Suchergebnisse

European Space Agency ; Centre National D'etudes Spatiales ; CNRS/INSU-IN2P3-INP (France) ; Agenzia Spaziale Italiana (ASI) ; Italian National Research Council ; Istituto Nazionale Astrofisica (INAF) ; National Aeronautics & Space Administration (NASA) ; United States Department of Energy (DOE) ; Science & Technology Facilities Council (STFC) ; UKSA (UK) ; Consejo Superior de Investigaciones Cientificas (CSIC) ; MINECO (Spain) ; JA (Spain) ; RES (Spain) ; CSC (Finland) ; Finnish Funding Agency for Technology & Innovation (TEKES) ; AoF (Finland) ; Helmholtz Association German Aerospace Centre (DLR) ; Max Planck Society ; CSA (Canada) ; DTU Space (Denmark) ; SER/SSO (Switzerland) ; RCN (Norway) ; Science Foundation Ireland ; Portuguese Foundation for Science and Technology ; ERC (EU) ; European Union (EU) ; Labex ILP

The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. ; We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 <ℓ< 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology. ; Centre National D'etudes Spatiales ; CNRS/INSU-IN2P3-INP (France) ; European Space Agency ; Italian Space Agency (ASI) ; Italian National Research Council ; Istituto Nazionale Astrofisica (INAF) ; National Aeronautics & Space Administration (NASA) ; United States Department of Energy (DOE) ; UKSA (UK) ; Consejo Superior de Investigaciones Cientificas (CSIC) ; MINECO (Spain) ; RES (Spain) ; Finnish Funding Agency for Technology & Innovation (TEKES) ; AoF (Finland) ; CSC (Finland) ; Helmholtz Association ; German Aerospace Centre (DLR) ; Max Planck Society ; CSA (Canada) ; DTU Space (Denmark) ; SER/SSO (Switzerland) ; RCN (Norway) ; Science Foundation Ireland ; Portuguese Foundation for Science and Technology ; ERC (EU) ; European Union (EU) ; J.A. (Spain) ; Science & Technology Facilities Council (STFC) ST/L000768/1

Acknowledgements. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration ; This paper describes the identification, modelling, and removal of previously unexplained systematic effects in the polarization data of the Planck High Frequency Instrument (HFI) on large angular scales, including new mapmaking and calibration procedures, new and more complete end-to-end simulations, and a set of robust internal consistency checks on the resulting maps. These maps, at 100, 143, 217, and 353 GHz, are early versions of those that will be released in final form later in 2016. The improvements allow us to determine the cosmic reionization optical depth τ using, for the first time, the low-multipole EE data from HFI, reducing significantly the central value and uncertainty, and hence the upper limit. Two different likelihood procedures are used to constrain τ from two estimators of the CMB E- and B-mode angular power spectra at 100 and 143 GHz, after debiasing the spectra from a small remaining systematic contamination. These all give fully consistent results. A further consistency test is performed using cross-correlations derived from the Low Frequency Instrument maps of the Planck 2015 data release and the new HFI data. For this purpose, end-to-end analyses of systematic effects from the two instruments are used to demonstrate the near independence of their dominant systematic error residuals. The tightest result comes from the HFI-based τ posterior distribution using the maximum likelihood power spectrum estimator from EE data only, giving a value 0.055 ± 0.009. In a companion paper these results are discussed in the context of the best-fit PlanckΛCDM cosmological model and recent models of reionization. ; European Space Agency ; Centre National D'etudes Spatiales ; CNRS/INSU-IN2P3-INP (France) ; Italian Space Agency (ASI) ; Italian National Research Council ; Istituto Nazionale Astrofisica (INAF) ; National Aeronautics & Space Administration (NASA) ; United States Department of Energy (DOE) ; Science & Technology Facilities Council (STFC) ; UKSA (UK) ; Consejo Superior de Investigaciones Cientificas (CSIC) ; RES (Spain) ; MINECO (Spain) ; CSC (Finland) ; AoF (Finland) ; Finnish Funding Agency for Technology & Innovation (TEKES) ; Helmholtz Association ; German Aerospace Centre (DLR) ; Max Planck Society ; CSA (Canada) ; DTU Space (Denmark) ; SER/SSO (Switzerland) ; RCN (Norway) ; Science Foundation Ireland ; Portuguese Foundation for Science and Technology ; ERC (EU) ; European Union (EU) ; J.A. (Spain) ; Science & Technology Facilities Council (STFC) ST/L000768/1 ST/L000393/1 ST/M004856/1

