Author: "Massardi, Marcella" / Database: OpenAIRE - Searchworks@Jio Institute Digital Library Search Results

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33 results on '"Massardi, Marcella"'

1. The ALMA Science Archive development and the ARI-L project

Author: Massardi, Marcella
Abstract: In the ALMA 2030 development roadmap a crucial role is assigned to the evolution of the ALMA Science Archive to improve the user experience and maximize the scientific exploitation of ALMA data. To date, the Archive accounts for 10 cycles of data summing up to 1.4 PB of raw data and images representative of the data content that cover all the possible science categories from solar observations to cosmology. Most of the data are still unpublished: the ALMA Science Archive is a gold mine for archival users! The expected telescope upgrade will costitute a huge challenge in the archival data management. In view of the next decade telescope development, several upgrades have already been applied to improve the Archive features and offer easy access and experience to the miners. In this talk I will present some of the already available features and examples of their application to science cases. In particular, I will focus on the results of the Additional Representative Images for Legacy (ARI-L) project that has been a European Development project for ALMA Upgrade leaded by the Italian node of the EU ARC. It increased the legacy value of the ALMA Science Archive by bringing the reduction level of ALMA data from Cycles 2-4 close to that of data from more recent Cycles processed for imaging with the ALMA Pipeline. The project produced, assessed the quality of, and delivered to the ALMA Science Archive more than 300000 images for more than 88.5% of the observational datasets from Cycles 2 to 4 processable with the ALMA Pipeline that were missing pipeline-generated images. ARI-L products are certified for quality and can be downloaded from the ALMA Science Archive as ``external products''. The ARI-L project documentation and website are publicly available through the ALMA science portal (https://almascience.org/alma-data/aril).
Published: 2023
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2. The MAYA 2022 conference

Author: Muller, Sebastien, Borkar, Abhijeet, Immer, Katharina, Liuzzo, Elisabetta, Massardi, Marcella, Popping, Gergö, and Sanchez-Monge, Alvaro
Abstract: The first Meeting for ALMA Young Astronomers (MAYA) organised by the European ALMA Regional Centre (ARC) network (Hatziminaoglou et al. 2015) took place online from 2 to 4 March 2022. It was a successful and inspiring event, well attended, with 40–80 participants at any one time. After two years of limited opportunities for socialising because of the COVID-19 pandemic, the event was aimed at gathering together early-career scientists, primarily graduate students and junior postdocs, and giving them the chance to present their work based on ALMA data to their peers, to interact with each other, and to build new collaborations and projects., Published in The Messenger vol. 187, pp. 36-38, June 2022.
Published: 2022

3. Overview of the Additional Representative Images for Legacy (ARI-L) Development Project for the ALMA Science Archive

Author: Massardi, Marcella, Stoehr, Felix, Bendo, George J., Bonato, Matteo, Brand, Jan, Galluzzi, Vincenzo, Guglielmetti, Fabrizia, Knapic, Cristina, Liuzzo, Elisabetta, Marchili, Nicola, Richards, Anita M. S., and Rygl, Kazi L. J.
Abstract: The Additional Representative Images for Legacy (ARI-L) project is a European Development project for ALMA Upgrade approved by the Joint ALMA Observatory and ESO in 2019. It aims to increase the legacy value of the ALMA Science Archive by bringing the reduction level of ALMA data from Cycles 2 to 4 close to that of data from more recent cycles processed for imaging with the ALMA Pipeline. To date, ARI-L has produced, assessed the quality of, and delivered more than 150000 images. These represent more than 85% of the science datasets from Cycles 2 to 4 processable with the ALMA Pipeline but lacking pipeline-generated images, and accordingly the project accomplished all its goals during its official runtime., Published in The Messenger vol. 188, pp. 31-35, September 2022.
Published: 2022
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4. The ALPINE–ALMA [C II] survey

Author: Loiacono, Federica, Decarli, Roberto, Gruppioni, Carlotta, Talia, Margherita, Cimatti, Andrea, Zamorani, Gianni, Pozzi, Francesca, Yan, Lin, Lemaux, Brian C., Riechers, Dominik A., Le Fèvre, Olivier, Bèthermin, Matthieu, Capak, Peter, Cassata, Paolo, Faisst, Andreas, Schaerer, Daniel, Silverman, John D., Bardelli, Sandro, Boquien, Médéric, Burkutean, Sandra, Dessauges-Zavadsky, Miroslava, Fudamoto, Yoshinobu, Fujimoto, Seiji, Ginolfi, Michele, Hathi, Nimish P., Jones, Gareth C., Khusanova, Yana, Koekemoer, Anton M., Lagache, Guilaine, Lubin, Lori M., Massardi, Marcella, Oesch, Pascal, Romano, Michael, Vallini, Livia, Vergani, Daniela, Zucca, Elena, Loiacono, Federica, Decarli, Roberto, Gruppioni, Carlotta, Talia, Margherita, Cimatti, Andrea, Zamorani, Gianni, Pozzi, Francesca, Yan, Lin, Lemaux, Brian C., Riechers, Dominik A., Le Fèvre, Olivier, Bèthermin, Matthieu, Capak, Peter, Cassata, Paolo, Faisst, Andrea, Schaerer, Daniel, Silverman, John D., Bardelli, Sandro, Boquien, Médéric, Burkutean, Sandra, Dessauges-Zavadsky, Miroslava, Fudamoto, Yoshinobu, Fujimoto, Seiji, Ginolfi, Michele, Hathi, Nimish P., Jones, Gareth C., Khusanova, Yana, Koekemoer, Anton M., Lagache, Guilaine, Lubin, Lori M., Massardi, Marcella, Oesch, Pascal, Romano, Michael, Vallini, Livia, Vergani, Daniela, and Zucca, Elena
Subjects: galaxies: evolution – galaxies: high-redshift – galaxies: ISM – submillimeter: galaxies – galaxies: luminosity function, mass function
Abstract: We present the first [C II] 158 µm luminosity function (LF) at z ∼ 5 from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). A search performed over the 118 ALPINE pointings revealed several serendipitous lines. Based on their fidelity, we selected 14 lines for the final catalog. According to the redshift of their counterparts, we identified eight out of 14 detections as [C II] lines at z ∼ 5, and two as CO transitions at lower redshifts. The remaining four lines have an elusive identification in the available catalogs and we considered them as [C II] candidates. We used the eight confirmed [C II] and the four [C II] candidates to build one of the first [C II] LFs at z ∼ 5. We found that 11 out of these 12 sources have a redshift very similar to that of the ALPINE target in the same pointing, suggesting the presence of overdensities around the targets. Therefore, we split the sample in two (a “clustered” and “field” sub–sample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the [C II] LF between z ∼ 5 and z ∼ 0. By converting the [C II] luminosity to star formation rate we evaluated the cosmic star formation rate density (SFRD) at z ∼ 5. The clustered sample results in a SFRD ∼ 10 times higher than previous measurements from UV–selected galaxies. On the other hand, from the field sample (likely representing the average galaxy population) we derived a SFRD ∼ 1.6 higher compared to current estimates from UV surveys but compatible within the errors. Because of the large uncertainties, observations of larger samples are necessary to better constrain the SFRD at z ∼ 5. This study represents one of the first efforts aimed at characterizing the demography of [C II] emitters at z ∼ 5 using a mm–selection of galaxies.
Published: 2021

