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1. New Interpretable Statistics for Large Scale Structure Analysis and Generation

Author: Allys, E., Marchand, T., Cardoso, J. -F., Villaescusa-Navarro, F., Ho, S., and Mallat, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We introduce Wavelet Phase Harmonics (WPH) statistics: interpretable low-dimensional statistics that describe 2D non-Gaussian fields. These statistics are built from WPH moments, which were recently introduced in the data science and machine learning community. We apply WPH statistics to projected 2D matter density fields from the Quijote N-body simulations of the large-scale structure of the Universe. By computing Fisher information matrices, we find that the WPH statistics place more stringent constraints on four of five cosmological parameters when compared to statistics based on the combination of the power spectrum and bispectrum. We also use the WPH statistics with a maximum entropy model to statistically generate new 2D density fields that accurately reproduce the probability density function, the mean and standard deviation of the power spectrum, the bispectrum, and Minkowski functionals of the input density fields. Although other methods are efficient for either parameter estimates or statistical syntheses of the large-scale structure, WPH statistics are the first statistics that achieve state-of-the-art results for both tasks as well as being interpretable., Comment: 21 pages, accepted in PRD. New version with clarified explanations
Published: 2020
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2. Planck 2018 results

Author: Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Battye, R, Benabed, K, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Carron, J, Challinor, A, Chiang, HC, Chluba, J, Colombo, LPL, Combet, C, Contreras, D, Crill, BP, Cuttaia, F, de Bernardis, P, de Zotti, G, Delabrouille, J, Delouis, J-M, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, Farhang, M, Fergusson, J, Fernandez-Cobos, R, Finelli, F, Forastieri, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Gerbino, M, Ghosh, T, González-Nuevo, J, Górski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Hamann, J, Handley, W, Hansen, FK, Herranz, D, Hildebrandt, SR, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Karakci, A, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Knox, L, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Lemos, P, Lesgourgues, J, Levrier, F, Lewis, A, and Liguori, M
Subjects: Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, cosmic background radiation, cosmological parameters, errata, addenda, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: In the original version, the bounds given in Eqs. (87a) and (87b) on the contribution to the early-time optical depth, (15,30), contained a numerical error in deriving the 95th percentile from the Monte Carlo samples. The corrected 95% upper bounds are: τ(15,30) < 0:018 (lowE, flat τ(15, 30), FlexKnot), (1) τ(15, 30) < 0:023 (lowE, flat knot, FlexKnot): (2) These bounds are a factor of 3 larger than the originally reported results. Consequently, the new bounds do not significantly improve upon previous results from Planck data presented in Millea & Bouchet (2018) as was stated, but are instead comparable. Equations (1) and (2) give results that are now similar to those of Heinrich & Hu (2021), who used the same Planck 2018 data to derive a 95% upper bound of 0.020 using the principal component analysis (PCA) model and uniform priors on the PCA mode amplitudes.
Published: 2021

3. Planck intermediate results. LVI. Detection of the CMB dipole through modulation of the thermal Sunyaev-Zeldovich effect: Eppur si muove II

Author: Planck Collaboration, 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., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Calabrese, E., Cardoso, J. -F., Casaponsa, B., Chiang, H. C., Combet, C., Contreras, D., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Di Valentino, E., Diego, J. M., Doré, O., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Fernandez-Cobos, R., Finelli, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R. T., Gerbino, M., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Handley, W., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Mennella, A., Migliaccio, M., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Natoli, P., Pagano, L., Paoletti, D., Perrotta, F., Pettorino, V., Piacentini, F., Polenta, G., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Spencer, L. D., Sullivan, R. M., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The largest temperature anisotropy in the cosmic microwave background (CMB) is the dipole, which has been measured with increasing accuracy for more than three decades, particularly with the Planck satellite. The simplest interpretation of the dipole is that it is due to our motion with respect to the rest frame of the CMB. Since current CMB experiments infer temperature anisotropies from angular intensity variations, the dipole modulates the temperature anisotropies with the same frequency dependence as the thermal Sunyaev-Zeldovich (tSZ) effect. We present the first, and significant, detection of this signal in the tSZ maps and find that it is consistent with direct measurements of the CMB dipole, as expected. The signal contributes power in the tSZ maps, which is modulated in a quadrupolar pattern, and we estimate its contribution to the tSZ bispectrum, noting that it contributes negligible noise to the bispectrum at relevant scales., Comment: 15 pages, 8 figures. Added references, small clarifying and language edits. All results remain the same
Published: 2020
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4. Planck 2018 results. V. CMB power spectra and likelihoods

Author: Planck Collaboration, 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., Butler, R. C., Calabrese, E., Cardoso, J. -F., Carron, J., Casaponsa, B., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., 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., Fernandez-Cobos, R., 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., Giraud-Héraud, Y., 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., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-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., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Millea, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Natoli, P., Nørgaard-Nielsen, H. U., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Peiris, H. V., Perrotta, F., Pettorino, V., Piacentini, F., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper describes the 2018 Planck CMB likelihoods, following a hybrid approach similar to the 2015 one, with different approximations at low and high multipoles, and implementing several methodological and analysis refinements. With more realistic simulations, and better correction and modelling of systematics, we can now make full use of the High Frequency Instrument polarization data. The low-multipole 100x143 GHz EE cross-spectrum constrains the reionization optical-depth parameter $\tau$ to better than 15% (in combination with with the other low- and high-$\ell$ likelihoods). We also update the 2015 baseline low-$\ell$ joint TEB likelihood based on the Low Frequency Instrument data, which provides a weaker $\tau$ constraint. At high multipoles, a better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (polarization efficiency or PE) allow us to fully use the polarization spectra, improving the constraints on the $\Lambda$CDM parameters by 20 to 30% compared to TT-only constraints. Tests on the modelling of the polarization demonstrate good consistency, with some residual modelling uncertainties, the accuracy of the PE modelling being the main limitation. Using our various tests, simulations, and comparison between different high-$\ell$ implementations, we estimate the consistency of the results to be better than the 0.5$\sigma$ level. Minor curiosities already present before (differences between $\ell$<800 and $\ell$>800 parameters or the preference for more smoothing of the $C_\ell$ peaks) are shown to be driven by the TT power spectrum and are not significantly modified by the inclusion of polarization. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations. (Abridged), Comment: Revised to match version published in Astronomy & Astrophysics
Published: 2019
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5. Planck 2018 results. VII. Isotropy and Statistics of the CMB

Author: Planck Collaboration, Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., 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., Casaponsa, B., Chiang, H. C., Colombo, L. P. L., Combet, C., Contreras, D., Crill, B. P., 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., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fernandez-Cobos, R., 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., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Hamann, J., Handley, W., Hansen, F. K., 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., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-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., Meinhold, P. R., 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., Perrotta, F., Pettorino, V., Piacentini, F., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Savelainen, M., Scott, D., Shellard, E. P. S., Sirignano, C., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., Zibin, J. P., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Analysis of the Planck 2018 data set indicates that the statistical properties of the cosmic microwave background (CMB) temperature anisotropies are in excellent agreement with previous studies using the 2013 and 2015 data releases. In particular, they are consistent with the Gaussian predictions of the $\Lambda$CDM cosmological model, yet also confirm the presence of several so-called "anomalies" on large angular scales. The novelty of the current study, however, lies in being a first attempt at a comprehensive analysis of the statistics of the polarization signal over all angular scales, using either maps of the Stokes parameters, $Q$ and $U$, or the $E$-mode signal derived from these using a new methodology (which we describe in an appendix). Although remarkable progress has been made in reducing the systematic effects that contaminated the 2015 polarization maps on large angular scales, it is still the case that residual systematics (and our ability to simulate them) can limit some tests of non-Gaussianity and isotropy. However, a detailed set of null tests applied to the maps indicates that these issues do not dominate the analysis on intermediate and large angular scales (i.e., $\ell \lesssim 400$). In this regime, no unambiguous detections of cosmological non-Gaussianity, or of anomalies corresponding to those seen in temperature, are claimed. Notably, the stacking of CMB polarization signals centred on the positions of temperature hot and cold spots exhibits excellent agreement with the $\Lambda$CDM cosmological model, and also gives a clear indication of how Planck provides state-of-the-art measurements of CMB temperature and polarization on degree scales., Comment: Paper VII of the Planck 2018 release, revised to closely match version published in Astronomy and Astrophysics
Published: 2019
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6. Planck 2018 results. IX. Constraints on primordial non-Gaussianity

Author: Planck Collaboration, Akrami, Y., Arroja, F., 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., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Casaponsa, B., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., 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., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Frailis, M., Fraisse, A. A., Franceschi, E., Frolov, A., Galeotta, S., Ganga, K., Génova-Santos, R. T., Gerbino, M., 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., Jung, G., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meerburg, P. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Münchmeyer, M., Natoli, P., Oppizzi, F., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Perrotta, F., Pettorino, V., Piacentini, F., Polenta, G., Puget, J. -L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Savelainen, M., Scott, D., Shellard, E. P. S., Shiraishi, M., Sirignano, C., Sirri, G., Smith, K., Spencer, L. D., Stanco, L., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory
Abstract: We analyse the Planck full-mission cosmic microwave background (CMB) temperature and E-mode polarization maps to obtain constraints on primordial non-Gaussianity (NG). We compare estimates obtained from separable template-fitting, binned, and modal bispectrum estimators, finding consistent values for the local, equilateral, and orthogonal bispectrum amplitudes. Our combined temperature and polarization analysis produces the following results: f_NL^local = -0.9 +\- 5.1; f_NL^equil = -26 +\- 47; and f_NL^ortho = - 38 +\- 24 (68%CL, statistical). These results include the low-multipole (4 <= l < 40) polarization data, not included in our previous analysis, pass an extensive battery of tests, and are stable with respect to our 2015 measurements. Polarization bispectra display a significant improvement in robustness; they can now be used independently to set NG constraints. We consider a large number of additional cases, e.g. scale-dependent feature and resonance bispectra, isocurvature primordial NG, and parity-breaking models, where we also place tight constraints but do not detect any signal. The non-primordial lensing bispectrum is detected with an improved significance compared to 2015, excluding the null hypothesis at 3.5 sigma. We present model-independent reconstructions and analyses of the CMB bispectrum. Our final constraint on the local trispectrum shape is g_NLl^local = (-5.8 +\-6.5) x 10^4 (68%CL, statistical), while constraints for other trispectra are also determined. We constrain the parameter space of different early-Universe scenarios, including general single-field models of inflation, multi-field and axion field parity-breaking models. Our results provide a high-precision test for structure-formation scenarios, in complete agreement with the basic picture of the LambdaCDM cosmology regarding the statistics of the initial conditions (abridged)., Comment: 50 pages, 20 figures
Published: 2019

