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I. INCARICHI ATTUALI

[Marzo 2017 --] Vice Direttore Dipartimento di Fisica

[Marzo 2017 --] Professore ordinario presso l'Universita' di Roma ``Tor Vergata'' 

[Dicembre 2013 --] Presidente della struttura di coordinamento del dottorato dell'Universita' di Roma ``Tor Vergata''

[Maggio 2013 --] Rappresentate eletto per la macroarea di Scienze presso la struttura di coordinamento del dottorato dell'Universita' di Roma, ``Tor Vergata'' Roma, ``Tor Vergata'' 

[Marzo 2003 --] Ricercatore Associato presso l'Harvard Smithsonian Center for Astrophysics, Cambridge, MA, USA  

[1999--] Ricercatore Associato del consorsio Planck/LFI per la realizzazione e l'analisi dati del satellite Planck dell'ESA 

 

II. PRECEDENTI INCARICHI PROFESSIONALI E SCIENTIFICI

[Novembre 2007 -2011] Coordinatore del dottorato in Astronomia dell'Universita' di Roma "Tor Vergata"

[Novembre 2006-2010] Direttore della Sezione Romana della RIAA

[Novembre 2009 -- Febbraio 2017] Professore associato confermato presso l'Universita' di Roma ``Tor Vergata''

[Novembre 2006 --Novembre 2009 ] Professore associato non confermato presso l'Universita' di Roma, ``Tor Vergata'' 

[Ottobre 2003 - Ottobre 2006] Professore a contratto presso l'Universita' di Roma ``Tor Vergata'', con contratto del MIUR relativo all'operazione ``rientro dei cervelli'' 

[Ottobre 2001 -- 2003] Ricercatore associato presso il Department of Physics, University of Durham, UK 

[Novembre 1999 --Settembre 2001] ``ESA Research fellowship'' presso l'Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA 

[Giugno 1999 -- Novembre 1999] Visiting Scientist presso l'Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA

[2000--2012] Coordinatore di due gruppi di ricerca internazionali, ``X-ray Data Assembly'' e ``Simulation of Clusters of Galaxies'', connessi alla missione dell'ESA ``Planck'', dal 2000 

III. ATTIVITA' DI RICERCA

Studio del mezzo intergalattico, degli ammassi di galassie e della struttura su larga scala dell'universo nelle bande delle microonde e a raggi X, dal punto di vista teorico, fenomenologico e di analisi dati. 

IV. PROGETTI DI RICERCA INTERNAZIONALI E NAZIONALI FINANZIATI

Pluriennale esperienza nella preparazione di domande di finanziamento per progetti di ricerca. Di seguito vengono riassunti i dati relativi ad alcuni progetti proposti, sia nazionali che internazionali. Il totale dei finanziamenti ottenuti ammonta a circa 2 Milioni di Euro. "TITOLO Progetto", Ente,Nazione, Durata in mesi, Ruolo Ricoperto "Clusters in X-rays", ASI-INAF, Italy, 24 Coordinatore Unita' di Ricerca "Cosmic Microwave Background Polarization Network", Regione Lazio, Italy, 36 Investigatore Principale "Detection of Hot Warm Intergalactic Medium around compact groups", NASA, USA, 24 Investigatore Principale "Entropy profiles of mass selected groups observed with Chandra", NASA,USA, 24 Investigatore Principale "Study of Clusters of Galaxies and the Large Scale Structure of the Universe Using the Ultimate and Most advanced X-Ray Observatories Chandra and XMM-Newton", MIUR, Italy, 36 Investigatore Principale "ARGOX: Advanced Research European into Galaxy Clusters Observed in the X-ray", European Re-Integration grant, European Community, 36 Investigatore Principale "X-Ray properties of a mass-selected gruop catalog", NASA, USA, 24 Investigatore Principale "Entropy profiles of mass selected groups observed with Chandra", NASA,USA, 24 Investigatore Principale "The quest of the shock in the merging cluster A3667", NASA, USA, 24 Investigatore Principale "Study of a Cold Front in a massive cooling flow cluster of galaxies with strong lensing", NASA, USA , 24 Investigatore Principale "Study of a Cold Fronts in relaxed clusters", NASA, USA , 24 Investigatore Principale "Study of a Cooling flow Clusters with Chandra", ESA, Europe , 24 Investigatore Principale "Deep Study of the Cold Front in A3667", NASA, USA , 24 Investigatore Principale "Cosmologia e Fisica Fondamentale dallo Spazio", ASI, Italy , 12 Responsabile sottogruppo "Study of the excess of point sources around high redshift clusters", NASA, USA , 24 Investigatore Principale "LoCuSS: High Accuracy Cluster Mass Comparison with Chandra and HST", NASA, USA , 24 Investigatore Principale "LoCuSS: An Unbiased Mutli-wavelength Study of the Cluster Quadchotomy-Gas Cooling and Cluster Merging At z=0.2 ", NASA, USA , 24 Investigatore Principale "Relics and Halos at Intermediate Redshift: Testing the Merging Paradigm in the Massive Galaxy Cluster RXCJ1314.4-2515", NASA, USA , 24 Investigatore Principale "Cluster and Galaxy Interactions in Dense Environment: The Shapley Supercluster Core", NASA, USA , 24 Investigatore Principale "Testing the merger--radio halo connection in the massive galaxy cluster RXCJ2003.5--2323", NASA, USA , 36 Investigatore Principale "Weighing galaxy clusters with strong and weak lensing", PRIN-INAF, Italy , 24 Coordinatore Unita' di Ricerca "Tracing the evolution of the physical properties in X-ray galaxy clusters", ASI, Italy , 24 Coordinatore Unita' di Ricerca "CHANDRA ARCHIVAL STUDY OF PLANCK CLUSTERS", NASA, USA , 24 Investigatore Principale "A DETAILED CHANDRA/HST STUDY OF THE FIRST z=1 CLUSTER BLINDLY DISCOVERED IN THE PLANCK ALL SKY SURVEY", HST NASA, USA, 24 Investigatore Principale "Unveiling the most massive clusters at z>0.5 with Planck and XMM-Newton", NASA, USA, 24 Investigatore Principale

 

V. PRODUZIONE SCIENTIFICA E ATTIVITA' DI SERVIZIO PROFESSIONALE

Autore di piu' di 170 articoli pubblicati su riviste internazionali con referre;

piu' di 21000 citazioni;

H index 67; 

Superamento di tutte e 3 le mediane per gli ordinari nel SSD di riferimento; 

Presente nell'elenco dei top italian scientists of the Virtual Italian Academy (http://www.topitalianscientists.org);

Referee per il programma VTR del MIUR dal 2004;

Membro del Peer Review Panel del satellite Chandra;

Referee per il programma COFIN del MIUR dal 2002;

Referee per ApJ, A&A and MNRAS dal 2000.

I. CURRENT SCIENTIFIC AND PROFESSIONAL POSITIONS

[Marzo 2017 --] Deputy Director Department of Physics [Marzo 2017 --] Full Professor at the Universita' di Roma ``Tor Vergata''

[December 2013 --] President of the steering committee of the PhD program at the Universita' di Roma, ``Tor Vergata''

[May 2013 --] Rappresentate eletto per la macroarea di Scienze presso la struttura di coordinamento del dottorato dell'Universita' di Roma ``Tor Vergata''

[March 2003 --] Researcher Associate position at the Harvard Smith- sonian Center for Astrophysics, Cambridge, MA, USA.

[1999--] Associate researcher of the Planck/LFI consortium 

 

II. PAST SCIENTIFIC AND PROFESSIONAL POSITIONS

[November 2007 -2011] Coordinator of the PhD program in Astronomy of the Universita' di Roma Tor Vergata

[November 2006-2010] Director the Roman Section of the RIAA

[November 2006 --February 2017 ] Associate Professor at the Universita' di Roma ``Tor Vergata'' 

[October 2003 - October 2006] Assistent Professor at the Universita’ di Roma “Tor Vergata” in connection with the MIUR program ”rientro dei cervelli”

[Ottobre 2001 -- 2003] Associate Researcher at the Departement of Physiscs, university of Durham, UK 

[November 1999 --September 2001] ``ESA Research fellowship'' at the Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA 

[June 1999 -- November 1999] Visiting Scientist at the Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA III.

 

RESEARCH ACTIVITY

Study of the intergalactic medium, of the clusters of galaxies, and the large scale structure of the Universe in the microwave and X-ray bands.  

 

IV. NATIONAL AND INTERNATIONAL FUNDED PROJECT 

Funded projects for a total amount of about 2 Million Euros. "Project Title", Institute,Country, Length of the project in months, Role "Clusters in X-rays", ASI-INAF, Italy, 24 Coordinator of the Research Unit "Cosmic Microwave Background Polarization Network", Regione Lazio, Italy, 36, Principal Investigator "Detection of Hot Warm Intergalactic Medium around compact groups", NASA, USA, 24 Principal Investigator "Entropy profiles of mass selected groups observed with Chandra", NASA,USA, 24 Principal Investigator "Study of Clusters of Galaxies and the Large Scale Structure of the Universe Using the Ultimate and Most advanced X-Ray Observatories Chandra and XMM-Newton", MIUR, Italy, 36 Principal Investigator "ARGOX: Advanced Research European into Galaxy Clusters Observed in the X-ray", European Re-Integration grant, European Community, 36 Principal Investigator "X-Ray properties of a mass-selected gruop catalog", NASA, USA, 24 Principal Investigator "Entropy profiles of mass selected groups observed with Chandra", NASA,USA, 24 Principal Investigator "The quest of the shock in the merging cluster A3667", NASA, USA, 24 Principal Investigator "Study of a Cold Front in a massive cooling flow cluster of galaxies with strong lensing", NASA, USA , 24 Principal Investigator "Study of a Cold Fronts in relaxed clusters", NASA, USA , 24 Principal Investigator "Study of a Cooling flow Clusters with Chandra", ESA, Europe , 24 Principal Investigator "Deep Study of the Cold Front in A3667", NASA, USA , 24 Principal Investigator "Cosmologia e Fisica Fondamentale dallo Spazio", ASI, Italy , 12 Working Group Coordinator "Study of the excess of point sources around high redshift clusters", NASA, USA , 24 Principal Investigator "LoCuSS: High Accuracy Cluster Mass Comparison with Chandra and HST", NASA, USA , 24 Principal Investigator "LoCuSS: An Unbiased Mutli-wavelength Study of the Cluster Quadchotomy-Gas Cooling and Cluster Merging At z=0.2 ", NASA, USA , 24 Principal Investigator "Relics and Halos at Intermediate Redshift: Testing the Merging Paradigm in the Massive Galaxy Cluster RXCJ1314.4-2515", NASA, USA , 24 Principal Investigator "Cluster and Galaxy Interactions in Dense Environment: The Shapley Supercluster Core", NASA, USA , 24 Principal Investigator "Testing the merger--radio halo connection in the massive galaxy cluster RXCJ2003.5--2323", NASA, USA , 36 Principal Investigator "Weighing galaxy clusters with strong and weak lensing", PRIN-INAF, Italy , 24 Research Unit Coordinator "Tracing the evolution of the physical properties in X-ray galaxy clusters", ASI, Italy , 24 Research Unit Coordinator "CHANDRA ARCHIVAL STUDY OF PLANCK CLUSTERS", NASA, USA , 24 Principal Investigator "A DETAILED CHANDRA/HST STUDY OF THE FIRST z=1 CLUSTER BLINDLY DISCOVERED IN THE PLANCK ALL SKY SURVEY", HST NASA, USA, 24 Principal Investigator "Unveiling the most massive clusters at z>0.5 with Planck and XMM-Newton", NASA, USA, 24 Principal Investigator

 

V. PRODUCTIVITY AND PROFESSIONAL SERVICES

Author of more than 170 articles in refereed international journals; 

more than 21,000 citations;

H index 67; 

listed in the top italian scientists of the Virtual Italian Academy (http://www.topitalianscientists.org)

Referee for the VTR program of the MIUR, since 2004;

Chandra Satellite Peer Review Panel Referee for the COFIN program of the MIUR, since 2002