5. The ALPINE-ALMA [C II] survey:Luminosity function of serendipitous [C II] line emitters at z similar to 5

Author: Loiacono, Federica, Decarli, Roberto, Gruppioni, Carlotta, Talia, Margherita, Cimatti, Andrea, Zamorani, Gianni, Pozzi, Francesca, Yan, Lin, Lemaux, Brian C., Riechers, Dominik A., Le Fevre, Olivier, Bethermin, Matthieu, Capak, Peter, Cassata, Paolo, Faisst, Andreas, Schaerer, Daniel, Silverman, John D., Bardelli, Sandro, Boquien, Mederic, Burkutean, Sandra, Dessauges-Zavadsky, Miroslava, Fudamoto, Yoshinobu, Fujimoto, Seiji, Ginolfi, Michele, Hathi, Nimish P., Jones, Gareth C., Khusanova, Yana, Koekemoer, Anton M., Lagache, Guilaine, Lubin, Lori M., Massardi, Marcella, Oesch, Pascal, Romano, Michael, Vallini, Livia, Vergani, Daniela, and Zucca, Elena
Subjects: ISM [galaxies], mass function, galaxies [submillimeter], evolution [galaxies], high-redshift [galaxies], luminosity function [galaxies]
Abstract: We present the first [C II] 158 mu m luminosity function (LF) at z similar to 5 from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). A study of the 118 ALPINE pointings revealed several serendipitous lines. Based on their fidelity, we selected 14 lines for the final catalog. According to the redshift of their counterparts, we identified eight out of 14 detections as [C II] lines at z similar to 5, along with two as CO transitions at lower redshifts. The remaining four lines have an elusive identification in the available catalogs and we considered them as [C II] candidates. We used the eight confirmed [C II] and the four [C II] candidates to build one of the first [C II] LFs at z similar to 5. We found that 11 out of these 12 sources have a redshift very similar to that of the ALPINE target in the same pointing, suggesting the presence of overdensities around the targets. Therefore, we split the sample in two (a "clustered" and "field" subsample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the [C II] LF between z similar to 5 and z similar to 0. By converting the [C II] luminosity to the star-formation rate, we evaluated the cosmic star-formation rate density (SFRD) at z similar to 5. The clustered sample results in a SFRD similar to 10 times higher than previous measurements from UV-selected galaxies. On the other hand, from the field sample (likely representing the average galaxy population), we derived a SFRD similar to 1.6 higher compared to current estimates from UV surveys but compatible within the errors. Because of the large uncertainties, observations of larger samples will be necessary to better constrain the SFRD at z similar to 5. This study represents one of the first efforts aimed at characterizing the demography of [C II] emitters at z similar to 5 using a mm selection of galaxies.
Published: 2021

6. The ALPINE-ALMA [C II] survey. Luminosity function of serendipitous [C II] line emitters at z \ensuremath∼ 5

Author: Decarli, Roberto, Gruppioni, Carlotta, Talia, Margherita, Cimatti, Andrea, Zamorani, Gianni, Pozzi, Francesca, Yan, Lin, Lemaux, Brian C., Riechers, Dominik A., Le Fèvre, Olivier, Béthermin, Matthieu, Capak, Peter, Cassata, Paolo, Faisst, Andreas, Schaerer, Daniel, Silverman, John D., Bardelli, Sandro, Boquien, Médéric, Burkutean, Sandra, Dessauges-Zavadsky, Miroslava, Fudamoto, Yoshinobu, Fujimoto, Seiji, Ginolfi, Michele, Hathi, Nimish P., Jones, Gareth C., Khusanova, Yana, Koekemoer, Anton M., Lagache, Guilaine, Lubin, Lori M., Massardi, Marcella, Oesch, Pascal, Romano, Michael, Vallini, Livia, Vergani, Daniela, Zucca, Elena, Loiacono, Federica, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute for Educational Technology = The Istituto per le Tecnologie Didattiche (ITD), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Ithaca], Cornell University [New York], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Cosmic Dawn Center (DAWN), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), IT University of Copenhagen (ITU), and Università degli studi di Genova = University of Genoa (UniGe)
Subjects: submillimeter: galaxies, galaxies: luminosity function, galaxies: high-redshift, mass function, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, galaxies: ISM
Published: 2021

7. User interaction models towards the SKA

Author: Massardi, Marcella
Abstract: SKA is an evolutionary jump, not only in data size, but also in the astronomical user approach to the facility. User support upport and efficient interfaces allow a broader community to access the resources offered by SKA and maximize the telescope scientific outcome. The ALMA experience paves the ways but gaps remain in the system and user approach. AENEAS WP5 is focused on the interface between a distributed European SKA Regional Centre (ESRC) and a distributed body of end users whose goal is the exploitation of SKA data for knowledge creation. WP5 therefore studied the design of “user interaction models” that could be implemented for the ESRC. In the presentation we summarize the ingredients define a recommended user interaction scheme for the SRC and the identify some actions to build it.
Published: 2019
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8. Radio sources in next-generation CMB surveys

Author: De Zotti, Gianfranco, Bonato, Matteo, Negrello, Mattia, Herranz, Diego, Lopez-Caniego, Marcos, Trombetti, Tiziana, Burigana, Carlo, Massardi, Marcella, Bonavera, Laura, Gonzalez-Nuevo, Joaquin, Galluzzi, Vincenzo, and Hanany, Shaul
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: CMB surveys provide, for free, blindly selected samples of extragalactic radio sources at much higher frequencies than traditional radio surveys. Next-generation, ground-based CMB experiments with arcmin resolution at mm wavelengths will provide samples of thousands radio sources allowing the investigation of the evolutionary properties of blazar populations, the study of the earliest and latest stages of radio activity, the discovery of rare phenomena and of new transient sources and events. Space-borne experiments will extend to sub-mm wavelengths the determinations of the SEDs of many hundreds of blazars, in temperature and in polarization, allowing us to investigate the flow and the structure of relativistic jets close to their base, and the electron acceleration mechanisms. A real breakthrough will be achieved in the caracterization of the polarization properties. The first direct counts in polarization will be obtained, enabling a solid assessment of the extra-galactic source contamination of CMB maps and allowing us to understand structure and intensity of magnetic fields, particle densities and structures of emitting regions close to the base of the jet., Science white paper submitted to the Astro2020 US Decadal Survey
Published: 2019

9. Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds (Corrigendum)

