Creat membership Creat membership
Sign in

Forgot password?

Confirm
  • Forgot password?
    Sign Up
  • Confirm
    Sign In
home > search

Now showing items 49 - 64 of 102

  • Planck pre-launch status: The Planck-LFI programme RID A-2699-2012 RID A-2137-2010

    Mandolesi, N.   Bersanelli, M.   Butler, R. C.   Artal, E.   Baccigalupi, C.   Balbi, A.   Banday, A. J.   Barreiro, R. B.   Bartelmann, M.   Bennett, K.   Bhandari, P.   Bonaldi, A.   Borrill, J.   Bremer, M.   Burigana, C.   Bowman, R. C.   Cabella, P.   Cantalupo, C.   Cappellini, B.   Courvoisier, T.   Crone, G.   Cuttaia, F.   Danese, L.   D'Arcangelo, O.   Davies, R. D.   Davis, R. J.   De Angelis, L.   de Gasperis, G.   De Rosa, A.   De Troia, G.   de Zotti, G.   Dick, J.   Dickinson, C.   Diego, J. M.   Donzelli, S.   Doerl, U.   Dupac, X.   Ensslin, T. A.   Eriksen, H. K.   Falvella, M. C.   Finelli, F.   Frailis, M.   Franceschi, E.   Gaier, T.   Galeotta, S.   Gasparo, F.   Giardino, G.   Gomez, F.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Hansen, F.   Hell, R.   Herranz, D.   Herreros, J. M.   Hildebrandt, S.   Hovest, W.   Hoyland, R.   Huffenberger, K.   Janssen, M.   Jaffe, T.   Keihanen, E.   Keskitalo, R.   Kisner, T.   Kurki-Suonio, H.   Lahteenmaki, A.   Lawrence, C. R.   Leach, S. M.   Leahy, J. P.   Leonardi, R.   Levin, S.   Lilje, P. B.   Lopez-Caniego, M.   Lowe, S. R.   Lubin, P. M.   Maino, D.   Malaspina, M.   Maris, M.   Marti-Canales, J.   Martinez-Gonzalez, E.   Massardi, M.   Matarrese, S.   Matthai, F.   Meinhold, P.   Melchiorri, A.   Mendes, L.   Mennella, A.   Morgante, G.   Morigi, G.   Morisset, N.   Moss, A.   Nash, A.   Natoli, P.   Nesti, R.   Paine, C.   Partridge, B.   Pasian, F.   Passvogel, T.   Pearson, D.   Perez-Cuevas, L.   Perrotta, F.   Polenta, G.   Popa, L. A.   Poutanen, T.   Prezeau, G.   Prina, M.   Rachen, J. P.   Rebolo, R.   Reinecke, M.   Ricciardi, S.   Riller, T.   Rocha, G.   Roddis, N.   Rohlfs, R.   Rubino-Martin, J. A.   Salerno, E.   Sandri, M.   Scott, D.   Seiffert, M.   Silk, J.   Simonetto, A.   Smoot, G. F.   Sozzi, C.   Sternberg, J.   Stivoli, F.   Stringhetti, L.   Tauber, J.   Terenzi, L.   Tomasi, M.   Tuovinen, J.   Tuerler, M.   Valenziano, L.   Varis, J.   Vielva, P.   Villa, F.   Vittorio, N.   Wade, L.   White, M.   White, S.   Wilkinson, A.   Zacchei, A.   Zonca, A.  

    This paper provides an overview of the Low Frequency Instrument (LFI) programme within the ESA Planck mission. The LFI instrument has been developed to produce high precision maps of the microwave sky at frequencies in the range 27-77 GHz, below the peak of the cosmic microwave background (CMB) radiation spectrum. The scientific goals are described, ranging from fundamental cosmology to Galactic and extragalactic astrophysics. The instrument design and development are outlined, together with the model philosophy and testing strategy. The instrument is presented in the context of the Planck mission. The LFI approach to ground and inflight calibration is described. We also describe the LFI ground segment. We present the results of a number of tests demonstrating the capability of the LFI data processing centre (DPC) to properly reduce and analyse LFI flight data, from telemetry information to calibrated and cleaned time ordered data, sky maps at each frequency (in temperature and polarization), component emission maps (CMB and diffuse foregrounds), catalogs for various classes of sources (the Early Release Compact Source Catalogue and the Final Compact Source Catalogue). The organization of the LFI consortium is briefly presented as well as the role of the core team in data analysis and scientific exploitation. All tests carried out on the LFI flight model demonstrate the excellent performance of the instrument and its various subunits. The data analysis pipeline has been tested and its main steps verified. In the first three months after launch, the commissioning, calibration,
    Download Collect
  • Planck early results. XV. Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources

    Aatrokoski, J.   Ade, P. A. R.   Aghanim, N.   Aller, H. D.   Aller, M. F.   Angelakis, E.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Balbi, A.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Battaner, E.   Benabed, K.   Benoit, A.   Berdyugin, A.   Bernard, J. -P.   Bersanelli, M.   Bhatia, R.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Bucher, M.   Burigana, C.   Burrows, D. N.   Cabella, P.   Capalbi, M.   Cappellini, B.   Cardoso, J. -F.   Catalano, A.   Cavazzuti, E.   Cayon, L.   Challinor, A.   Chamballu, A.   Chary, R. -R.   Chiang, L. -Y   Christensen, P. R.   Clements, D. L.   Colafrancesco, S.   Colombi, S.   Couchot, F.   Coulais, A.   Cutini, S.   Cuttaia, F.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Gasperis, G.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Delouis, J. -M.   Dickinson, C.   Dole, H.   Donzelli, S.   Dore, O.   Doerl, U.   Douspis, M.   Dupac, X.   Efstathiou, G.   Ensslin, T. A.   Finelli, F.   Forni, O.   Frailis, M.   Franceschi, E.   Fuhrmann, L.   Galeotta, S.   Ganga, K.   Gargano, F.   Gasparrini, D.   Gehrels, N.   Giard, M.   Giardino, G.   Giglietto, N.   Giommi, P.   Giordano, F.   Giraud-Heraud, Y.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gratton, S.   Gregorio, A.   Gruppuso, A.   Harrison, D.   Henrot-Versille, S.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Hovest, W.   Hoyland, R. J.   Huffenberger, K. M.   Jaffe, A. H.   Juvela, M.   Keihanen, E.   Keskitalo, R.   King, O.   Kisner, T. S.   Kneissl, R.   Knox, L.   Krichbaum, T. P.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Laureijs, R. J.   Lavonen, N.   Lawrence, C. R.   Leach, S.   Leonardi, R.   Leon-Tavares, J.   Linden-Vornle, M.   Lindfors, E.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maffei, B.   Maino, D.   Mandolesi, N.   Mann, R.   Maris, M.   Martinez-Gonzalez, E.   Masi, S.   Massardi, M.   Matarrese, S.   Matthai, F.   Max-Moerbeck, W.   Mazziotta, M. N.   Mazzotta, P.   Melchiorri, A.   Mendes, L.   Mennella, A.   Michelson, P. F.   Mingaliev, M.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Monte, C.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Murphy, A.   Naselsky, P.   Natoli, P.   Nestoras, I.   Netterfield, C. B.   Nieppola, E.   Nilsson, K.   Norgaard-Nielsen, H. U.   Noviello, F.   Novikov, D.   Novikov, I.   O'Dwyer, I. J.   Osborne, S.   Pajot, F.   Partridge, B.   Pasian, F.   Patanchon, G.   Pavlidou, V.   Pearson, T. J.   Perdereau, O.   Perotto, L.   Perri, M.   Perrotta, F.   Piacentini, F.   Piat, M.   Plaszczynski, S.   Platania, P.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Poutanen, T.   Prezeau, G.   Procopio, P.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Raino, S.   Reach, W. T.   Readhead, A.   Rebolo, R.   Reeves, R.   Reinecke, M.   Reinthal, R.   Renault, C.   Ricciardi, S.   Richards, J.   Riller, T.   Riquelme, D.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rowan-Robinson, M.   Rubino-Martin, J. A.   Rusholme, B.   Saarinen, J.   Sandri, M.   Savolainen, P.   Scott, D.   Seiffert, M. D.   Sievers, A.   Sillanpaa, A.   Smoot, G. F.   Sotnikova, Y.   Starck, J. -L.   Stevenson, M.   Stivoli, F.   Stolyarov, V.   Sudiwala, R.   Sygnet, J. -F.   Takalo, L.   Tammi, J.   Tauber, J. A.   Terenzi, L.   Thompson, D. J.   Toffolatti, L.   Tomasi, M.   Tornikoski, M.   Torre, J. -P.   Tosti, G.   Tramacere, A.   Tristram, M.   Tuovinen, J.   Turler, M.   Turunen, M.   Umana, G.   Ungerechts, H.   Valenziano, L.   Valtaoja, E.   Varis, J.   Verrecchia, F.   Vielva, P.   Villa, F.   Vittorio, N.   Wandelt, B. D.   Wu, J.   Yvon, D.   Zacchei, A.   Zensus, J. A.   Zhou, X.   Zonca, A.  