Referee for ApJ, A&A and MNRAS since 2000,

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(2016). Planck 2015 results: XXVIII. the Planck Catalogue of Galactic cold clumps. 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(2015). Planck intermediate results: XXV. the Andromeda galaxy as seen by Planck. 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(2015). Planck intermediate results. XXII. Frequency dependence of thermal emission fromGalactic dust in intensity and polarization. ASTRONOMY & ASTROPHYSICS, 576.";s:4:"data";s:4:"2015";s:2:"id";s:20:"PUBBLICAZIONE_308313";s:6:"handle";s:11:"2108/177899";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:123:"Planck intermediate results. XXII. 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Isotropy and statistics of the CMB";s:9:"metadata6";s:3232:"Tauber, J; Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Cruz, M; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Ensslin, Ta; Eriksen, Hk; Fantaye, Y; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Frommert, M; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hansen, M; Hanson, D; Harrison, Dl; Helou, G; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kim, J; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Mangilli, A; Marinucci, D; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcewen, Jd; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mikkelsen, K; Mitra, S; Miville-Deschenes, M-; Molinari, D; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pogosyan, D; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Racine, B; Rath, C; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Renzi, A; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Rotti, A; Roudier, G; Rubino-Martin, Ja; Ruiz-Granados, B; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Souradeep, T; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, F; Sutter, P; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Turler, M; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Wehus, Ik; White, M; Wilkinson, A; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321534";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:42;a:14:{s:9:"citazione";s:191:"Ade, P., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., et al. (2014). Planck intermediate results XIII. Constraints on peculiar velocities. ASTRONOMY & ASTROPHYSICS, 561.";s:4:"data";s:7:"2014-01";s:2:"id";s:20:"PUBBLICAZIONE_178217";s:6:"handle";s:10:"2108/86828";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:68:"Planck intermediate results XIII. Constraints on peculiar velocities";s:9:"metadata6";s:2282:"Ade, P; Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Balbi, A; Banday, A; Barreiro, R; Battaner, E; Benabed, K; Benoit-Levy, A; Bernard, J; Bersanelli, M; Bielewicz, P; Bikmaev, I; Bobin, J; Bock, J; Bonaldi, A; Bond, J; Borrill, J; Bouchet, F; Burigana, C; Butler, R; Cabella, P; Cardoso, J; Catalano, A; Chamballu, A; Chiang, L; Chon, G; Christensen, P; Clements, D; Colombi, S; Colombo, L; Crill, B; Cuttaia, F; Da Silva, A; Dahle, H; Davies, R; Davis, R; de Bernardis, P; de Gasperis, G; de Zotti, G; Delabrouille, J; Democles, J; Diego, J; Dolag, K; Dole, H; Donzelli, S; Dore, O; Doerl, U; Douspis, M; Dupac, X; Ensslin, T; Finelli, F; Flores-Cacho, I; Forni, O; Frailis, M; Frommert, M; Galeotta, S; Ganga, K; Genova-Santos, R; Giard, M; Giardino, G; Gonzalez-Nuevo, J; Gregorio, A; Gruppuso, A; Hansen, F; Harrison, D; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, S; Hivon, E; Holmes, W; Hovest, W; Huffenberger, K; Hurier, G; Jaffe, T; Jaffe, A; Jasche, J; Jones, W; Juvela, M; Keihanen, E; Keskitalo, R; Khamitov, I; Kisner, T; Knoche, J; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J; Lasenby, A; Lawrence, C; Le Jeune, M; Leonardi, R; Lilje, P; Linden-Vornle, M; Lopez-Caniego, M; Macias-Perez, J; Maino, D; Mak, D; Mandolesi, N; Maris, M; Marleau, F; Martinez-Gonzalez, E; Masi, S; Matarrese, S; Mazzotta, P; Melchiorri, A; Melin, J; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, J; Naselsky, P; Nati, F; Natoli, P; Netterfield, C; Norgaard-Nielsen, H; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Pagano, L; Paoletti, D; Perdereau, O; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Popa, L; Poutanen, T; Pratt, G; Puget, J; Puisieux, S; Rachen, J; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Roman, M; Rubino-Martin, J; Rusholme, B; Sandri, M; Savini, G; Scott, D; Spencer, L; Sunyaev, 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; Vittorio, N; Wade, L; Welikala, N; Yvon, D; Zacchei, A; Zibin, J; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321299";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:43;a:14:{s:9:"citazione";s:189:"Abergel, A., Ade, P., Aghanim, N., Alves, M., Aniano, G., Armitage-Caplan, C., et al. (2014). Planck 2013 results. XI. All-sky model of thermal dust emission. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255352";s:6:"handle";s:11:"2108/177413";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2440:"This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 GHz, and IRAS 100 mu m data. Using a modified blackbody fit to the data we present all-sky maps of the dust optical depth, temperature, and spectral index over the 353-3000 GHz range. This model is a good representation of the IRAS and Planck data at 5 0 between 353 and 3000 GHz (850 and 100 mu m). It shows variations of the order of 30% compared with the widely-used model of Finkbeiner, Davis, and Schlegel. The Planck data allow us to estimate the dust temperature uniformly over the whole sky, down to an angular resolution of 5 0, providing an improved estimate of the dust optical depth compared to previous all-sky dust model, especially in high-contrast molecular regions where the dust temperature varies strongly at small scales in response to dust evolution, extinction, and/or local production of heating photons. An increase of the dust opacity at 353 GHz, tau(353)/N-H, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, T-obs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at HI column densities lower than 10(20) cm(-2) that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between tau(353)/N-H and T-obs while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields. This e ff ect is compatible with the view that, in the diffuse ISM, Tobs responds to spatial variations of the dust opacity, due to variations of dust properties, in addition to (small) variations of the radiation field strength. The implication is that in the di ff use high-latitude ISM tau(353) is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau(353) with dust extinction estimated using colour excess measurements on stars is strong. To estimate Galactic E(B-V) in extragalactic fields at high latitude we develop a new method based on the thermal dust radiance, instead of the dust optical depth, calibrated to E(B-V) using reddening measurements of quasars deduced from Sloan Digital Sky Survey data.";s:9:"metadata5";s:63:"Planck 2013 results. XI. All-sky model of thermal dust emission";s:9:"metadata6";s:3149:"Abergel, A; Ade, Par; Aghanim, N; Alves, Mir; Aniano, G; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Chamballu, A; Chary, R-; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clemens, M; Clements, Dl; Colombi, S; Colombo, Lpl; Combet, C; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Draine, Bt; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Falgarone, E; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Galeotta, S; Ganga, K; Ghosh, T; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Grenier, Ia; Gruppuso, A; Guillet, V; Hansen, Fk; Hanson, D; Harrison, Dl; Helou, G; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewell, J; Joncas, G; Jones, Wc; Juvela, M; Keihaenen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Laehteenmaeki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Levrier, F; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcgehee, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Verstraete, L; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Welikala, N; Ysard, N; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201323195";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:44;a:14:{s:9:"citazione";s:254:"Abergel, A., Ade, P., Aghanim, N., Alves, M., Aniano, G., Arnaud, M., et al. (2014). Planck intermediate results XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies. ASTRONOMY & ASTROPHYSICS, 566, A55.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_185764";s:6:"handle";s:10:"2108/88787";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:132:"Planck intermediate results XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies";s:9:"metadata6";s:2462:"Abergel, A; Ade, P; Aghanim, N; Alves, M; Aniano, G; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, A; Barreiro, R; Bartlett, J; Battaner, E; Benabed, K; Benoit-Lévy, A; Bernard, J; Bersanelli, M; Bielewicz, P; Bobin, J; Bonaldi, A; Bond, J; Bouchet, F; Boulanger, F; Burigana, C; Cardoso, J; Catalano, A; Chamballu, A; Chiang, H; Christensen, P; Clements, D; Colombi, S; Colombo, L; Couchot, F; Crill, B; Cuttaia, F; Danese, L; Davis, R; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Désert, F; Dickinson, C; Diego, J; Dole, H; Donzelli, S; Doré, O; Douspis, M; Dupac, X; Efstathiou, G; Enßlin, T; Eriksen, H; Falgarone, E; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Ghosh, T; Giard, M; Giraud-Héraud, Y; González-Nuevo, J; Górski, K; Gregorio, A; Gruppuso, A; Guillet, V; Hansen, F; Harrison, D; Helou, G; Henrot-Versillé, S; Hernández-Monteagudo, C; Herranz, D; Hildebrandt, S; Hivon, E; Hobson, M; Holmes, W; Hornstrup, A; Hovest, W; Huffenberger, K; Jaffe, A; Jaffe, T; Joncas, G; Jones, A; Jones, W; Juvela, M; Kalberla, P; Keihänen, E; Kerp, J; Keskitalo, R; Kisner, T; Kneissl, R; Knoche, J; Kunz, M; Kurki-Suonio, H; Lagache, G; Lähteenmäki, A; Lamarre, J; Lasenby, A; Lawrence, C; Leonardi, R; Levrier, F; Liguori, M; Lilje, P; Linden-Vørnle, M; López-Caniego, M; Lubin, P; Macías-Pérez, J; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, D; Martin, P; Martínez-González, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschênes, M; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, J; Naselsky, P; Nati, F; Natoli, P; Noviello, F; Novikov, D; Novikov, I; Oxborrow, C; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Pratt, G; Prunet, S; Puget, J; Rachen, J; Reach, W; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rusholme, B; Sandri, M; Savini, G; Spencer, L; Starck, J; Sureau, F; Sutton, D; Suur-Uski, A; Sygnet, J; Tauber, J; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Verstraete, L; Vielva, P; Villa, F; Wade, L; Wandelt, B; Winkel, B; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201323270";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:45;a:14:{s:9:"citazione";s:173:"Ade, P., Aghanim, N., Alves, M., Armitage-Caplan, C., Arnaud, M., Ashdown, M., et al. (2014). Planck 2013 results. XIII. Galactic CO emission. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255347";s:6:"handle";s:11:"2108/177437";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1651:"Rotational transition lines of CO play a major role in molecular radio astronomy as a mass tracer and in particular in the study of star formation and Galactic structure. Although a wealth of data exists for the Galactic plane and some well-known molecular clouds, there is no available high sensitivity all-sky survey of CO emission to date. Such all-sky surveys can be constructed using the Planck HFI data because the three lowest CO rotational transition lines at 115, 230 and 345 GHz significantly contribute to the signal of the 100, 217 and 353 GHz HFI channels, respectively. Two different component separation methods are used to extract the CO maps from Planck HFI data. The maps obtained are then compared to one another and to existing external CO surveys. From these quality checks the best CO maps, in terms of signal to noise ratio and/or residual contamination by other emission, are selected. Three different sets of velocity-integrated CO emission maps are produced with different trade-offs between signal-to-noise, angular resolution, and reliability. Maps for the CO J = 1 -> 0, J = 2 -> 1, and J = 3 -> 2 rotational transitions are presented and described in detail. They are shown to be fully compatible with previous surveys of parts of the Galactic plane as well as with undersampled surveys of the high latitude sky. The Planck HFI velocity-integrated CO maps for the J = 1 -> 0, J = 2 -> 1, and J = 3 -> 2 rotational transitions provide an unprecedented all-sky CO view of the Galaxy. These maps are also of great interest to monitor potential CO contamination of the Planck studies of the cosmological microwave background.";s:9:"metadata5";s:47:"Planck 2013 results. XIII. Galactic CO emission";s:9:"metadata6";s:3103:"Ade, Par; Aghanim, N; Alves, Mir; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardos, J-; Catalano, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Combet, C; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Dempsey, Jt; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Falgarone, E; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Fukui, Y; Galeotta, S; Ganga, K; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Handa, T; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hily-Blant, P; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Hurier, G; Jaffe, Ah; Jaffe, Tr; Jewell, J; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffein, B; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcgehee, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Moore, Tjt; Morgante, G; Morino, J; Mortlock, D; Munshi, D; Murphy, Ja; Nakajima, T; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviellon, F; Novikov, D; Novikov, I; Okuda, T; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Thomas, Hs; Toffolatti, L; Tomasi, M; Torii, K; Tristram, M; Tucci, M; Tuovinen, J; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Wehus, Ik; Yamamoto, H; Yoda, T; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321553";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:46;a:14:{s:9:"citazione";s:222:"Ade, P., Aghanim, N., Alves, M., Arnaud, M., Atrio-Barandela, F., Aumont, J., et al. (2014). Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds. ASTRONOMY & ASTROPHYSICS, 565, A103.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_185763";s:6:"handle";s:10:"2108/88789";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:91:"Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds";s:9:"metadata6";s:2336:"Ade, P; Aghanim, N; Alves, M; Arnaud, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, A; Barreiro, R; Battaner, E; Benabed, K; Benoit-Lévy, A; Bernard, J; Bersanelli, M; Bielewicz, P; Bobin, J; Bonaldi, A; Bond, J; Borrill, J; Bouchet, F; Boulanger, F; Burigana, C; Cardoso, J; Casassus, S; Catalano, A; Chamballu, A; Chen, X; Chiang, H; Chiang, L; Christensen, P; Clements, D; Colombi, S; Colombo, L; Couchot, F; Crill, B; Cuttaia, F; Danese, L; Davies, R; Davis, R; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Désert, F; Dickinson, C; Diego, J; Donzelli, S; Doré, O; Dupac, X; Enßlin, T; Eriksen, H; Finelli, F; Forni, O; Franceschi, E; Galeotta, S; Ganga, K; Génova-Santos, R; Ghosh, T; Giard, M; González-Nuevo, J; Górski, K; Gregorio, A; Gruppuso, A; Hansen, F; Harrison, D; Helou, G; Hernández-Monteagudo, C; Hildebrandt, S; Hivon, E; Hobson, M; Hornstrup, A; Jaffe, A; Jaffe, T; Jones, W; Keihänen, E; Keskitalo, R; Kneissl, R; Knoche, J; Kunz, M; Kurki-Suonio, H; Lähteenmäki, A; Lamarre, J; Lasenby, A; Lawrence, C; Leonardi, R; Liguori, M; Lilje, P; Linden-Vørnle, M; López-Caniego, M; Macías-Pérez, J; Maffei, B; Maino, D; Mandolesi, N; Marshall, D; Martin, P; Martínez-González, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Meinhold, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Miville-Deschênes, M; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Nørgaard-Nielsen, H; Noviello, F; Novikov, D; Novikov, I; Oxborrow, C; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Patanchon, G; Pearson, T; Peel, M; Perdereau, O; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Pratt, G; Prunet, S; Puget, J; Rachen, J; Rebolo, R; Reich, W; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rubiño-Martín, J; Rusholme, B; Sandri, M; Savini, G; Scott, D; Spencer, L; Stolyarov, V; Sutton, D; Suur-Uski, A; Sygnet, J; Tauber, J; Tavagnacco, D; Terenzi, L; Tibbs, C; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Verstraete, L; Vielva, P; Villa, F; Wandelt, B; Watson, R; Wilkinson, A; Ysard, N; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201322612";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:47;a:14:{s:9:"citazione";s:197:"Ade, P., Aghanim, N., Argueeso, F., Armitage-Caplan, C., Arnaud, M., Ashdown, M., et al. (2014). Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255350";s:6:"handle";s:11:"2108/177409";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:769:"The Planck Catalogue of Compact Sources (PCCS) is the catalogue of sources detected in the first 15 months of Planck operations, the "nominal" mission. It consists of nine single-frequency catalogues of compact sources, both Galactic and extragalactic, detected over the entire sky. The PCCS covers the frequency range 30-857 GHz with higher sensitivity (it is 90% complete at 180 mJy in the best channel) and better angular resolution (from 32.88' to 4.33') than previous all-sky surveys in this frequency band. By construction its reliability is >80% and more than 65% of the sources have been detected in at least two contiguous Planck channels. In this paper we present the construction and validation of the PCCS, its contents and its statistical characterization.";s:9:"metadata5";s:68:"Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources";s:9:"metadata6";s:3113:"Ade, Par; Aghanim, N; Argueeso, F; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Beelen, A; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Carvalho, P; Catalano, A; Challinor, A; Chamballu, A; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clemens, M; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, Dl; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leon-Tavares, J; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcgehee, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Negrello, M; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, Tj; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Walter, B; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321524";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:48;a:14:{s:9:"citazione";s:209:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, E., et al. (2014). Planck 2013 results. XVII. Gravitational lensing by large-scale structure. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255344";s:6:"handle";s:11:"2108/177439";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1754:"On the arcminute angular scales probed by Planck, the cosmic microwave background (CMB) anisotropies are gently perturbed by gravitational lensing. Here we present a detailed study of this effect, detecting lensing independently in the 100, 143, and 217 GHz frequency bands with an overall significance of greater than 25 sigma. We use the temperature-gradient correlations induced by lensing to reconstruct a (noisy) map of the CMB lensing potential, which provides an integrated measure of the mass distribution back to the CMB last-scattering surface. Our lensing potential map is significantly correlated with other tracers of mass, a fact which we demonstrate using several representative tracers of large-scale structure. We estimate the power spectrum of the lensing potential, finding generally good agreement with expectations from the best-fitting ACDM model for the Planck temperature power spectrum, showing that this measurement at z = 1100 correctly predicts the properties of the lower-redshift, later-time structures which source the lensing potential. When combined with the temperature power spectrum, our measurement provides degeneracy-breaking power for parameter constraints; it improves CMB-alone constraints on curvature by a factor of two and also partly breaks the degeneracy between the amplitude of the primordial perturbation power spectrum and the optical depth to reionization, allowing a measurement of the optical depth to reionization which is independent of large-scale polarization data. Discarding scale information, our measurement corresponds to a 4% constraint on the amplitude of the lensing potential power spectrum, or a 2% constraint on the root-mean-squared amplitude of matter fluctuations at z similar to 2.";s:9:"metadata5";s:73:"Planck 2013 results. XVII. Gravitational lensing by large-scale structure";s:9:"metadata6";s:3072:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, E; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Basak, S; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Dechelette, T; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dunkley, J; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Ho, S; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lavabre, A; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Lewis, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Mangilli, A; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeaul, G; Prunet, S; Puget, J-; Pullen, Ar; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Smith, K; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, E; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, M; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321543";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:49;a:14:{s:9:"citazione";s:182:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. IX. HFI spectral response. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255335";s:6:"handle";s:11:"2108/177445";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2339:"The Planck High Frequency Instrument (HFI) spectral response was determined through a series of ground based tests conducted with the HFI focal plane in a cryogenic environment prior to launch. The main goal of the spectral transmission tests was to measure the relative spectral response (including the level of out-of-band signal rejection) of all HFI detectors to a known source of electromagnetic radiation individually. This was determined by measuring the interferometric output of a continuously scanned Fourier transform spectrometer with all HFI detectors. As there is no on-board spectrometer within HFI, the ground-based spectral response experiments provide the definitive data set for the relative spectral calibration of the HFI. Knowledge of the relative variations in the spectral response between HFI detectors allows for a more thorough analysis of the HFI data. The spectral response of the HFI is used in Planck data analysis and component separation, this includes extraction of CO emission observed within Planck bands, dust emission, Sunyaev-Zeldovich sources, and intensity to polarization leakage. The HFI spectral response data have also been used to provide unit conversion and colour correction analysis tools. While previous papers describe the pre-flight experiments conducted on the Planck HFI, this paper focusses on the analysis of the pre-flight spectral response measurements and the derivation of data products, e.g. band-average spectra, unit conversion coefficients, and colour correction coefficients, all with related uncertainties. Verifications of the HFI spectral response data are provided through comparisons with photometric HFI flight data. This validation includes use of HFI zodiacal emission observations to demonstrate out-of-band spectral signal rejection better than 10(8). The accuracy of the HFI relative spectral response data is verified through comparison with complementary flight-data based unit conversion coefficients and colour correction coefficients. These coefficients include those based upon HFI observations of CO, dust, and Sunyaev-Zeldovich emission. General agreement is observed between the ground-based spectral characterization of HFI and corresponding in-flight observations, within the quoted uncertainty of each; explanations are provided for any discrepancies.";s:9:"metadata5";s:46:"Planck 2013 results. IX. HFI spectral response";s:9:"metadata6";s:2786:"Ade, P; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Combet, C; Comis, B; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Falgarone, E; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Ciard, M; Giraud-Heraud, Y; Gonzadlez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Hurier, G; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneiss, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcgehee, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; North, C; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rusholme, B; Santos, D; Savini, G; Scott, D; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321531";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:50;a:14:{s:9:"citazione";s:202:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. VI. High Frequency Instrument data processing. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255353";s:6:"handle";s:11:"2108/177401";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:66:"Planck 2013 results. VI. High Frequency Instrument data processing";s:9:"metadata6";s:3066:"Ade, PAR; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bowyer, Jw; Bridges, M; Bucher, M; Burigana, C; Cardoso, J-; Catalano, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Combet, C; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rose, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dunkley, J; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Girard, D; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Hansen, Fk; Hanson, D; Harrison, D; Helou, G; Henrot-Versille, S; Herent, O; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hou, Z; Hovest, W; Huffenberger, Km; Hurier, G; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Le Jaune, M; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Mactavish, Cj; Maffei, B; Mandolesi, N; Maris, M; Marleau, F; Marshall, J; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcgehee, P; Meinhold, Pr; Melchiorri, A; Melot, F; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Mottet, S; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; North, C; Noviello, F; Novikov, D; Novikov, I; Orieux, F; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Pasian, F; Patanchon, G; Perdereaun, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Racine, B; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rusholme, B; Sanselme, L; Santos, D; Sauve, A; Savini, G; Scott, D; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureae, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Techene, S; Terenzi, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vibert, L; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321570";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:51;a:14:{s:9:"citazione";s:204:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. VIII. HFI photometric calibration and mapmaking. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255364";s:6:"handle";s:11:"2108/177423";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1788:"This paper describes the methods used to produce photometrically calibrated maps from the Planck High Frequency Instrument (HFI) cleaned, time-ordered information. HFI observes the sky over a broad range of frequencies, from 100 to 857 GHz. To obtain the best calibration accuracy over such a large range, two different photometric calibration schemes have to be used. The 545 and 857 GHz data are calibrated by comparing flux-density measurements of Uranus and Neptune with models of their atmospheric emission. The lower frequencies (below 353 GHz) are calibrated using the solar dipole. A component of this anisotropy is time-variable, owing to the orbital motion of the satellite in the solar system. Photometric calibration is thus tightly linked to mapmaking, which also addresses low-frequency noise removal. By comparing observations taken more than one year apart in the same configuration, we have identified apparent gain variations with time. These variations are induced by non-linearities in the read-out electronics chain. We have developed an effective correction to limit their effect on calibration. We present several methods to estimate the precision of the photometric calibration. We distinguish relative uncertainties (between detectors, or between frequencies) and absolute uncertainties. Absolute uncertainties lie in the range from 0.54% to 10% from 100 to 857 GHz. We describe the pipeline used to produce the maps from the HFI timelines, based on the photometric calibration parameters, and the scheme used to set the zero level of the maps a posteriori. We also discuss the cross-calibration between HFI and the SPIRE instrument on board Herschel. Finally we summarize the basic characteristics of the set of HFI maps included in the 2013 Planck data release.";s:9:"metadata5";s:68:"Planck 2013 results. VIII. HFI photometric calibration and mapmaking";s:9:"metadata6";s:2910:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bertincourt, B; Bielewicz, P; Bobin, J; Bock, Jj; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Combet, C; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Filliard, C; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Helou, G; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Le Jeune, M; Lellouch, E; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Maurin, L; Mazzotta, P; Mcgehee, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Moreno, R; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, Tj; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rusholme, B; Santos, D; Savini, G; Scott, D; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Techene, S; Terenzi, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321538";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:52;a:14:{s:9:"citazione";s:233:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. X. HFI energetic particle effects: characterization, removal, and simulation. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255362";s:6:"handle";s:11:"2108/177427";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1641:"We describe the detection, interpretation, and removal of the signal resulting from interactions of high energy particles with the Planck High Frequency Instrument (HFI). There are two types of interactions: heating of the 0.1 K bolometer plate; and glitches in each detector time stream. The transient responses to detector glitch shapes are not simple single- pole exponential decays and fall into three families. The glitch shape for each family has been characterized empirically in flight data and these shapes have been used to remove glitches from the detector time streams. The spectrum of the count rate per unit energy is computed for each family and a correspondence is made to the location on the detector of the particle hit. Most of the detected glitches are from Galactic protons incident on the die frame supporting the micro- machined bolometric detectors. In the Planck orbit at L2, the particle flux is around 5 cm 2 s 1 and is dominated by protons incident on the spacecraft with energy > 39 MeV, at a rate of typically one event per second per detector. Di ff erent categories of glitches have di ff erent signatures in the time stream. Two of the glitch types have a low amplitude component that decays over nearly 1 s. This component produces excess noise if not properly removed from the time- ordered data. We have used a glitch detection and subtraction method based on the joint fit of population templates. The application of this novel glitch subtraction method removes excess noise from the time streams. Using realistic simulations, we find that this method does not introduce signal bias into the Planck data.";s:9:"metadata5";s:97:"Planck 2013 results. X. HFI energetic particle effects: characterization, removal, and simulation";s:9:"metadata6";s:2744:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, P; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Gana, K; Giard, M; Girard, D; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcgehee, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Miniussi, A; Mitra, A; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Mottet, S; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Racine, B; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rusholme, B; Sanselme, L; Santos, D; Sauve, A; Savini, G; Scott, D; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321577";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:53;a:14:{s:9:"citazione";s:190:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XII. Diffuse component separation. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255336";s:6:"handle";s:11:"2108/176795";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:54:"Planck 2013 results. XII. Diffuse component separation";s:9:"metadata6";s:3307:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Castex, G; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Cruz, M; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dobler, G; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dunkley, J; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Falgarone, E; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, Dl; Helou, G; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huey, G; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewell, J; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Le Jeune, M; Leach, S; Leahy, Jp; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Marcos-Caballero, A; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mikkelsen, K; Mitra, S; Miville-Deschenes, M-; Molinari, D; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, Tj; Perdereau, O; Perotto, L; Perrotta, F; Pettorino, V; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Platania, P; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Renzi, A; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Roman, M; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Salerno, E; Sandri, M; Santos, D; Savini, G; Schiavon, F; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Viel, M; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Wehus, Ik; Wilkinson, A; Xia, J-; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321580";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:54;a:14:{s:9:"citazione";s:179:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XIV. Zodiacal emission. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255331";s:6:"handle";s:11:"2108/177451";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1511:"The Planck satellite provides a set of all-sky maps at nine frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and di ff use interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through di ff erent columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model -a di ff use cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are di ff erent from those in the di ff use cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies.";s:9:"metadata5";s:43:"Planck 2013 results. XIV. Zodiacal emission";s:9:"metadata6";s:2955:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colley, J-; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Helou, G; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Mottet, S; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; O'Sullivan, C; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polegre, Am; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Smoot, Gf; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Umana, G; Valenziano, L; Valivlita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321562";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:55;a:14:{s:9:"citazione";s:185:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XVI. Cosmological parameters. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255346";s:6:"handle";s:11:"2108/134725";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:49:"Planck 2013 results. XVI. Cosmological parameters";s:9:"metadata6";s:3362:"Ade, P; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Calabrese, E; Cappellini, B; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dunkley, J; Dupac, X; Efstathiou, G; Elsner, F; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Gaier, Tc; Galeotta, S; Galli, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gjerlow, E; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Haissinski, J; Hamann, J; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hou, Z; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewell, J; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Lattanzi, M; Laureijs, Rj; Lawrence, Cr; Leach, S; Leahy, Jp; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Lewis, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Melin, J-; Mendes, L; Menegoni, E; Mennella, A; Migliaccio, M; Millea, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, D; Pearson, Tj; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Pettorino, V; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Platania, P; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savelainen, M; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, A; Wandelt, Bd; Wehus, Ik; White, M; White, Sdm; Wilkinson, A; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321591";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:56;a:14:{s:9:"citazione";s:221:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XVIII. The gravitational lensing-infrared background correlation. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255334";s:6:"handle";s:11:"2108/177447";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1660:"The multi-frequency capability of the Planck satellite provides information both on the integrated history of star formation (via the cosmic infrared background, or CIB) and on the distribution of dark matter (via the lensing effect on the cosmic microwave background, or CMB). The conjunction of these two unique probes allows us to measure directly the connection between dark and luminous matter in the high redshift (1 <= z <= 3) Universe. We use a three-point statistic optimized to detect the correlation between these two tracers, using lens reconstructions at 100, 143, and 217 GHz, together with CIB measurements at 100-857 GHz. Following a thorough discussion of possible contaminants and a suite of consistency tests, we report the first detection of the correlation between the CIB and CMB lensing. The well matched redshift distribution of these two signals leads to a detection significance with a peak value of 42/19 sigma (statistical/statistical + systematics) at 545 GHz and a correlation as high as 80% across these two tracers. Our full set of multi-frequency measurements (both CIB auto-and CIB-lensing cross-spectra) are consistent with a simple halo-based model, with a characteristic mass scale for the halos hosting CIB sources of log(10)(M/M-circle dot) = 10.5 +/- 0.6. Leveraging the frequency dependence of our signal, we isolate the high redshift contribution to the CIB, and constrain the star formation rate (SFR) density at z >= 1. We measure directly the SFR density with around 2 sigma significance for three redshift bins between z = 1 and 7, thus opening a new window into the study of the formation of stars at early times.";s:9:"metadata5";s:85:"Planck 2013 results. XVIII. The gravitational lensing-infrared background correlation";s:9:"metadata6";s:2906:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Basak, S; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bethermin, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lacasa, F; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Serra, P; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321540";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:57;a:14:{s:9:"citazione";s:208:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255340";s:6:"handle";s:11:"2108/177421";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:72:"Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts";s:9:"metadata6";s:3257:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Barrena, R; Bartlett, Jg; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bikmaev, I; Blanchard, A; Bobin, J; Bock, Jj; Boehringer, H; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Bourdin, H; Bridges, M; Brown, Ml; Bucher, M; Burenin, R; Burigana, C; Butler, Rc; Cardoso, J-; Carvalho, P; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chiang, L-; Chiang, Hc; Chon, G; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Da Silva, A; Dahle, H; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Democles, J; Desert, F-; Dickinson, C; Diego, Jm; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Flores-Cacho, I; Forni, O; Frailis, M; Franceschi, E; Fromenteau, S; Galeotta, S; Ganga, K; Genova-Santos, Rt; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Hurier, G; Jaffe, Tr; Jaffe, Ah; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Khamitov, I; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Liddle, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Marcos-Caballero, A; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Melin, J-; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Roman, M; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, A; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Weller, J; White, M; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321521";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:58;a:14:{s:9:"citazione";s:246:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XXI. Power spectrum and high-order statistics of the Planck all-sky Compton parameter map. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255328";s:6:"handle";s:11:"2108/177419";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1457:"We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 100 to 857 GHz frequency channel maps from the Planck survey. This map shows an obvious galaxy cluster tSZ signal that is well matched with blindly detected clusters in the Planck SZ catalogue. To characterize the signal in the tSZ map we have computed its angular power spectrum. At large angular scales (l < 60), the major foreground contaminant is the diffuse thermal dust emission. At small angular scales (l > 500) the clustered cosmic infrared background and residual point sources are the major contaminants. These foregrounds are carefully modelled and subtracted. We thus measure the tSZ power spectrum over angular scales 0.17 degrees less than or similar to theta less than or similar to 3.0 degrees that were previously unexplored. The measured tSZ power spectrum is consistent with that expected from the Planck catalogue of SZ sources, with clear evidence of additional signal from unresolved clusters and, potentially, diffuse warm baryons. Marginalized band-powers of the Planck tSZ power spectrum and the best-fit model are given. The non-Gaussianity of the Compton parameter map is further characterized by computing its 1D probability distribution function and its bispectrum. The measured tSZ power spectrum and high order statistics are used to place constraints on sigma(8).";s:9:"metadata5";s:110:"Planck 2013 results. XXI. Power spectrum and high-order statistics of the Planck all-sky Compton parameter map";s:9:"metadata6";s:3058:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, B; Bartlett, Jg; Battanerioo, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Carvalho, P; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Comis, B; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Da Silva, A; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dolag, K; Dole, H; Donzelli, S; Dore, A; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Flores-Cacho, I; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Genova-Santos, Rt; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Hurier, G; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lacasa, F; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Loen-Tavares, J; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Marcos-Caballero, A; Maris, M; Marshall, Dj; Martin, G; Macinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Melchiorri, A; Melin, J-; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Partridge, B; Pasian, F; Patanchonl, G; Perdereau, ; Perotto, L; Perrotta, F; Piacentini, F; Mae, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rossetl, C; Rossetti, M; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321522";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:59;a:14:{s:9:"citazione";s:187:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XXII. Constraints on inflation. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255361";s:6:"handle";s:11:"2108/134747";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2547:"We analyse the implications of the Planck data for cosmic inflation. The Planck nominal mission temperature anisotropy measurements, combined with the WMAP large-angle polarization, constrain the scalar spectral index to be n(s) = 0.9603 +/- 0:0073, ruling out exact scale invariance at over 5 sigma Planck establishes an upper bound on the tensor-to-scalar ratio of r < 0.11 (95% CL). The Planck data thus shrink the space of allowed standard inflationary models preferring potentials with V '' < 0. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n >= 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining dn(s)/dln k = -0.0134 +/- 0.0090. We verify these conclusions through a numerical analysis, which makes no slowroll approximation, and carry out a Bayesian parameter estimation and model-selection analysis for a number of inflationary models including monomial, natural, and hilltop potentials. For each model, we present the Planck constraints on the parameters of the potential and explore several possibilities for the post-inflationary entropy generation epoch, thus obtaining nontrivial data-driven constraints. We also present a direct reconstruction of the observable range of the inflaton potential. Unless a quartic term is allowed in the potential, we find results consistent with second-order slow-roll predictions. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit by delta 2 10; however, Bayesian evidence does not prefer these models. We constrain several single-field inflation models with generalized Lagrangians by combining power spectrum data with Planck bounds on fNL. Planck constrains with unprecedented accuracy the amplitude and possible correlation (with the adiabatic mode) of non-decaying isocurvature fluctuations. The fractional primordial contributions of cold dark matter (CDM) isocurvature modes of the types expected in the curvaton and axion scenarios have upper bounds of 0.25% and 3.9% (95% CL), respectively. In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anticorrelated isocurvature component can improve the 2 by approximately 4 as a result of slightly lowering the theoretical prediction for the 40 multipoles relative to the higher multipoles. Nonetheless, the data are consistent with adiabatic initial conditions.";s:9:"metadata5";s:51:"Planck 2013 results. XXII. Constraints on inflation";s:9:"metadata6";s:3121:"Ade, P; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Bartolo, N; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Calabrese, E; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dunkley, J; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Gauthier, C; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hamann, J; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihaenen, E; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Laehteenmaeki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leach, S; Leahy, Jp; Leonardi, R; Lesgourgues, J; Lewis, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Pandolfi, S; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savelainen, M; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Treguer-Goudineau, J; Tristram, M; Tucci, M; Tuovinen, J; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, M; Wilkinson, A; Yvon, D; Zacchei, A; Zibin, Jp; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321569";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:60;a:14:{s:9:"citazione";s:212:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XXIX. The Planck catalogue of Sunyaev-Zeldovich sources. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255332";s:6:"handle";s:11:"2108/177411";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1542:"We describe the all-sky Planck catalogue of clusters and cluster candidates derived from Sunyaev-Zeldovich (SZ) effect detections using the first 15.5 months of Planck satellite observations. The catalogue contains 1227 entries, making it over six times the size of the Planck Early SZ (ESZ) sample and the largest SZ-selected catalogue to date. It contains 861 confirmed clusters, of which 178 have been confirmed as clusters, mostly through follow-up observations, and a further 683 are previously-known clusters. The remaining 366 have the status of cluster candidates, and we divide them into three classes according to the quality of evidence that they are likely to be true clusters. The Planck SZ catalogue is the deepest all-sky cluster catalogue, with redshifts up to about one, and spans the broadest cluster mass range from (0.1 to 1.6) x 10(15) M-circle dot. Confirmation of cluster candidates through comparison with existing surveys or cluster catalogues is extensively described, as is the statistical characterization of the catalogue in terms of completeness and statistical reliability. The outputs of the validation process are provided as additional information. This gives, in particular, an ensemble of 813 cluster redshifts, and for all these Planck clusters we also include a mass estimated from a newly-proposed SZ-mass proxy. A refined measure of the SZ Compton parameter for the clusters with X-ray counter-parts is provided, as is an X-ray flux for all the Planck clusters not previously detected in X-ray surveys.";s:9:"metadata5";s:76:"Planck 2013 results. XXIX. The Planck catalogue of Sunyaev-Zeldovich sources";s:9:"metadata6";s:3527:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Aussel, H; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Barrena, R; Bartelinann, M; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J; Bersanelli, M; Bielewicz, P; Bikmaev, I; Bobin, J; Bock, Jj; Boehringer, H; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burenin, R; Burigana, C; Butier, Rc; Cardoso, J-; Carvalho, P; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Chon, G; Christensen, Pr; Churazov, E; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Comis, B; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Da Silva, A; Dahle, H; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouilie, J; Delouis, J-; Democles, J; Desert, F-; Dickinson, C; Diego, Im; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Eisenhardt, Prm; Ensslin, Ta; Eriksen, Hk; Feroz, F; Finelli, F; Flores-Cacho, I; Forni, O; Frailis, M; Franceschi, E; Fromenteau, S; Galeotta, S; Ganga, K; Genova-Santos, Rt; Giard, M; Giardino, G; Gilfanov, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Grainge, Kjb; Gratton, S; Gregorio, A; Groeneboom, Ne; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Hempel, A; Elenrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Homstrup, A; Hovest, W; Huffenberger, Km; Hurier, G; Hurley-Walker, N; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Khamitov, I; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kinti-Stionio, H; Laeache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Li, C; Liddle, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Mactavish, Cj; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshal, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mei, S; Meinhold, Pr; Meichiorri, A; Melin, J-; Mendes, L; Mennelia, A; Migliaccio, M; Mikkeisen, K; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Nesvadba, Nph; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novilov, I; O'Dwyer, Ij; Olamaie, M; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Pearson, Tj; Perdereau, O; Perotto, L; Perrott, Yc; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pletrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, O; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rumsey, C; Rusholme, B; Sandri, M; Santos, D; Saunders, Rde; Savini, G; Schammel, Mp; Scott, D; Seiffert, Md; Shellard, Eps; Shimwell, Tw; Spencer, Ld; Stanford, Sa; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vibert, L; Vielva, P; Vilia, F; Vittorio, N; Wade, La; Wandelt, Bd; White, M; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321523";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:61;a:14:{s:9:"citazione";s:219:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XXV. Searches for cosmic strings and other topological defects. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255342";s:6:"handle";s:11:"2108/177407";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2115:"Planck data have been used to provide stringent new constraints on cosmic strings and other defects. We describe forecasts of the CMB power spectrum induced by cosmic strings, calculating these from network models and simulations using line-of-sight Boltzmann solvers. We have studied Nambu-Goto cosmic strings, as well as field theory strings for which radiative effects are important, thus spanning the range of theoretical uncertainty in the underlying strings models. We have added the angular power spectrum from strings to that for a simple adiabatic model, with the extra fraction defined as f(10) at multipole l = 10. This parameter has been added to the standard six parameter fit using CO S M OM C with flat priors. For the Nambu-Goto string model, we have obtained a constraint on the string tension of G mu/c(2) < 1.5 x 10(-7) and f(10) < 0.015 at 95% confidence that can be improved to G mu/c(2) < 1.3 x 10(-7) and f(10) < 0.010 on inclusion of high-l CMB data. For the Abelian-Higgs field theory model we find, G mu(AH)/c2 < 3.2x10(-7) and f(10) < 0.028. The marginalised likelihoods for f(10) and in the f(10)-Omega(b)h(2) plane are also presented. We have additionally obtained comparable constraints on f(10) for models with semilocal strings and global textures. In terms of the effective defect energy scale these are somewhat weaker at G mu/c(2) < 1.1 x 10(-6). We have made complementarity searches for the specific non-Gaussian signatures of cosmic strings, calibrating with all-sky Planck resolution CMB maps generated from networks of post-recombination strings. We have validated our non-Gaussian searches using these simulated maps in a Planck-realistic context, estimating sensitivities of up to Delta G mu/c(2) approximate to 4 x 10(-7). We have obtained upper limits on the string tension at 95% confidence of G mu/c(2) < 9.0 x 10(-7) with modal bispectrum estimation and G mu/c(2) < 7.8 x 10(-7) for real space searches with Minkowski functionals. These are conservative upper bounds because only post-recombination string contributions have been included in the non-Gaussian analysis.";s:9:"metadata5";s:83:"Planck 2013 results. XXV. Searches for cosmic strings and other topological defects";s:9:"metadata6";s:2903:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, L-; Chiang, Hc; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dunkley, J; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Tr; Jaffe, Ah; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Matarrese, S; Matthai, F; Mazzotta, P; Mcewen, Jd; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Raeth, C; Rebolo, R; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ringeval, C; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321621";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:62;a:14:{s:9:"citazione";s:211:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XXVI. Background geometry and topology of the Universe. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255359";s:6:"handle";s:11:"2108/177405";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2999:"The new cosmic microwave background (CMB) temperature maps from Planck provide the highest-quality full-sky view of the surface of last scattering available to date. This allows us to detect possible departures from the standard model of a globally homogeneous and isotropic cosmology on the largest scales. We search for correlations induced by a possible non-trivial topology with a fundamental domain intersecting, or nearly intersecting, the last scattering surface (at comoving distance chi(rec)), both via a direct search for matched circular patterns at the intersections and by an optimal likelihood search for specific topologies. For the latter we consider flat spaces with cubic toroidal (T3), equal-sided chimney (T2) and slab (T1) topologies, three multi-connected spaces of constant positive curvature (dodecahedral, truncated cube and octahedral) and two compact negative-curvature spaces. These searches yield no detection of the compact topology with the scale below the diameter of the last scattering surface. For most compact topologies studied the likelihood maximized over the orientation of the space relative to the observed map shows some preference for multi-connected models just larger than the diameter of the last scattering surface. Since this effect is also present in simulated realizations of isotropic maps, we interpret it as the inevitable alignment of mild anisotropic correlations with chance features in a single sky realization; such a feature can also be present, in milder form, when the likelihood is marginalized over orientations. Thus marginalized, the limits on the radius R-i of the largest sphere inscribed in topological domain (at log-likelihood-ratio Delta ln L > -5 relative to a simply-connected flat Planck best-fit model) are: in a flat Universe, R-i > 0.92 chi(rec) for the T3 cubic torus; R-i > 0.71 chi(rec) for the T2 chimney; R-i > 0.50 chi(rec) for the T1 slab; and in a positively curved Universe, R-i > 1.03 chi(rec) for the dodecahedral space; R-i > 1.0 chi(rec) for the truncated cube; and R-i > 0.89 chi(rec) for the octahedral space. The limit for a wider class of topologies, i. e., those predicting matching pairs of back-to-back circles, among them tori and the three spherical cases listed above, coming from the matched-circles search, is R-i > 0.94 chi(rec) at 99% confidence level. Similar limits apply to a wide, although not exhaustive, range of topologies. We also perform a Bayesian search for an anisotropic global Bianchi VIIh geometry. In the non-physical setting where the Bianchi cosmology is decoupled from the standard cosmology, Planck data favour the inclusion of a Bianchi component with a Bayes factor of at least 1.5 units of log-evidence. Indeed, the Bianchi pattern is quite efficient at accounting for some of the large-scale anomalies found in Planck data. However, the cosmological parameters that generate this pattern are in strong disagreement with those found from CMB anisotropy data alone. In the";s:9:"metadata5";s:75:"Planck 2013 results. XXVI. Background geometry and topology of the Universe";s:9:"metadata6";s:2914:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Fabre, O; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, Dl; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Mcewen, Jd; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pogosyan, D; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Riazuelo, A; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321546";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:63;a:14:{s:9:"citazione";s:237:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2014). Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255327";s:6:"handle";s:11:"2108/177415";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2597:"We present new measurements of cosmic infrared background (CIB) anisotropies using Planck. Combining HFI data with IRAS, the angular auto-and cross-frequency power spectrum is measured from 143 to 3000 GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas used to compute the CIB power spectrum and bispectrum are about 2240 and 4400 deg(2), respectively. After careful removal of the contaminants (cosmic microwave background anisotropies, Galactic dust, and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles l similar to 150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from l similar to 130 to 1100, with a total signal to noise ratio of around 6, 19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches are developed for modelling CIB power spectrum anisotropies. The first approach takes advantage of the unique measurements by Planck at large angular scales, and models only the linear part of the power spectrum, with a mean bias of dark matter haloes hosting dusty galaxies at a given redshift weighted by their contribution to the emissivities. The second approach is based on a model that associates star-forming galaxies with dark matter haloes and their subhaloes, using a parametrized relation between the dust-processed infrared luminosity and (sub-) halo mass. The two approaches simultaneously fit all auto-and cross-power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log (M-eff/ M-circle dot) = 12.6 and that CIB galaxies have warmer temperatures as redshift increases. The CIB bispectrum is steeper than that expected from the power spectrum, although well fitted by a power law; this gives some information about the contribution of massive haloes to the CIB bispectrum. Finally, we show that the same halo occupation distribution can fit all power spectra simultaneously. The precise measurements enabled by Planck pose new challenges for the modelling of CIB anisotropies, indicating the power of using CIB anisotropies to understand the process of galaxy formation.";s:9:"metadata5";s:101:"Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation";s:9:"metadata6";s:3081:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bethermin, M; Bielewicz, P; Blagrave, K; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chen, X; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Ghosh, T; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Helou, G; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Kalberla, P; Keihanen, E; Kerp, J; Keskitalo, R; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lacasa, F; Lagache, G; Lahteenmaki, A; Lamarre, J-; Langer, M; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Serra, P; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Welikala, N; White, M; White, Sdm; Winkel, B; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201322093";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:64;a:14:{s:9:"citazione";s:197:"Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandelals, E., et al. (2014). Planck 2013 results. XIX. The integrated Sachs-Wolfe effect. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255330";s:6:"handle";s:11:"2108/177453";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2178:"Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4 sigma, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-l and high-l temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5 sigma. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3 sigma, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4 sigma signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5 sigma at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within Lambda CMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.";s:9:"metadata5";s:59:"Planck 2013 results. XIX. The integrated Sachs-Wolfe effect";s:9:"metadata6";s:3172:"Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandelals, E; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Bartlett, Jg; Bartolo, N; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, E; Coulais, A; Crill, Bp; Curto, A; Cuttaia, E; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Dickinson, C; Diego, Jm; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Fergusson, J; Finelli, F; Fomi, O; Fosalba, P; Frailis, M; Franceschi, E; Frommert, M; Galeotta, S; Ganga, K; Genova-Santos, Rt; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Ek; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Ho, S; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Ilic, S; Jaffe, Ah; Jaffe, Tr; Jasche, J; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Laehteenmaeki, A; Lamarre, J-; Langer, M; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Mangilli, A; Marcos-Caballero, A; Maris, M; Marshall, Dj; Martins, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthais, E; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, E; Pagano, L; Pajot, F; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Racine, B; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Renzi, A; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Schaefer, Bm; Schiavon, F; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutter, P; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Viel, M; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, M; Xia, J-; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321526";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:65;a:14:{s:9:"citazione";s:208:"Ade, P., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., et al. (2014). Planck intermediate results XVI. Profile likelihoods for cosmological parameters. ASTRONOMY & ASTROPHYSICS, 566, A54.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_185765";s:6:"handle";s:10:"2108/88788";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:80:"Planck intermediate results XVI. Profile likelihoods for cosmological parameters";s:9:"metadata6";s:2329:"Ade, P; Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, A; Barreiro, R; Bartlett, J; Battaner, E; Benabed, K; Benoit-Lévy, A; Bernard, J; Bersanelli, M; Bielewicz, P; Bobin, J; Bonaldi, A; Bond, J; Bouchet, F; Burigana, C; Cardoso, J; Catalano, A; Chamballu, A; Chiang, H; Christensen, P; Clements, D; Colombi, S; Colombo, L; Couchot, F; Cuttaia, F; Danese, L; Davies, R; Davis, R; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Dickinson, C; Diego, J; Dole, H; Donzelli, S; Doré, O; Douspis, M; Dupac, X; Enßlin, T; Eriksen, H; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Galli, S; Ganga, K; Giard, M; Giraud-Héraud, Y; González-Nuevo, J; Górski, K; Gregorio, A; Gruppuso, A; Hansen, F; Harrison, D; Henrot-Versillé, S; Hernández-Monteagudo, C; Herranz, D; Hildebrandt, S; Hivon, E; Hobson, M; Holmes, W; Hornstrup, A; Hovest, W; Huffenberger, K; Jaffe, A; Jaffe, T; Jones, W; Juvela, M; Keihänen, E; Keskitalo, R; Kisner, T; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lähteenmäki, A; Lamarre, J; Lasenby, A; Lawrence, C; Leonardi, R; Liddle, A; Liguori, M; Lilje, P; Linden-Vørnle, M; López-Caniego, M; Lubin, P; Macías-Pérez, J; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Martin, P; Martínez-González, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschênes, M; Moneti, A; Montier, L; Morgante, G; Munshi, D; Murphy, J; Naselsky, P; Nati, F; Natoli, P; Noviello, F; Novikov, D; Novikov, I; Oxborrow, C; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Perdereau, O; Perotto, L; Perrotta, F; Pettorino, V; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Popa, L; Pratt, G; Puget, J; Rachen, J; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rouillé d’Orfeuil, B; Rubiño-Martín, J; Rusholme, B; Sandri, M; Savelainen, M; Savini, G; Spencer, L; Spinelli, M; Starck, J; Sureau, F; Sutton, D; Suur-Uski, A; Sygnet, J; Tauber, J; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Wade, L; Wandelt, B; White, M; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201323003";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:66;a:14:{s:9:"citazione";s:181:"Ade, P., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.j., et al. (2014). Planck 2013 results. XXXI. Consistency of the Planck data. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255343";s:6:"handle";s:11:"2108/177441";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2949:"The Planck design and scanning strategy provide many levels of redundancy that can be exploited to provide tests of internal consistency. One of the most important is the comparison of the 70 GHz (amplifier) and 100 GHz (bolometer) channels. Based on different instrument technologies, with feeds located differently in the focal plane, analysed independently by different teams using different software, and near the minimum of diffuse foreground emission, these channels are in effect two different experiments. The 143 GHz channel has the lowest noise level on Planck, and is near the minimum of unresolved foreground emission. In this paper, we analyse the level of consistency achieved in the 2013 Planck data. We concentrate on comparisons between the 70, 100, and 143 GHz channel maps and power spectra, particularly over the angular scales of the first and second acoustic peaks, on maps masked for diffuse Galactic emission and for strong unresolved sources. Difference maps covering angular scales from 8 degrees to 15 ' are consistent with noise, and show no evidence of cosmic microwave background structure. Including small but important corrections for unresolved-source residuals, we demonstrate agreement (measured by deviation of the ratio from unity) between 70 and 100 GHz power spectra averaged over 70 <= l <= 390 at the 0.8% level, and agreement between 143 and 100 GHz power spectra of 0.4% over the same l range. These values are within and consistent with the overall uncertainties in calibration given in the Planck 2013 results. We also present results based on the 2013 likelihood analysis showing consistency at the 0.35% between the 100, 143, and 217 GHz power spectra. We analyse calibration procedures and beams to determine what fraction of these differences can be accounted for by known approximations or systematic errors that could be controlled even better in the future, reducing uncertainties still further. Several possible small improvements are described. Subsequent analysis of the beams quantifies the importance of asymmetry in the near sidelobes, which was not fully accounted for initially, affecting the 70/100 ratio. Correcting for this, the 70, 100, and 143 GHz power spectra agree to 0.4% over the first two acoustic peaks. The likelihood analysis that produced the 2013 cosmological parameters incorporated uncertainties larger than this. We show explicitly that correction of the missing near sidelobe power in the HFI channels would result in shifts in the posterior distributions of parameters of less than 0.3 sigma except for As, the amplitude of the primordial curvature perturbations at 0.05 Mpc(-1), which changes by about 1 sigma. We extend these comparisons to include the sky maps from the complete nine-year mission of the Wilkinson Microwave Anisotropy Probe (WMAP), and find a roughly 2% difference between the Planck and WMAP power spectra in the region of the first acoustic peak.";s:9:"metadata5";s:57:"Planck 2013 results. XXXI. Consistency of the Planck data";s:9:"metadata6";s:2353:"Ade, Par; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bond, Jr; Borrill, J; Bouchet, Fr; Burigana, C; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Christensen, Pr; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Desert, F-; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Hansen, Fk; Hanson, D; Harrison, Dl; Henrot-Versille, S; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Keihaenen, E; Keskitalo, R; Knoche, J; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Lawrence, Cr; Leonardi, R; Leon-Tavares, J; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maino, D; Mandolesi, N; Maris, M; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Matarrese, S; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Oxborrow, Ca; Pagano, L; Pajot, F; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, D; Pearson, Tj; Perdereau, O; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Pratt, Gw; Prunet, S; Puget, J-; Rachen, Jp; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Ristorcelli, I; Rocha, G; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Scott, D; Stolyarov, V; Sudiwala, R; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Wade, La; Wandelt, Bd; Wehus, Ik; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201423743";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:67;a:14:{s:9:"citazione";s:193:"Ade, P.A.R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, E., et al. (2014). Planck 2013 results. VII. HFI time response and beams. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255363";s:6:"handle";s:11:"2108/177403";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:53:"Planck 2013 results. VII. HFI time response and beams";s:9:"metadata6";s:2843:"Ade, P A R; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, E; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bond, Jr; Borrill, J; Bouchet, Fr; Bowyer, Jw; Bridges, M; Bucher, M; Burigana, C; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, E; Danese, L; Davies, Rd; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dunkley, J; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Fraisse, Aa; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Haissinski, J; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hou, Z; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Kneiss, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Leroy, C; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Mactavish, Cj; Maffei, B; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matsumura, T; Matthai, E; Mazzotta, P; Mcgehee, P; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, Ja; Naselsky, P; Nati, E; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polegre, Am; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rowan-Robinson, M; Rusholme, B; Sandri, M; Santos, D; Sauve, A; Savini, G; Scott, D; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sureau, E; Sutton, D; Suur-Uski, A; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Tomasi, M; Tristram, M; Tucci, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321535";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:68;a:14:{s:9:"citazione";s:204:"Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., et al. (2014). Planck 2013 results. II. Low Frequency Instrument data processing. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255329";s:6:"handle";s:11:"2108/177425";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1304:"We describe the data processing pipeline of the Planck Low Frequency Instrument (LFI) data processing centre (DPC) to create and characterize full-sky maps based on the first 15.5 months of operations at 30, 44, and 70 GHz. In particular, we discuss the various steps involved in reducing the data, from telemetry packets through to the production of cleaned, calibrated timelines and calibrated frequency maps. Data are continuously calibrated using the modulation induced on the mean temperature of the cosmic microwave background radiation by the proper motion of the spacecraft. Sky signals other than the dipole are removed by an iterative procedure based on simultaneous fitting of calibration parameters and sky maps. Noise properties are estimated from time-ordered data after the sky signal has been removed, using a generalized least squares map-making algorithm. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices, required to compute statistical uncertainties on LFI and Planck products, are also produced. Main beams are estimated down to the approximate to-20 dB level using Jupiter transits, which are also used for the geometrical calibration of the focal plane.";s:9:"metadata5";s:65:"Planck 2013 results. II. Low Frequency Instrument data processing";s:9:"metadata6";s:2937:"Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cappellini, B; Cardoso, J-; Catalano, A; Chamballu, A; Chen, X; Chiang, L-; Christensen, Pr; Church, S; Colombi, S; Colombo, Lpl; Crill, Bp; Cruz, M; Curto, A; Cattaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Falvella, Mc; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Gaier, Tc; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gjerlow, E; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewel, J; Jones, Wc; Juvela, M; Kangaslahti, P; Keihanen, E; Keskitalo, R; Kiiveri, K; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Lattanzi, M; Laureijs, Rj; Lawrence, Cr; Leach, S; Leahy, Jp; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lindholm, V; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Je; Maggio, G; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Moneti, A; Montier, L; Morgantes, G; Morisset, N; Mortlock, D; Moss, A; Munshi, D; Naseisky, P; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Paci, F; Pagano, L; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Peel, M; Perdereau, O; Perotto, L; Perrotta, F; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Platania, P; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Ricciardi, S; Riller, T; Robbers, G; Rocha, G; Rosset, C; Rossetti, M; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Salerno, E; Sandri, M; Santos, D; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Watson, R; Wehus, Ik; White, Sdm; Wilkson, A; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321550";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:69;a:14:{s:9:"citazione";s:193:"Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., et al. (2014). Planck 2013 results. III. LFI systematic uncertainties. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255333";s:6:"handle";s:11:"2108/177449";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1035:"We present the current estimate of instrumental and systematic effect uncertainties for the Planck-Low Frequency Instrument relevant to the first release of the Planck cosmological results. We give an overview of the main effects and of the tools and methods applied to assess residuals in maps and power spectra. We also present an overall budget of known systematic effect uncertainties, which are dominated by sidelobe straylight pick-up and imperfect calibration. However, even these two effects are at least two orders of magnitude weaker than the cosmic microwave background fluctuations as measured in terms of the angular temperature power spectrum. A residual signal above the noise level is present in the multipole range l < 20, most notably at 30GHz, and is probably caused by residual Galactic straylight contamination. Current analysis aims to further reduce the level of spurious signals in the data and to improve the systematic effects modelling, in particular with respect to straylight and calibration uncertainties.";s:9:"metadata5";s:54:"Planck 2013 results. III. LFI systematic uncertainties";s:9:"metadata6";s:2801:"Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Chamballu, A; Chiang, L-; Cristensen, Pr; Church, S; Olombi, Sc; Colombo, Lpl; Crill, Bp; Cruz, M; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rose, A; de Zotti, G; Delabrouillei, J; Dick, J; Dickinson, C; Diego, Jm; Dole, H; Donzeli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Gaier, Tc; Galeotta, S; Ganga, K; Giard, M; Giraud-Heraud, Y; Gjerlow, E; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewell, J; Jones, Wc; Juvela, M; Kaneaslahti, P; Keihanen, E; Keskitalo, R; Kuveri, K; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lindholm, V; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Mieliaccio, M; Mitra, S; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Paci, F; Pagano, L; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, D; Peel, M; Perdereau, O; Perotto, L; Perrotta, F; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Platania, P; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, I; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Ricciardi, S; Riller, T; Rocha, G; Rosset, C; Rossetti, M; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Salltos, D; Scott, D; Seitiert, Ma; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Stueau, F; Sutton, D; Sum-Uski, A-; Sygnet, J-; Tauber, Ja; Tavaenacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Turler, M; Umana, G; Valenziano, L; Vaiiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Watson, R; Wilkinson, A; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321574";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:70;a:14:{s:9:"citazione";s:215:"Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., et al. (2014). Planck 2013 results. IV. Low Frequency Instrument beams and window functions. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255348";s:6:"handle";s:11:"2108/177417";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1789:"This paper presents the characterization of the in-flight beams, the beam window functions, and the associated uncertainties for the Planck Low Frequency Instrument (LFI). Knowledge of the beam profiles is necessary for determining the transfer function to go from the observed to the actual sky anisotropy power spectrum. The main beam distortions affect the beam window function, complicating the reconstruction of the anisotropy power spectrum at high multipoles, whereas the sidelobes affect the low and intermediate multipoles. The in-flight assessment of the LFI main beams relies on the measurements performed during Jupiter observations. By stacking the data from multiple Jupiter transits, the main beam profiles are measured down to -20 dB at 30 and 44 GHz, and down to -25 dB at 70 GHz. The main beam solid angles are determined to better than 0.2% at each LFI frequency band. The Planck pre-launch optical model is conveniently tuned to characterize the main beams independently of any noise effects. This approach provides an optical model whose beams fully reproduce the measurements in the main beam region, but also allows a description of the beams at power levels lower than can be achieved by the Jupiter measurements themselves. The agreement between the simulated beams and the measured beams is better than 1% at each LFI frequency band. The simulated beams are used for the computation of the window functions for the effective beams. The error budget for the window functions is estimated from both main beam and sidelobe contributions, and accounts for the radiometer bandshapes. The total uncertainties in the effective beam window functions are: 2% and 1.2% at 30 and 44 GHz, respectively (at l approximate to 600), and 0.7% at 70 GHz (at l approximate to 1000).";s:9:"metadata5";s:76:"Planck 2013 results. IV. Low Frequency Instrument beams and window functions";s:9:"metadata6";s:2680:"Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Chamballu, A; Chiang, L-; Christensen, Pr; Church, S; Colombi, S; Colombo, Lpl; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Gaier, Tc; Galeotta, S; Ganga, K; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewell, J; Jones, Wc; Juvela, M; Kangaslahti, P; Keihanen, E; Keskitalo, R; Kiiveri, K; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lindholm, V; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Paci, F; Pagano, L; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Perdereau, O; Perotto, L; Perrotta, F; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Platania, P; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Ricciardi, S; Riller, T; Rocha, G; Rosset, C; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321544";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:71;a:14:{s:9:"citazione";s:178:"Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., et al. (2014). Planck 2013 results. V. LFI calibration. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255337";s:6:"handle";s:11:"2108/177443";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:2166:"We discuss the methods employed to photometrically calibrate the data acquired by the Low Frequency Instrument on Planck. Our calibration is based on a combination of the orbital dipole plus the solar dipole, caused respectively by the motion of the Planck spacecraft with respect to the Sun and by motion of the solar system with respect to the cosmic microwave background (CMB) rest frame. The latter provides a signal of a few mK with the same spectrum as the CMB anisotropies and is visible throughout the mission. In this data release we rely on the characterization of the solar dipole as measured by WMAP. We also present preliminary results (at 44 GHz only) on the study of the Orbital Dipole, which agree with the WMAP value of the solar system speed within our uncertainties. We compute the calibration constant for each radiometer roughly once per hour; in order to keep track of changes in the detectors' gain. Since non-idealities in the optical response of the beams proved to be important, we implemented a fast convolution algorithm which considers the full beam response in estimating the signal generated by the dipole. Moreover, in order to further reduce the impact of residual systematics due to sidelobes, we estimated time variations in the calibration constant of the 30 GHz radiometers (the ones with the largest sidelobes) using the signal of an internal reference load at 4 K instead of the CMB dipole. We have estimated the accuracy of the LFI calibration following two strategies: (1) we have run a set of simulations to assess the impact of statistical errors and systematic effects in the instrument and in the calibration procedure; and (2) we have performed a number of internal consistency checks on the data and on the brightness temperature of Jupiter. Errors in the calibration of this Planck/LFI data release are expected to be about 0.6% at 44 and 70 GHz, and 0.8% at 30 GHz. Both these preliminary results at low and high l are consistent with WMAP results within uncertainties and comparison of power spectra indicates good consistency in the absolute calibration with HFI (0.3%) and a 1.4 sigma discrepancy with WMAP (0.9%).";s:9:"metadata5";s:39:"Planck 2013 results. V. LFI calibration";s:9:"metadata6";s:2794:"Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cappellini, B; Cardoso, J-; Catalano, A; Chamballu, A; Chen, X; Chiang, L-; Christensen, Pr; Church, S; Colombi, S; Colombo, Lpl; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Dickinson, C; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Gaier, Tc; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Giraud-Heraud, Y; Gjerlow, E; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jewell, J; Jones, Wc; Juvela, M; Kangaslahti, P; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leach, S; Leahy, Jp; Leonard, R; Lesgourgues, J; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Maino, D; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Novikov, D; Novikov, I; O'Dwyer, Ij; Osborne, S; Paci, F; Pagano, L; Paladini, R; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Pearson, D; Peel, M; Perdereau, O; Perotto, L; Perrotta, F; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Rebolo, R; Reinecke, M; Remazeilles, M; Ricciardi, S; Riller, T; Rocha, G; Rosset, C; Rossetti, M; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sureau, F; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Tuerler, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Watson, R; Wilkinson, A; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321527";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:72;a:14:{s:9:"citazione";s:210:"Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., et al. (2014). Planck 2013 results. XXVII. Doppler boosting of the CMB: Eppur si muove. ASTRONOMY & ASTROPHYSICS, 571.