Mills SU(2) and SU(3) propagators
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Paulo J. Silva, Tereza Mendes, Attilio Cucchieri, and Orlando Oliveira
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Physics ,Quantum chromodynamics ,Nuclear and High Energy Physics ,High Energy Physics::Lattice ,High Energy Physics::Phenomenology ,Lattice field theory ,General Physics and Astronomy ,Yang–Mills existence and mass gap ,Lattice QCD ,Yang–Mills theory ,High Energy Physics::Theory ,Hamiltonian lattice gauge theory ,Lattice gauge theory ,INFRAVERMELHO ,Gauge theory ,Mathematical physics - Abstract
The infrared behavior of gluon and ghost propagators in Yang–Mills gauge theories is of central importance for the understanding of confinement in QCD. While analytic studies using Schwinger–Dyson equations predict the same infrared exponents for the SU(2) and SU(3) gauge groups, lattice simulations usually assume that the two cases are different, although their qualitative infrared features may be the same. We carry out a comparative study of lattice (Landau) propagators for both gauge groups. Our data were especially produced with equivalent lattice parameters to allow a careful comparison of the two cases.
- Published
- 2007
10. Aplicações da espectroscopia no infravermelho no controle de qualidade de medicamentos contendo diclofenaco de potássio. Parte I: dosagem por regressão multivariada
- Author
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Jorcen Simon de Souza and Marco Flôres Ferrão
- Subjects
Pharmacology ,Physics ,Quimiometria ,Diclofenac ,Controle de qualidade ,Non-steroidal anti-inflammatory drugs (NSAIDs) ,Pharmaceutical Science ,Drugs quality control ,Antiinflamatórios não-esteróides ,DRIFTS ,Infravermelho ,Diclofenaco ,Chemometrics ,Humanities - Abstract
No presente trabalho são combinadas as potencialidades das ferramentas quimiométricas e as facilidades na obtenção de espectros pela técnica de espectroscopia por refletância difusa no infravermelho médio com transformada de Fourier (DRIFTS), visando à dosagem do fármaco diclofenaco de potássio. Foram formuladas 20 diferentes concentrações do princípio ativo em excipiente amido entre 0,15 e 0,50 mg/g, com variação de aproximadamente 0,02 mg/g na concentração entre cada amostra. Das 20 amostras, 14 foram empregadas para a calibração e 6 para validação. Os espectros foram adquiridos em um espectrômetro NICOLET Magna 550, em duplicata das amostras. Para a construção dos modelos de regressão multivariada, as informações espectrais foram processadas no aplicativo Pirouette® 2.7 da Infometrix, utilizando-se as regiões 3.715-3.088 cm-1 e 1.634 -1.191 cm-1. A calibração foi realizada pelo método de regressão dos mínimos quadrados parciais (PLS), utilizando pré-processamento autoescalado, e tratamento com correção do espalhamento de luz (MSC). Foram selecionados os melhores modelos, considerando os valores do coeficiente de correlação (R²) e da raiz quadrada dos erros médios quadráticos de validação (RMSEV). Os resultados permitem concluir que modelos de calibração, empregando dados DRIFTS e regressão PLS, podem ser empregados como alternativa na dosagem de diclofenaco de potássio, agregando como vantagens frente aos métodos usuais, a não geração de resíduos, a fácil realização da análise e o baixo custo operacional. In this work the alternative method for quantification of potassium diclofenac was studied, using diffuse reflectance infrared Fourier transform spectrocopy (DRIFTS), together with partial least squares regression (PLS). Two spectra of 20 samples with different concentrations (0.15-0.50 mg/g) of potassium diclofenac in starch had been colleted in Nicolet Magna 550 spectrophotometer, with resolution of the 4 cm-1 and 32 scans. For multivariate regression 14 samples had been used for calibration set and 6 samples had been used for validation set. For the PLS modeling, the spectral information (3715-3088 cm-1 and 1634-1191 cm-1) after multiplicative scatter correction (MSC) and autoscaling preprocess, had been processed in Pirouette® 2.7. The best models with better coefficient regression (R²), these were improved using root mean square error of validation (RMSEV). The new technique propose using DRIFTS/PLS shows an excellent choices for the quality control of the productive process of factories and drugstores that produce or handle these materials in large scale, presenting low time of analysis, no sample destruction and no wastes production.
- Published
- 2006
11. 'Vendo o invisível': experimentos de visualização do infravermelho feitos com materiais simples e de baixo custo
- Author
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Daniel Neves Micha, Germano Maioli Penello, Rudy Massami Sakamoto Kawabata, and Teo Camarotti
- Subjects
infravermelho ,espectro eletromagnético ,câmera digital ,webcam ,ensino de física experimental ,Physics ,QC1-999 - Abstract
Utilizando materiais e equipamentos simples e de fácil obtenção no dia a dia, apresentamos neste trabalho duas experiências com a intenção de auxiliar a introdução experimental ao espectro eletromagnético. Particular ênfase é dada à faixa espectral do infravermelho próximo e suas aplicações no cotidiano. A fim de visualizar essa região do espectro, uma webcam foi devidamente alterada de forma a tornar-se sensível a tal radiação. Na primeira parte deste trabalho, fazemos uma introdução sobre os emissores e sensores de radiação infravermelha. Na segunda parte, apresentamos os experimentos e os resultados obtidos.
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12. A revised distance scale of planetary nebulae
- Author
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R. Ortiz
- Subjects
Physics ,Nebula ,Astrophysics::High Energy Astrophysical Phenomena ,Extinction (astronomy) ,Astronomy ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Planetary nebula ,Galaxy ,Photometry (astronomy) ,Space and Planetary Science ,Bulge ,INFRAVERMELHO ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Large Magellanic Cloud ,Astrophysics::Galaxy Astrophysics - Abstract
Context. The advent of large-scale, high-sensitivity surveys of the Galaxy (2MASS, WISE, Spitzer, etc.) has allowed detection of a large number of planetary nebulae (PNe), some of them at large distances. Aims. I propose a new distance scale of planetary nebulae, based on two main quantities: the flux density (or magnitude) at 8 μm and the nebular apparent size. Methods. I used these quantities to calculate the specific intensity of the radiation I8 μm, which decreases as the nebula evolves. The PNe situated in the Large Magellanic Cloud (LMC) with 8 μm photometry obtained by Spitzer and diameter obtained from HST observations were used as calibrators. Results. After calibration, I recalculated distances of PNe in the LMC, and they show a one-sigma spread of 10 kpc (20%). Eventually, I applied the method to a sample of 47 Galactic PNe observed during the Spitzer survey. These results showed agreement within 0.2 dex with the distances determined with another method of calibrating with PNe in the LMC. Conclusions. The main advantage of the present distance scale is that it is nearly “extinction free”, which makes it especially suited to PNe severely affected by interstellar extinction, such as the Galactic disc and bulge. On the other hand, the method requires an unbiased determination of the nebular size, which might be quite uncertain for PNe with extended faint features, such as haloes and ansae.
- Published
- 2013
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