7. Planck intermediate results

Author: Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Calabrese, E, Cardoso, J-F, Casaponsa, B, Chiang, HC, Combet, C, Contreras, D, Crill, BP, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Dupac, X, Enßlin, TA, Eriksen, HK, Fernandez-Cobos, R, Finelli, F, Frailis, M, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Gerbino, M, González-Nuevo, J, Górski, KM, Gruppuso, A, Gudmundsson, JE, Handley, W, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lamarre, J-M, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Macías-Pérez, JF, Maino, D, Mandolesi, N, Marcos-Caballero, A, Maris, M, Martin, PG, Martínez-González, E, Matarrese, S, Mauri, N, McEwen, JD, Mennella, A, Migliaccio, M, Molinari, D, Moneti, A, Montier, L, Morgante, G, Moss, A, Natoli, P, Pagano, L, Paoletti, D, Perrotta, F, Pettorino, V, Piacentini, F, Polenta, G, Rachen, JP, Reinecke, M, and Remazeilles, M
Subjects: Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, cosmic background radiation, cosmology: observations, relativistic processes, reference systems, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: The largest temperature anisotropy in the cosmic microwave background (CMB) is the dipole, which has been measured with increasing accuracy for more than three decades, particularly with the Planck satellite. The simplest interpretation of the dipole is that it is due to our motion with respect to the rest frame of the CMB. Since current CMB experiments infer temperature anisotropies from angular intensity variations, the dipole modulates the temperature anisotropies with the same frequency dependence as the thermal Sunyaev-Zeldovich (tSZ) effect. We present the first, and significant, detection of this signal in the tSZ maps and find that it is consistent with direct measurements of the CMB dipole, as expected. The signal contributes power in the tSZ maps, which is modulated in a quadrupolar pattern, and we estimate its contribution to the tSZ bispectrum, noting that it contributes negligible noise to the bispectrum at relevant scales.
Published: 2020

8. Planck 2018 results

Author: Akrami, Y, Arroja, F, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Casaponsa, B, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Crill, BP, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Delouis, J-M, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, Fergusson, J, Fernandez-Cobos, R, Finelli, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Gerbino, M, González-Nuevo, J, Górski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Hamann, J, Handley, W, Hansen, FK, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Jung, G, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Ma, Y-Z, Macías-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Marcos-Caballero, A, Maris, M, Martin, PG, Martínez-González, E, and Matarrese, S
Subjects: Particle and High Energy Physics, Physical Sciences, cosmic background radiation, cosmology: observations, cosmology: theory, early Universe, inflation, methods: data analysis, astro-ph.CO, gr-qc, hep-ph, hep-th, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We analyse the Planck full-mission cosmic microwave background (CMB) temperature and E-mode polarization maps to obtain constraints on primordial non-Gaussianity (NG). We compare estimates obtained from separable template-fitting, binned, and optimal modal bispectrum estimators, finding consistent values for the local, equilateral, and orthogonal bispectrum amplitudes. Our combined temperature and polarization analysis produces the following final results: flocalNL= -0.9 ± 5.1; fequilNL= -26 ± 47; and forthoNL= -38 ± 24 (68% CL, statistical). These results include low-multipole (4 ≤ ℓ < 40) polarization data that are not included in our previous analysis. The results also pass an extensive battery of tests (with additional tests regarding foreground residuals compared to 2015), and they are stable with respect to our 2015 measurements (with small fluctuations, at the level of a fraction of a standard deviation, which is consistent with changes in data processing). Polarizationonly bispectra display a significant improvement in robustness; they can now be used independently to set primordial NG constraints with a sensitivity comparable to WMAP temperature-based results and they give excellent agreement. In addition to the analysis of the standard local, equilateral, and orthogonal bispectrum shapes, we consider a large number of additional cases, such as scale-dependent feature and resonance bispectra, isocurvature primordial NG, and parity-breaking models, where we also place tight constraints but do not detect any signal. The nonprimordial lensing bispectrum is, however, detected with an improved significance compared to 2015, excluding the null hypothesis at 3.5σ. Beyond estimates of individual shape amplitudes, we also present model-independent reconstructions and analyses of the Planck CMB bispectrum. Our final constraint on the local primordial trispectrum shape is glocalNL= (-5.8 ± 6.5) × 104(68% CL, statistical), while constraints for other trispectrum shapes are also determined. Exploiting the tight limits on various bispectrum and trispectrum shapes, we constrain the parameter space of different early-Universe scenarios that generate primordial NG, including general single-field models of inflation, multi-field models (e.g. curvaton models), models of inflation with axion fields producing parity-violation bispectra in the tensor sector, and inflationary models involving vector-like fields with directionally-dependent bispectra. Our results provide a high-precision test for structure-formation scenarios, showing complete agreement with the basic picture of the CDM cosmology regarding the statistics of the initial conditions, with cosmic structures arising from adiabatic, passive, Gaussian, and primordial seed perturbations.
Published: 2020

9. Planck 2018 results

Author: Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Carron, J, Casaponsa, B, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Crill, BP, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Delouis, J-M, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, Fernandez-Cobos, R, Finelli, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Gerbino, M, Ghosh, T, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Hamann, J, Handley, W, Hansen, FK, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, PB, Lilley, M, Lindholm, V, López-Caniego, M, Lubin, PM, Ma, Y-Z, Macías-Pérez, JF, and Maggio, G
Subjects: Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, Generic health relevance, cosmic background radiation, cosmology: observations, cosmological parameters, methods: data analysis, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release. The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (ℓ < 30) and high (ℓ ≥ 30) multipoles, implementing several methodological and data-analysis refinements compared to previous releases. With more realistic simulations, and better correction and modelling of systematic effects, we can now make full use of the CMB polarization observed in the High Frequency Instrument (HFI) channels. The low-multipole EE cross-spectra from the 100 GHz and 143 GHz data give a constraint on the λCDM reionization optical-depth parameter τ to better than 15% (in combination with the TT low-ℓ data and the high-ℓ temperature and polarization data), tightening constraints on all parameters with posterior distributions correlated with τ. We also update the weaker constraint on τ from the joint TEB likelihood using the Low Frequency Instrument (LFI) channels, which was used in 2015 as part of our baseline analysis. At higher multipoles, the CMB temperature spectrum and likelihood are very similar to previous releases. A better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (i.e., the polarization efficiencies) allow us to make full use of polarization spectra, improving the λCDM constraints on the parameters θMC, ωc, ωb, and H0 by more than 30%, and ns by more than 20% compared to TT-only constraints. Extensive tests on the robustness of the modelling of the polarization data demonstrate good consistency, with some residual modelling uncertainties. At high multipoles, we are now limited mainly by the accuracy of the polarization efficiency modelling. Using our various tests, simulations, and comparison between different high-multipole likelihood implementations, we estimate the consistency of the results to be better than the 0.5σ level on the λCDM parameters, as well as classical single-parameter extensions for the joint likelihood (to be compared to the 0.3σ levels we achieved in 2015 for the temperature data alone on λCDM only). Minor curiosities already present in the previous releases remain, such as the differences between the best-fit λCDM parameters for the ℓ < 800 and ℓ > 800 ranges of the power spectrum, or the preference for more smoothing of the power-spectrum peaks than predicted in λCDM fits. These are shown to be driven by the temperature power spectrum and are not significantly modified by the inclusion of the polarization data. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations.
Published: 2020

10. Planck 2018 results. IV. Diffuse component separation

Author: Planck Collaboration, Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Calabrese, E., Cardoso, J. -F., Carron, J., Casaponsa, B., Challinor, A., Colombo, L. P. L., Combet, C., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Di Valentino, E., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., 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., Handley, W., Hansen, F. K., Helou, G., Herranz, D., Huang, Z., Jaffe, A. H., Karakci, A., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Natoli, P., Oppizzi, F., Pagano, L., Paoletti, D., Partridge, B., Peel, M., Pettorino, V., Piacentini, F., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Seljebotn, D. S., Sirignano, C., Spencer, L. D., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Thommesen, H., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present full-sky maps of the cosmic microwave background (CMB) and polarized synchrotron and thermal dust emission, derived from the third set of Planck frequency maps. These products have significantly lower contamination from instrumental systematic effects than previous versions. The methodologies used to derive these maps follow those described in earlier papers, adopting four methods (Commander, NILC, SEVEM, and SMICA) to extract the CMB component, as well as three methods (Commander, GNILC, and SMICA) to extract astrophysical components. Our revised CMB temperature maps agree with corresponding products in the Planck 2015 delivery, whereas the polarization maps exhibit significantly lower large-scale power, reflecting the improved data processing described in companion papers; however, the noise properties of the resulting data products are complicated, and the best available end-to-end simulations exhibit relative biases with respect to the data at the few percent level. Using these maps, we are for the first time able to fit the spectral index of thermal dust independently over 3 degree regions. We derive a conservative estimate of the mean spectral index of polarized thermal dust emission of beta_d = 1.55 +/- 0.05, where the uncertainty marginalizes both over all known systematic uncertainties and different estimation techniques. For polarized synchrotron emission, we find a mean spectral index of beta_s = -3.1 +/- 0.1, consistent with previously reported measurements. We note that the current data processing does not allow for construction of unbiased single-bolometer maps, and this limits our ability to extract CO emission and correlated components. The foreground results for intensity derived in this paper therefore do not supersede corresponding Planck 2015 products. For polarization the new results supersede the corresponding 2015 products in all respects., Comment: 74 pages, A&A, 641, A4
Published: 2018
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11. Planck 2018 results. III. High Frequency Instrument data processing and frequency maps

Author: Planck Collaboration, 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., 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., Couchot, F., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Di Valentino, E., 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., 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., González-Nuevo, J., Górski, K. M., Gratton, S., Gruppuso, A., Gudmundsson, J. E., Handley, W., Hansen, F. K., Henrot-Versillé, S., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Karakci, A., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., 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., Mottet, S., Natoli, P., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Perdereau, O., Perrotta, F., Pettorino, V., Piacentini, F., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Roudier, G., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Vansyngel, F., Van Tent, B., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper presents the High Frequency Instrument (HFI) data processing procedures for the Planck 2018 release. Major improvements in mapmaking have been achieved since the previous 2015 release. They enabled the first significant measurement of the reionization optical depth parameter using HFI data. This paper presents an extensive analysis of systematic effects, including the use of simulations to facilitate their removal and characterize the residuals. The polarized data, which presented a number of known problems in the 2015 Planck release, are very significantly improved. Calibration, based on the CMB dipole, is now extremely accurate and in the frequency range 100 to 353 GHz reduces intensity-to-polarization leakage caused by calibration mismatch. The Solar dipole direction has been determined in the three lowest HFI frequency channels to within one arc minute, and its amplitude has an absolute uncertainty smaller than $0.35\mu$K, an accuracy of order $10^{-4}$. This is a major legacy from the HFI for future CMB experiments. The removal of bandpass leakage has been improved by extracting the bandpass-mismatch coefficients for each detector as part of the mapmaking process; these values in turn improve the intensity maps. This is a major change in the philosophy of "frequency maps", which are now computed from single detector data, all adjusted to the same average bandpass response for the main foregrounds. Simulations reproduce very well the relative gain calibration of detectors, as well as drifts within a frequency induced by the residuals of the main systematic effect. Using these simulations, we measure and correct the small frequency calibration bias induced by this systematic effect at the $10^{-4}$ level. There is no detectable sign of a residual calibration bias between the first and second acoustic peaks in the CMB channels, at the $10^{-3}$ level., Comment: Accepted for publication on A&A (AA/2018/32909)
Published: 2018
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12. Planck 2018 results. XII. Galactic astrophysics using polarized dust emission

