ALBERT

Description: Using data collected at the Pierre Auger Observatory during the past 3.7 years, we demonstrated a correlation between the arrival directions of cosmic rays with energy above 6 x 10(19) electron volts and the positions of active galactic nuclei (AGN) lying within approximately 75 megaparsecs. We rejected the hypothesis of an isotropic distribution of these cosmic rays with at least a 99% confidence level from a prescribed a priori test. The correlation we observed is compatible with the hypothesis that the highest-energy particles originate from nearby extragalactic sources whose flux has not been substantially reduced by interaction with the cosmic background radiation. AGN or objects having a similar spatial distribution are possible sources.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pierre Auger Collaboration -- Abraham, J -- Abreu, P -- Aglietta, M -- Aguirre, C -- Allard, D -- Allekotte, I -- Allen, J -- Allison, P -- Alvarez, C -- Alvarez-Muniz, J -- Ambrosio, M -- Anchordoqui, L -- Andringa, S -- Anzalone, A -- Aramo, C -- Argiro, S -- Arisaka, K -- Armengaud, E -- Arneodo, F -- Arqueros, F -- Asch, T -- Asorey, H -- Assis, P -- Atulugama, B S -- Aublin, J -- Ave, M -- Avila, G -- Backer, T -- Badagnani, D -- Barbosa, A F -- Barnhill, D -- Barroso, S L C -- Bauleo, P -- Beatty, J -- Beau, T -- Becker, B R -- Becker, K H -- Bellido, J A -- Benzvi, S -- Berat, C -- Bergmann, T -- Bernardini, P -- Bertou, X -- Biermann, P L -- Billoir, P -- Blanch-Bigas, O -- Blanco, F -- Blasi, P -- Bleve, C -- Blumer, H -- Bohacova, M -- Bonifazi, C -- Bonino, R -- Boratav, M -- Brack, J -- Brogueira, P -- Brown, W C -- Buchholz, P -- Bueno, A -- Busca, N G -- Caballero-Mora, K S -- Cai, B -- Camin, D V -- Caruso, R -- Carvalho, W -- Castellina, A -- Catalano, O -- Cataldi, G -- Cazon-Boado, L -- Cester, R -- Chauvin, J -- Chiavassa, A -- Chinellato, J A -- Chou, A -- Chye, J -- Clark, P D J -- Clay, R W -- Colombo, E -- Conceicao, R -- Connolly, B -- Contreras, F -- Coppens, J -- Cordier, A -- Cotti, U -- Coutu, S -- Covault, C E -- Creusot, A -- Cronin, J -- Dagoret-Campagne, S -- Daumiller, K -- Dawson, B R -- de Almeida, R M -- De Donato, C -- de Jong, S J -- De La Vega, G -- de Mello Junior, W J M -- de Mello Neto, J R T -- De Mitri, I -- de Souza, V -- Del Peral, L -- Deligny, O -- Selva, A Della -- Fratte, C Delle -- Dembinski, H -- Di Giulio, C -- Diaz, J C -- Dobrigkeit, C -- D'Olivo, J C -- Dornic, D -- Dorofeev, A -- Dos Anjos, J C -- Dova, M T -- D'Urso, D -- Duvernois, M A -- Engel, R -- Epele, L -- Erdmann, M -- Escobar, C O -- Etchegoyen, A -- Facal San Luis, P -- Falcke, H -- Farrar, G -- Fauth, A C -- Fazzini, N -- Fernandez, A -- Ferrer, F -- Ferry, S -- Fick, B -- Filevich, A -- Filipcic, A -- Fleck, I -- Fonte, R -- Fracchiolla, C E -- Fulgione, W -- Garcia, B -- Garcia Gamez, D -- Garcia-Pinto, D -- Garrido, X -- Geenen, H -- Gelmini, G -- Gemmeke, H -- Ghia, P L -- Giller, M -- Glass, H -- Gold, M S -- Golup, G -- Albarracin, F Gomez -- Berisso, M Gomez -- Herrero, R Gomez -- Goncalves, P -- Goncalves do Amaral, M -- Gonzalez, D -- Gonzalez, J G -- Gonzalez, M -- Gora, D -- Gorgi, A -- Gouffon, P -- Grassi, V -- Grillo, A -- Grunfeld, C -- Guardincerri, Y -- Guarino, F -- Guedes, G P -- Gutierrez, J -- Hague, J D -- Hamilton, J C -- Hansen, P -- Harari, D -- Harmsma, S -- Harton, J L -- Haungs, A -- Hauschildt, T -- Healy, M D -- Hebbeker, T -- Heck, D -- Hojvat, C -- Holmes, V C -- Homola, P -- Horandel, J -- Horneffer, A -- Horvat, M -- Hrabovsky, M -- Huege, T -- Iarlori, M -- Insolia, A -- Ionita, F -- Italiano, A -- Kaducak, M -- Kampert, K H -- Keilhauer, B -- Kemp, E -- Kieckhafer, R M -- Klages, H O -- Kleifges, M -- Kleinfeller, J -- Knapik, R -- Knapp, J -- Koang, D-H -- Kopmann, A -- Krieger, A -- Kromer, O -- Kumpel, D -- Kunka, N -- Kusenko, A -- La Rosa, G -- Lachaud, C -- Lago, B L -- Lebrun, D -- Lebrun, P -- Lee, J -- Leigui de Oliveira, M A -- Letessier-Selvon, A -- Leuthold, M -- Lhenry-Yvon, I -- Lopez, R -- Lopez Aguera, A -- Lozano Bahilo, J -- Maccarone, M C -- Macolino, C -- Maldera, S -- Malek, M -- Mancarella, G -- Mancenido, M E -- Mandat, D -- Mantsch, P -- Mariazzi, A G -- Maris, I C -- Martello, D -- Martinez, J -- Martinez Bravo, O -- Mathes, H J -- Matthews, J -- Matthews, J A J -- Matthiae, G -- Maurizio, D -- Mazur, P O -- McCauley, T -- McEwen, M -- McNeil, R R -- Medina, M C -- Medina-Tanco, G -- Meli, A -- Melo, D -- Menichetti, E -- Menschikov, A -- Meurer, Chr -- Meyhandan, R -- Micheletti, M I -- Miele, G -- Miller, W -- Mollerach, S -- Monasor, M -- Monnier Ragaigne, D -- Montanet, F -- Morales, B -- Morello, C -- Moreno, E -- Moreno, J C -- Morris, C -- Mostafa, M -- Muller, M A -- Mussa, R -- Navarra, G -- Navarro, J L -- Navas, S -- Nellen, L -- Newman-Holmes, C -- Newton, D -- Thi, T Nguyen -- Nierstenhofer, N -- Nitz, D -- Nosek, D -- Nozka, L -- Oehlschlager, J -- Ohnuki, T -- Olinto, A -- Olmos-Gilbaja, V M -- Ortiz, M -- Ostapchenko, S -- Otero, L -- Pakk Selmi-Dei, D -- Palatka, M -- Pallotta, J -- Parente, G -- Parizot, E -- Parlati, S -- Pastor, S -- Patel, M -- Paul, T -- Pavlidou, V -- Payet, K -- Pech, M -- Pekala, J -- Pelayo, R -- Pepe, I M -- Perrone, L -- Petrera, S -- Petrinca, P -- Petrov, Y -- Ngoc, Dieppham -- Ngoc, Dongpham -- Pham Thi, T N -- Pichel, A -- Piegaia, R -- Pierog, T -- Pimenta, M -- Pinto, T -- Pirronello, V -- Pisanti, O -- Platino, M -- Pochon, J -- Porter, T A -- Privitera, P -- Prouza, M -- Quel, E J -- Rautenberg, J -- Reucroft, S -- Revenu, B -- Rezende, F A S -- Ridky, J -- Riggi, S -- Risse, M -- Riviere, C -- Rizi, V -- Roberts, M -- Robledo, C -- Rodriguez, G -- Rodriguez Frias, D -- Rodriguez Martino, J -- Rodriguez Rojo, J -- Rodriguez-Cabo, I -- Ros, G -- Rosado, J -- Roth, M -- Rouille-d'Orfeuil, B -- Roulet, E -- Rovero, A C -- Salamida, F -- Salazar, H -- Salina, G -- Sanchez, F -- Santander, M -- Santo, C E -- Santos, E