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1. Multipole analysis of cluster weak lensing shear in The Three Hundred project

Author

Payerne C., Hanser C., Murray C., Amouroux N., and Combet C.

Subjects
Physics, QC1-999
Abstract

Weak gravitational lensing is an important tool to estimate the masses of galaxy clusters, as it allows us to directly access their projected surface mass density along the line of sight in a manner largely independent of their dynamical state. Moreover, we can extract information on the projected shape of the cluster mass distribution. In this work, we generate mock catalogs of lensed background galaxies to measure the individual lensing properties of galaxy clusters from the simulation project The Three Hundred. By repeating the analysis for different projections of the same cluster, we find that the use of shear multipoles provides constraints on the ellipticity of the cluster projected mass density but does not have a significant impact on the cluster mass reconstruction compared to the standard approach.

Published
2024
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2. CLMM: a LSST-DESC Cluster weak Lensing Mass Modeling library for cosmology

Author

Aguena, M., Avestruz, C., Combet, C., Fu, S., Herbonnet, R., Malz, A. I., Penna-Lima, M., Ricci, M., Vitenti, S. D. P., Baumont, L., Fan, H., Fong, M., Ho, M., Kirby, M., Payerne, C., Boutigny, D., Lee, B., Liu, B., McClintock, T., Miyatake, H., Sifón, C., von der Linden, A., Wu, H., Yoon, M., and Collaboration, The LSST Dark Energy Science

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the v1.0 release of CLMM, an open source Python library for the estimation of the weak lensing masses of clusters of galaxies. CLMM is designed as a standalone toolkit of building blocks to enable end-to-end analysis pipeline validation for upcoming cluster cosmology analyses such as the ones that will be performed by the LSST-DESC. Its purpose is to serve as a flexible, easy-to-install and easy-to-use interface for both weak lensing simulators and observers and can be applied to real and mock data to study the systematics affecting weak lensing mass reconstruction. At the core of CLMM are routines to model the weak lensing shear signal given the underlying mass distribution of galaxy clusters and a set of data operations to prepare the corresponding data vectors. The theoretical predictions rely on existing software, used as backends in the code, that have been thoroughly tested and cross-checked. Combined, theoretical predictions and data can be used to constrain the mass distribution of galaxy clusters as demonstrated in a suite of example Jupyter Notebooks shipped with the software and also available in the extensive online documentation., Comment: 21 pages, 6 figures, accepted for publication by MNRAS

Published
2021
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3. Erratum: Planck 2018 results: VI. Cosmological parameters (Astronomy and Astrophysics (2020) 641 (A6) DOI: 10.1051/0004-6361/201833910)

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, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, 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, JM, 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, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Lemos, P, Lesgourgues, J, Levrier, F, Lewis, A, and Liguori, M

Subjects
cosmic background radiation, cosmological parameters, errata, addenda, Astronomy & Astrophysics, Astronomical and 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

4. 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

5. Planck intermediate results. LVII. Joint Planck LFI and HFI data processing

Author

Planck Collaboration, Akrami, Y., Andersen, K. J., Ashdown, M., 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., Burigana, C., Butler, R. C., Calabrese, E., Casaponsa, B., 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., Di Valentino, E., Diego, J. M., Doré, O., Douspis, M., Dupac, X., Eriksen, H. K., Fernandez-Cobos, R., Finelli, F., Frailis, M., Fraisse, A. A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Handley, W., Helou, G., Herranz, D., Hildebrandt, S. R., 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., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P. 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., Meinhold, P. R., Mennella, A., Migliaccio, M., Mitra, S., Molinari, D., Montier, L., Morgante, G., Moss, A., Natoli, P., Paoletti, D., Partridge, B., Patanchon, G., Pearson, D., Pearson, T. J., Perrotta, F., Piacentini, F., Polenta, G., 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., Sirignano, C., Sirri, G., Spencer, L. D., Suur-Uski, A. -S., Svalheim, T. L., Tauber, J. A., Tavagnacco, D., Tenti, M., Terenzi, L., Thommesen, H., Toffolatti, L., Tomasi, M., Tristram, 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 the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck analysis efforts, and combines some of the most powerful features of the separate LFI and HFI analysis pipelines. The net effect of the improvements is lower levels of noise and systematics in both frequency and component maps at essentially all angular scales, as well as notably improved internal consistency between the various frequency channels. Based on the NPIPE maps, we present the first estimate of the Solar dipole determined through component separation across all nine Planck frequencies. The amplitude is ($3366.6 \pm 2.7$)$\mu$K, consistent with, albeit slightly higher than, earlier estimates. From the large-scale polarization data, we derive an updated estimate of the optical depth of reionization of $\tau = 0.051 \pm 0.006$, which appears robust with respect to data and sky cuts. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations., Comment: 97 pages, 93 figures and 16 tables, abstract abridged for arXiv submission, accepted for publication in A&A