    Spectral energy distributions (SEDs) and radio continuum spectra are presented for a northern sample of 104 extragalactic radio sources, based on the Planck Early Release Compact Source Catalogue (ERCSC) and simultaneous multifrequency data. The nine Planck frequencies, from 30 to 857 GHz, are complemented by a set of simultaneous observations ranging from radio to gamma-rays. This is the first extensive frequency coverage in the radio and millimetre domains for an essentially complete sample of extragalactic radio sources, and it shows how the individual shocks, each in their own phase of development, shape the radio spectra as they move in the relativistic jet. The SEDs presented in this paper were fitted with second and third degree polynomials to estimate the frequencies of the synchrotron and inverse Compton (IC) peaks, and the spectral indices of low and high frequency radio data, including the Planck ERCSC data, were calculated. SED modelling methods are discussed, with an emphasis on proper, physical modelling of the synchrotron bump using multiple components. Planck ERCSC data also suggest that the original accelerated electron energy spectrum could be much harder than commonly thought, with power-law index around 1.5 instead of the canonical 2.5. The implications of this are discussed for the acceleration mechanisms effective in blazar shocks. Furthermore in many cases the Planck data indicate that gamma-ray emission must originate in the same shocks that produce the radio emission.
    Download Collect
  • Planck intermediate results XXXVI. Optical identification and redshifts of Planck SZ sources with telescopes at the Canary Islands observatories

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Barrena, R.   Bartolo, N.   Battaner, E.   Benabed, K.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bikmaev, I.   Bohringer, H.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Burenin, R.   Burigana, C.   Calabrese, E.   Cardoso, J. -F.   Catalano, A.   Chamballu, A.   Chary, R. -R.   Chiang, H. C.   Chon, G.   Christensen, P. R.   Clements, D. L.   Colombo, L. P. L.   Combet, C.   Comis, B.   Crill, B. P.   Curto, A.   Cuttaia, F.   Dahle, H.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Diego, J. M.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Dupac, X.   Efstathiou, G.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Ferragamo, A.   Finelli, F.   Forni, O.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Fromenteau, S.   Galeotta, S.   Galli, S.   Ganga, K.   Genova-Santos, R. T.   Giard, M.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gruppuso, A.   Hansen, F. K.   Harrison, D. L.   Hempel, A.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hornstrup, A.   Hovest, W.   Huffenberger, K. M.   Hurier, G.   Jaffe, T. R.   Keihanen, E.   Keskitalo, R.   Khamitov, I.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leonardi, R.   Leon-Tavares, J.   Levrier, F.   Lietzen, H.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maffei, B.   Maino, D.   Mandolesi, N.   Maris, M.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   McGehee, P.   Melchiorri, A.   Mennella, A.   Migliaccio, M.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Novikov, D.   Novikov, I.   Oxborrow, C. A.   Pagano, L.   Pajot, F.   Paoletti, D.   Pasian, F.   Perdereau, O.   Pettorino, V.   Piacentini, F.   Piat, M.   Pierpaoli, E.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Pratt, G. W.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Santos, D.   Savelainen, M.   Savini, G.   Scott, D.   Stolyarov, V.   Streblyanska, A.   Sudiwala, R.   Sunyaev, R.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tramonte, D.   Tristram, M.   Tucci, M.   Valenziano, L.   Valiviita, J.   Van Tent, B.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   Wehus, I. K.   Yvon, D.   Zacchei, A.   Zonca, A.  

    We present the results of approximately three years of observations of Planck Sunyaev-Zeldovich (SZ) sources with telescopes at the Canary Islands observatories as part of the general optical follow-up programme undertaken by the Planck Collaboration. In total, 78 SZ sources are discussed. Deep-imaging observations were obtained for most of these sources; spectroscopic observations in either in long-slit or multi-object modes were obtained for many. We effectively used 37.5 clear nights. We found optical counterparts for 73 of the 78 candidates. This sample includes 53 spectroscopic redshift determinations, 20 of them obtained with a multi-object spectroscopic mode. The sample contains new redshifts for 27 Planck clusters that were not included in the first Planck SZ source catalogue (PSZ1).
    Download Collect
  • Planck 2015 results III. LFI systematic uncertainties

    Ade, P. A. R.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartolo, N.   Basak, S.   Battaglia, P.   Battaner, E.   Benabed, K.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Burigana, C.   Butler, R. C.   Calabrese, E.   Catalano, A.   Christensen, P. R.   Colombo, L. P. L.   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.   Dickinson, C.   Diego, J. M.   Dore, O.   Ducout, A.   Dupac, X.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Finelli, F.   Frailis, M.   Franceschet, C.   Franceschi, E.   Galeotta, S.   Galli, S.   Ganga, K.   Ghosh, T.   Giard, M.   Giraud-Heraud, Y.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Hansen, F. K.   Harrison, D. L.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Hornstrup, A.   Hovest, W.   Huffenberger, K. M.   Hurier, G.   Jaffe, A. H.   Jaffe, T. R.   Keihanen, E.   Keskitalo, R.   Kiiveri, K.   Kisner, T. S.   Knoche, J.   Krachmalnicoff, N.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leahy, J. P.   Leonardi, R.   Levrier, F.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lindholm, V.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maffei, B.   Maggio, G.   Maino, D.   Mandolesi, N.   Mangilli, A.   Maris, M.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   Meinhold, P. R.   Mennella, A.   Migliaccio, M.   Mitra, S.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Murphy, J. A.   Nati, F.   Natoli, P.   Noviello, F.   Paci, F.   Pagano, L.   Pajot, F.   Paoletti, D.   Partridge, B.   Pasian, F.   Pearson, T. J.   Perdereau, O.   Pettorino, V.   Piacentini, F.   Pointecouteau, E.   Polenta, G.   Pratt, G. W.   Puget, J. -L.   Rachen, J. P.   Reinecke, M.   Remazeilles, M.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Santos, D.   Savelainen, M.   Scott, D.   Stolyarov, V.   Stompor, R.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Tavagnacco, D.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Tucci, M.   Umana, G.   Valenziano, L.   Valiviita, J.   Van Tent, B.   Vassallo, T.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   Watson, R.   Wehus, I. K.   Yvon, D.   Zacchei, A.   Zibin, J. P.   Zonca, A.  