The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007–2013)/ERC grant agreement No. 267934. ; Adam, R., Ade, P.A.R., Aghanim, N., Alves, M.I.R., Arnaud, M., Arzoumanian, D., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., Couchot, F., 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., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Hanson, D., Harrison, D.L., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.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., 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-Vørnle, M., López-Caniego, M., Lubin, P.M., Macías-Pérez, J.F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M.-A., ...

The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. 267934. ; Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Benabed, K., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Burigana, C., Calabrese, E., Cardoso, J.-F., Chiang, H.C., Colombo, L.P.L., Combet, C., Comis, B., Crill, B.P., Curto, A., Cuttaia, F., Davis, R.J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J.-M., Di Valentino, E., Dickinson, C., Diego, J.M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fantaye, Y., Finelli, F., Frailis, M., Fraisse, A.A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R.T., Gerbino, M., Ghosh, T., Giard, M., González-Nuevo, J., Górski, K.M., Gregorio, A., Gruppuso, A., Gudmundsson, J.E., Hansen, F.K., Helou, G., Herranz, D., Hivon, E., Huang, Z., Jaffe, A.H., Jones, W.C., Keihänen, E., Keskitalo, R., Kisner, T.S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Le Jeune, M., Levrier, F., Liguori, M., Lilje, P.B., López-Caniego, M., Lubin, P.M., MacIás-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P.G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J.D., Melchiorri, ...

The Planck Collaboration acknowledges the support of ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union's Horizon 2020 Research & Innovation Framework Programme/ERC grant agreement ERC-2016-ADG-742719. This research has received funding from the Agence Nationale de la Recherche (ANR-17-CE31-0022). ; Aghanim, N., Akrami, Y., Alves, M.I.R., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Benabed, K., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Bucher, M., Burigana, C., Calabrese, E., Cardoso, J.-F., Carron, J., Chary, R.-R., Chiang, H.C., Colombo, L.P.L., Combet, C., Crill, B.P., Cuttaia, F., De Bernardis, P., De Zotti, G., Delabrouille, J., Delouis, J.-M., Di Valentino, E., Dickinson, C., Diego, J.M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fantaye, Y., Fernandez-Cobos, R., Ferrière, K., Finelli, F., Forastieri, F., Frailis, M., Fraisse, A.A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R.T., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K.M., Gratton, S., Green, G., Gruppuso, A., Gudmundsson, J.E., Guillet, V., Handley, W., Hansen, F.K., Helou, G., Herranz, D., Hivon, E., Huang, Z., Jaffe, A.H., Jones, W.C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Le Jeune, M., Levrier, F., Liguori, M., Lilje, P.B., Lindholm, V., López-Caniego, ...

La versión del editor incluye 'erratum'. ; (…) CSIC, MINECO, JA, and RES (Spain); the European Research Council under the European Union's Seventh Framework Programme (FP/2007- 2013)/ERC [grant agreement no. 616170]; the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [grant agreement no 725456 CMBSPEC] ; Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Battye, R., Benabed, K., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Carron, J., Challinor, A., Chiang, H.C., Chluba, J., Colombo, L.P.L., Combet, C., Contreras, D., Crill, B.P., Cuttaia, F., De Bernardis, P., De Zotti, G., Delabrouille, J., Delouis, J.-M., Di Valentino, E., Diego, J.M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Fantaye, Y., Farhang, M., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Frailis, M., Fraisse, A.A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R.T., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K.M., Gratton, S., Gruppuso, A., Gudmundsson, J.E., Hamann, J., Handley, W., Hansen, F.K., Herranz, D., Hildebrandt, S.R., Hivon, E., Huang, Z., Jaffe, A.H., Jones, W.C., Karakci, A., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T.S., Knox, L., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Le Jeune, M., Lemos, P., Lesgourgues, J., Levrier, F., Lewis, A., Liguori, M., Lilje, P.B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P.M., Ma, Y.-Z., Maciás-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Maris, M., Martin, P.G., Martinelli, M., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J.D., ...