Published
2020
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6. 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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7. Planck intermediate results: LVI. Detection of the CMB dipole through modulation of the thermal Sunyaev-Zeldovich effect: Eppur si muove II

Author

Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Calabrese, E, Cardoso, JF, 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, JM, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Maciás-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
cosmic background radiation, cosmology: observations, relativistic processes, reference systems, astro-ph.CO, Astronomy & Astrophysics, Astronomical and 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 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

9. Planck intermediate results: LVII. Joint Planck LFI and HFI data processing

Author

Akrami, Y, Andersen, KJ, Ashdown, M, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Burigana, C, Butler, RC, Calabrese, E, Casaponsa, B, Chiang, HC, Colombo, LPL, Combet, C, 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, Eriksen, HK, Fernandez-Cobos, R, Finelli, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Gerbino, M, Ghosh, T, González-Nuevo, J, Górski, KM, Gruppuso, A, Gudmundsson, JE, Handley, W, Helou, G, Herranz, D, Hildebrandt, SR, 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, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lilley, M, Lindholm, V, López-Caniego, M, Lubin, PM, MacÍas-Pérez, JF, Maino, D, Mandolesi, N, Marcos-Caballero, A, Maris, M, Martin, PG, Martínez-González, E, Matarrese, S, Mauri, N, McEwen, JD, Meinhold, PR, Mennella, A, Migliaccio, M, Mitra, S, Molinari, D, Montier, L, Morgante, G, Moss, A, Natoli, P, Paoletti, D, Partridge, B, Patanchon, G, Pearson, D, and Pearson, TJ

Subjects
cosmic background radiation, cosmology: observations, cosmological parameters, Galaxy: general, methods: data analysis, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck analysis efforts, and combines some of the most powerful features of the separate LFI and HFI analysis pipelines. For example, following the LFI 2018 processing procedure, NPIPE uses foreground polarization priors during the calibration stage in order to break scanning-induced degeneracies. Similarly, NPIPE employs the HFI 2018 time-domain processing methodology to correct for bandpass mismatch at all frequencies. In addition, NPIPE introduces several improvements, including, but not limited to: inclusion of the 8% of data collected during repointing manoeuvres; smoothing of the LFI reference load data streams; in-flight estimation of detector polarization parameters; and construction of maximally independent detector-set split maps. For component-separation purposes, important improvements include: maps that retain the CMB Solar dipole, allowing for high-precision relative calibration in higher-level analyses; well-defined single-detector maps, allowing for robust CO extraction; and HFI temperature maps between 217 and 857 GHz that are binned into 0′.9 pixels (Nside = 4096), ensuring that the full angular information in the data is represented in the maps even at the highest Planck resolutions. The net effect of these improvements is lower levels of noise and systematics in both frequency and component maps at essentially all angular scales, as well as notably improved internal consistency between the various frequency channels. Based on the NPIPE maps, we present the first estimate of the Solar dipole determined through component separation across all nine Planck frequencies. The amplitude is (3366.6 ± 2.7) μK, consistent with, albeit slightly higher than, earlier estimates. From the large-scale polarization data, we derive an updated estimate of the optical depth of reionization of τ = 0.051 ± 0.006, which appears robust with respect to data and sky cuts. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations.

Published
2020

10. 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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11. 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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12. 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

13. Planck 2018 results: VII. Isotropy and statistics of the CMB

Author

Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, Casaponsa, B, Chiang, HC, Colombo, LPL, Combet, C, Contreras, D, Crill, BP, De Bernardis, P, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, 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, González-Nuevo, J, Górski, KM, 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, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Ma, YZ, Maciás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Marcos-Caballero, A, Maris, M, Martin, PG, Martínez-González, E, Matarrese, S, Mauri, N, McEwen, JD, Meinhold, PR, and Mennella, A

Subjects
cosmology: observations, cosmic background radiation, polarization, methods: data analysis, methods: statistical, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
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 ΛCDM 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., ℓ 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 ΛCDM 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.