Author: Planck Collaboration, 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., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-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., Patanchon, G., Perrotta, F., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Vansyngel, F., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present 353 GHz full-sky maps of the polarization fraction $p$, angle $\psi$, and dispersion of angles $S$ of Galactic dust thermal emission produced from the 2018 release of Planck data. We confirm that the mean and maximum of $p$ decrease with increasing $N_H$. The uncertainty on the maximum polarization fraction, $p_\mathrm{max}=22.0$% at 80 arcmin resolution, is dominated by the uncertainty on the zero level in total intensity. The observed inverse behaviour between $p$ and $S$ is interpreted with models of the polarized sky that include effects from only the topology of the turbulent Galactic magnetic field. Thus, the statistical properties of $p$, $\psi$, and $S$ mostly reflect the structure of the magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map $S \times p$, looking for residual trends. While $p$ decreases by a factor of 3--4 between $N_H=10^{20}$ cm$^{-2}$ and $N_H=2\times 10^{22}$ cm$^{-2}$, $S \times p$ decreases by only about 25%, a systematic trend observed in both the diffuse ISM and molecular clouds. Second, we find no systematic trend of $S \times p$ with the dust temperature, even though in the diffuse ISM lines of sight with high $p$ and low $S$ tend to have colder dust. We also compare Planck data with starlight polarization in the visible at high latitudes. The agreement in polarization angles is remarkable. Two polarization emission-to-extinction ratios that characterize dust optical properties depend only weakly on $N_H$ and converge towards the values previously determined for translucent lines of sight. We determine an upper limit for the polarization fraction in extinction of 13%, compatible with the $p_\mathrm{max}$ observed in emission. These results provide strong constraints for models of Galactic dust in diffuse gas., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2018
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13. Planck 2018 results. I. Overview and the cosmological legacy of Planck

Author: Planck Collaboration, Akrami, Y., Arroja, F., 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., Casaponsa, B., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Contreras, D., Crill, B. P., Cuttaia, F., de Bernardis, P., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Di Valentino, E., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fantaye, Y., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Frailis, M., 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., Helou, G., Herranz, D., 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., Langer, M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Leahy, J. 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., Macías-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., Meerburg, P. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Millea, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Mottet, S., Münchmeyer, M., Natoli, P., Nørgaard-Nielsen, H. U., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Pearson, T. J., Peel, M., Peiris, H. V., 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, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Shiraishi, M., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Terenzi, L., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, M., White, S. D. M., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The European Space Agency's Planck satellite, which was dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013, producing deep, high-resolution, all-sky maps in nine frequency bands from 30 to 857GHz. This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard cosmological model and some of the tightest limits available on deviations from that model. The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and low redshift, describing the cosmological information in over a billion map pixels with just six parameters. With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the six parameters to better than 1% (simultaneously), with the best-determined parameter (theta_*) now known to 0.03%. We describe the multi-component sky as seen by Planck, the success of the LCDM model, and the connection to lower-redshift probes of structure formation. We also give a comprehensive summary of the major changes introduced in this 2018 release. The Planck data, alone and in combination with other probes, provide stringent constraints on our models of the early Universe and the large-scale structure within which all astrophysical objects form and evolve. We discuss some lessons learned from the Planck mission, and highlight areas ripe for further experimental advances., Comment: 61 pages, 40 figures, matches version accepted by A&A
Published: 2018
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14. Planck 2018 results. II. Low Frequency Instrument data processing

Author: Planck Collaboration, Akrami, Y., Argüeso, F., 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., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Colombo, L. P. L., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Di Valentino, E., Dickinson, C., Diego, J. M., Donzelli, S., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Finelli, F., Frailis, M., 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., 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., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-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., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Molinari, D., Montier, L., Morgante, G., Moss, A., Natoli, P., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Peel, M., Perrotta, F., Pettorino, V., Piacentini, F., Polenta, G., Puget, J. -L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Roudier, G., Rubiño-Martín, J. A., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Seljebotn, D. S., Sirignano, C., Sirri, G., Spencer, L. D., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Terenzi, L., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Vansyngel, F., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Watson, R., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a final description of the data-processing pipeline for the Planck, Low Frequency Instrument (LFI), implemented for the 2018 data release. Several improvements have been made with respect to the previous release, especially in the calibration process and in the correction of instrumental features such as the effects of nonlinearity in the response of the analogue-to-digital converters. We provide a brief pedagogical introduction to the complete pipeline, as well as a detailed description of the important changes implemented. Self-consistency of the pipeline is demonstrated using dedicated simulations and null tests. We present the final version of the LFI full sky maps at 30, 44, and 70 GHz, both in temperature and polarization, together with a refined estimate of the Solar dipole and a final assessment of the main LFI instrumental parameters.
Published: 2018
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15. Planck 2018 results. VIII. Gravitational lensing

Author: Planck Collaboration, 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., 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., Jeune, M. Le, Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-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, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, M., White, S. D. M., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present measurements of the cosmic microwave background (CMB) lensing potential using the final $\textit{Planck}$ 2018 temperature and polarization data. We increase the significance of the detection of lensing in the polarization maps from $5\,\sigma$ to $9\,\sigma$. Combined with temperature, lensing is detected at $40\,\sigma$. We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles $8 \le L \le 400$. We find good consistency between lensing constraints and the results from the $\textit{Planck}$ CMB power spectra within the $\rm{\Lambda CDM}$ model. Combined with baryon density and other weak priors, the lensing analysis alone constrains $\sigma_8 \Omega_{\rm m}^{0.25}=0.589\pm 0.020$ ($1\,\sigma$ errors). Also combining with baryon acoustic oscillation (BAO) data, we find tight individual parameter constraints, $\sigma_8=0.811\pm0.019$, $H_0=67.9_{-1.3}^{+1.2}\,\text{km}\,\text{s}^{-1}\,\rm{Mpc}^{-1}$, and $\Omega_{\rm m}=0.303^{+0.016}_{-0.018}$. Combining with $\textit{Planck}$ CMB power spectrum data, we measure $\sigma_8$ to better than $1\,\%$ precision, finding $\sigma_8=0.811\pm 0.006$. We find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using $\textit{Planck}$ cosmic infrared background (CIB) maps we make a combined estimate of the lensing potential over $60\,\%$ of the sky with considerably more small-scale signal. We demonstrate delensing of the $\textit{Planck}$ power spectra, detecting a maximum removal of $40\,\%$ of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance (abridged)., Comment: Abstract abridged for arxiv submission. Lensing data products available at https://wiki.cosmos.esa.int/planck-legacy-archive/index.php/Lensing. Matches version accepted by A&A, with minor updates from v1
Published: 2018
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16. Planck 2018 results. X. Constraints on inflation

Author: Planck Collaboration, Akrami, Y., Arroja, F., 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., Butler, R. C., Calabrese, E., Cardoso, J. -F., Carron, J., Challinor, A., Chiang, H. C., 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., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gauthier, C., 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., Hooper, D. C., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Lesgourgues, J., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lindholm, V., Lpez-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-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., Meerburg, P. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Münchmeyer, M., Natoli, P., Nørgaard-Nielsen, H. U., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Peiris, H. V., 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, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Shiraishi, M., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, S. D. M., Zacchei, A., Zibin, J. P., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on the implications for cosmic inflation of the 2018 Release of the Planck CMB anisotropy measurements. The results are fully consistent with the two previous Planck cosmological releases, but have smaller uncertainties thanks to improvements in the characterization of polarization at low and high multipoles. Planck temperature, polarization, and lensing data determine the spectral index of scalar perturbations to be $n_\mathrm{s}=0.9649\pm 0.0042$ at 68% CL and show no evidence for a scale dependence of $n_\mathrm{s}.$ Spatial flatness is confirmed at a precision of 0.4% at 95% CL with the combination with BAO data. The Planck 95% CL upper limit on the tensor-to-scalar ratio, $r_{0.002}<0.10$, is further tightened by combining with the BICEP2/Keck Array BK15 data to obtain $r_{0.002}<0.056$. In the framework of single-field inflationary models with Einstein gravity, these results imply that: (a) slow-roll models with a concave potential, $V" (\phi) < 0,$ are increasingly favoured by the data; and (b) two different methods for reconstructing the inflaton potential find no evidence for dynamics beyond slow roll. Non-parametric reconstructions of the primordial power spectrum consistently confirm a pure power law. A complementary analysis also finds no evidence for theoretically motivated parameterized features in the Planck power spectrum, a result further strengthened for certain oscillatory models by a new combined analysis that includes Planck bispectrum data. The new Planck polarization data provide a stringent test of the adiabaticity of the initial conditions. The polarization data also provide improved constraints on inflationary models that predict a small statistically anisotropic quadrupolar modulation of the primordial fluctuations. However, the polarization data do not confirm physical models for a scale-dependent dipolar modulation., Comment: References added and minor improvements. BICEP2/Keck Array BK15 is used in the place of BICEP2/Keck Array BK14
Published: 2018
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17. Planck 2018 results. VI. Cosmological parameters

Author: Planck Collaboration, 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., Jeune, M. Le, 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., Macías-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., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Millea, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Montier, L., Morgante, G., Moss, A., Natoli, P., Nørgaard-Nielsen, H. U., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Peiris, H. V., 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, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valenziano, L., Valiviita, J., Van Tent, B., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, M., White, S. D. M., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted "base $\Lambda$CDM" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\Omega_c h^2 = 0.120\pm 0.001$, baryon density $\Omega_b h^2 = 0.0224\pm 0.0001$, scalar spectral index $n_s = 0.965\pm 0.004$, and optical depth $\tau = 0.054\pm 0.007$ (in this abstract we quote $68\,\%$ confidence regions on measured parameters and $95\,\%$ on upper limits). The angular acoustic scale is measured to $0.03\,\%$ precision, with $100\theta_*=1.0411\pm 0.0003$. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-$\Lambda$CDM cosmology, the inferred late-Universe parameters are: Hubble constant $H_0 = (67.4\pm 0.5)$km/s/Mpc; matter density parameter $\Omega_m = 0.315\pm 0.007$; and matter fluctuation amplitude $\sigma_8 = 0.811\pm 0.006$. We find no compelling evidence for extensions to the base-$\Lambda$CDM model. Combining with BAO we constrain the effective extra relativistic degrees of freedom to be $N_{\rm eff} = 2.99\pm 0.17$, and the neutrino mass is tightly constrained to $\sum m_\nu< 0.12$eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base -$\Lambda$CDM at over $2\,\sigma$, which pulls some parameters that affect the lensing amplitude away from the base-$\Lambda$CDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. (Abridged), Comment: 73 pages; Updated with published reionization result corrigendum on p59. Parameter tables and chains available at https://wiki.cosmos.esa.int/planck-legacy-archive/index.php/Cosmological_Parameters
Published: 2018
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18. The CMB angular power spectrum via component separation: a study on Planck data