    We present the current accounting of systematic effect uncertainties for the Low Frequency Instrument (LFI) that are relevant to the 2015 release of the Planck cosmological results, showing the robustness and consistency of our data set, especially for polarization analysis. We use two complementary approaches: (i) simulations based on measured data and physical models of the known systematic effects; and (ii) analysis of difference maps containing the same sky signal ("null-maps"). The LFI temperature data are limited by instrumental noise. At large angular scales the systematic effects are below the cosmic microwave background (CMB) temperature power spectrum by several orders of magnitude. In polarization the systematic uncertainties are dominated by calibration uncertainties and compete with the CMB E-modes in the multipole range 10-20. Based on our model of all known systematic effects, we show that these effects introduce a slight bias of around 0.2 sigma on the reionization optical depth derived from the 70 GHz EE spectrum using the 30 and 353 GHz channels as foreground templates. At 30 GHz the systematic effects are smaller than the Galactic foreground at all scales in temperature and polarization, which allows us to consider this channel as a reliable template of synchrotron emission. We assess the residual uncertainties due to LFI effects on CMB maps and power spectra after component separation and show that these effects are smaller than the CMB amplitude at all scales. We also assess the impact on non-Gaussianity studies and find it to be negligible. Some residuals still appear in null maps from particular sky survey pairs, particularly at 30 GHz, suggesting possible straylight contamination due to an imperfect knowledge of the beam far sidelobes.
    Download Collect
  • Planck intermediate results XVI. Profile likelihoods for cosmological parameters

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Battaner, E.   Benabed, K.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bobin, J.   Bonaldi, A.   Bond, J. R.   Bouchet, F. R.   Burigana, C.   Cardoso, J. -F.   Catalano, A.   Chamballu, A.   Chiang, H. C.   Christensen, P. R.   Clements, D. L.   Colombi, S.   Colombo, L. P. L.   Couchot, F.   Cuttaia, F.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Dickinson, C.   Diego, J. M.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Dupac, X.   Ensslin, T. A.   Eriksen, H. K.   Finelli, F.   Forni, O.   Frailis, M.   Franceschi, E.   Galeotta, S.   Galli, S.   Ganga, K.   Giard, M.   Giraud-Heraud, Y.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Hansen, F. K.   Harrison, D. L.   Henrot-Versille, S.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Hornstrup, A.   Hovest, W.   Huffenberger, K. M.   Jaffe, A. H.   Jaffe, T. R.   Jones, W. C.   Juvela, M.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Knox, L.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Lawrence, C. R.   Leonardi, R.   Liddle, A.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maffei, B.   Maino, D.   Mandolesi, N.   Maris, M.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Massardi, M.   Matarrese, S.   Mazzotta, P.   Melchiorri, A.   Mendes, L.   Mennella, A.   Migliaccio, M.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Noviello, F.   Novikov, D.   Novikov, I.   Oxborrow, C. A.   Pagano, L.   Pajot, F.   Paoletti, D.   Pasian, F.   Perdereau, O.   Perotto, L.   Perrotta, F.   Pettorino, V.   Piacentini, F.   Piat, M.   Pierpaoli, E.   Pietrobon, D.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Popa, L.   Pratt, G. W.   Puget, J. -L.   Rachen, J. P.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Ricciardi, S.   Riller, T.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Roudier, G.   d'Orfeuil, B. Rouille   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Savelainen, M.   Savini, G.   Spencer, L. D.   Spinelli, M.   Starck, J. -L.   Sureau, F.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Tucci, M.   Umana, G.   Valenziano, L.   Valiviita, J.   Van Tent, B.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   White, M.   Yvon, D.   Zacchei, A.   Zonca, A.  

    We explore the 2013 Planck likelihood function with a high-precision multi-dimensional minimizer (Minuit). This allows a refinement of the ACDM best-fit solution with respect to previously-released results, and the construction of frequentist confidence intervals using profile likelihoods. The agreement with the cosmological results from the Bayesian framework is excellent, demonstrating the robustness of the Planck results to the statistical methodology. We investigate the inclusion of neutrino masses, where more significant differences may appear due to the non-Gaussian nature of the posterior mass distribution. By applying the Feldman-Cousins prescription, we again obtain results very similar to those of the Bayesian methodology. However, the profile-likelihood analysis of the cosmic microwave background (CMB) combination (Planck+WP+highL) reveals a minimum well within the unphysical negative-mass region. We show that inclusion of the Planck CMB-lensing information regularizes this issue, and provide a robust frequentist upper limit Sigma m(v) <= 0.26 eV (95% confidence) from the CMB+lensing+BAO data combination.
    Download Collect
  • 1906 Management of BRCA 1/2 mutation carriers: 14 years of a multidisciplinary program

    Rocha, G.   Luís, A.   Clara, A.   Opini?o, A.   Bento, S.   Dupont, J.   Rodrigues, P.   Sim?es, C.   Parreira, J.   Fragoso, S.   Santos, S.   Machado, P.   Moura, M.   Rocha, M.   Faria, L.   Marques, J.C.   Moura, C.   Silva, J.   Vaz, F.  

    Download Collect
  • Planck intermediate results VIII. Filaments between interacting clusters

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Atrio-Barandela, F.   Aumont, J.   Baccigalupi, C.   Balbi, A.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Battaner, E.   Benabed, K.   Benoit, A.   Bernard, J. -P.   Bersanelli, M.   Bhatia, R.   Bikmaev, I.   Boehringer, H.   Bonaldi, A.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Bourdin, H.   Burenin, R.   Burigana, C.   Cabella, P.   Cardoso, J. -F.   Castex, G.   Catalano, A.   Cayon, L.   Chamballu, A.   Chary, R. -R.   Chiang, L. -Y.   Chon, G.   Christensen, P. R.   Clements, D. L.   Colafrancesco, S.   Colombo, L. P. L.   Comis, B.   Coulais, A.   Crill, B. P.   Cuttaia, F.   Da Silva, A.   Dahle, H.   Danese, L.   Davis, R. J.   de Bernardis, P.   de Gasperis, G.   de Zotti, G.   Delabrouille, J.   Democles, J.   Desert, F. -X.   Diego, J. M.   Dolag, K.   Dole, H.   Donzelli, S.   Dore, O.   Doerl, U.   Douspis, M.   Dupac, X.   Efstathiou, G.   Ensslin, T. A.   Eriksen, H. K.   Finelli, F.   Flores-Cacho, I.   Forni, O.   Frailis, M.   Franceschi, E.   Frommert, M.   Galeotta, S.   Ganga, K.   Genova-Santos, R. T.   Giard, M.   Gilfanov, M.   Giraud-Heraud, Y.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Hansen, F. K.   Harrison, D.   Hempel, A.   Henrot-Versille, S.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Hovest, W.   Hurier, G.   Jaffe, T. R.   Jaffe, A. H.   Jagemann, T.   Jones, W. C.   Juvela, M.   Khamitov, I.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Knox, L.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lamarre, J. -M.   Lasenby, A.   Lawrence, C. R.   Le Jeune, M.   Leonardi, R.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Luzzi, G.   Macias-Perez, J. F.   Maffei, B.   Maino, D.   Mandolesi, N.   Maris, M.   Marleau, F.   Marshall, D. J.   Martinez-Gonzalez, E.   Masi, S.   Massardi, M.   Matarrese, S.   Matthai, F.   Mazzotta, P.   Mei, S.   Melchiorri, A.   Melin, J. -B.   Mendes, L.   Mennella, A.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Norgaard-Nielsen, H. U.   Noviello, F.   Novikov, D.   Novikov, I.   Osborne, S.   Pajot, F.   Paoletti, D.   Pasian, F.   Patanchon, G.   Perdereau, O.   Perotto, L.   Perrotta, F.   Piacentini, F.   Piat, M.   Pierpaoli, E.   Piffaretti, R.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Popa, L.   Poutanen, T.   Pratt, G. W.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Ricciardi, S.   Riller, T.   Ristorcelli, I.   Rocha, G.   Roman, M.   Rosset, C.   Rossetti, M.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Savini, G.   Schaefer, B. M.   Scott, D.   Smoot, G. F.   Starck, J. -L.   Sudiwala, R.   Sunyaev, R.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Valenziano, L.   Van Tent, B.   Vielva, P.   Villa, F.   Vittorio, N.   Wade, L. A.   Wandelt, B. D.   Welikala, N.   White, S. D. M.   Yvon, D.   Zacchei, A.   Zonca, A.  