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255339";s:6:"handle";s:11:"2108/135044";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1084:"Our velocity relative to the rest frame of the cosmic microwave background (CMB) generates a dipole temperature anisotropy on the sky which has been well measured for more than 30 years, and has an accepted amplitude of v/c = 1 x 23(-10), or v = 369 km s(-1). In addition to this signal generated by Doppler boosting of the CMB monopole, our motion also modulates and aberrates the CMB temperature fluctuations (as well as every other source of radiation at cosmological distances). This is an order 10 3 e ff ect applied to fluctuations which are already one part in roughly 105, so it is quite small. Nevertheless, it becomes detectable with the all- sky coverage, high angular resolution, and low noise levels of the Planck satellite. Here we report a first measurement of this velocity signature using the aberration and modulation e ff ects on the CMB temperature anisotropies, finding a component in the known dipole direction, (l; b) = (264 ffi; 48 ffi), of 384 km s 1 +/- 78 km s 1 (stat :) +/- 115 km s 1 (syst :). This is a significant confirmation of the expected velocity.";s:9:"metadata5";s:71:"Planck 2013 results. XXVII. Doppler boosting of the CMB: Eppur si muove";s:9:"metadata6";s:2334:"Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Benabed, K; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Clements, Dl; Colombo, Lpl; Couchot, F; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Diego, Jm; Donzelli, S; Dore, O; Dupac, X; Efstathiou, G; Ensslin, Ta; Eriksen, Hk; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, Dl; Helou, G; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hovest, W; Huffenberger, Km; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leonardi, R; Lewis, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; Macias-Perez, Jf; Mandolesi, N; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Migliaccio, M; Mitra, S; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perrotta, F; Piacentini, F; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Pratt, Gw; Prezeau, G; Puget, J-; Rachen, Jp; Reach, Wt; Reinecke, M; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Rubino-Martin, Ja; Rusholme, B; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Spencer, Ld; Sunyaev, R; Sureau, F; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuerler, M; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, M; Yvon, D; Zacchei, A; Zibin, Jp; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321556";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:73;a:14:{s:9:"citazione";s:159:"Bartalucci, I., Mazzotta, P., Bourdin, H., & Vikhlinin, A. (2014). Chandra ACIS-I particle background: an analytical model. ASTRONOMY & ASTROPHYSICS, 566, A25.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_191025";s:6:"handle";s:10:"2108/91356";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:55:"Chandra ACIS-I particle background: an analytical model";s:9:"metadata6";s:52:"Bartalucci, I; Mazzotta, P; Bourdin, H; Vikhlinin, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201423443";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:74;a:14:{s:9:"citazione";s:227:"Giacintucci, S., Markevitch, M., Brunetti, G., Zuhone, J.a., Venturi, T., Mazzotta, P., et al. (2014). MAPPING THE PARTICLE ACCELERATION IN THE COOL CORE OF THE GALAXY CLUSTER RX J1720.1+2638. THE ASTROPHYSICAL JOURNAL, 795(1).";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255356";s:6:"handle";s:11:"2108/177431";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1377:"We present new deep, high-resolution radio images of the diffuse minihalo in the cool core of the galaxy cluster RX J1720.1+2638. The images have been obtained with the Giant Metrewave Radio Telescope at 317, 617, and 1280 MHz and with the Very Large Array at 1.5, 4.9, and 8.4 GHz, with angular resolutions ranging from 1 '' to 10 ''. This represents the best radio spectral and imaging data set for any minihalo. Most of the radio flux of the minihalo arises from a bright central component with a maximum radius of similar to 80 kpc. A fainter tail of emission extends out from the central component to form a spiral-shaped structure with a length of similar to 230 kpc, seen at frequencies 1.5 GHz and below. We find indication of a possible steepening of the total radio spectrum of the minihalo at high frequencies. Furthermore, a spectral index image shows that the spectrum of the diffuse emission steepens with increasing distance along the tail. A striking spatial correlation is observed between the minihalo emission and two cold fronts visible in the Chandra X-ray image of this cool core. These cold fronts confine the minihalo, as also seen in numerical simulations of minihalo formation by sloshing-induced turbulence. All these observations favor the hypothesis that the radio-emitting electrons in cluster cool cores are produced by turbulent re-acceleration.";s:9:"metadata5";s:88:"MAPPING THE PARTICLE ACCELERATION IN THE COOL CORE OF THE GALAXY CLUSTER RX J1720.1+2638";s:9:"metadata6";s:91:"Giacintucci, S; Markevitch, M; Brunetti, G; Zuhone, Ja; Venturi, T; Mazzotta, P; Bourdin, H";s:9:"metadata7";s:26:"10.1088/0004-637X/795/1/73";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:75;a:14:{s:9:"citazione";s:198:"Giacintucci, S., Markevitch, M., Venturi, T., Clarke, T.e., Cassano, R., & Mazzotta, P. (2014). NEW DETECTIONS OF RADIO MINIHALOS IN COOL CORES OF GALAXY CLUSTERS. THE ASTROPHYSICAL JOURNAL, 781(1).";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255357";s:6:"handle";s:11:"2108/177429";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1617:"Cool cores of some galaxy clusters exhibit faint radio "minihalos." Their origin is unclear, and their study has been limited by their small number. We undertook a systematic search for minihalos in a large sample of X-ray luminous clusters with high-quality radio data. In this article, we report four new minihalos (Lambda 478, ZwCl 3146, RXJ 1532.9+3021, and A 2204) and five candidates found in the reanalyzed archival Very Large Array observations. The radio luminosities of our minihalos and candidates are in the range of 10(23-25) W Hz(-1) at 1.4 GHz, which is consistent with these types of radio sources. Their sizes (40-160 kpc in radius) are somewhat smaller than those of previously known minihalos. We combine our new detections with previously known minihalos, obtaining a total sample of 21 objects, and briefly compare the cluster radio properties to the average X-ray temperature and the total masses estimated from Planck. We find that nearly all clusters hosting minihalos are hot and massive. Beyond that, there is no clear correlation between the minihalo radio power and cluster temperature or mass (in contrast with the giant radio halos found in cluster mergers, whose radio luminosity correlates with the cluster mass). Chandra X-ray images indicate gas sloshing in the cool cores of most of our clusters, with minihalos contained within the sloshing regions in many of them. This supports the hypothesis that radio-emitting electrons are reaccelerated by sloshing. Advection of relativistic electrons by the sloshing gas may also play a role in the formation of the less extended minihalos.";s:9:"metadata5";s:66:"NEW DETECTIONS OF RADIO MINIHALOS IN COOL CORES OF GALAXY CLUSTERS";s:9:"metadata6";s:78:"Giacintucci, S; Markevitch, M; Venturi, T; Clarke, Te; Cassano, R; Mazzotta, P";s:9:"metadata7";s:25:"10.1088/0004-637X/781/1/9";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:76;a:14:{s:9:"citazione";s:246:"Macario, G., Intema, H.t., Ferrari, C., Bourdin, H., Giacintucci, S., Venturi, T., et al. (2014). Discovery of large-scale diffuse radio emission and of a new galaxy cluster in the surroundings of MACS J0520.7-1328. ASTRONOMY & ASTROPHYSICS, 565.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255345";s:6:"handle";s:11:"2108/177435";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1299:"We report the discovery of large-scale diffuse radio emission south-east of the galaxy cluster MACS J0520.7-1328, detected through high-sensitivity Giant Metrewave Radio Telescope 323 MHz observations. This emission is dominated by an elongated diffuse radio source and surrounded by other features of lower surface brightness. Patches of these faint sources are marginally detected in a 1.4 GHz image obtained through a re-analysis of archival NVSS data. Interestingly, the elongated radio source coincides with a previously unclassified extended X-ray source. We perform a multi-wavelength analysis based on archival infrared, optical, and X-ray Chandra data. We find that this source is a low-temperature (similar to 3.6 keV) cluster of galaxies, with indications of a disturbed dynamical state, located at a redshift that is consistent with the one of the main galaxy cluster MACS J0520.7-132 (z = 0.336). We suggest that the diffuse radio emission is associated to non-thermal components in the intracluster and intergalactic medium in and around the newly detected cluster. We are planning deeper multi-wavelength and multi-frequency radio observations to accurately investigate the dynamical scenario of the two clusters and to address the nature of the complex radio emission more precisely.";s:9:"metadata5";s:116:"Discovery of large-scale diffuse radio emission and of a new galaxy cluster in the surroundings of MACS J0520.7-1328";s:9:"metadata6";s:179:"Macario, G; Intema, Ht; Ferrari, C; Bourdin, H; Giacintucci, S; Venturi, T; Mazzotta, P; Bartalucci, I; Johnston-Hollitt, M; Cassano, R; Dallacasa, D; Pratt, Gw; Kale, R; Brown, S";s:9:"metadata7";s:27:"10.1051/0004-6361/201323275";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:77;a:14:{s:9:"citazione";s:282:"Martino, R., Mazzotta, P., Bourdin, H., Smith, G.P., Bartalucci, I., Marrone, D.P., et al. (2014). LoCuSS: hydrostatic mass measurements of the high-L-X cluster sample cross-calibration of Chandra and XMM-Newton. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 443(3), 2342-2360.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255360";s:6:"handle";s:11:"2108/134697";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:112:"LoCuSS: hydrostatic mass measurements of the high-L-X cluster sample cross-calibration of Chandra and XMM-Newton";s:9:"metadata6";s:99:"Martino, R; Mazzotta, P; Bourdin, H; Smith, GP; Bartalucci, I; Marrone, DP; Finoguenov, A; Okabe, N";s:9:"metadata7";s:21:"10.1093/mnras/stu1267";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:78;a:14:{s:9:"citazione";s:248:"Rasia, E., Lau, E.t., Borgani, S., Nagai, D., Dolag, K., Avestruz, C., et al. (2014). TEMPERATURE STRUCTURE OF THE INTRACLUSTER MEDIUM FROM SMOOTHED-PARTICLE HYDRODYNAMICS AND ADAPTIVE-MESH REFINEMENT SIMULATIONS. THE ASTROPHYSICAL JOURNAL, 791(2).";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_255354";s:6:"handle";s:11:"2108/177433";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1391:"Analyses of cosmological hydrodynamic simulations of galaxy clusters suggest that X-ray masses can be underestimated by 10%-30%. The largest bias originates from both violation of hydrostatic equilibrium (HE) and an additional temperature bias caused by inhomogeneities in the X-ray-emitting intracluster medium (ICM). To elucidate this large dispersion among theoretical predictions, we evaluate the degree of temperature structures in cluster sets simulated either with smoothed-particle hydrodynamics (SPH) or adaptive-mesh refinement (AMR) codes. We find that the SPH simulations produce larger temperature variations connected to the persistence of both substructures and their stripped cold gas. This difference is more evident in nonradiative simulations, whereas it is reduced in the presence of radiative cooling. We also find that the temperature variation in radiative cluster simulations is generally in agreement with that observed in the central regions of clusters. Around R500 the temperature inhomogeneities of the SPH simulations can generate twice the typical HE mass bias of the AMR sample. We emphasize that a detailed understanding of the physical processes responsible for the complex thermal structure in ICM requires improved resolution and high-sensitivity observations in order to extend the analysis to higher temperature systems and larger cluster-centric radii.";s:9:"metadata5";s:126:"TEMPERATURE STRUCTURE OF THE INTRACLUSTER MEDIUM FROM SMOOTHED-PARTICLE HYDRODYNAMICS AND ADAPTIVE-MESH REFINEMENT SIMULATIONS";s:9:"metadata6";s:131:"Rasia, E; Lau, Et; Borgani, S; Nagai, D; Dolag, K; Avestruz, C; Granato, Gl; Mazzotta, P; Murante, G; Nelson, K; Ragone-Figueroa, C";s:9:"metadata7";s:26:"10.1088/0004-637X/791/2/96";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:79;a:14:{s:9:"citazione";s:196:"Tauber, J., Ade, P., Aghanim, N., Alves, M., Armitage-Caplan, C., Arnaud, M., et al. (2014). Planck 2013 results. I. Overview of products and scientific results. ASTRONOMY & ASTROPHYSICS, 571, A1.