Author: Umiltà, C., Cardoso, J. F., Benabed, K., and Jeune, M. Le
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the extent to which foreground cleaned CMB maps can be used to estimate the cosmological parameters at small scales. We use the SMICA method, a blind separation technique which works directly at the spectral level. In this work we focus on the small scales of the CMB angular power spectrum, which are chiefly affected by noise and extragalactic foregrounds, such as point sources. We adapt SMICA to use only cross-spectra between data maps, thus avoiding the noise bias. In this study, performed both on simulations and on Planck 2015 data, we fit for extragalactic point sources by modeling them as shot noise of two independent populations. In simulations we correctly recover the point source emission law, and obtain a CMB angular power spectrum that has an average foreground residual of one fifth of the CMB power at $\ell \geq$ 2200. On Planck data, the recovered point source emission law corresponds to external estimates, with some offsets at the highest and lowest frequencies, possibly due to frequency decoherence of point sources. The CMB angular power spectrum residuals are consistent with what we find in simulations. The cosmological parameters obtained from the simulations and the data show offsets up to 1$\sigma$ on average from their expected values. Biases on cosmological parameters in simulations represent the expected level of bias in Planck data. The results on cosmological parameters depend on the detail of the foreground residual contamination in the spectrum, and need a tailored modeling of the likelihood foreground model.
Published: 2018
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19. Planck 2018 results. XI. Polarized dust foregrounds

Author: Planck Collaboration, 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., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Bucher, M., Burigana, C., Calabrese, E., Cardoso, J. -F., Carron, J., Chiang, H. C., Combet, C., Crill, B. P., de Bernardis, P., de Zotti, G., Delabrouille, J., Delouis, J. -M., Di Valentino, E., Dickinson, C., Diego, J. M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Falgarone, E., Fantaye, Y., 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., Ghosh, T., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Guillet, V., Handley, W., Hansen, F. K., Herranz, D., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Lasenby, A., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Martin, P. G., Martínez-González, E., Matarrese, S., McEwen, J. D., Meinhold, P. R., Melchiorri, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Natoli, P., Pagano, L., Paoletti, D., Pettorino, V., Piacentini, F., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Soler, J. D., Spencer, L. D., Tauber, J. A., Tavagnacco, D., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Vansyngel, F., Van Tent, F., Vielva, P., Villa, F., Vittorio, N., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The study of polarized dust emission has become entwined with the analysis of the cosmic microwave background (CMB) polarization. We use new Planck maps to characterize Galactic dust emission as a foreground to the CMB polarization. We present Planck EE, BB, and TE power spectra of dust polarization at 353 GHz for six nested sky regions covering from 24 to 71 % of the sky. We present power-law fits to the angular power spectra, yielding evidence for statistically significant variations of the exponents over sky regions and a difference between the values for the EE and BB spectra. The TE correlation and E/B power asymmetry extend to low multipoles that were not included in earlier Planck polarization papers. We also report evidence for a positive TB dust signal. Combining data from Planck and WMAP, we determine the amplitudes and spectral energy distributions (SEDs) of polarized foregrounds, including the correlation between dust and synchrotron polarized emission, for the six sky regions as a function of multipole. This quantifies the challenge of the component separation procedure required for detecting the reionization and recombination peaks of primordial CMB B modes. The SED of polarized dust emission is fit well by a single-temperature modified blackbody emission law from 353 GHz to below 70 GHz. For a dust temperature of 19.6 K, the mean spectral index for dust polarization is $\beta_{\rm d}^{P} = 1.53\pm0.02 $. By fitting multi-frequency cross-spectra, we examine the correlation of the dust polarization maps across frequency. We find no evidence for decorrelation. If the Planck limit for the largest sky region applies to the smaller sky regions observed by sub-orbital experiments, then decorrelation might not be a problem for CMB experiments aiming at a primordial B-mode detection limit on the tensor-to-scalar ratio $r\simeq0.01$ at the recombination peak., Comment: Final version to appear in A&A
Published: 2018
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20. Planck intermediate results. LII. Planet flux densities

Author: Planck Collaboration, 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., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Carron, J., Chiang, H. C., Colombo, L. P. L., Comis, B., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Di Valentino, E., Dickinson, C., Diego, J. M., Doré, O., Ducout, A., Dupac, X., 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., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Helou, G., Henrot-Versillé, S., Herranz, D., Hivon, E., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Lellouch, E., Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., 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., Moreno, R., Morgante, G., Natoli, P., Oxborrow, C. A., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Perdereau, O., Piacentini, F., Plaszczynski, S., Polenta, G., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, E., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirri, G., Spencer, L. D., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Wehus, I. K., and Zacchei, A.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of $\beta _\mathrm{ring} = 2.30\pm0.03$ over the 30-1000 GHz frequency range. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 0.997, 0.997, 1.018, and 1.032 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent-level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2%. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science., Comment: 20 pages, 14 figures, abstract abridged for arXiv submission
Published: 2016
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21. Planck intermediate results. LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters

Author: Planck Collaboration, Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Calabrese, E., Cardoso, J. -F., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Crill, B. P., Curto, A., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Di Valentino, E., Dickinson, C., Diego, J. M., Doré, O., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R. T., Gerbino, M., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., 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., Jeune, M. Le, Levrier, F., Lewis, A., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-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., Meinhold, P. R., Mennella, A., Migliaccio, M., Millea, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Narimani, A., Natoli, P., Oxborrow, C. A., Pagano, L., Paoletti, D., Patanchon, G., Patrizii, L., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Stanco, L., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, M., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The six parameters of the standard $\Lambda$CDM model have best-fit values derived from the Planck temperature power spectrum that are shifted somewhat from the best-fit values derived from WMAP data. These shifts are driven by features in the Planck temperature power spectrum at angular scales that had never before been measured to cosmic-variance level precision. We investigate these shifts to determine whether they are within the range of expectation and to understand their origin in the data. Taking our parameter set to be the optical depth of the reionized intergalactic medium $\tau$, the baryon density $\omega_{\rm b}$, the matter density $\omega_{\rm m}$, the angular size of the sound horizon $\theta_*$, the spectral index of the primordial power spectrum, $n_{\rm s}$, and $A_{\rm s}e^{-2\tau}$ (where $A_{\rm s}$ is the amplitude of the primordial power spectrum), we examine the change in best-fit values between a WMAP-like large angular-scale data set (with multipole moment $\ell<800$ in the Planck temperature power spectrum) and an all angular-scale data set ($\ell<2500$ Planck temperature power spectrum), each with a prior on $\tau$ of $0.07\pm0.02$. We find that the shifts, in units of the 1$\sigma$ expected dispersion for each parameter, are $\{\Delta \tau, \Delta A_{\rm s} e^{-2\tau}, \Delta n_{\rm s}, \Delta \omega_{\rm m}, \Delta \omega_{\rm b}, \Delta \theta_*\} = \{-1.7, -2.2, 1.2, -2.0, 1.1, 0.9\}$, with a $\chi^2$ value of 8.0. We find that this $\chi^2$ value is exceeded in 15% of our simulated data sets, and that a parameter deviates by more than 2.2$\sigma$ in 9% of simulated data sets, meaning that the shifts are not unusually large. Comparing $\ell<800$ instead to $\ell>800$, or splitting at a different multipole, yields similar results. We examine the $\ell<800$ model residuals in the $\ell>800$ power spectrum data and find that the features there... [abridged], Comment: 22 pages, 17 figures, abstract abridged for Arxiv submission
Published: 2016
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22. Planck intermediate results. L. Evidence for spatial variation of the polarized thermal dust spectral energy distribution and implications for CMB $B$-mode analysis

Author: Planck Collaboration, 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., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., López-Caniego, M., Lubin, P. M., Macías-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, A., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Naselsky, P., Nørgaard-Nielsen, H. U., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Patrizii, L., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Plaszczynski, S., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Stanco, L., Suur-Uski, A. -S., Tauber, J. A., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Vansyngel, J., Van Tent, F., Vielva, P., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The characterization of the Galactic foregrounds has been shown to be the main obstacle in the challenging 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, and its potential impact on the determination of the tensor-to-scalar ratio. We use the correlation ratio of the $C_\ell^{BB}$ 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 those data still allow a decorrelation between the dust at 150 and 353GHz of the order of the one we measure. Finally we show that either spatial variation of the dust SED or of the dust polarization angle could produce decorrelations between 217- and 353-GHz data similar to those we observe in the data.
Published: 2016
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23. Planck intermediate results. XLV. Radio spectra of northern extragalactic radio sources

Author: Planck Collaboration, 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., Bendo, G. J., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Catalano, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, H. C., Christensen, P. R., Clements, D. L., 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., 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., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., 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., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Israel, F. P., 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., Lähteenmäki, A., 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., Madden, S., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Pearson, T. J., Peel, M., Perdereau, O., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Sudiwala, R., 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., Watson, R., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Continuum spectra covering centimetre to submillimetre wavelengths are presented for a northern sample of 104 extragalactic radio sources, mainly active galactic nuclei, based on four-epoch Planck data. The nine Planck frequencies, from 30 to 857 GHz, are complemented by a set of simultaneous ground-based radio observations between 1.1 and 37 GHz. The single-survey Planck data confirm that the flattest high-frequency radio spectral indices are close to zero, indicating that the original accelerated electron energy spectrum is much harder than commonly thought, with power-law index around 1.5 instead of the canonical 2.5. The radio spectra peak at high frequencies and exhibit a variety of shapes. For a small set of low-z sources, we find a spectral upturn at high frequencies, indicating the presence of intrinsic cold dust. Variability can generally be approximated by achromatic variations, while sources with clear signatures of evolving shocks appear to be limited to the strongest outbursts., Comment: 39 pages, 113 figures. Accepted by A&A
Published: 2016
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24. Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies

Author: Planck Collaboration, 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., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Calabrese, E., Cardoso, J. -F., Carron, J., Chiang, H. C., Colombo, L. P. L., Comis, B., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., de Bernardis, P., de Zotti, G., Delabrouille, J., Di Valentino, E., Dickinson, C., Diego, J. M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fantaye, Y., 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., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Helou, G., Henrot-Versillé, S., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Langer, M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-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, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Natoli, P., Oxborrow, C. A., Pagano, L., Paoletti, D., Patanchon, G., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Plaszczynski, S., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Soler, J. D., Spencer, L. D., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Using the Planck 2015 data release (PR2) temperature maps, we separate Galactic thermal dust emission from cosmic infrared background (CIB) anisotropies. For this purpose, we implement a specifically tailored component-separation method, the so-called generalized needlet internal linear combination (GNILC) method, which uses spatial information (the angular power spectra) to disentangle the Galactic dust emission and CIB anisotropies. We produce significantly improved all-sky maps of Planck thermal dust emission, with reduced CIB contamination, at 353, 545, and 857 GHz. By reducing the CIB contamination of the thermal dust maps, we provide more accurate estimates of the local dust temperature and dust spectral index over the sky with reduced dispersion, especially at high Galactic latitudes above $b = \pm 20{\deg}$. We find that the dust temperature is $T = (19.4 \pm 1.3)$ K and the dust spectral index is $\beta = 1.6 \pm 0.1$ averaged over the whole sky, while $T = (19.4 \pm 1.5)$ K and $\beta = 1.6 \pm 0.2$ on 21 % of the sky at high latitudes. Moreover, subtracting the new CIB-removed thermal dust maps from the CMB-removed Planck maps gives access to the CIB anisotropies over 60 % of the sky at Galactic latitudes $|b| > 20{\deg}$. Because they are a significant improvement over previous Planck products, the GNILC maps are recommended for thermal dust science. The new CIB maps can be regarded as indirect tracers of the dark matter and they are recommended for exploring cross-correlations with lensing and large-scale structure optical surveys. The reconstructed GNILC thermal dust and CIB maps are delivered as Planck products., Comment: 26 pages, 25 figures (reduced in quality for arXiv), 1 table. Updated to match version accepted by A&A
Published: 2016
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25. Planck intermediate results. XLIX. Parity-violation constraints from polarization data