Published
2020

14. Planck 2018 results: IV. Diffuse component separation

Author

Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Calabrese, E, Cardoso, JF, Carron, J, Casaponsa, B, Challinor, A, Colombo, LPL, Combet, C, Crill, BP, Cuttaia, F, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Dickinson, C, Diego, JM, Donzelli, S, Doré, O, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Falgarone, E, 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, Handley, W, Hansen, FK, Helou, G, Herranz, D, Hildebrandt, SR, Huang, Z, Jaffe, AH, Karakci, A, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Lubin, PM, Ma, YZ, Maciás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Marcos-Caballero, A, Maris, M, Martin, PG, and Martínez-González, E

Subjects
ISM: general, cosmology: observations, cosmic background radiation, diffuse radiation, Galaxy: general, astro-ph.CO, Astronomical and Space Sciences, Astronomy & 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 closely 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° regions. We derive a conservative estimate of the mean spectral index of polarized thermal dust emission of βd = 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 βs = -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.

Published
2020

15. 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

16. Planck 2018 results: IX. Constraints on primordial non-Gaussianity

Author

Akrami, Y, Arroja, F, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, 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, JM, 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, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Ma, YZ, Maciás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Marcos-Caballero, A, Maris, M, Martin, PG, Martínez-González, E, and Matarrese, S

Subjects
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
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

17. 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

18. Planck 2018 results: III. High frequency instrument data processing and frequency maps

Author

Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Calabrese, E, Cardoso, JF, Carron, J, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Couchot, F, Crill, BP, Cuttaia, F, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, 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, Ghosh, T, González-Nuevo, J, Górski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Handley, W, Hansen, FK, Henrot-Versillé, S, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Karakci, A, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Ma, YZ, Maciás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Martin, PG, Martínez-González, E, Matarrese, S, and Mauri, N

Subjects
cosmology: observations, cosmic background radiation, surveys, methods: data analysis, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
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 Planck 2015 release, many of which were used and described already in an intermediate paper dedicated to the Planck polarized data at low multipoles. These improvements enabled the first significant measurement of the reionization optical depth parameter using Planck-HFI data. This paper presents an extensive analysis of systematic effects, including the use of end-to-end 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, especially the leakage from intensity to polarization. Calibration, based on the cosmic microwave background (CMB) dipole, is now extremely accurate and in the frequency range 100-353 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 μK, an accuracy of order 10-4. This is a major legacy from the Planck HFI for future CMB experiments. The removal of bandpass leakage has been improved for the main high-frequency foregrounds 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. End-to-end simulations have been shown to 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 (analogue-to-digital convertor non-linearity residuals). Using these simulations, we have been able to 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.

Published
2020

19. Planck 2018 results: I. Overview and the cosmological legacy of Planck

Author

Aghanim, N, Akrami, Y, Arroja, F, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Battye, R, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, Carron, J, Casaponsa, B, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Contreras, D, Crill, BP, Cuttaia, F, De Bernardis, P, De Zotti, G, Delabrouille, J, Delouis, JM, Désert, FX, Di Valentino, E, Dickinson, C, Diego, JM, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, 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, RT, Gerbino, M, Ghosh, T, González-Nuevo, J, Górski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Hamann, J, Handley, W, Hansen, FK, Helou, G, 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, JM, Langer, M, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, and Leahy, JP

Subjects
cosmology: observations, cosmology: theory, cosmic background radiation, surveys, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
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 857 GHz. 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 ΛCDM 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 (θ∗) now known to 0.03%. We describe the multi-component sky as seen by Planck, the success of the ΛCDM 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.