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Alves, M. I. R., Arnaud, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Ysard, N., Yvon, D., ZACCHEI, Andrea, Zonca, A., Borrill, J., Bouchet, F. R., Boulanger, F., BURIGANA, CARLO, Cardoso, J. -F., Casassus, S., Mazzotta, P., Catalano, A., Chamballu, A., Chen, X., Chiang, H. C., Chiang, L. -Y., Christensen, P. R., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Meinhold, P. R., Crill, B. P., CUTTAIA, FRANCESCO, Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., De Rosa, A., de Zotti, G., Delabrouille, J., Désert, F. -X., Melchiorri, A., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Dupac, X., Enßlin, T. A., Eriksen, H. K., FINELLI, FABIO, Forni, O., FRANCESCHI, ENRICO, Mendes, L., GALEOTTA, Samuele, Ganga, K., Génova-Santos, R. T., Ghosh, T., Giard, M., González-Nuevo, J., Górski, K. M., Gregorio, A., GRUPPUSO, ALESSANDRO, Hansen, F. K., Mennella, A., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Hornstrup, A., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Migliaccio, M., Keihänen, E., Keskitalo, R., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Miville-Deschênes, M. -A., Leonardi, R., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Marshall, D. J., Moneti, A., Martin, P. G., Martínez-González, E., Masi, S., MASSARDI, MARCELLA, Matarrese, S., Montier, L., MORGANTE, GIANLUCA, Benabed, K., Mortlock, D., Munshi, D., Naselsky, P., Nati, F., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Benoit-Lévy, A., Pagano, L., Pajot, F., Paladini, R., PAOLETTI, DANIELA, Patanchon, G., Pearson, T. J., Peel, M., Perdereau, O., Perrotta, F., Piacentini, F., Bernard, J. -P., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Pratt, G. W., Prunet, S., Bersanelli, M., Puget, J. -L., Rachen, J. P., Rebolo, R., Reich, W., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Bielewicz, P., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., SANDRI, MAURA, Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Bobin, J., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., TERENZI, LUCA, Tibbs, C. T., Toffolatti, L., Tomasi, M., Tristram, M., Bonaldi, A., Tucci, M., VALENZIANO, LUCA, Valiviita, J., Van Tent, B., Varis, J., Verstraete, L., Vielva, P., VILLA, FABRIZIO, Wandelt, B. D., Watson, R., Bond, J. R., Wilkinson, A., Cardiff University, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Grupo de Investigación BIOCOST, University of A Coruña (UDC), Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Département d'Electronique, des Détecteurs et d'Informatique (ex SEDI) (DEDI), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Odontostomatologia, Seconda Università degli studi di Napoli, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Imperial College London, Cavendish Laboratory, University of Cambridge [UK] (CAM), Laboratoire de microbiologie, Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-AP-HP Hôpital Raymond Poincaré [Garches], School of Physics and Astronomy [Manchester], University of Manchester [Manchester], Laboratoire de Bactério-Virologie, Centre Hospitalier Universitaire de l'Hôtel Dieu (CHU Hôtel Dieu), Istituto Nazionale di Astrofisica (INAF), Department of Astronomy, University of Rome, Università degli Studi di Roma 'La Sapienza' [Rome], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica, Dipartimento di Fisica, Universita` di Roma Tor Vergata, Università degli Studi di Roma Tor Vergata [Roma], Institut National de la Recherche Scientifique [Québec] (INRS), University of Southern California (USC), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Max-Planck-Institut für Radioastronomie (MPIFR), PLANCK, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpital Raymond Poincaré [AP-HP], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Seconda Università degli Studi di Napoli = Second University of Naples, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Département de Physique des Particules (ex SPP) (DPhP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Spinning dust, Astronomy, Cosmic microwave background, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, CMB cold spot, Interstellar medium, Photometry (optics), 13. Climate action, Space and Planetary Science, 0103 physical sciences, Emissivity, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Optical depth, ComputingMilieux_MISCELLANEOUS
Abstract: Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1deg-smoothed maps from 0.408 GHz up to 3000 GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5sigma) excess emission at frequencies between 20 and 60 GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact HII regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the submillimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14-20 K and an average emissivity index of +1.8, while the non-AME regions are typically warmer, at 20-27 K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase (Abridged).
Published: 2018

10. The ALMA Re-Imaging development study

Author: MASSARDI, MARCELLA, GIANNETTI, ANDREA, Stoehr, Felix, BRAND, JAN, BURKUTEAN, SANDRA, LIUZZO, Elisabetta Teodorina, BONATO, MATTEO, Mancuso, Claudia, Rygl, Kazi, Paladino, Rosita, and Richards, Anita
Published: 2018

11. ALMA FITS header keywords: a study from the archive User perspective

Author: LIUZZO, Elisabetta Teodorina, MASSARDI, MARCELLA, Rygl, Kazi L.J., Stoehr, Felix, GIANNETTI, ANDREA, BONATO, MATTEO, BURKUTEAN, SANDRA, Richards, Anita, and Lacy, Mark
Published: 2018

12. Advanced European Network Of E-Infrastructures For Astronomy With The Ska

Author: Massardi Marcella
Abstract: Here, I present the AENEAS (Advanced European Network of E-infrastructures for Astronomy with the SKA) project has been funded in the Horizon 2020 Work Programme call “Research and Innovation Actions for International Co-operation on high-end e-infrastructure requirements” supporting the Square Kilometre Array (SKA). INAF is contributing to all the AENEAS working packages and leading the WP5 - Access and Knowledge Creation (WP leader M. Massardi IRA-ARC), participants from IRA (Brand, Nanni, Venturi) ,OACT(Becciani, Costa, Umana), OATS (Smareglia, Knapic, Taffoni)
Published: 2017
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13. The Alma Re-Imaging (Ari) Development Study

Author: Massardi Marcella
Abstract: Here it is presented the ALMA Re-Imaging (ARI) development study which the IT ARC node is leading.
Published: 2017
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14. The Main Sequence Of Star Forming Galaxies And Agns At High-Z: Evidence For In Situ Coevolution

Author: Mancuso Claudia, Lapi Andrea, Massardi Marcella, and Danese Luigi
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Galaxies, High redshift, Main sequence, Co evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We provide a novel, unifying physical interpretation on the origin, the average shape, the scatter and the cosmic evolution for the main sequence of star forming galaxies and AGNs at high redshift (z>1). We achieve this goal in a model independent way, starting from redshift-dependent SFR functions based on the latest UV/ far-IR data from HST/Herschel and related statistics of strong gravitationally lensed sources (see for details Fig. 1 in Mancuso, Lapi et al. 2016a, ApJ 823,128). We also used deterministic evolutionary tracks for the history of star formation and black hole accretion, inspired by the in situ co-evolution scenario (see Fig. 2), and gauged on a wealth of multiwavelength observations including the observed Eddington ratio distribution. We validated our ingredients against many observables (see Mancuso, Lapi et al. 2016A, ApJ 823,128). The resulting Main Sequences are in excellent agreement with current observational data. We also provided a new interpretation for off-main sequence galaxies and AGNs in terms of the in situ coevolution scenario.
Published: 2017
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15. Planck 2013 results. XXI. Cosmology with the all-sky Planck Compton parameter y-map

Author: Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, ANNA VALENTINA, Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Carvalho, P., Catalano, A., Challinor, A., Chamballu, A., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Comis, B., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Da Silva, A., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Flores Cacho, I., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Génova Santos, R. T., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lacasa, F., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leahy, J. P., Leonardi, R., León Tavares, J., Lesgourgues, J., Liguori, Michele, Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Marcos Caballero, A., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, Marcella, Matarrese, Sabino, Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. B., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., 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, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., 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, L. A., Wandelt, B. D., White, S. D. M., Yvon, D., Zacchei, A., and Zonca, A.
Published: 2014