CSIC, MINECO, JA, and RES (Spain); the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC [grant agreement no. 616170] (.) ; Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Benabed, K., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bucher, M., Burigana, C., Calabrese, E., Cardoso, J.-F., Carron, J., Challinor, A., Chiang, H.C., Colombo, L.P.L., Combet, C., Crill, B.P., Cuttaia, F., De Bernardis, P., De Zotti, G., Delabrouille, J., Di Valentino, E., Diego, J.M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Fantaye, Y., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Frailis, M., Fraisse, A.A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R.T., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K.M., Gratton, S., Gruppuso, A., Gudmundsson, J.E., Hamann, J., Handley, W., Hansen, F.K., Herranz, D., Hivon, E., Huang, Z., Jaffe, A.H., Jones, W.C., Karakci, A., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Knox, L., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Le Jeune, M., Levrier, F., Lewis, A., Liguori, M., Lilje, P.B., Lindholm, V., López-Caniego, M., Lubin, P.M., Ma, Y.-Z., Maciás-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Maris, M., Martin, P.G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J.D., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M.-A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Natoli, P., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Perrotta, F., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J.-L., Rachen, J.P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, ...

Galactic structure, stellar clusters and populations.-- et al. ; Planck data when combined with ancillary data provide a unique opportunity to separate the diffuse emission components of the inner Galaxy. The purpose of the paper is to elucidate the morphology of the various emission components in the strong star-formation region lying inside the solar radius and to clarify the relationship between the various components. The region of the Galactic plane covered is l = 300° → 0° → 60° wherestar-formation is highest and the emission is strong enough to make meaningful component separation. The latitude widths in this longitude range lie between 1° and 2°, which correspond to FWHM z-widths of 100−200 pc at a typical distance of 6 kpc. The four emission components studied here are synchrotron, free-free, anomalous microwave emission (AME), and thermal (vibrational) dust emission. These components are identified by constructing spectral energy distributions (SEDs) at positions along the Galactic plane using the wide frequency coverage of Planck (28.4−857 GHz) in combination with low-frequency radio data at 0.408−2.3 GHz plus WMAP data at 23−94 GHz, along with far-infrared (FIR) data from COBE-DIRBE and IRAS. The free-free component is determined from radio recombination line (RRL) data. AME is found to be comparable in brightness to the free-free emission on the Galactic plane in the frequency range 20−40 GHz with a width in latitude similar to that of the thermal dust; it comprises 45 ± 1% of the total 28.4 GHz emission in the longitude range l = 300° → 0° → 60°. The free-free component is the narrowest, reflecting the fact that it is produced by current star-formation as traced by the narrow distribution of OB stars. It is the dominant emission on the plane between 60 and 100 GHz. RRLs from this ionized gas are used to assess its distance, leading to a free-free z-width of FWHM ≈ 100 pc. The narrow synchrotron component has a low-frequency brightness spectral index βsynch ≈ −2.7 that is similar to the broad synchrotron component indicating that they are both populated by the cosmic ray electrons of the same spectral index. The width of this narrow synchrotron component is significantly larger than that of the other three components, suggesting that it is generated in an assembly of older supernova remnants that have expanded to sizes of order 150 pc in 3 × 105 yr; pulsars of a similar age have a similar spread in latitude. The thermal dust is identified in the SEDs with average parameters of Tdust = 20.4 ± 0.4 K, βFIR = 1.94 ± 0.03 (> 353 GHz), and βmm = 1.67 ± 0.02 (< 353 GHz). The latitude distributions of gamma-rays, CO, and the emission in high-frequency Planck bands have similar widths, showing that they are all indicators of the total gaseous matter on the plane in the inner Galaxy. ; The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The research leading to these results has received funding from an STFC Consolidated Grant (No. ST/L000768/1), as well as the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement Nos. 267934 and 307209. ; Peer Reviewed