Published
2020

20. Planck 2018 results: X. Constraints on inflation

Author

Akrami, Y, Arroja, F, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, Carron, J, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Contreras, D, Crill, BP, Cuttaia, F, De Bernardis, P, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Diego, JM, Donzelli, S, 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, Forastieri, F, Frailis, M, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Gauthier, C, 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, Hivon, E, Hooper, DC, 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, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Lesgourgues, J, Levrier, F, Lewis, A, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Lubin, PM, and Ma, YZ

Subjects
inflation, cosmic background radiation, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We report on the implications for cosmic inflation of the 2018 release of the Planck cosmic microwave background (CMB) anisotropy measurements. The results are fully consistent with those reported using the data from 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 ns = 0.9649 ± 0.0042 at 68% CL. We find no evidence for a scale dependence of ns, either as a running or as a running of the running. The Universe is found to be consistent with spatial flatness with a precision of 0.4% at 95% CL by combining Planck with a compilation of baryon acoustic oscillation data. The Planck 95% CL upper limit on the tensor-to-scalar ratio, r0.002 < 0.10, is further tightened by combining with the BICEP2/Keck Array BK15 data to obtain r0.002 < 0.056. In the framework of standard single-field inflationary models with Einstein gravity, these results imply that: (a) the predictions of slow-roll models with a concave potential, V″(φ) < 0, are increasingly favoured by the data; and (b) based on two different methods for reconstructing the inflaton potential, we find no evidence for dynamics beyond slow roll. Three different methods for the non-parametric reconstruction of the primordial power spectrum consistently confirm a pure power law in the range of comoving scales 0.005 Mpc-1 k 0.2 Mpc-1. A complementary analysis also finds no evidence for theoretically motivated parameterized features in the Planck power spectra. For the case of oscillatory features that are logarithmic or linear in k, this result is further strengthened by a new combined analysis including the Planck bispectrum data. The new Planck polarization data provide a stringent test of the adiabaticity of the initial conditions for the cosmological fluctuations. In correlated, mixed adiabatic and isocurvature models, the non-adiabatic contribution to the observed CMB temperature variance is constrained to 1.3%, 1.7%, and 1.7% at 95% CL for cold dark matter, neutrino density, and neutrino velocity, respectively. Planck power spectra plus lensing set constraints on the amplitude of compensated cold dark matter-baryon isocurvature perturbations that are consistent with current complementary measurements. The polarization data also provide improved constraints on inflationary models that predict a small statistically anisotropic quadupolar modulation of the primordial fluctuations. However, the polarization data do not support physical models for a scale-dependent dipolar modulation. All these findings support the key predictions of the standard single-field inflationary models, which will be further tested by future cosmological observations.

Published
2020

21. Planck 2018 results: VI. Cosmological parameters

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, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, 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, JM, 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, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Lemos, P, Lesgourgues, J, Levrier, F, Lewis, A, and Liguori, M

Subjects
cosmic background radiation, cosmological parameters, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5σ level. We find good consistency with the standard spatially-flat 6-parameter ΛCDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted "base ΛCDM"in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density ωch2 = 0.120 ± 0.001, baryon density ωbh2 = 0.0224 ± 0.0001, scalar spectral index ns = 0.965 ± 0.004, and optical depth τ = 0.054 ± 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 100θ∗ = 1.0411 ± 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-ΛCDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H0 = (67.4 ± 0.5) km s-1 Mpc-1; matter density parameter ωm = 0.315 ± 0.007; and matter fluctuation amplitude σ8 = 0.811 ± 0.006. We find no compelling evidence for extensions to the base-ΛCDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be Neff = 2.99 ± 0.17, in agreement with the Standard Model prediction Neff = 3.046, and find that the neutrino mass is tightly constrained to mν < 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base ΛCDM at over 2σ, which pulls some parameters that affect the lensing amplitude away from the ΛCDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, ωK = 0.001 ± 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w0 = -1.03 ± 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r0.002 < 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-ΛCDM cosmology are in excellent agreement with observations. The Planck base-ΛCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey's combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6σ, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data.

Published
2020

22. Planck 2018 results: XI. Polarized dust foregrounds

Author

Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Bucher, M, Burigana, C, Calabrese, E, Cardoso, JF, Carron, J, Chiang, HC, Combet, C, Crill, BP, De Bernardis, P, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Dickinson, C, Diego, JM, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Falgarone, E, Fantaye, Y, Ferrière, K, Finelli, F, Forastieri, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, RT, Ghosh, T, González-Nuevo, J, Górski, KM, Gruppuso, A, Gudmundsson, JE, Guillet, V, Handley, W, Hansen, FK, Herranz, D, Huang, Z, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lamarre, JM, Lasenby, A, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Lubin, PM, Ma, YZ, Maciás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Martin, PG, Martínez-González, E, Matarrese, S, McEwen, JD, Meinhold, PR, Melchiorri, A, Migliaccio, M, Miville-Deschênes, MA, Molinari, D, Moneti, A, Montier, L, Morgante, G, Natoli, P, Pagano, L, and Paoletti, D