M -- Sarazin, F -- Sarkar, S -- Sato, R -- Scherini, V -- Schieler, H -- Schmidt, F -- Schmidt, T -- Scholten, O -- Schovanek, P -- Schussler, F -- Sciutto, S J -- Scuderi, M -- Segreto, A -- Semikoz, D -- Settimo, M -- Shellard, R C -- Sidelnik, I -- Siffert, B B -- Sigl, G -- De Grande, N Smetniansky -- Smialkowski, A -- Smida, R -- Smith, A G K -- Smith, B E -- Snow, G R -- Sokolsky, P -- Sommers, P -- Sorokin, J -- Spinka, H -- Squartini, R -- Strazzeri, E -- Stutz, A -- Suarez, F -- Suomijarvi, T -- Supanitsky, A D -- Sutherland, M S -- Swain, J -- Szadkowski, Z -- Takahashi, J -- Tamashiro, A -- Tamburro, A -- Tascau, O -- Tcaciuc, R -- Thomas, D -- Ticona, R -- Tiffenberg, J -- Timmermans, C -- Tkaczyk, W -- Todero Peixoto, C J -- Tome, B -- Tonachini, A -- Torresi, D -- Travnicek, P -- Tripathi, A -- Tristram, G -- Tscherniakhovski, D -- Tueros, M -- Tunnicliffe, V -- Ulrich, R -- Unger, M -- Urban, M -- Valdes Galicia, J F -- Valino, I -- Valore, L -- van den Berg, A M -- van Elewyck, V -- Vazquez, R A -- Veberic, D -- Veiga, A -- Velarde, A -- Venters, T -- Verzi, V -- Videla, M -- Villasenor, L -- Vorobiov, S -- Voyvodic, L -- Wahlberg, H -- Wainberg, O -- Waldenmaier, T -- Walker, P -- Warner, D -- Watson, A A -- Westerhoff, S -- Wieczorek, G -- Wiencke, L -- Wilczynska, B -- Wilczynski, H -- Wileman, C -- Winnick, M G -- Wu, H -- Wundheiler, B -- Xu, J -- Yamamoto, T -- Younk, P -- Zas, E -- Zavrtanik, D -- Zavrtanik, M -- Zech, A -- Zepeda, A -- Ziolkowski, M -- Kegl, B -- New York, N.Y. -- Science. 2007 Nov 9;318(5852):938-43.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17991855" target="_blank"〉PubMed〈/a〉

Description: Cold molecular clouds are the birthplaces of stars and planets, where dense cores of gas collapse to form protostars. The dust mixed in these clouds is thought to be made of grains of an average size of 0.1 micrometer. We report the widespread detection of the coreshine effect as a direct sign of the existence of grown, micrometer-sized dust grains. This effect is seen in half of the cores we have analyzed in our survey, spanning all Galactic longitudes, and is dominated by changes in the internal properties and local environment of the cores, implying that the coreshine effect can be used to constrain fundamental core properties such as the three-dimensional density structure and ages and also the grain characteristics themselves.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pagani, Laurent -- Steinacker, Jurgen -- Bacmann, Aurore -- Stutz, Amelia -- Henning, Thomas -- New York, N.Y. -- Science. 2010 Sep 24;329(5999):1622-4. doi: 10.1126/science.1193211.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Laboratoire d'Etude du Rayonnement et de la Matiere en Astrophysique (LERMA) and UMR 8112 du CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, 75014 Paris, France. laurent.pagani@obspm.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20929841" target="_blank"〉PubMed〈/a〉