    Context. About half of the baryons of the Universe are expected to be in the form of filaments of hot and low-density intergalactic medium. Most of these baryons remain undetected even by the most advanced X-ray observatories, which are limited in sensitivity to the diffuse low-density medium. Aims. The Planck satellite has provided hundreds of detections of the hot gas in clusters of galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an ideal instrument for studying extended low-density media through the tSZ effect. In this paper we use the Planck data to search for signatures of a fraction of these missing baryons between pairs of galaxy clusters. Methods. Cluster pairs are good candidates for searching for the hotter and denser phase of the intergalactic medium (which is more easily observed through the SZ effect). Using an X-ray catalogue of clusters and the Planck data, we selected physical pairs of clusters as candidates. Using the Planck data, we constructed a local map of the tSZ effect centred on each pair of galaxy clusters. ROSAT data were used to construct X-ray maps of these pairs. After modelling and subtracting the tSZ effect and X-ray emission for each cluster in the pair, we studied the residuals on both the SZ and X-ray maps. Results. For the merging cluster pair A399-A401 we observe a significant tSZ effect signal in the intercluster region beyond the virial radii of the clusters. A joint X-ray SZ analysis allows us to constrain the temperature and density of this intercluster medium. We obtain a temperature of kT = 7.1 +/- 0.9 keV (consistent with previous estimates) and a baryon density of (3.7 +/- 0.2) x 10(-4) cm(-3). Conclusions. The Planck satellite mission has provided the first SZ detection of the hot and diffuse intercluster gas.
    Download Collect
  • Planck 2015 results XIII. Cosmological parameters

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Bartolo, N.   Battaner, E.   Battye, R.   Benabed, K.   Benoit, A.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bock, J. J.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Boulanger, F.   Bucher, M.   Burigana, C.   Butler, R. C.   Calabrese, E.   Cardoso, J. -F.   Catalano, A.   Challinor, A.   Chamballu, A.   Chary, R. -R.   Chiang, H. C.   Chluba, J.   Christensen, P. R.   Church, S.   Clements, D. L.   Colombi, S.   Colombo, L. P. L.   Combet, C.   Coulais, A.   Crill, B. P.   Curto, A.   Cuttaia, F.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Desert, F. -X.   Di Valentino, E.   Dickinson, C.   Diego, J. M.   Dolag, K.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Ducout, A.   Dunkley, J.   Dupac, X.   Efstathiou, G.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Farhang, M.   Fergusson, J.   Finelli, F.   Forni, O.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Frejsel, A.   Galeotta, S.   Galli, S.   Ganga, K.   Gauthier, C.   Gerbino, M.   Ghosh, T.   Giard, M.   Giraud-Heraud, Y.   Giusarma, E.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gratton, S.   Gregorio, A.   Gruppuso, A.   Gudmundsson, J. E.   Hamann, J.   Hansen, F. K.   Hanson, D.   Harrison, D. L.   Helou, G.   Henrot-Versille, S.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Hornstrup, A.   Hovest, W.   Huang, Z.   Huffenberger, K. M.   Hurier, G.   Jaffe, A. H.   Jaffe, T. R.   Jones, W. C.   Juvela, M.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Knox, L.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leahy, J. P.   Leonardi, R.   Lesgourgues, J.   Levrier, F.   Lewis, A.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maggio, G.   Maino, D.   Mandolesi, N.   Mangilli, A.   Marchini, A.   Maris, M.   Martin, P. G.   Martinelli, M.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   McGehee, P.   Meinhold, P. R.   Melchiorri, A.   Melin, J. -B.   Mendes, L.   Mennella, A.   Migliaccio, M.   Millea, M.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Moss, A.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Netterfield, C. B.   Norgaard-Nielsen, H. U.   Noviello, F.   Novikov, D.   Novikov, I.   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.   Pointecouteau, E.   Polenta, G.   Popa, L.   Pratt, G. W.   Prezeau, G.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Reach, W. T.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   d'Orfeui, B. Rouille   Rowan-Robinson, M.   Rubino-Martin, J. A.   Rusholme, B.   Said, N.   Salvatelli, V.   Salvati, L.   Sandri, M.   Santos, D.   Savelainen, M.   Savini, G.   Scott, D.   Seiffert, M. D.   Serra, P.   Shellard, E. P. S.   Spencer, L. D.   Spinelli, M.   Stolyarov, V.   Stompor, R.   Sudiwala, R.   Sunyaev, R.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Trombetti, T.   Tucci, M.   Tuovinen, J.   Turler, M.   Umana, G.   Valenziano, L.   Valiviita, J.   Van Tent, F.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   Wehus, I. K.   White, M.   White, S. D. M.   Wilkinson, A.   Yvon, D.   Zacchei, A.   Zonca, A.  

    This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Our results are in very good agreement with the 2013 analysis of the Planck nominal-mission temperature data, but with increased precision. The temperature and polarization power spectra are consistent with the standard spatially-flat 6-parameter Lambda CDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted "base Lambda CDM" in this paper). From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H-0 =3D (67.8 +/- 0.9) km s(-1)Mpc(-1), a matter density parameter Omega(m) =3D 0.308 +/- 0.012, and a tilted scalar spectral index with ns =3D 0.968 +/- 0.006, consistent with the 2013 analysis. Note that in this abstract we quote 68% confidence limits on measured parameters and 95% upper limits on other parameters. We present the first results of polarization measurements with the Low Frequency Instrument at large angular scales. Combined with the Planck temperature and lensing data, these measurements give a reionization optical depth of tau =3D 0.066 +/- 0.016, corresponding to a reionization redshift of z(re) =3D 8.8(-1.4)(+1.7) These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. We find no evidence for any departure from base Lambda CDM in the neutrino sector of the theory; for example, combining Planck observations with other astrophysical data we find N-eff =3D 3.15 +/- 0.23 for the effective number of relativistic degrees of freedom, consistent with the value N-eff =3D 3.046 of the Standard Model of particle physics. The sum of neutrino masses is constrained to Sigma m(v) < 0.23 eV. The spatial curvature of our Universe is found to be very close to zero, with vertical bar Omega(K)vertical bar < 0.005. Adding a tensor component as a single-parameter extension to base Lambda CDM we find an upper limit on the tensor-to-scalar ratio of r(0.002) < 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP B-mode data to our analysis leads to a tighter constraint of r(0.002) < 0.09 and disfavours inflationary models with a V(phi) proportional to phi(2) potential. The addition of Planck polarization data leads to strong constraints on deviations from a purely adiabatic spectrum of fluctuations. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w =3D -1.006 +/- 0.045, consistent with the expected value for a cosmological constant. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base Lambda CDM cosmology are in excellent agreement with observations. We also constraints on annihilating dark matter and on possible deviations from the standard recombination history. In neither case do we find no evidence for new physics. The Planck results for base Lambda CDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. We show that these tensions cannot easily be resolved with simple modifications of the base Lambda CDM cosmology. Apart from these tensions, the base Lambda CDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets.
    Download Collect
  • Planck 2015 results XXVI. The Second Planck Catalogue of Compact Sources