Author: Planck Collaboration, 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., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Calabrese, E., Cardoso, J. -F., Carron, J., Chiang, H. C., Colombo, L. P. L., Comis, B., Contreras, D., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Désert, F. -X., Di Valentino, E., Dickinson, C., Diego, J. M., Doré, O., Ducout, A., Dupac, X., Dusini, S., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R. T., Gerbino, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Henrot-Versillé, S., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Langer, M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Leahy, J. P., Levrier, F., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Morgante, G., Moss, A., Natoli, P., Pagano, L., Paoletti, D., Patanchon, G., Patrizii, L., Perotto, L., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Spencer, L. D., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Parity violating extensions of the standard electromagnetic theory cause in vacuo rotation of the plane of polarization of propagating photons. This effect, also known as cosmic birefringence, impacts the cosmic microwave background (CMB) anisotropy angular power spectra, producing non-vanishing $T$--$B$ and $E$--$B$ correlations that are otherwise null when parity is a symmetry. Here we present new constraints on an isotropic rotation, parametrized by the angle $\alpha$, derived from Planck 2015 CMB polarization data. To increase the robustness of our analyses, we employ two complementary approaches, in harmonic space and in map space, the latter based on a peak stacking technique. The two approaches provide estimates for $\alpha$ that are in agreement within statistical uncertainties and very stable against several consistency tests. Considering the $T$--$B$ and $E$--$B$ information jointly, we find $\alpha = 0.31^{\circ} \pm 0.05^{\circ} \, ({\rm stat.})\, \pm 0.28^{\circ} \, ({\rm syst.})$ from the harmonic analysis and $\alpha = 0.35^{\circ} \pm 0.05^{\circ} \, ({\rm stat.})\, \pm 0.28^{\circ} \, ({\rm syst.})$ from the stacking approach. These constraints are compatible with no parity violation and are dominated by the systematic uncertainty in the orientation of Planck's polarization-sensitive bolometers., Comment: 15 pages, 8 figures. Accepted for publication in Astronomy and Astrophysics
Published: 2016
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26. Planck intermediate results. XLVII. Planck constraints on reionization history

Author: Planck Collaboration, Adam, R., Aghanim, N., 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., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Calabrese, E., Cardoso, J. -F., Carron, J., Chiang, H. C., Colombo, L. P. L., Combet, C., Comis, B., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Di Valentino, E., Dickinson, C., Diego, J. M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fantaye, Y., 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., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Helou, G., Henrot-Versillé, S., Herranz, D., Hivon, E., Huang, Z., Ili_, S., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Knox, L., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Langer, M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., López-Caniego, M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Naselsky, P., Natoli, P., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Plaszczynski, S., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirri, G., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, M., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate constraints on cosmic reionization extracted from the Planck cosmic microwave background (CMB) data. We combine the Planck CMB anisotropy data in temperature with the low-multipole polarization data to fit LCDM models with various parameterizations of the reionization history. We obtain a Thomson optical depth tau=0.058 +/- 0.012 for the commonly adopted instantaneous reionization model. This confirms, with only data from CMB anisotropies, the low value suggested by combining Planck 2015 results with other data sets and also reduces the uncertainties. We reconstruct the history of the ionization fraction using either a symmetric or an asymmetric model for the transition between the neutral and ionized phases. To determine better constraints on the duration of the reionization process, we also make use of measurements of the amplitude of the kinetic Sunyaev-Zeldovich (kSZ) effect using additional information from the high resolution Atacama Cosmology Telescope and South Pole Telescope experiments. The average redshift at which reionization occurs is found to lie between z=7.8 and 8.8, depending on the model of reionization adopted. Using kSZ constraints and a redshift-symmetric reionization model, we find an upper limit to the width of the reionization period of Dz < 2.8. In all cases, we find that the Universe is ionized at less than the 10% level at redshifts above z~10. This suggests that an early onset of reionization is strongly disfavoured by the Planck data. We show that this result also reduces the tension between CMB-based analyses and constraints from other astrophysical sources., Comment: 19 pages, 18 figures. accepted in A&A
Published: 2016
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27. Planck intermediate results. XLVI. Reduction of large-scale systematic effects in HFI polarization maps and estimation of the reionization optical depth

Author: Planck Collaboration, Aghanim, N., 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., 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., Carron, J., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Comis, B., Coulais, A., 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., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fantaye, Y., 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., Hansen, F. K., Helou, G., Henrot-Versillé, S., Herranz, D., Hivon, E., Huang, Z., Ilic, S., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Knox, L., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Langer, M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Leahy, J. P., Levrier, F., Liguori, M., Lilje, P. B., López-Caniego, M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Mottet, S., Naselsky, P., Natoli, P., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Plaszczynski, S., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirri, G., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Watson, R., Wehus, I. K., White, M., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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 $\tau$ 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 $\tau$ 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 $\tau$ posterior distribution using the maximum likelihood power spectrum estimator from $EE$ data only, giving a value $0.055\pm 0.009$. In a companion paper these results are discussed in the context of the best-fit Planck $\Lambda$CDM cosmological model and recent models of reionization., Comment: 53 pages, corresponding author: J.-L. Puget, submitted to Astronomy and Astrophysics
Published: 2016
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28. Planck intermediate results. XLIV. The structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap

Author: Planck Collaboration, Aghanim, N., Alves, M. I. R., Arzoumanian, D., 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., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Bucher, M., Burigana, C., Calabrese, E., Cardoso, J. -F., Chiang, H. C., Colombo, L. P. L., Combet, C., Comis, B., Couchot, F., Coulais, A., 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., Ferrière, K., 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., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Guillet, V., Hansen, F. K., Helou, G., Henrot-Versillé, S., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Langer, M., Lasenby, A., Lattanzi, M., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., López-Caniego, M., Lubin, P. M., Macías-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, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Naselsky, P., Natoli, P., Neveu, J., Nørgaard-Nielsen, H. U., Oppermann, N., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Plaszczynski, S., Polenta, G., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Ristorcelli, I., Rocha, G., Rossetti, M., Roudier, G., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Soler, J. D., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Vansyngel, F., Van Tent, F., Vielva, P., Villa, F., Wandelt, B. D., Wehus, I. K., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We study the statistical properties of interstellar dust polarization at high Galactic latitude, using the Stokes parameter Planck maps at 353 GHz. Our aim is to advance the understanding of the magnetized interstellar medium (ISM), and to provide a model of the polarized dust foreground for cosmic microwave background component-separation procedures. Focusing on the southern Galactic cap, we examine the statistical distributions of the polarization fraction ($p$) and angle ($\psi$) to characterize the ordered and turbulent components of the Galactic magnetic field (GMF) in the solar neighbourhood. We relate patterns at large angular scales in polarization to the orientation of the mean (ordered) GMF towards Galactic coordinates $(l_0,b_0)=(70^\circ \pm 5^\circ,24^\circ \pm 5^\circ)$. The histogram of $p$ shows a wide dispersion up to 25 %. The histogram of $\psi$ has a standard deviation of $12^\circ$ about the regular pattern expected from the ordered GMF. We use these histograms to build a phenomenological model of the turbulent component of the GMF, assuming a uniform effective polarization fraction ($p_0$) of dust emission. To model the Stokes parameters, we approximate the integration along the line of sight (LOS) as a sum over a set of $N$ independent polarization layers, in each of which the turbulent component of the GMF is obtained from Gaussian realizations of a power-law power spectrum. We are able to reproduce the observed $p$ and $\psi$ distributions using: a $p_0$ value of (26 $\pm$ 3)%; a ratio of 0.9 $\pm$ 0.1 between the strengths of the turbulent and mean components of the GMF; and a small value of $N$. We relate the polarization layers to the density structure and to the correlation length of the GMF along the LOS.
Published: 2016
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29. Planck intermediate results

Author: Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Carron, J, Chiang, HC, Colombo, LPL, Comis, B, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Di Valentino, E, Dickinson, C, Diego, JM, Doré, O, Ducout, A, Dupac, X, Elsner, F, Enßlin, TA, Eriksen, HK, Falgarone, E, Fantaye, Y, Finelli, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Gerbino, M, González-Nuevo, J, Górski, KM, Gruppuso, A, Gudmundsson, JE, Hansen, FK, Helou, G, Henrot-Versillé, S, Herranz, D, Hivon, E, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Lellouch, E, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Ma, Y-Z, Macías-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Maris, M, Martin, PG, Martínez-González, E, Matarrese, S, Mauri, N, McEwen, JD, and Melchiorri, A
Subjects: Space Sciences, Physical Sciences, Astronomical Sciences, cosmic background radiation, cosmology: observations, planets and satellites: general, astro-ph.EP, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of βring = 2.30 ± 0.03 over the 30-1000 GHz frequency range. Estimates of the polarization amplitude of the planets have also been made in the four bands that have polarization-sensitive detectors (100-353 GHz); this analysis provides a 95% confidence level upper limit on Mars's polarization of 1.8, 1.7, 1.2, and 1.7% at 100, 143, 217, and 353 GHz, respectively. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 1.004, 1.002, 1.021, and 1.033 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2%. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.
Published: 2017