Extragalactic astronomy.-- et al. ; The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiralarms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission (≳0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 μm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 μm emission). We also fit spectral energy distributions for individual 5′ pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 ± 1.0) K with a spectral index of 1.62 ± 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20–60 GHz, which corresponds to a star formation rate of around 0.12 M⊙ yr-1. We find a 2.3σ detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 ± 0.3 Jy, which is in line with expectations from our Galaxy. ; The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 307209, as well as funding from an STFC Consolidated Grant (No. ST/L000768/1). The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). ; Peer Reviewed

Cosmology (including clusters of galaxies).-- et al. ; We present the results of approximately three years of observations of Planck Sunyaev-Zeldovich (SZ) sources with the Russian-Turkish 1.5 m telescope (RTT150), as a part of the optical follow-up programme undertaken by the Planck collaboration. During this time period approximately 20% of all dark and grey clear time available at the telescope was devoted to observations of Planck objects. Some observations of distant clusters were also done at the 6 m Bolshoi Telescope Alt-azimutalnyi (BTA) of the Special Astrophysical Observatory of the Russian Academy of Sciences. In total, deep, direct images of more than one hundred fields were obtained in multiple filters. We identified 47 previously unknown galaxy clusters, 41 of which are included in the Planck catalogue of SZ sources. The redshifts of 65 Planck clusters were measured spectroscopically and 14 more were measured photometrically. We discuss the details of cluster optical identifications and redshift measurements. We also present new spectroscopic redshifts for 39 Planck clusters that were not included in the Planck SZ source catalogue and are published here for the first time. ; The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). This work was supported by Russian Foundation for Basic Research, grants 13-02-12250-ofim, 13-02-01464, 14-22-03111-ofim, by Programs of the Russian Academy of Sciences P-21 and OPhN-17 and by the subsidy of the Russian Government to Kazan Federal University (agreement No.02.A03.21.0002). ; Peer Reviewed

Interstellar and circumstellar matter.-- et al. ; Within ten nearby (d < 450 pc) Gould belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the gas column density structures, quantified by the gradient of the column density, NH. The selected regions, covering several degrees in size, are analysed at an effective angular resolution of 10′ FWHM, thus sampling physical scales from 0.4 to 40 pc in the nearest cloud. The column densities in the selected regions range from NH≈ 1021 to1023 cm-2, and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analysed in bins of column density using the novel statistical tool called "histogram of relative orientations". Throughout this study, we assume that the polarized emission observed by Planck at 353 GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing NH, from mostly parallel or having no preferred orientation to mostly perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfvénic or sub-Alfvénic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution. ; The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. ; Peer Reviewed

Planck Collaboration. ; The characterization of the Galactic foregrounds has been shown to be the main obstacle in thechallenging quest to detect primordial B-modes in the polarized microwave sky. We make use of the Planck-HFI 2015 data release at high frequencies to place new constraints on the properties of the polarized thermal dust emission at high Galactic latitudes. Here, we specifically study the spatial variability of the dust polarized spectral energy distribution (SED), and its potential impact on the determination of the tensor-to-scalar ratio, r. We use the correlation ratio of the angular power spectra between the 217 and 353 GHz channels as a tracer of these potential variations, computed on different high Galactic latitude regions, ranging from 80% to 20% of the sky. The new insight from Planck data is a departure of the correlation ratio from unity that cannot be attributed to a spurious decorrelation due to the cosmic microwave background, instrumental noise, or instrumental systematics. The effect is marginally detected on each region, but the statistical combination of all the regions gives more than 99% confidence for this variation in polarized dust properties. In addition, we show that the decorrelation increases when there is a decrease in the mean column density of the region of the sky being considered, and we propose a simple power-law empirical model for this dependence, which matches what is seen in the Planck data. We explore the effect that this measured decorrelation has on simulations of the BICEP2-Keck Array/Planck analysis and show that the 2015 constraints from these data still allow a decorrelation between the dust at 150 and 353 GHz that is compatible with our measured value. Finally, using simplified models, we show that either spatial variation of the dust SED or of the dust polarization angle are able to produce decorrelations between 217 and 353 GHz data similar to the values we observe in the data. ; The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. 267934. ; Peer Reviewed