    Ade, P. A. R.   Aghanim, N.   Argueeso, F.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartolo, N.   Battaner, E.   Beichman, C.   Benabed, K.   Benoit, A.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bock, J. J.   Boehringer, H.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Boulanger, F.   Bucher, M.   Burigana, C.   Butler, R. C.   Calabrese, E.   Cardoso, J. -F.   Carvalho, P.   Catalano, A.   Challinor, A.   Chamballu, A.   Chary, R. -R.   Chiang, H. C.   Christensen, P. R.   Clemens, M.   Clements, D. L.   Colombi, S.   Colombo, L. P. L.   Combet, C.   Couchot, F.   Coulais, A.   Crill, B. P.   Curto, A.   Cuttaia, F.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Desert, F. -X.   Dickinson, C.   Diego, J. M.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Ducout, A.   Dupac, X.   Efstathiou, G.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Falgarone, E.   Fergusson, J.   Finelli, F.   Forni, O.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Frejsel, A.   Galeotta, S.   Galli, S.   Ganga, K.   Giard, M.   Giraud-Heraud, Y.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gratton, S.   Gregorio, A.   Gruppuso, A.   Gudmundsson, J. E.   Hansen, F. K.   Hanson, D.   Harrison, D. L.   Helou, G.   Henrot-Versille, S.   Hernandez-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.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leahy, J. P.   Leonardi, R.   Leon-Tavares, J.   Lesgourgues, J.   Levrier, F.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maggio, G.   Maino, D.   Mandolesi, N.   Mangilli, A.   Maris, M.   Marshall, D. J.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   McGehee, P.   Meinhold, P. R.   Melchiorri, A.   Mendes, L.   Mennella, A.   Migliaccio, M.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Moss, A.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Negrello, M.   Netterfield, C. B.   Norgaard-Nielsen, H. U.   Noviello, F.   Novikov, D.   Novikov, I.   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.   Pointecouteau, E.   Polenta, G.   Pratt, G. W.   Prezeau, G.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Reach, W. T.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   Rowan-Robinson, M.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Sanghera, H. S.   Santos, D.   Savelainen, M.   Savini, G.   Scott, D.   Seiffert, M. D.   Shellard, E. P. S.   Spencer, L. D.   Stolyarov, V.   Sudiwala, R.   Sunyaev, R.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tornikoski, M.   Tristram, M.   Tucci, M.   Tuovinen, J.   Turler, M.   Umana, G.   Valenziano, L.   Valiviita, J.   Van Tent, B.   Vielva, P.   Villa, F.   Wade, L. A.   Walter, B.   Wandelt, B. D.   Wehus, I. K.   Yvon, D.   Zacchei, A.   Zonca, A.  

    The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogues, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalogue. The second ( PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow us to increase the number of objects in the catalogue, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC).
    Download Collect
  • Planck intermediate results XLIII. Spectral energy distribution of dust in clusters of galaxies

    Adam, R.   Ade, P. A. R.   Aghanim, N.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartolo, N.   Battaner, E.   Benabed, K.   Benoit-Levy, A.   Bersanelli, M.   Bielewicz, P.   Bikmaev, I.   Bonaldi, A.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Burenin, R.   Burigana, C.   Calabrese, E.   Cardoso, J. -F.   Catalano, A.   Chiang, H. C.   Christensen, P. R.   Churazov, E.   Colombo, L. P. L.   Combet, C.   Comis, B.   Couchot, F.   Crill, B. P.   Curto, A.   Cuttaia, F.   Danese, L.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Desert, F. -X.   Diego, J. M.   Dole, H.   Dore, O.   Douspis, M.   Ducout, A.   Dupac, X.   Elsner, F.   Ensslin, T. A.   Finelli, F.   Forni, O.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Galeotta, S.   Ganga, K.   Genova-Santos, R. T.   Giard, M.   Giraud-Heraud, Y.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Gudmundsson, J. E.   Hansen, F. K.   Harrison, D. L.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Hornstrup, A.   Hovest, W.   Hurier, G.   Jaffe, A. H.   Jaffe, T. R.   Jones, W. C.   Keihanen, E.   Keskitalo, R.   Khamitov, I.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leonardi, R.   Levrier, F.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Macias-Perez, J. F.   Maffei, B.   Maggio, G.   Mandolesi, N.   Mangilli, A.   Maris, M.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   Melchiorri, A.   Mennella, A.   Migliaccio, M.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Norgaard-Nielsen, H. U.   Novikov, D.   Novikov, I.   Oxborrow, C. A.   Pagano, L.   Pajot, F.   Paoletti, D.   Pasian, F.   Perdereau, O.   Perotto, L.   Pettorino, V.   Piacentini, F.   Piat, M.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Pratt, G. W.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   Rubino-Martin, J. A.   Rusholme, B.   Santos, D.   Savelainen, M.   Savini, G.   Scott, D.   Stolyarov, V.   Stompor, R.   Sudiwala, R.   Sunyaev, R.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Tucci, M.   Valenziano, L.   Valiviita, J.   Van Tent, F.   Vielva, P.   Villa, F.   Wade, L. A.   Wehus, I. K.   Yvon, D.   Zacchei, A.   Zonca, A.  

    Although infrared (IR) overall dust emission from clusters of galaxies has been statistically detected using data from the Infrared Astronomical Satellite (IRAS), it has not been possible to sample the spectral energy distribution (SED) of this emission over its peak, and thus to break the degeneracy between dust temperature and mass. By complementing the IRAS spectral coverage with Planck satellite data from 100 to 857 GHz, we provide new constraints on the IR spectrum of thermal dust emission in clusters of galaxies. We achieve this by using a stacking approach for a sample of several hundred objects from the Planck cluster sample. This procedure averages out fluctuations from the IR sky, allowing us to reach a significant detection of the faint cluster contribution. We also use the large frequency range probed by Planck, together with component-separation techniques, to remove the contamination from both cosmic microwave background anisotropies and the thermal Sunyaev-Zeldovich effect (tSZ) signal, which dominate at v <=3D 353 GHz. By excluding dominant spurious signals or systematic effects, averaged detections are reported at frequencies 353 GHz <=3D v <=3D 5000 GHz. We confirm the presence of dust in clusters of galaxies at low and intermediate redshifts, yielding an SED with a shape similar to that of the Milky Way. Planck's resolution does not allow us to investigate the detailed spatial distribution of this emission (e.g. whether it comes from intergalactic dust or simply the dust content of the cluster galaxies), but the radial distribution of the emission appears to follow that of the stacked SZ signal, and thus the extent of the clusters. The recovered SED allows us to constrain the dust mass responsible for the signal and its temperature.
    Download Collect
  • Planck early results. XIX. All-sky temperature and dust optical depth from Planck and IRAS. Constraints on the "dark gas" in our Galaxy

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Balbi, A.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Battaner, E.   Benabed, K.   Benoit, A.   Bernard, J. -P.   Bersanelli, M.   Bhatia, R.   Bock, J. J.   Bonaldi, A.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Boulanger, F.   Bucher, M.   Burigana, C.   Cabella, P.   Cardoso, J. -F.   Catalano, A.   Cayon, L.   Challinor, A.   Chamballu, A.   Chiang, L. -Y   Chiang, C.   Christensen, P. R.   Clements, D. L.   Colombi, S.   Couchot, F.   Coulais, A.   Crill, B. P.   Cuttaia, F.   Dame, T. M.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Gasperis, G.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Delouis, J. -M.   Desert, F. -X.   Dickinson, C.   Dobashi, K.   Donzelli, S.   Dore, O.   Doerl, U.   Douspis, M.   Dupac, X.   Efstathiou, G.   Ensslin, T. A.   Eriksen, H. K.   Falgarone, E.   Finelli, F.   Forni, O.   Fosalba, P.   Frailis, M.   Franceschi, E.   Fukui, Y.   Galeotta, S.   Ganga, K.   Giard, M.   Giardino, G.   Giraud-Heraud, Y.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gratton, S.   Gregorio, A.   Grenier, I. A.   Gruppuso, A.   Hansen, F. K.   Harrison, D.   Helou, G.   Henrot-Versille, S.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Hovest, W.   Hoyland, R. J.   Huffenberger, K. M.   Jaffe, A. H.   Jones, W. C.   Juvela, M.   Kawamura, A.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Kneissl, R.   Knox, L.   Kurki-Suonio, H.   Lagache, G.   Lamarre, J. -M.   Lasenby, A.   Laureijs, R. J.   Lawrence, C. R.   Leach, S.   Leonardi, R.   Leroy, C.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   MacTavish, C. J.   Maffei, B.   Maino, D.   Mandolesi, N.   Mann, R.   Maris, M.   Martin, P.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   Matthai, F.   Mazzotta, P.   McGehee, P.   Meinhold, P. R.   Melchiorri, A.   Mendes, L.   Mennella, A.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Murphy, A.   Naselsky, P.   Natoli, P.   Netterfield, C. B.   Norgaard-Nielsen, H. U.   Noviello, F.   Novikov, D.   Novikov, I.   O'Dwyer, I. J.   Onishi, T.   Osborne, S.   Pajot, F.   Paladini, R.   Paradis, D.   Pasian, F.   Patanchon, G.   Perdereau, O.   Perotto, L.   Perrotta, F.   Piacentini, F.   Piat, M.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Poutanen, T.   Prezeau, G.   Prunet, S.   Puget, J. -L.   Reach, W. T.   Reinecke, M.   Renault, C.   Ricciardi, S.   Riller, T.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rowan-Robinson, M.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Santos, D.   Savini, G.   Scott, D.   Seiffert, M. D.   Shellard, P.   Smoot, G. F.   Starck, J. -L.   Stivoli, F.   Stolyarov, V.   Stompor, R.   Sudiwala, R.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Torre, J. -P.   Tristram, M.   Tuovinen, J.   Umana, G.   Valenziano, L.   Vielva, P.   Villa, F.   Vittorio, N.   Wade, L. A.   Wandelt, B. D.   Wilkinson, A.   Yvon, D.   Zacchei, A.   Zonca, A.  