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_240864";s:6:"handle";s:11:"2108/121852";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1869:"The ESA's Planck satellite, dedicated to studying the early Universe and its subsequent evolution, was launched 14 May 2009 and has been scanning the microwave and submillimetre sky continuously since 12 August 2009. This paper gives an overview of the mission and its performance, the processing, analysis, and characteristics of the data, the scientific results, and the science data products and papers in the release. The science products include maps of the CMB and diffuse extragalactic foregrounds, a catalogue of compact Galactic and extragalactic sources, and a list of sources detected through the SZ effect. The likelihood code used to assess cosmological models against the Planck data and a lensing likelihood are described. Scientific results include robust support for the standard six-parameter LCDM model of cosmology and improved measurements of its parameters, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for these parameters and others derived from them are significantly different from those previously determined. Several large-scale anomalies in the temperature distribution of the CMB, first detected by WMAP, are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at greater than 25 sigma. Planck finds no evidence for non-Gaussianity in the CMB. Planck's results agree well with results from the measurements of baryon acoustic oscillations. Planck finds a lower Hubble constant than found in some more local measures. Some tension is also present between the amplitude of matter fluctuations derived from CMB data and that derived from SZ data. The Planck and WMAP power spectra are offset from each other by an average level of about 2% around the first acoustic peak.";s:9:"metadata5";s:67:"Planck 2013 results. I. Overview of products and scientific results";s:9:"metadata6";s:5005:"Tauber, J; Ade, Par; Aghanim, N; Alves, Mir; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Aussel, H; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Barrena, R; Bartelmann, M; Bartlett, Jg; Bartolo, N; Basak, S; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bertincourt, B; Bethermin, M; Bielewicz, P; Bikmaev, I; Blanchard, A; Bobin, J; Bock, Jj; Bohringer, H; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Boulanger, F; Bourdin, H; Bowyer, Jw; Bridges, M; Brown, Ml; Bucher, M; Burenin, R; Burigana, C; Butler, Rc; Calabrese, E; Cappellini, B; Cardoso, J-; Carr, R; Carvalho, P; Casale, M; Castex, G; Catalano, A; Challinor, A; Chamballu, A; Chary, R-; Chen, X; Chiang, Hc; Chiang, L-; Chon, G; Christensen, Pr; Churazov, E; Church, S; Clemens, M; Clements, Dl; Colombi, S; Colombo, Lpl; Combet, C; Comis, B; Couchot, F; Coulais, A; Crill, Bp; Cruz, M; Curto, A; Cuttaia, F; Da Silva, A; Dahle, H; Danese, L; Davies, Rd; Davis, Rj; De Bernardis, P; De Rosa, A; De Zotti, G; Dechelette, T; Delabrouille, J; Delouis, J-; Democles, J; Desert, F-; Dick, J; Dickinson, C; Diego, Jm; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dunkley, J; Dupac, X; Efstathiou, G; Elsner, F; Ensslin, Ta; Eriksen, Hk; Fabre, O; Falgarone, E; Falvella, Mc; Fantaye, Y; Fergusson, J; Filliard, C; Finelli, F; Flores-Cacho, I; Foley, S; Forni, O; Fosalba, P; Frailis, M; Fraisse, Aa; Franceschi, E; Freschi, M; Fromenteau, S; Frommert, M; Gaier, Tc; Galeotta, S; Gallegos, J; Galli, S; Gandolfo, B; Ganga, K; Gauthier, C; Genova-Santos, Rt; Ghosh, T; Giard, M; Giardino, G; Gilfanov, M; Girard, D; Giraud-Heraud, Y; Gjerlow, E; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Gudmundsson, Je; Haissinski, J; Hamann, J; Hansen, Fk; Hansen, M; Hanson, D; Harrison, Dl; Heavens, A; Helou, G; Hempel, A; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Ho, S; Hobson, M; Holmes, Wa; Hornstrup, A; Hou, Z; Hovest, W; Huey, G; Huffenberger, Km; Hurier, G; Ilic, S; Jaffe, Ah; Jaffe, Tr; Jasche, J; Jewell, J; Jones, Wc; Juvela, M; Kalberla, P; Kangaslahti, P; Keihanen, E; Kerp, J; Keskitalo, R; Khamitov, I; Kiiveri, K; Kim, J; Kisner, Ts; Kneissl, R; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lacasa, F; Lagache, G; Lahteenmaki, A; Lamarre, J-; Langer, M; Lasenby, A; Lattanzi, M; Laureijs, Rj; Lavabre, A; Lawrence, Cr; Le Jeune, M; Leach, S; Leahy, Jp; Leonardi, R; Leon-Tavares, J; Leroy, C; Lesgourgues, J; Lewis, A; Li, C; Liddle, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lindholm, V; Lopez-Caniego, M; Lowe, S; Lubin, Pm; Macias-Perez, Jf; Mactavish, Cj; Maffei, B; Maggio, G; Maino, D; Mandolesi, N; Mangilli, A; Marcos-Caballero, A; Marinucci, D; Maris, M; Marleau, F; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matsumura, T; Matthai, F; Maurin, L; Mazzotta, P; Mcdonald, A; Mcewen, Jd; Mcgehee, P; Mei, S; Meinhold, Pr; Melchiorri, A; Melin, J-; Mendes, L; Menegoni, E; Mennella, A; Migliaccio, M; Mikkelsen, K; Millea, M; Miniscalco, R; Mitra, S; Miville-Deschenes, M-; Molinari, D; Moneti, A; Montier, L; Morgante, G; Morisset, N; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Nati, F; Natoli, P; Negrello, M; Nesvadba, Nph; Netterfield, Cb; Norgaard-Nielsen, Hu; North, C; Noviello, F; Novikov, D; Novikov, I; O'Dwyer, Ij; Orieux, F; Osborne, S; O'Sullivan, C; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paladini, R; Pandolfi, S; Paoletti, D; Partridge, B; Pasian, F; Patanchon, G; Paykari, P; Pearson, D; Pearson, Tj; Peel, M; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Pettorino, V; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Platania, P; Pogosyan, D; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Pullen, Ar; Rachen, Jp; Racine, B; Rahlin, A; Rath, C; Reach, Wt; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Renzi, A; Riazuelo, A; Ricciardi, S; Riller, T; Ringeval, C; Ristorcelli, I; Robbers, G; Rocha, G; Roman, M; Rosset, C; Rossetti, M; Roudier, G; Rowan-Robinson, M; Rubino-Martin, Ja; Ruiz-Granados, B; Rusholme, B; Salerno, E; Sandri, M; Sanselme, L; Santos, D; Savelainen, M; Savini, G; Schaefer, Bm; Schiavon, F; Scott, D; Seiffert, Md; Serra, P; Shellard, Eps; Smith, K; Smoot, Gf; Souradeep, T; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutter, P; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Taylor, D; Terenzi, L; Texier, D; Toffolatti, L; Tomasi, M; Torre, J-; Tristram, M; Tucci, M; Tuovinen, J; Turler, M; Tuttlebee, M; Umana, G; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vibert, L; Viel, M; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; Watson, C; Watson, R; Wehus, Ik; Welikala, N; Weller, J; White, M; White, Sdm; Wilkinson, A; Winkel, B; Xia, J-; Yvon, D; Zacchei, A; Zibin, Jp; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321529";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:80;a:14:{s:9:"citazione";s:200:"Tauber, J., Ade, P., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., et al. (2014). Planck 2013 results. XXIV. Constraints on primordial non-gaussianity. ASTRONOMY & ASTROPHYSICS, 571, A24.";s:4:"data";s:4:"2014";s:2:"id";s:20:"PUBBLICAZIONE_240862";s:6:"handle";s:11:"2108/121850";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";s:127:"cosmic background radiation / cosmology: observations / cosmology: theory / early Universe / inflation / methods: data analysis";s:9:"metadata3";s:53:"Settore MAT/06 - Probabilita' e Statistica Matematica";s:9:"metadata4";s:1966:"The Planck nominal mission cosmic microwave background (CMB) maps yield unprecedented constraints on primordial non-Gaussianity (NG). Using three optimal bispectrum estimators, separable template-fitting (KSW), binned, and modal, we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result fNLlocal = 2.7 ± 5.8, fNLequil = -42 ± 75, and fNLorth = -25 ± 39 (68% CL statistical). Non-Gaussianity is detected in the data; using skew-Cℓ statistics we find a nonzero bispectrum from residual point sources, and the integrated-Sachs-Wolfe-lensing bispectrum at a level expected in the ΛCDM scenario. The results are based on comprehensive cross-validation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are confirmed by skew-Cℓ, wavelet bispectrum and Minkowski functional estimators. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and thus derive constraints on early-Universe scenarios that generate primordial NG, including general single-field models of inflation, excited initial states (non-Bunch-Davies vacua), and directionally-dependent vector models. We provide an initial survey of scale-dependent feature and resonance models. These results bound both general single-field and multi-field model parameter ranges, such as the speed of sound, cs ≥ 0.02 (95% CL), in an effective field theory parametrization, and the curvaton decay fraction rD ≥ 0.15 (95% CL). The Planck data significantly limit the viable parameter space of the ekpyrotic/cyclic scenarios. The amplitude of the four-point function in the local model τNL< 2800 (95% CL). Taken together, these constraints represent the highest precision tests to date of physical mechanisms for the origin of cosmic structure.";s:9:"metadata5";s:68:"Planck 2013 results. XXIV. Constraints on primordial non-gaussianity";s:9:"metadata6";s:3054:"Tauber, J; Ade, Par; Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, Aj; Barreiro, Rb; Bartlett, Jg; Bartolo, N; Battaner, E; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, J-; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, Jj; Bonaldi, A; Bonavera, L; Bond, Jr; Borrill, J; Bouchet, Fr; Bridges, M; Bucher, M; Burigana, C; Butler, Rc; Cardoso, J-; Catalano, A; Challinor, A; Chamballu, A; Chiang, Hc; Chiang, L-; Christensen, Pr; Church, S; Clements, Dl; Colombi, S; Colombo, Lpl; Couchot, F; Coulais, A; Crill, Bp; Curto, A; Cuttaia, F; Danese, L; Davies, Rd; Davis, Rj; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Delouis, J-; Desert, F-; Diego, Jm; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dunkley, J; Dupac, X; Efstathiou, G; Elsner, F; Ensslin, Ta; Eriksen, Hk; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, Km; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Fk; Hanson, D; Harrison, D; Heavens, A; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, Sr; Hivon, E; Hobson, M; Holmes, Wa; Hornstrup, A; Hovest, W; Huffenberger, Km; Jaffe, Ah; Jaffe, Tr; Jones, Wc; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, Ts; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lacasa, F; Lagache, G; Lahteenmaki, A; Lamarre, J-; Lasenby, A; Laureijs, Rj; Lawrence, Cr; Leahy, Jp; Leonardi, R; Lesgourgues, J; Lewis, A; Liguori, M; Lilje, Pb; Linden-Vornle, M; Lopez-Caniego, M; Lubin, Pm; MacIas-Perez, Jf; Maffei, B; Maino, D; Mandolesi, N; Mangilli, A; Marinucci, D; Maris, M; Marshall, Dj; Martin, Pg; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Matthai, F; Mazzotta, P; Meinhold, Pr; Melchiorri, A; Mendes, L; Mennella, A; Migliaccio, M; Mitra, S; Miville-Deschenes, M-; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Murphy, Ja; Naselsky, P; Natoli, P; Netterfield, Cb; Norgaard-Nielsen, Hu; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, Ca; Paci, F; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Peiris, Hv; Perdereau, O; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Poutanen, T; Pratt, Gw; Prezeau, G; Prunet, S; Puget, J-; Rachen, Jp; Racine, B; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Renzi, A; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Roudier, G; Rubino-Martin, Ja; Rusholme, B; Sandri, M; Santos, D; Savini, G; Scott, D; Seiffert, Md; Shellard, Eps; Smith, K; Spencer, Ld; Starck, J-; Stolyarov, V; Stompor, R; Sudiwala, R; Sunyaev, R; Sureau, F; Sutter, P; Sutton, D; Suur-Uski, A-; Sygnet, J-; Tauber, Ja; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Tuovinen, J; Valenziano, L; Valiviita, J; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, La; Wandelt, Bd; White, M; White, Sdm; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321554";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:81;a:14:{s:9:"citazione";s:212:"Ade, P., Aghanim, N., Alves, M., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2013). Planck intermediate results. XII: Diffuse Galactic components in the Gould Belt system. ASTRONOMY & ASTROPHYSICS, 557.";s:4:"data";s:7:"2013-09";s:2:"id";s:20:"PUBBLICAZIONE_178670";s:6:"handle";s:10:"2108/86836";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:86:"Planck intermediate results. XII: Diffuse Galactic components in the Gould Belt system";s:9:"metadata6";s:2254:"Ade, P; Aghanim, N; Alves, M; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Balbi, A; Banday, A; Barreiro, R; Bartlett, J; Battaner, E; Bedini, L; Benabed, K; Benoit, A; Bernard, J; Bersanelli, M; Bonaldi, A; Bond, J; Borrill, J; Bouchet, F; Boulanger, F; Burigana, C; Butler, R; Cabella, P; Cardoso, J; Chen, X; Chiang, L; Christensen, P; Clements, D; Colombi, S; Colombo, L; Coulais, A; Cuttaia, F; Davies, R; Davis, R; de Bernardis, P; de Gasperis, G; de Zotti, G; Delabrouille, J; Dickinson, C; Diego, J; Dobler, G; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Ensslin, T; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Genova-Santos, R; Ghosh, T; Giard, M; Giardino, G; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, K; Gregorio, A; Gruppuso, A; Hansen, F; Harrison, D; Hernandez-Monteagudo, C; Hildebrandt, S; Hivon, E; Hobson, M; Holmes, W; Hornstrup, A; Hovest, W; Huffenberger, K; Jaffe, T; Jaffe, A; Juvela, M; Keihanen, E; Keskitalo, R; Kisner, T; Knoche, J; Kunz, M; Kurki-Suonio, H; Lagache, G; Lahteenmaki, A; Lamarre, J; Lasenby, A; Lawrence, C; Leach, S; Leonardi, R; Lilje, P; Linden-Vornle, M; Lubin, P; Macias-Perez, J; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marshall, D; Martin, P; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Melchiorri, A; Mennella, A; Mitra, S; Miville-Deschenes, M; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, J; Naselsky, P; Nati, F; Natoli, P; Norgaard-Nielsen, H; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, C; Pajot, F; Paladini, R; Paoletti, D; Peel, M; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Popa, L; Poutanen, T; Pratt, G; Prunet, S; Puget, J; Rachen, J; Reach, W; Rebolo, R; Reinecke, M; Renault, C; Ricciardi, S; Ristorcelli, I; Rocha, G; Rosset, C; Rubino-Martin, J; Rusholme, B; Salerno, E; Sandri, M; Savini, G; Scott, D; Spencer, L; Stolyarov, V; Sudiwala, R; Suur-Uski, A; Sygnet, J; Tauber, J; Terenzi, L; Tibbs, C; Toffolatti, L; Tomasi, M; Tristram, M; Valenziano, L; Van Tent, B; Varis, J; Vielva, P; Villa, F; Vittorio, N; Wade, L; Wandelt, B; Ysard, N; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201321160";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:82;a:14:{s:9:"citazione";s:271:"Ade, P., Aghanim, N., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., et al. (2013). Planck intermediate results XI. The gas content of dark matter halos: the Sunyaev-Zeldovich-stellar mass relation for locally brightest galaxies. ASTRONOMY & ASTROPHYSICS, 557.";s:4:"data";s:7:"2013-09";s:2:"id";s:20:"PUBBLICAZIONE_178671";s:6:"handle";s:10:"2108/86838";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:144:"Planck intermediate results XI. The gas content of dark matter halos: the Sunyaev-Zeldovich-stellar mass relation for locally brightest galaxies";s:9:"metadata6";s:2537:"Ade, P; Aghanim, N; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Balbi, A; Banday, A; Barreiro, R; Barrena, R; Bartlett, J; Battaner, E; Benabed, K; Bernard, J; Bersanelli, M; Bikmaev, I; Bock, J; Boehringer, H; Bonaldi, A; Bond, J; Borrill, J; Bouchet, F; Bourdin, H; Burenin, R; Burigana, C; Butler, R; Cabella, P; Chamballu, A; Chary, R; Chiang, L; Chon, G; Christensen, P; Clements, D; Colafrancesco, S; Colombi, S; Colombo, L; Comis, B; Coulais, A; Crill, B; Cuttaia, F; Da Silva, A; Dahle, H; Davis, R; de Bernardis, P; de Gasperis, G; de Rosa, A; de Zotti, G; Delabrouille, J; Democles, J; Diego, J; Dole, H; Donzelli, S; Dore, O; Douspis, M; Dupac, X; Efstathiou, G; Ensslin, T; Finelli, F; Flores-Cacho, I; Forni, O; Frailis, M; Franceschi, E; Frommert, M; Galeotta, S; Ganga, K; Genova-Santos, R; Giard, M; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, K; Gregorio, A; Gruppuso, A; Hansen, F; Harrison, D; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, S; Hivon, E; Hobson, M; Holmes, W; Hornstrup, A; Hovest, W; Huffenberger, K; Hurier, G; Jaffe, T; Jaffe, A; Jones, W; Juvela, M; Keihanen, E; Keskitalo, R; Khamitov, I; Kisner, T; Kneissl, R; Knoche, J; Kunz, M; Kurki-Suonio, H; Laheenmaki, A; Lamarre, J; Lasenby, A; Lawrence, C; Le Jeune, M; Leonardi, R; Lilje, P; Linden-Vornle, M; Lopez-Caniego, M; Lubin, P; Luzzi, G; Macias-Perez, J; MacTavish, C; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Marleau, F; Marshall, D; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Mei, S; Melchiorri, A; Melin, J; Mendes, L; Mennella, A; Mitra, S; Miville-Deschenes, M; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, J; Naselsky, P; Nati, F; Natoli, P; Norgaard-Nielsen, H; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, C; Pajot, F; Paoletti, D; Perotto, L; Perrotta, F; Piacentini, F; Piat, M; Pierpaoli, E; Piffaretti, R; Plaszczynski, S; Pointecouteau, E; Polenta, G; Popa, L; Poutanen, T; Pratt, G; Prunet, S; Puget, J; Rachen, J; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Ricciardi, S; Ristorcelli, I; Rocha, G; Roman, M; Rosset, C; Rossetti, M; Rubino-Martin, J; Rusholme, B; Sandri, M; Savini, G; Scott, D; Spencer, L; Starck, J; Stolyarov, V; Sudiwala, R; Sunyaev, R; Sutton, D; Suur-Uski, A; Sygnet, J; Tauber, J; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Valenziano, L; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, L; Wandelt, B; Wang, W; Welikala, N; Weller, J; White, S; White, M; Yvon, D; Zacchei, A; Zonca, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201220941";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:83;a:14:{s:9:"citazione";s:268:"Ade, P., Aghanim, N., Argueeso, F., Arnaud, M., Ashdown, M., Atrio-Barandela, F., et al. (2013). Planck intermediate results VI. The dynamical structure of PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters. ASTRONOMY & ASTROPHYSICS, 550, A132-A132.";s:4:"data";s:4:"2013";s:2:"id";s:20:"PUBBLICAZIONE_163347";s:6:"handle";s:10:"2108/77250";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:128:"Planck intermediate results VI. 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(2013). Planck intermediate results II. Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin imager for 11 galaxy clusters. ASTRONOMY & ASTROPHYSICS, 550.";s:4:"data";s:4:"2013";s:2:"id";s:20:"PUBBLICAZIONE_163353";s:6:"handle";s:10:"2108/77228";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:153:"Planck intermediate results II. 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(2013). Planck intermediate results IX. Detection of the Galactic haze with Planck. ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, 554.";s:4:"data";s:4:"2013";s:2:"id";s:20:"PUBBLICAZIONE_163533";s:6:"handle";s:10:"2108/77253";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:74:"Planck intermediate results IX. Detection of the Galactic haze with Planck";s:9:"metadata6";s:2602:"Ade, P. A. R; Aghanim, N; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Balbi, A; Banday, A. J; Barreiro, R. B; Bartlett, J. G; Battaner, E. ; Benabed, K; Benoit, A; Bernard, J. -P; Bersanelli, M. ; Bonaldi, A; Bond, J. R; Borrill, J; Bouchet, F. R; Burigana, C; Cabella, P; Cardoso, J. -F; Catalano, A; Cayon, L; Chary, R. -R; Chiang, L. -Y; Christensen, P. R. ; Clements, D. L; Colombo, L. P. L; Coulais, A; Crill, B. P; Cuttaia, F; Danese, L; D'Arcangelo, O; Davis, R. 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