30. Planck intermediate results

Author: Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Calabrese, E, Cardoso, J-F, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Crill, BP, Curto, A, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Di Valentino, E, Dickinson, C, Diego, JM, Doré, O, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, Finelli, F, Forastieri, F, Frailis, M, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Gerbino, M, González-Nuevo, J, Górski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Knox, L, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, PB, Lilley, M, Lindholm, V, López-Caniego, M, Lubin, PM, Ma, Y-Z, Macías-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, PG, Martínez-González, E, Matarrese, S, Mauri, N, McEwen, JD, and Meinhold, PR
Subjects: Astronomical Sciences, Physical Sciences, cosmology: observations, cosmic background radiation, cosmological parameters, cosmology: theory, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: The six parameters of the standard ΛCDM model have best-fit values derived from the Planck temperature power spectrum that are shifted somewhat from the best-fit values derived from WMAP data. These shifts are driven by features in the Planck temperature power spectrum at angular scales that had never before been measured to cosmic-variance level precision. We have investigated these shifts to determine whether they are within the range of expectation and to understand their origin in the data. Taking our parameter set to be the optical depth of the reionized intergalactic medium, the baryon density ωb, the matter density ωm, the angular size of the sound horizon the spectral index of the primordial power spectrum, ns, and Ase-2τ (where As is the amplitude of the primordial power spectrum), we have examined the change in best-fit values between a WMAP-like large angular-scale data set (with multipole moment < 800 in the Planck temperature power spectrum) and an all angular-scale data set (< 2500Planck temperature power spectrum), each with a prior on τ of 0.07 ± 0.02. We find that the shifts, in units of the 1σ expected dispersion for each parameter, are {value of 8.0. We find that this χ2 value is exceeded in 15% of our simulated data sets, and that a parameter deviates by more than 2.2σ in 9% of simulated data sets, meaning that the shifts are not unusually large. Comparing < 800 instead to > 800, or splitting at a different multipole, yields similar results. We examined the < 800 model residuals in the > 800 power spectrum data and find that the features there that drive these shifts are a set of oscillations across a broad range of angular scales. Although they partly appear similar to the effects of enhanced gravitational lensing, the shifts in ΛCDM parameters that arise in response to these features correspond to model spectrum changes that are predominantly due to non-lensing effects; the only exception is, which, at fixed Ase-2τ, affects the > 800 temperature power spectrum solely through the associated change in As and the impact of that on the lensing potential power spectrum. We also ask, "what is it about the power spectrum at < 800 that leads to somewhat different best-fit parameters than come from the full range?" We find that if we discard the data at < 30, where there is a roughly 2σ downward fluctuation in power relative to the model that best fits the full range, the < 800 best-fit parameters shift significantly towards the < 2500 best-fit parameters. In contrast, including < 30, this previously noted "low-deficit" drives ns up and impacts parameters correlated with ns, such as ωm and H0. As expected, the < 30 data have a much greater impact on the < 800 best fit than on the < 2500 best fit. So although the shifts are not very significant, we find that they can be understood through the combined effects of an oscillatory-like set of high-residuals and the deficit in low-power, excursions consistent with sample variance that happen to map onto changes in cosmological parameters. Finally, we examine agreement between PlanckTT data and two other CMB data sets, namely the Planck lensing reconstruction and the TT power spectrum measured by the South Pole Telescope, again finding a lack of convincing evidence of any significant deviations in parameters, suggesting that current CMB data sets give an internally consistent picture of the ΛCDM model.
Published: 2017

31. Planck intermediate results. XLIII. The spectral energy distribution of dust in clusters of galaxies

Author: Planck Collaboration, Adam, R., Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoit-Lévy, 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., Désert, F. -X., Diego, J. M., Dole, H., Doré, 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., Génova-Santos, R. T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Harrison, D. L., Hernández-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., Keihänen, E., Keskitalo, R., Khamitov, I., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., 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., Macías-Pérez, J. F., Maffei, B., Maggio, G., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard-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., Rubiño-Martín, 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., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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 below 353 GHz. By excluding dominant spurious signals or systematic effects, averaged detections are reported at frequencies between 353 and 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 beam 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, as well as its temperature. We additionally explore the evolution of the IR emission as a function of cluster mass and redshift., Comment: 14 pages and 7 figures. Submitted to A&A
Published: 2016
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32. Planck intermediate results. XLII. Large-scale Galactic magnetic fields

Author: Planck Collaboration, 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-Lévy, 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., Doré, O., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Harrison, D. L., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hobson, M., Hornstrup, A., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, 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-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard-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., Rubiño-Martín, 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., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: 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., Comment: 31 pages, 16 figures, updated to match accepted A&A version
Published: 2016
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33. Planck intermediate results. XLI. A map of lensing-induced B-modes

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Battaner, E., Benabed, K., Benoit-Lévy, 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., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Catalano, A., Chiang, H. C., Christensen, P. R., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davis, R. J., de Bernardis, P., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Doré, O., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Harrison, D. L., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hornstrup, A., Hovest, W., Hurier, G., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Leonardi, R., Levrier, F., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, 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., Nørgaard-Nielsen, H. U., Novikov, D., Novikov, I., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pointecouteau, E., Polenta, G., Pratt, G. W., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, 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., 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., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The secondary cosmic microwave background (CMB) $B$-modes stem from the post-decoupling distortion of the polarization $E$-modes due to the gravitational lensing effect of large-scale structures. These lensing-induced $B$-modes constitute both a valuable probe of the dark matter distribution and an important contaminant for the extraction of the primary CMB $B$-modes from inflation. Planck provides accurate nearly all-sky measurements of both the polarization $E$-modes and the integrated mass distribution via the reconstruction of the CMB lensing potential. By combining these two data products, we have produced an all-sky template map of the lensing-induced $B$-modes using a real-space algorithm that minimizes the impact of sky masks. The cross-correlation of this template with an observed (primordial and secondary) $B$-mode map can be used to measure the lensing $B$-mode power spectrum at multipoles up to $2000$. In particular, when cross-correlating with the $B$-mode contribution directly derived from the Planck polarization maps, we obtain lensing-induced $B$-mode power spectrum measurement at a significance level of $12\,\sigma$, which agrees with the theoretical expectation derived from the Planck best-fit $\Lambda$CDM model. This unique nearly all-sky secondary $B$-mode template, which includes the lensing-induced information from intermediate to small ($10\lesssim \ell\lesssim 1000$) angular scales, is delivered as part of the Planck 2015 public data release. It will be particularly useful for experiments searching for primordial $B$-modes, such as BICEP2/Keck Array or LiteBIRD, since it will enable an estimate to be made of the lensing-induced contribution to the measured total CMB $B$-modes., Comment: 20 pages, 12 figures; Accepted for publication in A&A; The B-mode map is part of the PR2-2015 Cosmology Products; available as Lensing Products in the Planck Legacy Archive http://pla.esac.esa.int/pla/#cosmology; and described in the 'Explanatory Supplement' https://wiki.cosmos.esa.int/planckpla2015/index.php/Specially_processed_maps#2015_Lensing-induced_B-mode_map
Published: 2015
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34. Planck intermediate results. XL. The Sunyaev-Zeldovich signal from the Virgo cluster

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., 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., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Churazov, E., Clements, D. L., Colombo, L. P. L., Combet, C., Comis, B., 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., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-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., Jones, W. C., 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., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pearson, T. J., Perdereau, O., 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., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Schaefer, B. M., Scott, D., Soler, J. 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., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Weller, J., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Virgo cluster is the largest Sunyaev-Zeldovich (SZ) source in the sky, both in terms of angular size and total integrated flux. Planck's wide angular scale and frequency coverage, together with its high sensitivity, allow a detailed study of this large object through the SZ effect. Virgo is well resolved by Planck, showing an elongated structure, which correlates well with the morphology observed from X-rays, but extends beyond the observed X-ray signal. We find a good agreement between the SZ signal (or Compton paranmeter, y_c) observed by Planck and the expected signal inferred from X-ray observations and simple analytical models. Due to its proximity to us, the gas beyond the virial radius can be studied with unprecedented sensitivity by integrating the SZ signal over tens of square degrees. We study the signal in the outskirts of Virgo and compare it with analytical models and a constrained simulation of the environment of Virgo. Planck data suggest that significant amounts of low-density plasma surround Virgo out to twice the virial radius. We find the SZ signal in the outskirts of Virgo to be consistent with a simple model that extrapolates the inferred pressure at lower radii while assuming that the temperature stays in the keV range beyond the virial radius. The observed signal is also consistent with simulations and points to a shallow pressure profile in the outskirts of the cluster. This reservoir of gas at large radii can be linked with the hottest phase of the elusive warm/hot intergalactic medium. Taking the lack of symmetry of Virgo into account, we find that a prolate model is favoured by the combination of SZ and X-ray data, in agreement with predictions., Comment: 21 pages and 20 figures. Submitted to A&A
Published: 2015
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35. Planck 2015 results. XII. Full Focal Plane simulations

Author: Planck Collaboration, 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., Benabed, K., Benoît, A., Benoit-Lévy, 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., Castex, G., Catalano, A., Challinor, A., Chamballu, A., Chiang, H. C., Christensen, P. R., 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., Delouis, J. -M., Désert, F. -X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, 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., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., 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., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Karakci, A., Keihänen, E., Keskitalo, R., Kiiveri, K., 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., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-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., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Roman, M., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, 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., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Welikala, N., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the 8th Full Focal Plane simulation set (FFP8), deployed in support of the Planck 2015 results. FFP8 consists of 10 fiducial mission realizations reduced to 18144 maps, together with the most massive suite of Monte Carlo realizations of instrument noise and CMB ever generated, comprising $10^4$ mission realizations reduced to about $10^6$ maps. The resulting maps incorporate the dominant instrumental, scanning, and data analysis effects; remaining subdominant effects will be included in future updates. Generated at a cost of some 25 million CPU-hours spread across multiple high-performance-computing (HPC) platforms, FFP8 is used for the validation and verification of analysis algorithms, as well as their implementations, and for removing biases from and quantifying uncertainties in the results of analyses of the real data.
Published: 2015
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36. Planck 2013 results. XXXI. Consistency of the Planck data

Author: Planck Collaboration, Ade, P. A. R., Arnaud, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Levy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Cardoso, J. -F., Catalano, A., Challinor, A., Chamballu, A., Chiang, H. C., Christensen, R., Clements, D. L., Colombi, S., 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., Desert, F. -X., 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., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Gonzalez-Nuevo, J., Gorski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Hanson, D., Harrison, D. L., Henrot-Versille, S., Herranz, C. 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., Keihanen, E., Keskitalo, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leonardi, R., Leon-Tavares, J., Lesgourgues, J., Liguori, M., Lilje, P. B., Lilley, M., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P. M., Macias-Perez, J. F., Maino, D., Mandolesi, N., Maris, M., Martin, P. G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., 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., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, D., Pearson, T. J., Perdereau, O., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Ristorcelli, I., Rocha, G., Roudier, G., Rubino-Martin, J. A., Rusholme, B., Sandri, M., Scott, D., Stolyarov, V., Sudiwala, 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, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., White, S. D. M., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Planck design and scanning strategy provide many levels of redundancy that can be exploited to provide tests of internal consistency. One of the most important is the comparison of the 70GHz and 100GHz channels. Based on different instrument technologies, with feeds located differently in the focal plane, analysed independently by different teams using different software, and near the minimum of diffuse foreground emission, these channels are in effect two different experiments. The 143GHz channel has the lowest noise level on Planck, and is near the minimum of unresolved foreground emission. In this paper, we analyse the level of consistency achieved in the 2013 Planck data. We concentrate on comparisons between the 70/100/143GHz channel maps and power spectra, particularly over the angular scales of the first and second acoustic peaks, on maps masked for diffuse Galactic emission and for strong unresolved sources. Difference maps covering angular scales from 8deg-15arcmin are consistent with noise, and show no evidence of cosmic microwave background structure. Including small but important corrections for unresolved-source residuals, we demonstrate agreement between 70 and 100GHz power spectra averaged over 70
Published: 2015
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37. Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters

Author: Planck Collaboration, Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, 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., Chiang, H. C., Christensen, P. R., Clements, D. L., 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., Désert, F. -X., Di Valentino, E., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dunkley, J., 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., Gauthier, C., Gerbino, M., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hamann, J., Hansen, F. K., Harrison, D. L., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Leonardi, R., Lesgourgues, J., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lilley, M., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Macías-Pérez, J. F., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Meinhold, P. R., Melchiorri, A., Migliaccio, M., Millea, M., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Mottet, S., Munshi, D., Murphy, J. A., Narimani, A., Naselsky, P., Nati, F., Natoli, P., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., 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., d'Orfeuil, B. Rouillé, Rubiño-Martín, J. A., Rusholme, B., Salvati, L., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Serra, P., Spencer, L. D., Spinelli, M., Stolyarov, V., Stompor, 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., Umana, G., Valenziano, L., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlations of CMB data, using the hybrid approach employed previously: pixel-based at $\ell<30$ and a Gaussian approximation to the distribution of spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models, allowing further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction. Improvements in processing and instrumental models further reduce uncertainties. For temperature, we perform an analysis of end-to-end instrumental simulations fed into the data processing pipeline; this does not reveal biases from residual instrumental systematics. The $\Lambda$CDM cosmological model continues to offer a very good fit to Planck data. The slope of primordial scalar fluctuations, $n_s$, is confirmed smaller than unity at more than 5{\sigma} from Planck alone. We further validate robustness against specific extensions to the baseline cosmology. E.g., the effective number of neutrino species remains compatible with the canonical value of 3.046. This first detailed analysis of Planck polarization concentrates on E modes. At low $\ell$ we use temperature at all frequencies and a subset of polarization. The frequency range improves CMB-foreground separation. Within the baseline model this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically O($\mu$K$^2$); we recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization allows a separate determination of $\Lambda$CDM parameters consistent with those from temperature alone., Comment: This paper is associated with the 2015 Planck release (see http://www.cosmos.esa.int/web/planck/publications). Likelihood code & data available at http://www.cosmos.esa.int/web/planck/pla. Version accepted by A&A. Substancially extended (104 pages) with analysis of end-to-simulations of systematics further confirming the results. Abstract abridged
Published: 2015
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38. Planck 2015 results. XXVI. The Second Planck Catalogue of Compact Sources

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Argüeso, F., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Beichman, C., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Böhringer, 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., Désert, F. -X., 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., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., 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., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., León-Tavares, J., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, 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., Nørgaard-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., Prézeau, 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., Rubiño-Martín, 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., Türler, 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., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Second Planck Catalogue of Compact Sources is a catalogue of sources detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions of the Planck compact source catalogues. 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 sub-catalogues, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these catalogues 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 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 ERCSC catalogues., Comment: 39 pages and 33 figures. This paper is one of a set associated with the 2015 data release from Planck. Version accepted by Astronomy and Astrophysics
Published: 2015
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39. Planck 2015 results. XVI. Isotropy and statistics of the CMB

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Akrami, Y., Aluri, P. K., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, 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., Casaponsa, B., 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., Contreras, D., Couchot, F., Coulais, A., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Désert, F. -X., 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., Fantaye, Y., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gauthier, C., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., 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., Hornstrup, A., Hovest, W., Huang, Z., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kim, J., Kisner, T. S., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., Liu, H., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marinucci, D., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mikkelsen, K., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Pant, N., 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., Prézeau, G., 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., Rotti, A., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Souradeep, T., 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., Trombetti, T., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., Zibin, J. P., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We test the statistical isotropy and Gaussianity of the cosmic microwave background (CMB) anisotropies using observations made by the Planck satellite. Our results are based mainly on the full Planck mission for temperature, but also include some polarization measurements. In particular, we consider the CMB anisotropy maps derived from the multi-frequency Planck data by several component-separation methods. For the temperature anisotropies, we find excellent agreement between results based on these sky maps over both a very large fraction of the sky and a broad range of angular scales, establishing that potential foreground residuals do not affect our studies. Tests of skewness, kurtosis, multi-normality, N-point functions, and Minkowski functionals indicate consistency with Gaussianity, while a power deficit at large angular scales is manifested in several ways, for example low map variance. The results of a peak statistics analysis are consistent with the expectations of a Gaussian random field. The "Cold Spot" is detected with several methods, including map kurtosis, peak statistics, and mean temperature profile. We thoroughly probe the large-scale dipolar power asymmetry, detecting it with several independent tests, and address the subject of a posteriori correction. Tests of directionality suggest the presence of angular clustering from large to small scales, but at a significance that is dependent on the details of the approach. We perform the first examination of polarization data, finding the morphology of stacked peaks to be consistent with the expectations of statistically isotropic simulations. Where they overlap, these results are consistent with the Planck 2013 analysis based on the nominal mission data and provide our most thorough view of the statistics of the CMB fluctuations to date., Comment: Paper XVI of the Planck 2015 release. This is the version accepted by A&A. An additional section discussing the sensitivity of various anomalies to sky coverage has been included
Published: 2015
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40. Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Alves, M. I. R., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., 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., Christensen, P. R., 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., Delouis, J. -M., 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., Ghosh, T., 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., 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., Netterfield, C. B., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Orlando, E., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Peel, M., 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., Rubino-Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Stompor, R., Strong, A. W., 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., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vidal, M., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: (abridged) We discuss the Galactic foreground emission between 20 and 100GHz based on observations by Planck/WMAP. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with RRL templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude Halpha emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (~30%) of Halpha having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak ranging from below 20GHz to more than 50GHz. There is a strong tendency for the spinning dust component near many prominent HII regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photodissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the commander solution finds more anomalous microwave emission than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys (5-20GHz), will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck/WMAP data to make the highest S/N ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure..., Comment: Planck collaboration paper XXV from 2015 results. Accepted for publication in A&A. Corresponding authors: Clive Dickinson and Paddy Leahy. 46 pages, 33 figures
Published: 2015
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41. Planck 2015 results. V. LFI calibration

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaglia, P., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, 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., Chamballu, A., Christensen, P. R., Colombi, S., Colombo, L. P. L., 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., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D. L., Henrot-Versillé, S., 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., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Novikov, D., Novikov, I., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, E., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a description of the pipeline used to calibrate the Planck Low Frequency Instrument (LFI) timelines into thermodynamic temperatures for the Planck 2015 data release, covering four years of uninterrupted operations. As in the 2013 data release, our calibrator is provided by the spin-synchronous modulation of the cosmic microwave background dipole, but we now use the orbital component, rather than adopting the Wilkinson Microwave Anisotropy Probe (WMAP) solar dipole. This allows our 2015 LFI analysis to provide an independent Solar dipole estimate, which is in excellent agreement with that of HFI and within $1\sigma$ (0.3% in amplitude) of the WMAP value. This 0.3% shift in the peak-to-peak dipole temperature from WMAP and a global overhaul of the iterative calibration code increases the overall level of the LFI maps by 0.45% (30 GHz), 0.64% (44 GHz), and 0.82% (70 GHz) in temperature with respect to the 2013 Planck data release, thus reducing the discrepancy with the power spectrum measured by WMAP. We estimate that the LFI calibration uncertainty is now at the level of 0.20% for the 70 GHz map, 0.26% for the 44 GHz map, and 0.35% for the 30 GHz map. We provide a detailed description of the impact of all the changes implemented in the calibration since the previous data release., Comment: 25 pages, 19 figures, part of the Planck 2015 release. Submitted to A&A
Published: 2015
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42. Planck intermediate results. XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., 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., Calabrese, E., Cardoso, J. -F., Catalano, A., Chamballu, A., Chary, R. -R., Chiang, H. C., Christensen, P. R., Colombo, L. P. L., Combet, C., 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., Delouis, J. -M., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., 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., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hornstrup, A., Hovest, W., Huang, Z., Huffenberger, K. M., Hurier, G., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leonardi, R., León-Tavares, J., 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., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, 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., Oppermann, N., 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., Ponthieu, N., Pratt, G. W., 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., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Serra, P., Soler, J. D., Stolyarov, V., Sudiwala, R., Sunyaev, R., 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., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The quest for a B-mode imprint from primordial gravity waves on the polarization of the cosmic microwave background (CMB) requires the characterization of foreground polarization from Galactic dust. We present a statistical study of the filamentary structure of the 353 GHz Planck Stokes maps at high Galactic latitude, relevant to the study of dust emission as a polarized foreground to the CMB. We filter the intensity and polarization maps to isolate filaments in the range of angular scales where the power asymmetry between E-modes and B-modes is observed. Using the Smoothed Hessian Major Axis Filament Finder, we identify 259 filaments at high Galactic latitude, with lengths larger or equal to 2\deg\ (corresponding to 3.5 pc in length for a typical distance of 100 pc). These filaments show a preferred orientation parallel to the magnetic field projected onto the plane of the sky, derived from their polarization angles. We present mean maps of the filaments in Stokes I, Q, U, E, and B, computed by stacking individual images rotated to align the orientations of the filaments. Combining the stacked images and the histogram of relative orientations, we estimate the mean polarization fraction of the filaments to be 11 %. Furthermore, we show that the correlation between the filaments and the magnetic field orientations may account for the E and B asymmetry and the $C_{\ell}^{TE}/C_{\ell}^{EE}$ ratio, reported in the power spectra analysis of the Planck 353 GHz polarization maps. Future models of the dust foreground for CMB polarization studies will need to take into account the observed correlation between the dust polarization and the structure of interstellar matter., Comment: 18 pages, 15 figures. A&A accepted. Corresponding author: T. Ghosh
Published: 2015
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43. Planck Intermediate Results. XXXVI. Optical identification and redshifts of Planck SZ sources with telescopes in the Canary Islands Observatories

Author: Planck Collaboration, 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-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bikmaev, I., Böhringer, 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., Doré, 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., Génova-Santos, R. T., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gruppuso, A., Hansen, F. K., Harrison, D. L., Hempel, A., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, T. R., Keihänen, E., Keskitalo, R., Khamitov, I., Kisner, T. S., Knoche, J., Kunz, M., Kurki-Suonio, H., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leonardi, R., León-Tavares, J., Levrier, F., Lietzen, H., 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., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, 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., Rubiño-Martín, 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., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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)., Comment: 15 pages, 14 figures, accepted for publication in A&A
Published: 2015
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44. Planck intermediate results. XXXVII. Evidence of unbound gas from the kinetic Sunyaev-Zeldovich effect