    An all sky map of the apparent temperature and optical depth of thermal dust emission is constructed using the Planck-HFI (350 mu m to 2 mm) and IRAS (100 mu m) data. The optical depth maps are correlated with tracers of the atomic (H I) and molecular gas traced by CO. The correlation with the column density of observed gas is linear in the lowest column density regions at high Galactic latitudes. At high N-H, the correlation is consistent with that of the lowest N-H, for a given choice of the CO-to-H-2 conversion factor. In the intermediate N-H range, a departure from linearity is observed, with the dust optical depth in excess of the correlation. This excess emission is attributed to thermal emission by dust associated with a dark gas phase, undetected in the available H I and CO surveys. The 2D spatial distribution of the dark gas in the solar neighbourhood (vertical bar b(II)vertical bar > 10 degrees) is shown to extend around known molecular regions traced by CO. The average dust emissivity in the H I phase in the solar neighbourhood is found to be tau(D)/N-H(tot) = 5.2 x 10(-26) cm(2) at 857 GHz. It follows roughly a power law distribution with a spectral index beta = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. Taking into account the spectral shape of the dust optical depth, the emissivity is consistent with previous values derived from FIRAS measurements at high latitudes within 10%. The threshold for the existence of the dark gas is found at N-H(tot) = (8.0 +/- 0.58) x 10(20) H cm(-2) (A(V) = 0.4 mag). Assuming the same high frequency emissivity for the dust in the atomic and the molecular phases leads to an average X-CO = (2.54 +/- 0.13) x 10(20) H-2 cm(-2)/(K km s(-1)). The mass of dark gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighbourhood. The Galactic latitude distribution shows that its mass fraction is relatively constant down to a few degrees from the Galactic plane. A possible explanation for the dark gas lies in a dark molecular phase, where H-2 survives photodissociation but CO does not. The observed transition for the onset of this phase in the solar neighbourhood (A(V) = 0.4 mag) appears consistent with recent theoretical predictions. It is also possible that up to half of the dark gas could be in atomic form, due to optical depth effects in the Hi measurements.
    Download Collect
  • Planck intermediate results XLII. Large-scale Galactic magnetic fields

    Adam, R.   Ade, P. A. R.   Alves, M. I. R.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartolo, N.   Battaner, E.   Benabed, K.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Boulanger, F.   Bucher, M.   Burigana, C.   Butler, R. C.   Calabrese, E.   Cardoso, J. -F.   Catalano, A.   Chiang, H. C.   Christensen, P. R.   Colombo, L. P. L.   Combet, C.   Couchot, F.   Crill, B. P.   Curto, A.   Cuttaia, F.   Danese, L.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Dickinson, C.   Diego, J. M.   Dolag, K.   Dore, O.   Ducout, A.   Dupac, X.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Ferriere, K.   Finelli, F.   Forni, O.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Galeotta, S.   Ganga, K.   Ghosh, T.   Giard, M.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Gudmundsson, J. E.   Hansen, F. K.   Harrison, D. L.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hobson, M.   Hornstrup, A.   Hurier, G.   Jaffe, A. H.   Jaffe, T. R.   Jones, W. C.   Juvela, M.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leahy, J. P.   Leonardi, R.   Levrier, F.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maggio, G.   Maino, D.   Mandolesi, N.   Mangilli, A.   Maris, M.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   Melchiorri, A.   Mennella, A.   Migliaccio, M.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Munshi, D.   Murphy, J. A.   Naselsky, P.   Nati, F.   Natoli, P.   Norgaard-Nielsen, H. U.   Oppermann, N.   Orlando, E.   Pagano, L.   Pajot, F.   Paladini, R.   Paoletti, D.   Pasian, F.   Perotto, L.   Pettorino, V.   Piacentini, F.   Piat, M.   Pierpaoli, E.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Pratt, G. W.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rossetti, M.   Roudier, G.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Santos, D.   Savelainen, M.   Scott, D.   Spencer, L. D.   Stolyarov, V.   Stompor, R.   Strong, A. W.   Sudiwala, R.   Sunyaev, R.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Tucci, M.   Valenziano, L.   Valiviita, J.   Van Tent, F.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   Wehus, I. K.   Yvon, D.   Zacchei, A.   Zonca, A.  

    Recent models for the large-scale Galactic magnetic fields in the literature have been largely constrained by synchrotron emission and Faraday rotation measures. We use three different but representative models to compare their predicted polarized synchrotron and dust emission with that measured by the Planck satellite. We first update these models to match the Planck synchrotron products using a common model for the cosmic-ray leptons. We discuss the impact on this analysis of the ongoing problems of component separation in the Planck microwave bands and of the uncertain cosmic-ray spectrum. In particular, the inferred degree of ordering in the magnetic fields is sensitive to these systematic uncertainties, and we further show the importance of considering the expected variations in the observables in addition to their mean morphology. We then compare the resulting simulated emission to the observed dust polarization and find that the dust predictions do not match the morphology in the Planck data but underpredict the dust polarization away from the plane. We modify one of the models to roughly match both observables at high latitudes by increasing the field ordering in the thin disc near the observer. Though this specific analysis is dependent on the component separation issues, we present the improved model as a proof of concept for how these studies can be advanced in future using complementary information from ongoing and planned observational projects.
    Download Collect
  • Planck intermediate results XXXIX. The Planck list of high-redshift source candidates

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B. -   Bartolo, N.   Battaner, E.   Benabed, K.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Boulanger, F.   Burigana, C.   Butler, R. C.   Calabrese, E.   Catalano, A.   Chiang, H. C.   Christensen, P. R.   Clements, D. L.   Colombo, L. P. L.   Couchot, F.   Coulais, A.   Crill, B. P.   Curto, A.   Cuttaia, F.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Dickinson, C.   Diego, J. M.   Dole, H.   Dore, O.   Douspis, M.   Ducout, A.   Dupac, X.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Falgarone, E.   Finelli, F.   Flores-Cacho, I.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Galeotta, S.   Galli, S.   Ganga, K.   Giard, M.   Giraud-Heraud, Y.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Gudmundsson, J. E.   Hansen, F. K.   Harrison, D. L.   Helou, G.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Hornstrup, A.   Hovest, W.   Huffenberger, K. M.   Hurier, G.   Jaffe, A. H.   Jaffe, T. R.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leonardi, R.   Levrier, F.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Macias-Perez, J. F.   Maffei, B.   Maggio, G.   Maino, D.   Mandolesi, N.   Mangilli, A.   Maris, M.   Martin, P. G.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   Melchiorri, A.   Mennella, A.   Migliaccio, M.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Murphy, J. A.   Nati, F.   Natoli, P.   Nesvadba, N. P. H.   Noviello, F.   Novikov, D.   Novikov, I.   Oxborrow, C. A.   Pagano, L.   Pajot, F.   Paoletti, D.   Partridge, B.   Pasian, F.   Pearson, T. J.   Perdereau, O.   Perotto, L.   Pettorino, V.   Piacentini, F.   Piat, M.   Plaszczynski, S.   Pointecouteau, E.   Polenta, G.   Pratt, G. W.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Santos, D.   Savelainen, M.   Savini, G.   Scott, D.   Spencer, L. D.   Stolyarov, V.   Stompor, R.   Sudiwala, R.   Sunyaev, R.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Tucci, M.   Tuerler, M.   Umana, G.   Valenziano, L.   Valiviita, J.   Van Tent, F.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   Wehus, I. K.   Welikala, N.   Yvon, D.   Zacchei, A.   Zonca, A.  