16. The Polarized Radiation Imaging and Spectroscopy Mission

Author: André, Philippe, Baccigalupi, Carlo, Banday, Anthony, Barbosa, Domingos, Barreiro, Belen, Bartlett, James, Bartolo, Nicola, Battistelli, Elia, Battye, Richard, Bendo, George, Benoȋt, Alain, Bernard, Jean-Philippe, Bersanelli, Marco, Béthermin, Matthieu, Bielewicz, Pawel, Bonaldi, Anna, Bouchet, François, Boulanger, François, Brand, Jan, Bucher, Martin, Burigana, Carlo, Cai, Zhen-Yi, Camus, Philippe, Casas, Francisco, Casasola, Viviana, Castex, Guillaume, Challinor, Anthony, Chluba, Jens, Chon, Gayoung, Colafrancesco, Sergio, Comis, Barbara, Cuttaia, Francesco, D'Alessandro, Giuseppe, Da Silva, Antonio, Davis, Richard, de Avillez, Miguel, de Bernardis, Paolo, de Petris, Marco, de Rosa, Adriano, de Zotti, Gianfranco, Delabrouille, Jacques, Désert, François-Xavier, Dickinson, Clive, Diego, Jose Maria, Dunkley, Joanna, Enßlin, Torsten, Errard, Josquin, Falgarone, Edith, Ferreira, Pedro, Ferrière, Katia, Finelli, Fabio, Fletcher, Andrew, Fosalba, Pablo, Fuller, Gary, Galli, Silvia, Ganga, Ken, García-Bellido, Juan, Ghribi, Adnan, Giard, Martin, Giraud-Héraud, Yannick, Gonzalez-Nuevo, Joaquin, Grainge, Keith, Gruppuso, Alessandro, Hall, Alex, Hamilton, Jean-Christophe, Haverkorn, Marijke, Hernandez-Monteagudo, Carlos, Herranz, Diego, Jackson, Mark, Jaffe, Andrew, Khatri, Rishi, Kunz, Martin, Lamagna, Luca, Lattanzi, Massimiliano, Leahy, Paddy, Lesgourgues, Julien, Liguori, Michele, Liuzzo, Elisabetta, Lopez-Caniego, Marcos, Macias-Perez, Juan, Maffei, Bruno, Maino, Davide, Mangilli, Anna, Martinez-Gonzalez, Enrique, Martins, Carlos J.A.P., Masi, Silvia, Massardi, Marcella, Matarrese, Sabino, Melchiorri, Alessandro, Melin, Jean-Baptiste, Mennella, Aniello, Mignano, Arturo, Miville-Deschênes, Marc-Antoine, Monfardini, Alessandro, Murphy, Anthony, Naselsky, Pavel, Nati, Federico, Natoli, Paolo, Negrello, Mattia, Noviello, Fabio, O'Sullivan, Créidhe, Paci, Francesco, Pagano, Luca, Paladino, Rosita, Palanque-Delabrouille, Nathalie, Paoletti, Daniela, Peiris, Hiranya, Perrotta, Francesca, Piacentini, Francesco, Piat, Michel, Piccirillo, Lucio, Pisano, Giampaolo, Polenta, Gianluca, Pollo, Agnieszka, Ponthieu, Nicolas, Remazeilles, Mathieu, Ricciardi, Sara, Roman, Matthieu, Rosset, Cyrille, Rubino-Martin, Jose-Alberto, Salatino, Maria, Schillaci, Alessandro, Shellard, Paul, Silk, Joseph, Starobinsky, Alexei, Stompor, Radek, Sunyaev, Rashid, Tartari, Andrea, Terenzi, Luca, Toffolatti, Luigi, Tomasi, Maurizio, Trappe, Neil, Tristram, Matthieu, Trombetti, Tiziana, Tucci, Marco, Van de Weijgaert, Rien, Van Tent, Bartjan, Verde, Licia, Vielva, Patricio, Wandelt, Ben, Watson, Robert, Withington, Stafford, and Cabrera, Nicolas
Subjects: Astrophysics and Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013as a large-class mission for investigating within the framework of the ESA Cosmic Visionprogram a set of important scientific questions that require high resolution, high sensitivity, full-skyobservations of the sky emissionat wavelengths ranging from millimeter-wave to the far-infrared.PRISM's main objective is to explore the distant universe, probing cosmichistory from very early times until now as well as the structures, distribution ofmatter, and velocity flows throughout our Hubble volume. PRISM willsurvey the full sky in a large number of frequency bands in bothintensity and polarization and will measure the absolute spectrum of sky emission more thanthree orders of magnitude better than COBE FIRAS. The data obtained will allow usto precisely measure the absolute sky brightness and polarization of all the components of thesky emission in the observed frequency range,separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions.The aim of this Extended White Paper is to provide a more detailed overview of the highlightsof the new science that will be made possible by PRISM, which include: (1) the ultimategalaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 106clusters extending to large redshift, including a characterization of the gas temperature ofthe brightest ones (through the relativistic corrections to the classic SZ template) as wellas a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubblevolume; (2) a detailed characterization of the properties and evolution of dusty galaxies, wherethe most of the star formation in the universe took place, the faintest population of whichconstitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes fromprimordial gravity waves generated during inflation and from gravitational lensing, as wellas the ultimate search for primordial non-Gaussianity using CMB polarization, which is lesscontaminated by foregrounds on small scales than the temperature anisotropies; (4) a searchfor distortions from a perfect blackbody spectrum, which include some nearly certain signalsand others that are more speculative but more informative; and (5) a study of the role of themagnetic field in star formation and its interaction with other components of theinterstellar medium of our Galaxy. These are but a few of the highlights presented herealong with a description of the proposed instrument. PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM
Published: 2013

17. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

Author: Andre, Philippe, Baccigalupi, Carlo, Barbosa, Domingos, Bartlett, James, Bartolo, Nicola, Battistelli, Elia, Battye, Richard, Bendo, George, Bernard, Jean-Philippe, Bersanelli, Marco, Bethermin, Matthieu, Bielewicz, Pawel, Bonaldi, Anna, Bouchet, Francois, Boulanger, Francois, Brand, Jan, Bucher, Martin, Burigana, Carlo, Cai, Zhen-Yi, Casasola, Viviana, Castex, Guillaume, Challinor, Anthony, Chluba, Jens, Colafrancesco, Sergio, Cuttaia, Francesco, D Alessandro, Giuseppe, Davis, Richard, Avillez, Miguel, Bernardis, Paolo, Petris, Marco, Rosa, Adriano, Zotti, Gianfranco, Delabrouille, Jacques, Dickinson, Clive, Diego, Jose Maria, Falgarone, Edith, Ferreira, Pedro, Ferriere, Katia, Finelli, Fabio, Fletcher, Andrew, Fuller, Gary, Galli, Silvia, Ganga, Ken, Juan Garcia-Bellido, Ghribi, Adnan, Gonzalez-Nuevo, Joaquin, Grainge, Keith, Gruppuso, Alessandro, Hall, Alex, Hernandez-Monteagudo, Carlos, Jackson, Mark, Jaffe, Andrew, Khatri, Rishi, Lamagna, Luca, Lattanzi, Massimiliano, Leahy, Paddy, Liguori, Michele, Liuzzo, Elisabetta, Lopez-Caniego, Marcos, Macias-Perez, Juan, Maffei, Bruno, Maino, Davide, Masi, Silvia, Mangilli, Anna, Massardi, Marcella, Matarrese, Sabino, Melchiorri, Alessandro, Melin, Jean-Baptiste, Mennella, Aniello, Mignano, Arturo, Miville-Deschenes, Marc-Antoine, Nati, Federico, Natoli, Paolo, Negrello, Mattia, Noviello, Fabio, Paci, Francesco, Paladino, Rosita, Paoletti, Daniela, Perrotta, Francesca, Piacentini, Francesco, Piat, Michel, Piccirillo, Lucio, Pisano, Giampaolo, Polenta, Gianluca, Ricciardi, Sara, Roman, Matthieu, Rubino-Martin, Jose-Alberto, Salatino, Maria, Schillaci, Alessandro, Shellard, Paul, Silk, Joseph, Stompor, Radek, Sunyaev, Rashid, Tartari, Andrea, Terenzi, Luca, Toffolatti, Luigi, Tomasi, Maurizio, Trombetti, Tiziana, Tucci, Marco, Tent, Bartjan, Verde, Licia, Wandelt, Ben, Withington, Stafford, Starita, Sabine, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, INFN, Sezione di Padova, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Informatique pour la Mécanique et les Sciences de l'Ingénieur (LIMSI), Université Paris Saclay (COmUE)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université - UFR d'Ingénierie (UFR 919), Sorbonne Université (SU)-Sorbonne Université (SU)-Université Paris-Saclay-Université Paris-Sud - Paris 11 (UP11), Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), ASI-ASDC, APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Departamento de Fisica Teorica, Universidad Autonoma de Madrid (UAM), APC - THEORIE, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), ICRA and Physics Department, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Department of Applied Mathematics and Theoretical Physics (DAMTP), University of Cambridge [UK] (CAM), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Université Paris-Saclay-Sorbonne Université - UFR d'Ingénierie (UFR 919), Sorbonne Université (SU)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Saclay (COmUE), Istituto di Radioastronomia (IRA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik, Università degli Studi di Roma 'La Sapienza' [Rome], Department of Applied Mathematics and Theoretical Physics / Centre for Mathematical Sciences (DAMTP/CMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris-Sud - Paris 11 (UP11)-Sorbonne Université - UFR d'Ingénierie (UFR 919), Sorbonne Université (SU)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Saclay (COmUE), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut für theoretische Physik, and Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [MATH.MATH-MP]Mathematics [math]/Mathematical Physics [math-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics, [MATH.MATH-MP] Mathematics [math]/Mathematical Physics [math-ph]
Abstract: 20 pages Latex; PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in response to the Call for White Papers for the definition of the L2 and L3 Missions in the ESA Science Programme. PRISM would have two instruments: (1) an imager with a 3.5m mirror (cooled to 4K for high performance in the far-infrared---that is, in the Wien part of the CMB blackbody spectrum), and (2) an Fourier Transform Spectrometer (FTS) somewhat like the COBE FIRAS instrument but over three orders of magnitude more sensitive. Highlights of the new science (beyond the obvious target of B-modes from gravity waves generated during inflation) made possible by these two instruments working in tandem include: (1) the ultimate galaxy cluster survey gathering 10e6 clusters extending to large redshift and measuring their peculiar velocities and temperatures (through the kSZ effect and relativistic corrections to the classic y-distortion spectrum, respectively) (2) a detailed investigation into the nature of the cosmic infrared background (CIB) consisting of at present unresolved dusty high-z galaxies, where most of the star formation in the universe took place, (3) searching for distortions from the perfect CMB blackbody spectrum, which will probe a large number of otherwise inaccessible effects (e.g., energy release through decaying dark matter, the primordial power spectrum on very small scales where measurements today are impossible due to erasure from Silk damping and contamination from non-linear cascading of power from larger length scales). These are but a few of the highlights of the new science that will be made possible with PRISM.
Published: 2013

18. Planck 2013 results. XII. Component separation

Author: Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Castex, G., Catalano, A., Challinor, A., Chamballu, A., Chary, R. R., Chen, X., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dobler, G., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huey, G., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Keihånen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Le Jeune, M., Leach, S., Leahy, J. P., Leonardi, R., Lesgourgues, J., Liguori, Michele, Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Marcos Caballero, A., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, Marcella, Matarrese, Sabino, Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mikkelsen, K., Mitra, S., Miville Deschênes, M. A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O’Dwyer, I. J., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., 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, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., 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., Martín, J. A. Rubiño., Rusholme, B., Salerno, E., Sandri, M., Santos, D., Savini, G., Schiavon, F., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Viel, M., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wehus, I. K., Wilkinson, A., Xia, J. Q., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck has produced detailed all-sky observations over nine frequency bands between 30 and 857 GHz. These observations allow robust reconstruction of the primordial cosmic microwave background (CMB) temperature fluctuations over nearly the full sky, as well as new constraints on Galactic foregrounds. This paper describes the component separation framework adopted by Planck. We test four foreground-cleaned CMB maps derived using qualitatively different component separation algorithms. The quality of our reconstructions is evaluated through detailed simulations and internal comparisons, and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to l = 2000. The parameter constraints on LambdaCDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis. We choose two of the CMB maps for specific scientific goals. We also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission. The component maps are found to provide a faithful representation of the sky, as evaluated by simulations. For the low-frequency component, the spectral index varies widely over the sky, ranging from about beta = -4 to -2. Considering both morphology and prior knowledge of the low frequency components, the index map allows us to associate a steep spectral index (beta < -3.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of beta > -2.3 with strong free-free emission, and intermediate values with synchrotron emission., 31 pages, 32 figures, submitted to A&A
Published: 2013

19. A 20 GHz bright sample for δ > +72° — I. Catalogue

Author: Righini, S., Massardi, Marcella, and López-Caniego, M.
Subjects: Radio continuum: general, Methods: observational, active [Galaxies], general [Radio continuum], observational [Methods], Galaxies: active
Abstract: S. Righini et al., During 2010–11, the Medicina 32-m dish hosted the seven-feed 18–26.5 GHz receiver built for the Sardinia Radio Telescope, with the goal to perform its commissioning. This opportunity was exploited to carry out a pilot survey at 20 GHz over the area for δ > +72.◦3. This paper describes all the phases of the observations, as they were performed using new hardware and software facilities. The map-making and source extraction procedures are illustrated. A customized data reduction tool was used during the follow-up phase, which produced a list of 73 confirmed sources down to a flux density of 115 mJy. The resulting catalogue, presented here, is complete above 200 mJy. Source counts are in agreement with those provided by the Australia Telescope 20 GHz (AT20G) survey. This pilot activity paves the way for a larger project, the K-band Northern Wide Survey (KNoWS), whose final aim is to survey the whole Northern hemisphere down to a flux limit of 50 mJy (5σ).
Published: 2012

20. The Planck-ATCA Co-eval Observations project: the bright sample

Author: Massardi, Marcella, López-Caniego, M., and Zotti, G. de
Subjects: Radio continuum: general, active [Galaxies], general [Radio continuum], galaxies [Radio continuum], Galaxies: active, Cosmic background radiation, Radio continuum: galaxies
Abstract: 14 páginas, 11 figuras, 6 tablas.-- El Pdf del artículo es la versión pre-print: arXiv:1101.0225v2.-- et al., The Planck Australia Telescope Compact Array (Planck-ATCA) Co-eval Observations (PACO) have provided flux density measurements of well-defined samples of Australia Telescope 20 GHz (AT20G) radio sources at frequencies below and overlapping with Planck frequency bands, almost simultaneously with Planck observations. We have observed with the ATCA a total of 482 sources in the frequency range between 4.5 and 40 GHz in the period between 2009 July and 2010 August. Several sources were observed more than once. In this paper we present the aims of the project, the selection criteria, and the observation and data reduction procedures. We also discuss the data in total intensity for a complete sample of 189 sources with S20 GHz > 500 mJy, Galactic latitude |b| > 5° and declination δ < −30°, and some statistical analysis of the spectral behaviour and variability of this sample, referred to as the ‘bright PACO sample’. Finally, we discuss how these data could be used to transfer absolute calibrations to ground-based telescopes using the cosmic microwave background dipole calibrated flux densities measured by the Planck satellite, and we provide some test fluxes on bright calibrators., MM, AB and GDZ acknowledge financial support from ASI (ASI/INAF Agreement I/072/09/0 for the Planck LFI activity of Phase E2 and contract I/016/07/0 COFIS). MLC acknowledges partial financial support from the Spanish Ministerio de Ciencia e Innovación proyects AYA2010-21766-C03-01 and CSD2010-00064. RDE acknowledges support from an Australian Federation Fellowship (FF0345330).
Published: 2011