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aubourg, E., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoit-Lévy, A., Bersanelli, M., Bielewicz, P., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Calabrese, E., Cardoso, J. -F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Clements, D. L., Colombo, L. P. L., Combet, C., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R. T., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D. L., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Hornstrup, A., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kitaura, F., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leonardi, R., León-Tavares, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-Pérez, J. F., Maffei, B., Maino, D., Mak, D. S. Y., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., McGehee, P., Melchiorri, A., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., 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., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pointecouteau, E., Polenta, G., Ponthieu, N., Pratt, G. W., Puget, J. -L., Puisieux, S., Rachen, J. P., Racine, B., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., 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., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wang, W., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: By looking at the kinetic Sunyaev-Zeldovich effect (kSZ) in Planck nominal mission data, we present a significant detection of baryons participating in large-scale bulk flows around central galaxies (CGs) at redshift $z\approx 0.1$. We estimate the pairwise momentum of the kSZ temperature fluctuations at the positions of the CGC (Central Galaxy Catalogue) samples extracted from Sloan Digital Sky Survey (DR7) data. For the foreground-cleaned maps, we find $1.8$-$2.5\sigma$ detections of the kSZ signal, which are consistent with the kSZ evidence found in individual Planck raw frequency maps, although lower than found in the WMAP-9yr W band ($3.3\sigma$). We further reconstruct the peculiar velocity field from the CG density field, and compute for the first time the cross-correlation function between kSZ temperature fluctuations and estimates of CG radial peculiar velocities. This correlation function yields a $3.0$-$3.7$$\sigma$ detection of the peculiar motion of extended gas on Mpc scales, in flows correlated up to distances of 80-100 $h^{-1}$ Mpc. Both the pairwise momentum estimates and kSZ temperature-velocity field correlation find evidence for kSZ signatures out to apertures of 8 arcmin and beyond, corresponding to a physical radius of $> 1$ Mpc, more than twice the mean virial radius of halos. This is consistent with the predictions from hydro simulations that most of the baryons are outside the virialized halos. We fit a simple model, in which the temperature-velocity cross-correlation is proportional to the signal seen in a semi-analytic model built upon N-body simulations, and interpret the proportionality constant as an "effective" optical depth to Thomson scattering. We find $\tau_T=(1.4\pm0.5)\times 10^{-4}$; the simplest interpretation of this measurement is that much of the gas is in a diffuse phase, which contributes little signal to X-ray or thermal SZ observations., Comment: Current version matches accepted version in A&A
Published: 2015
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45. Planck intermediate results. XXVII. High-redshift infrared galaxy overdensity candidates and lensed sources discovered by Planck and confirmed by Herschel-SPIRE

Author: Planck Collaboration, Aghanim, N., Altieri, B., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Beelen, A., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bethermin, M., Bielewicz, P., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Calabrese, E., Canameras, R., Cardoso, J. -F., Catalano, A., Chamballu, A., Chary, R. -R., Chiang, H. C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Crill, B. P., Curto, A., Danese, L., Dassas, K., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Falgarone, E., Flores-Cacho, I., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Frye, B., Galeotta, S., Galli, S., Ganga, K., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guéry, D., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., 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., Floc'h, E. Le, Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacKenzie, T., Maffei, B., Mandolesi, N., Maris, M., Martin, P. G., Martinache, C., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mennella, A., Migliaccio, M., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Natoli, P., Negrello, M., Nesvadba, N. P. H., Novikov, D., Novikov, I., Omont, A., Pagano, L., Pajot, F., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ristorcelli, I., Rocha, G., Roudier, G., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Sunyaev, R., Sutton, D., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Valtchanov, I., Van Tent, B., Vieira, J. D., Vielva, P., Wade, L. A., Wandelt, B. D., Wehus, I. K., Welikala, N., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [Abridged] We use the Planck all-sky submm and mm maps to search for rare sources distinguished by extreme brightness, a few hundreds of mJy, and their potential for being situated at high redshift. These "cold" Planck sources, selected using the High Frequency Instrument (HFI) directly from the maps and from the Planck Catalogue of Compact Sources (PCCS), all satisfy the criterion of having their rest-frame far-infrared peak redshifted to the frequency range 353 and 857 GHz. This colour-selection favours galaxies in the redshift range z=2-4, which we consider as cold peaks in the cosmic infrared background (CIB). We perform a dedicated Herschel-SPIRE follow-up of 234 such Planck targets, finding a significant excess of red 350 and 500um sources, in comparison to reference SPIRE fields. About 94% of the SPIRE sources in the Planck fields are consistent with being overdensities of galaxies peaking at 350um. About 3% are candidate lensed systems, all 12 of which have secure spectroscopic confirmations, placing them at redshifts z>2.2. The galaxy overdensities are detected with high significance, half of the sample showing statistical significance above 10sigma. The SPIRE photometric redshifts of galaxies in overdensities suggest a peak at z~2. Under the Td=35K assumption, we derive an infrared (IR) luminosity for each SPIRE source of about 4x10^12 Lsun, yielding star formation rates of typically 700 Msun.yr^-1. If the observed overdensities are actual gravitationally-bound structures, the total total star formation rates reaches 7x10^3 Msun.yr^-1. Taken together, these sources show the signatures of high-z (z>$) protoclusters of intensively star-forming galaxies. All these observations confirm the uniqueness of our sample and demonstrate the ability of the all-sky Planck-HFI cold sources to select populations of cosmological and astrophysical interest for structure formation studies., Comment: Updated author list, in press and available at A&A http://dx.doi.org/10.1051/0004-6361/201424790 ; Full-res paper (3.6Mb) at A&A http://www.aanda.org/2015-press-releases/1095 ; Check also web story at ESA http://www.esa.int/Our_Activities/Space_Science/Herschel_and_Planck_find_missing_clue_to_galaxy_cluster_formation and NASA http://www.nasa.gov/jpl/herschel/planck/a-gold-mine-of-galaxy-nuggets/
Published: 2015
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46. Planck 2015 results. IX. Diffuse component separation: CMB maps

Author: Planck Collaboration, Adam, R., 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., Basak, S., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., 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., Casaponsa, B., Castex, G., Catalano, A., Challinor, A., Chamballu, A., Chary, R. -R., Chiang, H. C., Christensen, P. R., 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., Désert, F. -X., 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., Fantaye, Y., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., 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., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., 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., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Racine, B., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., 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., Trombetti, T., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present foreground-reduced CMB maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales $\ell\gtrsim40$. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with $\ell < 20$ are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27$\,\mu\textrm{K}$ averaged over 55 arcmin pixels, and between 4.5 and 6.1$\,\mu\textrm{K}$ averaged over 3.4 arcmin pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the $1\sigma$ level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses., Comment: 42 pages, 36 figures. Submitted to A&A
Published: 2015
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47. Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds

Author: Planck Collaboration, 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., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, 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., 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., Falceta-Gonçalves, D., 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., Gudmundsson, J. E., Guillet, V., Harrison, D. L., Helou, G., Hennebelle, P., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., 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., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., 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., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Soler, J. D., Stolyarov, V., Sudiwala, R., 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., Wehus, I. K., Ysard, N., Yvon, D., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: 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, $N_H$. The selected regions, covering several degrees in size, are analyzed 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 $N_H \approx 10^{21}$ to $10^{23}$ cm$^{-2}$, and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analyzed 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 $N_H$, from preferentially parallel or having no preferred orientation to preferentially perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfv\'enic or sub-Alfv\'enic 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., Comment: 28 pages, 20 figures. A&A accepted. Corresponding author: J.D. Soler
Published: 2015
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48. Planck 2015 results. XX. Constraints on inflation

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Arroja, F., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., 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., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Contreras, D., 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., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gauthier, C., Giard, M., Giraud-Heraud, Y., Gjerlow, E., Gonzalez-Nuevo, J., Gorski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hamann, J., Handley, W., Hansen, F. K., Hanson, D., 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., Huang, Z., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihanen, E., Keskitalo, R., Kim, J., 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., 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., Maris, M., 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., Molinari, D., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munchmeyer, M., 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., Pandolfi, S., Paoletti, D., Pasian, F., Patanchon, G., Pearson, T. J., Peiris, H. V., 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., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Shiraishi, M., 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., Trombetti, T., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., White, M., Yvon, D., Zacchei, A., Zibin, J. P., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the implications for cosmic inflation of the Planck measurements of the cosmic microwave background (CMB) anisotropies in both temperature and polarization based on the full Planck survey. The Planck full mission temperature data and a first release of polarization data on large angular scales measure the spectral index of curvature perturbations to be $n_\mathrm{s} = 0.968 \pm 0.006$ and tightly constrain its scale dependence to $d n_s/d \ln k =-0.003 \pm 0.007$ when combined with the Planck lensing likelihood. When the high-$\ell$ polarization data is included, the results are consistent and uncertainties are reduced. The upper bound on the tensor-to-scalar ratio is $r_{0.002} < 0.11$ (95% CL), consistent with the B-mode polarization constraint $r< 0.12$ (95% CL) obtained from a joint BICEP2/Keck Array and Planck analysis. These results imply that $V(\phi) \propto \phi^2$ and natural inflation are now disfavoured compared to models predicting a smaller tensor-to-scalar ratio, such as $R^2$ inflation. Three independent methods reconstructing the primordial power spectrum are investigated. The Planck data are consistent with adiabatic primordial perturbations. We investigate inflationary models producing an anisotropic modulation of the primordial curvature power spectrum as well as generalized models of inflation not governed by a scalar field with a canonical kinetic term. The 2015 results are consistent with the 2013 analysis based on the nominal mission data., Comment: 68 pages, 59 figures, 18 tables; updates to match the published version
Published: 2015
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49. Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect

Author: Planck Collaboration, 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., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Catalano, A., Challinor, A., Chiang, H. C., Christensen, P. R., Churazov, E., Clements, D. L., Colombo, L. P. L., Combet, C., Comis, B., 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., Désert, F. -X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, 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., Génova-Santos, R. T., Giard, M., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Harrison, D. L., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lacasa, F., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Macías-Pérez, J. F., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Melchiorri, A., Melin, J. -B., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Noviello, F., Novikov, D., Novikov, I., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., 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., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Sauvé, A., Savelainen, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Sunyaev, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tramonte, D., Tristram, M., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have constructed all-sky 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 survey. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterised in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales and CIB 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, 20-600. 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., Comment: 25 pages, 19 figures, submitted to A&A
Published: 2015
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50. Planck 2015 results. XIII. Cosmological parameters

Author: Planck Collaboration, 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., Martin, P. G., Martinelli, M., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Mazzotta, P., 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'Orfeuil, 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, B., 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., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results based on full-mission Planck observations of temperature and polarization anisotropies of the CMB. These data are consistent with the six-parameter inflationary LCDM cosmology. From the Planck temperature and lensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9) km/s/Mpc, a matter density parameter Omega_m = 0.308 +/- 0.012 and a scalar spectral index with n_s = 0.968 +/- 0.006. (We quote 68% errors on measured parameters and 95% limits on other parameters.) Combined with Planck temperature and lensing data, Planck LFI polarization measurements lead to a reionization optical depth of tau = 0.066 +/- 0.016. Combining Planck with other astrophysical data we find N_ eff = 3.15 +/- 0.23 for the effective number of relativistic degrees of freedom and the sum of neutrino masses is constrained to < 0.23 eV. Spatial curvature is found to be |Omega_K| < 0.005. For LCDM we find a limit on the tensor-to-scalar ratio of r <0.11 consistent with the B-mode constraints from an analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP data leads to a tighter constraint of r < 0.09. We find no evidence for isocurvature perturbations or cosmic defects. The equation of state of dark energy is constrained to w = -1.006 +/- 0.045. Standard big bang nucleosynthesis predictions for the Planck LCDM cosmology are in excellent agreement with observations. We investigate annihilating dark matter and deviations from standard recombination, finding no evidence for new physics. The Planck results for base LCDM are in agreement with BAO data and with the JLA SNe sample. However the amplitude of the fluctuations is found to be higher than inferred from rich cluster counts and weak gravitational lensing. Apart from these tensions, the base LCDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets., Comment: Abstract severely abridged. Revised to match version accepted by Astronomy & Astrophysics. Many minor changes, but basic results remain unchanged
Published: 2015
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