    The Planck mission, thanks to its large frequency range and all-sky coverage, has a unique potential for systematically detecting the brightest, and rarest, submillimetre sources on the sky, including distant objects in the high-redshift Universe traced by their dust emission. A novel method, based on a component-separation procedure using a combination of Planck and IRAS data, has been validated and characterized on numerous simulations, and applied to select the most luminous cold submillimetre sources with spectral energy distributions peaking between 353 and 857 GHz at 5' resolution. A total of 2151 Planck high-z source candidates (the PHZ) have been detected in the cleanest 26% of the sky, with flux density at 545 GHz above 500 mJy. Embedded in the cosmic infrared background close to the confusion limit, these high-z candidates exhibit colder colours than their surroundings, consistent with redshifts z > 2, assuming a dust temperature of T-xgal =3D 35K and a spectral index of beta(xgal) =3D 1.5. Exhibiting extremely high luminosities, larger than 10(14) L-circle dot, the PHZ objects may be made of multiple galaxies or clumps at high redshift, as suggested by a first statistical analysis based on a comparison with number count models. Furthermore, first follow-up observations obtained from optical to submillimetre wavelengths, which can be found in companion papers, have confirmed that this list consists of two distinct populations. A small fraction (around 3%) of the sources have been identified as strongly gravitationally lensed star-forming galaxies at redshift 2 to 4, while the vast majority of the PHZ sources appear as overdensities of dusty star-forming galaxies, having colours consistent with being at z > 2, and may be considered as proto-cluster candidates. The PHZ provides an original sample, which is complementary to the Planck Sunyaev-Zeldovich Catalogue (PSZ2); by extending the population of virialized massive galaxy clusters detected below z < 1.5 through their SZ signal to a population of sources at z > 1.5, the PHZ may contain the progenitors of today's clusters. Hence the Planck list of high-redshift source candidates opens a new window on the study of the early stages of structure formation, particularly understanding the intensively star-forming phase at high-z.
    Download Collect
  • Planck intermediate results I. Further validation of new Planck clusters with XMM-Newton

    Aghanim, N.   Collaboration, Planck   Arnaud, M.   Ashdown, M.   Atrio-Barandela, F.   Aumont, J.   Baccigalupi, C.   Balbi, A.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Battaner, E.   Benabed, K.   Bernard, J. -P.   Bersanelli, M.   Boehringer, H.   Bonaldi, A.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Bourdin, H.   Brown, M. L.   Burigana, C.   Butler, R. C.   Cabella, P.   Cardoso, J. -F.   Carvalho, P.   Catalano, A.   Cayon, L.   Chamballu, A.   Chary, R. -R.   Chiang, L. -Y.   Chon, G.   Christensen, P. R.   Clements, D. L.   Colafrancesco, S.   Colombi, S.   Coulais, A.   Crill, B. P.   Cuttaia, F.   da Silva, A.   Dahle, H.   Davis, R. J.   de Bernardis, P.   de Gasperis, G.   de Zotti, G.   Delabrouille, J.   Democles, J.   Desert, F. -X.   Diego, J. M.   Dolag, K.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Dupac, X.   Ensslin, T. A.   Eriksen, H. K.   Finelli, F.   Flores-Cacho, I.   Forni, O.   Fosalba, P.   Frailis, M.   Fromenteau, S.   Galeotta, S.   Ganga, K.   Genova-Santos, R. T.   Giard, M.   Gonzalez-Nuevo, J.   Gonzalez-Riestra, R.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Hansen, F. K.   Harrison, D.   Hempel, A.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hornstrup, A.   Huffenberger, K. M.   Hurier, G.   Jagemann, T.   Jasche, J.   Juvela, M.   Keihaenen, E.   Keskitalo, R.   Kisner, T. S.   Kneissl, R.   Knoche, J.   Knox, L.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Lawrence, C. R.   Leach, S.   Leonardi, R.   Liddle, A.   Lilje, P. B.   Lopez-Caniego, M.   Luzzi, G.   Macias-Perez, J. F.   Maino, D.   Mandolesi, N.   Mann, R.   Marleau, F.   Marshall, D. J.   Martinez-Gonzalez, E.   Masi, S.   Massardi, M.   Matarrese, S.   Matthai, F.   Mazzotta, P.   Meinhold, P. R.   Melchiorri, A.   Melin, J. -B.   Mendes, L.   Mennella, A.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Munshi, D.   Naselsky, P.   Natoli, P.   Norgaard-Nielsen, H. U.   Noviello, F.   Osborne, S.   Pasian, F.   Patanchon, G.   Perdereau, O.   Perrotta, F.   Piacentini, F.   Pierpaoli, E.   Plaszczynski, S.   Platania, P.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Popa, L.   Poutanen, T.   Pratt, G. W.   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.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Savini, G.   Schaefer, B. M.   Scott, D.   Smoot, G. F.   Starck, J. -L.   Stivoli, F.   Sunyaev, R.   Sutton, D.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Valenziano, L.   Van Tent, B.   Vielva, P.   Villa, F.   Vittorio, N.   Wandelt, B. D.   Weller, J.   White, S. D. M.   Yvon, D.   Zacchei, A.   Zonca, A.  

    We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 < S/N < 5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 < z < 0.94, demonstrating Planck's capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using Y-X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y-SZ-Y-X relation, with a turnover at Y-SZ similar to 4 x 10 (4) arcmin(2). We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the Y-X vs. Y-SZ and X-ray flux F-X vs. Y-SZ relations.
    Download Collect
  • Planck 2015 results XIV. Dark energy and modified gravity

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Aumont, J.   Baccigalupi, C.   Banday, A. J.   Barreiro, R. B.   Bartolo, N.   Battaner, E.   Battye, R.   Benabed, K.   Benoit, A.   Benoit-Levy, A.   Bernard, J. -P.   Bersanelli, M.   Bielewicz, P.   Bock, J. J.   Bonaldi, A.   Bonavera, L.   Bond, J. R.   Borrill, J.   Bouchet, F. R.   Bucher, M.   Burigana, C.   Butler, R. C.   Calabrese, E.   Cardoso, J. -F.   Catalano, A.   Challinor, A.   Chamballu, A.   Chiang, H. C.   Christensen, P. R.   Church, S.   Clements, D. L.   Colombi, S.   Colombo, L. P. L.   Combet, C.   Couchot, F.   Coulais, A.   Crill, B. P.   Curto, A.   Cuttaia, F.   Danese, L.   Davies, R. D.   Davis, R. J.   de Bernardis, P.   de Rosa, A.   de Zotti, G.   Delabrouille, J.   Desert, F. -X.   Diego, J. M.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Ducout, A.   Dupac, X.   Efstathiou, G.   Elsner, F.   Ensslin, T. A.   Eriksen, H. K.   Fergusson, J.   Finelli, F.   Forni, O.   Frailis, M.   Fraisse, A. A.   Franceschi, E.   Frejsel, A.   Galeotta, S.   Galli, S.   Ganga, K.   Giard, M.   Giraud-Heraud, Y.   Gjerlow, E.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gratton, S.   Gregorio, A.   Gruppuso, A.   Gudmundsson, J. E.   Hansen, F. K.   Hanson, D.   Harrison, D. L.   Heavens, A.   Helou, G.   Henrot-Versille, S.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Hornstrup, A.   Hovest, W.   Huang, Z.   Huffenberger, K. M.   Hurier, G.   Jaffe, A. H.   Jaffe, T. R.   Jones, W. C.   Juvela, M.   Keihanen, E.   Keskitalo, R.   Kisner, T. S.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lahteenmaki, A.   Lamarre, J. -M.   Lasenby, A.   Lattanzi, M.   Lawrence, C. R.   Leonardi, R.   Lesgourgues, J.   Levrier, F.   Lewis, A.   Liguori, M.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Lubin, P. M.   Ma, Y. -Z.   Macias-Perez, J. F.   Maggio, G.   Maino, D.   Mandolesi, N.   Mangilli, A.   Marchini, A.   Maris, M.   Martin, P. G.   Martinelli, M.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   McGehee, P.   Meinhold, P. R.   Melchiorri, A.   Mendes, L.   Mennella, A.   Migliaccio, M.   Mitra, S.   Miville-Deschenes, M. -A.   Moneti, A.   Montier, L.   Morgante, G.   Mortlock, D.   Moss, A.   Munshi, D.   Murphy, J. A.   Narimani, A.   Naselsky, P.   Nati, F.   Natoli, P.   Netterfield, C. B.   Norgaard-Nielsen, H. U.   Noviello, F.   Novikov, D.   Novikov, I.   Oxborrow, C. A.   Paci, F.   Pagano, L.   Pajot, F.   Paoletti, D.   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.   Pointecouteau, E.   Polenta, G.   Popa, L.   Pratt, G. W.   Prezeau, G.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Reach, W. T.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Renzi, A.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Roudier, G.   Rowan-Robinson, M.   Rubino-Martin, J. A.   Rusholme, B.   Salvatelli, V.   Sandri, M.   Santos, D.   Savelainen, M.   Savini, G.   Schaefer, B. M.   Scott, D.   Seiffert, M. D.   Shellard, E. P. S.   Spencer, L. D.   Stolyarov, V.   Stompor, R.   Sudiwala, R.   Sunyaev, R.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Tucci, M.   Tuovinen, J.   Valenziano, L.   Valiviita, J.   Van Tent, B.   Viel, M.   Vielva, P.   Villa, F.   Wade, L. A.   Wandelt, B. D.   Wehus, I. K.   White, M.   Yvon, D.   Zacchei, A.   Zonca, A.  