21. Optical Properties of High-Frequency Radio Sources from the Australia Telescope 20 GHz (AT20G) Survey

Author: Mahony, Elizabeth K., Sadler, Elaine M., Croom, Scott M., Ekers, Ronald D., Bannister, Keith W., Chhetri, Rajan, Hancock, Paul J., Johnston, Helen M., Massardi, Marcella, and Murphy, Tara
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Our current understanding of radio-loud AGN comes predominantly from studies at frequencies of 5 GHz and below. With the recent completion of the Australia Telescope 20 GHz (AT20G) survey, we can now gain insight into the high-frequency radio properties of AGN. This paper presents supplementary information on the AT20G sources in the form of optical counterparts and redshifts. Optical counterparts were identified using the SuperCOSMOS database and redshifts were found from either the 6dF Galaxy survey or the literature. We also report 144 new redshifts. For AT20G sources outside the Galactic plane, 78.5% have optical identifications and 30.9% have redshift information. The optical identification rate also increases with increasing flux density. Targets which had optical spectra available were examined to obtain a spectral classification. There appear to be two distinct AT20G populations; the high luminosity quasars that are generally associated with point-source optical counterparts and exhibit strong emission lines in the optical spectrum, and the lower luminosity radio galaxies that are generally associated with passive galaxies in both the optical images and spectroscopic properties. It is suggested that these different populations can be associated with different accretion modes (cold-mode or hot-mode). We find that the cold-mode sources have a steeper spectral index and produce more luminous radio lobes, but generally reside in smaller host galaxies than their hot-mode counterparts. This can be attributed to the fact that they are accreting material more efficiently. Lastly, we compare the AT20G survey with the S-cubed semi-empirical (S3-SEX) models and conclude that the S3-SEX models need refining to correctly model the compact cores of AGN. The AT20G survey provides the ideal sample to do this., Comment: Accepted for publication in MNRAS
Published: 2011
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22. The Planck-ATCA Co-eval Observations (PACO) project: the bright sample

Author: Massardi, Marcella, Bonaldi, Anna, Bonavera, Laura, López-Caniego, Marcos, De Zotti, Gianfranco, and Ekers, Ronald D.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Planck-ATCA Co-eval Observations (PACO) have provided flux density measurements of well defined samples of AT20G radio sources at frequencies below and overlapping with Planck frequency bands, almost simultaneously with Planck observations. We have observed with the Australia Telescope Compact Array (ATCA) a total of 482 sources in the frequency range between 4.5 and 40 GHz in the period between July 2009 and August 2010. Several sources were observed more than once. In this paper we present the aims of the project, the selection criteria, and the observation and data reduction procedures. We also discuss the data in total intensity for a complete sample of 189 sources with S(20 GHz)>500 mJy, Galactic latitude |b|>5deg, and declination, Comment: 15 pages, 11 figure. Accepted for publication on MNRAS. Catalogue available
Published: 2011
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23. The Planck-ATCA Coeval Observations (PACO) project: the faint sample

Author: Bonavera, Laura, Massardi, Marcella, Bonaldi, Anna, Gonzalez-Nuevo, Joaquin, De Zotti, Gianfranco, and Ekers, Ronald D.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Planck-ATCA Co-eval Observations (PACO) project collected data between 4.5 and 40 GHz for 482 sources selected within the Australia Telescope 20 GHz (AT20G) catalogue and observed with the Australia Telescope Compact Array (ATCA). Observations were done almost simultaneously with the Planck satellite, in the period between July 2009 and August 2010. In this paper we present and discuss the data for the complete sample of 159 sources with S(AT20G)>200 mJy in the Southern ecliptic pole region. The Planck Early Release Compact Source Catalogue (ERCSC) contains 57 of our sources. A comparison between the PACO catalogue and the ERCSC confirms that the reliability of the latter is better than 95 per cent. The missing ERCSC sources are typically associated with the Large Magellanic Cloud, the Milky Way or are otherwise extended. The spectral analysis of the PACO faint catalogue shows a spectral steepening of the sources at high frequencies, confirming the results obtained from the PACO bright sample. A comparison with AT20G measurements, carried out, on average, a few years earlier, has demonstrated that, on these timescales, our sources show a rather high variability with an rms amplitude of ~40 per cent at 20 GHz. The source spectral properties are found not to vary substantially with flux density, except for an increase of the fraction of steep spectrum sources at fainter flux densities. Our data also allow us to extend by a factor ~5 downwards in flux density the source counts at ~33 GHz and ~40 GHz obtained from Planck's Early Release Compact Source catalogue. This allows us to substantially improve our control on the contribution of unresolved extragalactic sources to the power spectrum of small scale fluctuations in CMB maps.
Published: 2011
Full Text: View/download PDF

24. The Australia Telescope 20GHz (AT20G) Survey: analysis of the extragalactic source sample

Author: Massardi, Marcella, Ekers, Ronald D., Murphy, Tara, Mahony, Elizabeth, Hancock, Paul J., Chhetri, Rajan, De Zotti, Gianfranco, Sadler, Elaine M., Burke-Spolaor, Sarah, Calabretta, Mark, Edwards, Philip G., Ekers, Jennifer A., Jackson, Carole A., Kesteven, Michael J., Newton-McGee, Katherine, Phillips, Chris, Ricci, Roberto, Roberts, Paul, Sault, Robert J., Staveley-Smith, Lister, Subrahmanyan, Ravi, Walker, Mark A., and Wilson, Warwick E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Australia Telescope 20 GHz (AT20G) survey is a blind survey of the whole Southern sky at 20 GHz with follow-up observations at 4.8, 8.6, and 20 GHz carried out with the Australia Telescope Compact Array (ATCA). In this paper we present an analysis of radio spectral properties in total intensity and polarisation, sizes, optical identifications, and redshifts of the sample of the 5808 extragalactic sources in the survey catalogue of confirmed sources over the whole Southern sky excluding the strip at Galactic latitude |b|500mJy, to 60% for S, Comment: 15 pages, 16 figures, accepted for publication in MNRAS
Published: 2010

25. The extragalactic sources at mm wavelengths and their role as CMB foregrounds

Author: Massardi, Marcella
Subjects: Settore FIS/05 - Astronomia e Astrofisica
Published: 2008