ESA ; CNES (France) ; CNRS/INSU-IN2P3-INP (France) ; ASI (Italy) ; CNR (Italy) ; INAF (Italy) ; NASA (USA) ; DoE (USA) ; STFC (UK) ; UKSA (UK) ; CSIC (Spain) ; MINECO (Spain) ; JA (Spain) ; RES (Spain) ; Tekes (Finland) ; AoF (Finland) ; CSC (Finland) ; DLR (Germany) ; MPG (Germany) ; CSA (Canada) ; DTU Space (Denmark) ; SER/SSO (Switzerland) ; RCN (Norway) ; SFI (Ireland) ; FCT/MCTES (Portugal) ; ERC (EU) ; PRACE (EU) ; UK BIS NEI grants ; Office of Science of the U.S. Department of Energy ; Canada Foundation for Innovation under Compute Canada ; Government of Ontario ; University of Toronto ; Science and Technology Facilities Council ; Office of Science of the U.S. Department of Energy: DE-AC02-05CH11231 ; Science and Technology Facilities Council: ST/L000768/1 ; Science and Technology Facilities Council: ST/L000652/1 ; Science and Technology Facilities Council: ST/J005673/1 ; Science and Technology Facilities Council: ST/M00418X/1 ; Science and Technology Facilities Council: ST/L000393/1 ; Science and Technology Facilities Council: ST/M007065/1 ; Science and Technology Facilities Council: ST/K00333X/1 ; The Planck full mission cosmic microwave background (CMB) temperature and E-mode polarization maps are analysed to obtain constraints on primordial non-Gaussianity (NG). Using three classes of optimal bispectrum estimators - separable template-fitting (KSW), binned, and modal we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result from temperature alone f(NL)(local) = 2.5 +/- 5.7, f(NL)(equil) = 16 +/- 70, and f(NL)(ortho) = 34 +/- 33 (68% CL, statistical). Combining temperature and polarization data we obtain f(NL)(local) = 0.8 +/- 5.0, f(NL)(equil) = 4 +/- 43, and f(NL)(ortho) = 26 +/- 21 (68% CL, statistical). The results are based on comprehensive cross-validation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are consistent with estimators based on measuring the Minkowski functionals of the CMB. The effect of time-domain de-glitching systematics on the bispectrum is negligible. In spite of these test outcomes we conservatively label the results including polarization data as preliminary, owing to a known mismatch of the noise model in simulations and the data. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and derive constraints on early universe scenarios that generate primordial NG, including general single-field models of inflation, axion inflation, initial state modifications, models producing parity-violating tensor bispectra, and directionally dependent vector models. We present a wide survey of scale-dependent feature and resonance models, accounting for the look elsewhere effect in estimating the statistical significance of features. We also look for isocurvature NG, and find no signal, but we obtain constraints that improve significantly with the inclusion of polarization. The primordial trispectrum amplitude in the local model is constrained to be g(NL)(local) = (9.0 +/- 7.7) x 10(4) (68% CL statistical), and we perform an analysis of trispectrum shapes beyond the local case. The global picture that emerges is one of consistency with the premises of the Lambda CDM cosmology, namely that the structure we observe today was sourced by adiabatic, passive, Gaussian, and primordial seed perturbations.