    We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG) beyond the standard cosmological constant scenario. We start with cases where the DE only directly affects the background evolution, considering Taylor expansions of the equation of state w(a), as well as principal component analysis and parameterizations related to the potential of a minimally coupled DE scalar field. When estimating the density of DE at early times, we significantly improve present constraints and find that it has to be below similar to 2% (at 95% confidence) of the critical density, even when forced to play a role for z < 50 only. We then move to general parameterizations of the DE or MG perturbations that encompass both effective field theories and the phenomenology of gravitational potentials in MG models. Lastly, we test a range of specific models, such as k-essence, f(R) theories, and coupled DE. In addition to the latest Planck data, for our main analyses, we use background constraints from baryonic acoustic oscillations, type-Ia supernovae, and local measurements of the Hubble constant. We further show the impact of measurements of the cosmological perturbations, such as redshift-space distortions and weak gravitational lensing. These additional probes are important tools for testing MG models and for breaking degeneracies that are still present in the combination of Planck and background data sets. All results that include only background parameterizations (expansion of the equation of state, early DE, general potentials in minimally-coupled scalar fields or principal component analysis) are in agreement with ACDM. When testing models that also change perturbations (even when the background is fixed to ACDM), some tensions appear in a few scenarios: the maximum one found is similar to 2 sigma for Planck TT + lowP when parameterizing observables related to the gravitational potentials with a chosen time dependence; the tension increases to, at most, 3 sigma when external data sets are included. It however disappears when including CMB lensing.
    Download Collect
  • Planck intermediate results III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal

    Ade, P. A. R.   Aghanim, N.   Arnaud, M.   Ashdown, M.   Atrio-Barandela, F.   Aumont, J.   Baccigalupi, C.   Balbi, A.   Banday, A. J.   Barreiro, R. B.   Bartlett, J. G.   Battaner, E.   Battye, R.   Benabed, K.   Bernard, J. -P.   Bersanelli, M.   Bhatia, R.   Bikmaev, I.   Boehringer, H.   Bonaldi, A.   Bond, J. R.   Borgani, S.   Borrill, J.   Bouchet, F. R.   Bourdin, H.   Brown, M. L.   Bucher, M.   Burenin, R.   Burigana, C.   Butler, R. C.   Cabella, P.   Cardoso, J. -F.   Carvalho, P.   Chamballu, A.   Chiang, L. -Y.   Chon, G.   Clements, D. L.   Colafrancesco, S.   Coulais, A.   Cuttaia, F.   Da Silva, A.   Dahle, H.   Davis, R. J.   de Bernardis, P.   de Gasperis, G.   Delabrouille, J.   Democles, J.   Desert, F. -X.   Diego, J. M.   Dolag, K.   Dole, H.   Donzelli, S.   Dore, O.   Douspis, M.   Dupac, X.   Efstathiou, G.   Ensslin, T. A.   Eriksen, H. K.   Finelli, F.   Flores-Cacho, I.   Forni, O.   Frailis, M.   Franceschi, E.   Frommert, M.   Galeotta, S.   Ganga, K.   Genova-Santos, R. T.   Giard, M.   Giraud-Heraud, Y.   Gonzalez-Nuevo, J.   Gorski, K. M.   Gregorio, A.   Gruppuso, A.   Hansen, F. K.   Harrison, D.   Hernandez-Monteagudo, C.   Herranz, D.   Hildebrandt, S. R.   Hivon, E.   Hobson, M.   Holmes, W. A.   Huffenberger, K. M.   Hurier, G.   Jagemann, T.   Juvela, M.   Keihanen, E.   Khamitov, I.   Kneissl, R.   Knoche, J.   Kunz, M.   Kurki-Suonio, H.   Lagache, G.   Lamarre, J. -M.   Lasenby, A.   Lawrence, C. R.   Le Jeune, M.   Leach, S.   Leonardi, R.   Liddle, A.   Lilje, P. B.   Linden-Vornle, M.   Lopez-Caniego, M.   Luzzi, G.   Macias-Perez, J. F.   Maino, D.   Mandolesi, N.   Maris, M.   Marleau, F.   Marshall, D. J.   Martinez-Gonzalez, E.   Masi, S.   Matarrese, S.   Matthai, F.   Mazzotta, P.   Meinhold, P. R.   Melchiorri, A.   Melin, J. -B.   Mendes, L.   Mitra, S.   Miville-Deschenes, M. -A.   Montier, L.   Morgante, G.   Munshi, D.   Natoli, P.   Norgaard-Nielsen, H. U.   Noviello, F.   Osborne, S.   Pajot, F.   Paoletti, D.   Partridge, B.   Pearson, T. J.   Perdereau, O.   Perrotta, F.   Piacentini, F.   Piat, M.   Pierpaoli, E.   Piffaretti, R.   Platania, P.   Pointecouteau, E.   Polenta, G.   Ponthieu, N.   Popa, L.   Poutanen, T.   Pratt, G. W.   Prunet, S.   Puget, J. -L.   Rachen, J. P.   Rebolo, R.   Reinecke, M.   Remazeilles, M.   Renault, C.   Ricciardi, S.   Ristorcelli, I.   Rocha, G.   Rosset, C.   Rossetti, M.   Rubino-Martin, J. A.   Rusholme, B.   Sandri, M.   Savini, G.   Scott, D.   Starck, J. -L.   Stivoli, F.   Stolyarov, V.   Sudiwala, R.   Sunyaev, R.   Sutton, D.   Suur-Uski, A. -S.   Sygnet, J. -F.   Tauber, J. A.   Terenzi, L.   Toffolatti, L.   Tomasi, M.   Tristram, M.   Valenziano, L.   Van Tent, B.   Vielva, P.   Villa, F.   Vittorio, N.   Wandelt, B. D.   Weller, J.   White, S. D. M.   Yvon, D.   Zacchei, A.   Zonca, A.  

    We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D-A(2) Y-500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M-WL-D-A(2) Y-500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R-500 are on average similar to 20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations.
    Download Collect
1 2 3 4 5 6 7

Contact

If you have any feedback, Please follow the official account to submit feedback.

Turn on your phone and scan

Submit Feedback