26. Statistical properties of extragalactic sources in the New Extragalactic WMAP Point Source (NEWPS) catalogue

Author: González-Nuevo González, Joaquín, Massardi, Marcella, Argüeso Gómez, Francisco, Herránz Muñoz, Diego, Toffolatti, Luigi, Sanz Estévez, José Luis, López Caniego, Marcos, and De Zotti, Gianfranco
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present results on spectral index distributions, number counts, redshift distribution and other general statistical properties of extragalactic point sources in the NEWPS5 sample L\'opez-Caniego et al. (2007). The flux calibrations at all the WMAP channels have been reassessed both by comparison with ground based observations and through estimates of the effective beam areas. The two methods yield consistent statistical correction factors. A search of the NED has yielded optical identifications for 89% of sources in the complete sub-sample of 252 sources with S/N>5 and S>1.1 Jy at 23 GHz; 5 sources turned out to be Galactic and were removed. The NED also yielded redshifts for 92% of the extragalactic sources at |b|>10deg. Their distribution was compared with model predictions; the agreement is generally good but a possible discrepancy is noted. Using the 5 GHz fluxes from the GB6 or PMN surveys, we find that 76% of the 191 extragalactic sources with S_23GHz>1.3,Jy can be classified as flat-spectrum sources between 5 and 23 GHz. A spectral steepening is observed at higher frequencies: only 59% of our sources are still flat-spectrum sources between 23 and 61 GHz and the average spectral indexes steepen from = 0.01\pm 0.03 to = 0.37\pm 0.03. We think, however, that the difference may be due to a selection effect. The source number counts have a close to Euclidean slope and are in good agreement with the predictions of the cosmological evolution model by De Zotti et al. (2005). The observed spectral index distributions were exploited to get model-independent extrapolations of counts to higher frequencies. The risks of such operations are discussed and reasons of discrepancies with other recent estimates are clarified., Comment: 8 pages, 4 figures. Accepted for publication in MNRAS
Published: 2008

27. The Australia Telescope 20 GHz (AT20G) Survey: The Bright Source Sample

Author: Massardi, Marcella, Ekers, Ronald D., Murphy, Tara, Ricci, Roberto, Sadler, Elaine M., Burke, Sarah, De Zotti, Gianfranco, Edwards, Philip G., Hancock, Paul J., Jackson, Carole A., Kesteven, Michael J., Mahony, Elizabeth, Phillips, Christopher J., Staveley--Smith, Lister, Subrahmanyan, Ravi, Walker, Mark A., and Wilson, Warwick E.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The Australia Telescope 20 GHz (AT20G) Survey is a blind survey of the whole Southern sky at 20 GHz (with follow-up observations at 4.8 and 8.6 GHz) carried out with the Australia Telescope Compact Array (ATCA) from 2004 to 2007. The Bright Source Sample (BSS) is a complete flux-limited subsample of the AT20G Survey catalogue comprising 320 extragalactic (|b|>1.5 deg) radio sources south of dec = -15 deg with S(20 GHz) > 0.50 Jy. Of these, 218 have near simultaneous observations at 8 and 5 GHz. In this paper we present an analysis of radio spectral properties in total intensity and polarisation, size, optical identifications and redshift distribution of the BSS sources. The analysis of the spectral behaviour shows spectral curvature in most sources with spectral steepening that increases at higher frequencies (the median spectral index \alpha, assuming S\propto \nu^\alpha, decreases from \alpha_{4.8}^{8.6}=0.11 between 4.8 and 8.6 GHz to \alpha_{8.6}^{20}=-0.16 between 8.6 and 20 GHz), even if the sample is dominated by flat spectra sources (85 per cent of the sample has \alpha_{8.6}^{20}>-0.5). The almost simultaneous spectra in total intensity and polarisation allowed us a comparison of the polarised and total intensity spectra: polarised fraction slightly increases with frequency, but the shapes of the spectra have little correlation. Optical identifications provided an estimation of redshift for 186 sources with a median value of 1.20 and 0.13 respectively for QSO and galaxies., Comment: 34 pages, 19 figures, tables of data included, replaced with version published in MNRAS
Published: 2007

28. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

Author: Prism, Collaboration, Andre, Philippe, Baccigalupi, Carlo, Barbosa, Domingos, Bartlett, James, Bartolo, Nicola, Battistelli, Elia, Battye, Richard, Bendo, George, Bernard, Jean-Philippe, Bersanelli, Marco, Bethermin, Matthieu, Bielewicz, Pawel, Bonaldi, Anna, Bouchet, Francois, Boulanger, Francois, Brand, Jan, Bucher, Martin, Burigana, Carlo, Cai, Zhen-Yi, Casasola, Viviana, Castex, Guillaume, Challinor, Anthony, Jens Chluba, Colafrancesco, Sergio, Cuttaia, Francesco, D Alessandro, Giuseppe, Davis, Richard, Avillez, Miguel, Bernardis, Paolo, Petris, Marco, Rosa, Adriano, Zotti, Gianfranco, Delabrouille, Jacques, Dickinson, Clive, Diego, Jose Maria, Falgarone, Edith, Ferreira, Pedro, Ferriere, Katia, Finelli, Fabio, Fletcher, Andrew, Fuller, Gary, Galli, Silvia, Ganga, Ken, Garcia-Bellido, Juan, Ghribi, Adnan, Gonzalez-Nuevo, Joaquin, Grainge, Keith, Gruppuso, Alessandro, Hall, Alex, Hernandez-Monteagudo, Carlos, Jackson, Mark, Jaffe, Andrew, Khatri, Rishi, Lamagna, Luca, Lattanzi, Massimiliano, Leahy, Paddy, Liguori, Michele, Liuzzo, Elisabetta, Lopez-Caniego, Marcos, Macias-Perez, Juan, Maffei, Bruno, Maino, Davide, Masi, Silvia, Mangilli, Anna, Massardi, Marcella, Matarrese, Sabino, Melchiorri, Alessandro, Melin, Jean-Baptiste, Mennella, Aniello, Mignano, Arturo, Miville-Deschenes, Marc-Antoine, Nati, Federico, Natoli, Paolo, Negrello, Mattia, Noviello, Fabio, Paci, Francesco, Paladino, Rosita, Paoletti, Daniela, Perrotta, Francesca, Piacentini, Francesco, Piat, Michel, Piccirillo, Lucio, Pisano, Giampaolo, Polenta, Gianluca, Ricciardi, Sara, Roman, Matthieu, Rubino-Martin, Jose-Alberto, Salatino, Maria, Schillaci, Alessandro, Shellard, Paul, Silk, Joseph, Stompor, Radek, Sunyaev, Rashid, Tartari, Andrea, Terenzi, Luca, Toffolatti, Luigi, Tomasi, Maurizio, Trombetti, Tiziana, Tucci, Marco, Tent, Bartjan, Verde, Licia, Wandelt, Ben, and Withington, Stafford
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in response to the Call for White Papers for the definition of the L2 and L3 Missions in the ESA Science Programme. PRISM would have two instruments: (1) an imager with a 3.5m mirror (cooled to 4K for high performance in the far-infrared---that is, in the Wien part of the CMB blackbody spectrum), and (2) an Fourier Transform Spectrometer (FTS) somewhat like the COBE FIRAS instrument but over three orders of magnitude more sensitive. Highlights of the new science (beyond the obvious target of B-modes from gravity waves generated during inflation) made possible by these two instruments working in tandem include: (1) the ultimate galaxy cluster survey gathering 10e6 clusters extending to large redshift and measuring their peculiar velocities and temperatures (through the kSZ effect and relativistic corrections to the classic y-distortion spectrum, respectively) (2) a detailed investigation into the nature of the cosmic infrared background (CIB) consisting of at present unresolved dusty high-z galaxies, where most of the star formation in the universe took place, (3) searching for distortions from the perfect CMB blackbody spectrum, which will probe a large number of otherwise inaccessible effects (e.g., energy release through decaying dark matter, the primordial power spectrum on very small scales where measurements today are impossible due to erasure from Silk damping and contamination from non-linear cascading of power from larger length scales). These are but a few of the highlights of the new science that will be made possible with PRISM., Comment: 20 pages Latex

29. High-resolution imaging of dusty galaxies in H-ATLAS/GAMA

Author: Thomson, Alasdair, Sadler, Elaine, Werf, Paul, Massardi, Marcella, Hopkins, Andrew, White, Glenn, Michalowski, Michal, Bremer, Malcolm, Birkinshaw, Mark, Andreani, Paola, Croom, Scott, Rob Ivison, Eales, Steve, Ibar, Edo, Lopez-Sanchez, Angel R., Hardcastle, Martin, Jarvis, Matt, Temi, Pasquale, Dunne, Loretta, Seymour, Nick, Clements, Dave, Bussmann, Shane, and Bourne, Nathan

30. Spectroscopic high-resolution observation of candidate lensed galaxies at 2.2< z< 2.6

Author: Massardi, Marcella, Werf, Paul, Norris, Ray, Ekers, Ron, Zotti, Gianfranco, Michalowski, Michal, Birkinshaw, Mark, Andreani, Paola, Emonts, Bjorn, Rob Ivison, Maiolino, Roberto, Eales, Steve, Bonavera, Laura, Ibar, Edo, Cooray, Asantha, Buttiglione, Sara, Danese, Luigi, Gonzalez-Nuevo Gonzalez, Joaquin, Lapi, Andrea, Vaccari, Mattia, Rodighiero, Giulia, Negrello, Mattia, Jarvis, Matt, Leeuw, Lerothodi, Temi, Pasquale, Lopez-Caniego, Marcos, and Herranz, Diego

31. Radio sources in next-generation CMB surveys

Author: De Zotti, Gianfranco, Bonato, Matteo, Negrello, Mattia, Herranz, Diego, Lopez-Caniego, Marcos, Trombetti, Tiziana, Burigana, Carlo, Massardi, Marcella, Bonavera, Laura, Gonzalez-Nuevo, Joaquin, Galluzzi, Vincenzo, and Hanany, Shaul
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, QB
Abstract: CMB surveys provide, for free, blindly selected samples of extragalactic radio sources at much higher frequencies than traditional radio surveys. Next-generation, ground-based CMB experiments with arcmin resolution at mm wavelengths will provide samples of thousands radio sources allowing the investigation of the evolutionary properties of blazar populations, the study of the earliest and latest stages of radio activity, the discovery of rare phenomena and of new transient sources and events. Space-borne experiments will extend to sub-mm wavelengths the determinations of the SEDs of many hundreds of blazars, in temperature and in polarization, allowing us to investigate the flow and the structure of relativistic jets close to their base, and the electron acceleration mechanisms. A real breakthrough will be achieved in the caracterization of the polarization properties. The first direct counts in polarization will be obtained, enabling a solid assessment of the extra-galactic source contamination of CMB maps and allowing us to understand structure and intensity of magnetic fields, particle densities and structures of emitting regions close to the base of the jet.

32. Redshift detection of the most distant lensed starbursts

Author: Dunne, Loretta, Werf, Paul, Massardi, Marcella, White, Glenn, Serjeant, Stephen, Michalowski, Michal, Thompson, Mark, Birkinshaw, Mark, Andreani, Paola, Stevens, Jamie, Omont, Alain, Smith, Matthew, Rob Ivison, Thomson, Alasdair, Eales, Steve, Ibar, Edo, Benford, Dominic, Dannerbauer, Helmut, Leeuw, Lerothodi, Temi, Pasquale, Negrello, Mattia, Clements, Dave, Bussmann, Shane, Maddox, Steve, Vis, Pieter, Vlahakis, Catherine, Verma, Aprajita, Dye, Simon, and Riechers, Dominik

33. The polarimetric multi-frequency radio sources properties

Author: Vincenzo Galluzzi, Marcella Massardi, Galluzzi, Vincenzo, and Massardi, Marcella
Subjects: cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Polarimetry, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Mathematical Physic, 010303 astronomy & astrophysics, Mathematical Physics, Astrophysics::Galaxy Astrophysics, Physics, polarization, Radio galaxie, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, Astronomy and Astrophysic, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The polarization properties of extragalactic radio sources at frequencies higher than [Formula: see text]GHz are still poorly constrained. However, their characterization would provide invaluable information about the physics of the emission processes and is crucial to estimate their contamination as foregrounds of the polarized Cosmic Microwave Background (CMB) angular power spectrum on scales [Formula: see text]arcmin. In this contribution, after summarizing the state-of-the-art of polarimetric observations in the millimetric wavelength bands, we present our observations of a complete sample of 53 sources with [Formula: see text]mJy carried out with the Australia Telescope Compact Array (ACTA) between [Formula: see text] and [Formula: see text]GHz. The analysis clearly shows that polarization properties cannot be simply inferred from total intensity ones, as the spectral behaviors of the two signals are typically different.
Published: 2016

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33 results on '"Massardi, Marcella"'

1. The ALMA Science Archive development and the ARI-L project

2. The MAYA 2022 conference

3. Overview of the Additional Representative Images for Legacy (ARI-L) Development Project for the ALMA Science Archive

4. The ALPINE–ALMA [C II] survey

5. The ALPINE-ALMA [C II] survey:Luminosity function of serendipitous [C II] line emitters at z similar to 5

6. The ALPINE-ALMA [C II] survey. Luminosity function of serendipitous [C II] line emitters at z \ensuremath∼ 5

7. User interaction models towards the SKA

8. Radio sources in next-generation CMB surveys

9. Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds (Corrigendum)

10. The ALMA Re-Imaging development study

11. ALMA FITS header keywords: a study from the archive User perspective

12. Advanced European Network Of E-Infrastructures For Astronomy With The Ska

13. The Alma Re-Imaging (Ari) Development Study

14. The Main Sequence Of Star Forming Galaxies And Agns At High-Z: Evidence For In Situ Coevolution

15. Planck 2013 results. XXI. Cosmology with the all-sky Planck Compton parameter y-map

16. The Polarized Radiation Imaging and Spectroscopy Mission

17. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

18. Planck 2013 results. XII. Component separation

19. A 20 GHz bright sample for δ > +72° — I. Catalogue

20. The Planck-ATCA Co-eval Observations project: the bright sample

21. Optical Properties of High-Frequency Radio Sources from the Australia Telescope 20 GHz (AT20G) Survey

22. The Planck-ATCA Co-eval Observations (PACO) project: the bright sample

23. The Planck-ATCA Coeval Observations (PACO) project: the faint sample

24. The Australia Telescope 20GHz (AT20G) Survey: analysis of the extragalactic source sample

25. The extragalactic sources at mm wavelengths and their role as CMB foregrounds

26. Statistical properties of extragalactic sources in the New Extragalactic WMAP Point Source (NEWPS) catalogue

27. The Australia Telescope 20 GHz (AT20G) Survey: The Bright Source Sample

28. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

29. High-resolution imaging of dusty galaxies in H-ATLAS/GAMA

30. Spectroscopic high-resolution observation of candidate lensed galaxies at 2.2< z< 2.6

31. Radio sources in next-generation CMB surveys

32. Redshift detection of the most distant lensed starbursts

33. The polarimetric multi-frequency radio sources properties

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33 results on '"Massardi, Marcella"'

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