Subjects
dust, extinction, ISM: magnetic fields, ISM: structure, cosmic background radiation, polarization, submillimeter: diffuse background, astro-ph.GA, astro-ph.CO, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

The study of polarized dust emission has become entwined with the analysis of the cosmic microwave background (CMB) polarization in the quest for the curl-like B-mode polarization from primordial gravitational waves and the low-multipole E-mode polarization associated with the reionization of the Universe. We used the new Planck PR3 maps to characterize Galactic dust emission at high latitudes as a foreground to the CMB polarization and use end-to-end simulations to compute uncertainties and assess the statistical significance of our measurements. We present Planck EE, BB, and TE power spectra of dust polarization at 353 GHz for a set of six nested high-Galactic-latitude 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, which for the largest sky region are αEE = -2.42 ± 0.02 and αBB = -2.54 ± 0.02, respectively. The spectra show that the TE correlation and E/B power asymmetry discovered by Planck extend to low multipoles that were not included in earlier Planck polarization papers due to residual data systematics. We also report evidence for a positive TB dust signal. Combining data from Planck and WMAP, we have determined 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 that is required for measuring the low-ℓ reionization CMB E-mode signal and 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 black-body emission law from 353 GHz to below 70 GHz. For a dust temperature of 19.6 K, the mean dust spectral index for dust polarization is βdP = 1.53±0.02. The difference between indices for polarization and total intensity is βdP-βdI = 0.05±0.03. By fitting multi-frequency cross-spectra between Planck data at 100, 143, 217, and 353 GHz, we examine the correlation of the dust polarization maps across frequency. We find no evidence for a loss of correlation and provide lower limits to the correlation ratio that are tighter than values we derive from the correlation of the 217- and 353 GHz maps alone. If the Planck limit on decorrelation for the largest sky region applies to the smaller sky regions observed by sub-orbital experiments, then frequency decorrelation of dust polarization might not be a problem for CMB experiments aiming at a primordial B-mode detection limit on the tensor-to-scalar ratio r≃ 0.01 at the recombination peak. However, the Planck sensitivity precludes identifying how difficult the component-separation problem will be for more ambitious experiments targeting lower limits on r.

Published
2020

23. Planck 2018 results: VIII. Gravitational lensing

Author

Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Calabrese, E, Cardoso, JF, Carron, J, Challinor, A, Chiang, HC, Colombo, LPL, Combet, C, Crill, BP, Cuttaia, F, De Bernardis, P, De Zotti, G, Delabrouille, J, Di Valentino, E, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, 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, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Karakci, A, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Knox, L, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Lubin, PM, Ma, YZ, Maciás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Marcos-Caballero, A, and Maris, M

Subjects
gravitational lensing: weak, cosmological parameters, cosmic background radiation, large-scale structure of Universe, cosmology: observations, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5σ to 9σ. Combined with temperature, lensing is detected at 40σ. We present an extensive set of tests of the robustness of the lensingpotential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8 ≤ L ≤ 400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the σCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains σ8Ω0.25m= 0.589 ± 0.020 (1σ errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, σ8 = 0.811 ± 0.019, H0 = 67.9+1.2-1.3km s-1Mpc-1, and m = 0.303+0.016-0.018. Combining with Planck CMB power spectrum data, we measure σ8 to better than 1% precision, finding σ8 = 0.811 ± 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in σ8 - m space; 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 the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck-only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal.We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, 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.

Published
2020

24. Planck 2018 results: XII. Galactic astrophysics using polarized dust emission

Author

Aghanim, N, Akrami, Y, Alves, MIR, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Bucher, M, Burigana, C, Calabrese, E, Cardoso, JF, Carron, J, Chary, RR, Chiang, HC, Colombo, LPL, Combet, C, Crill, BP, Cuttaia, F, De Bernardis, P, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Dickinson, C, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Falgarone, E, Fantaye, Y, Fernandez-Cobos, R, Ferrière, K, 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, Green, G, Gruppuso, A, Gudmundsson, JE, Guillet, V, Handley, W, Hansen, FK, Helou, G, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Lubin, PM, Ma, YZ, Maciás-Pérez, JF, and Maggio, G

Subjects
polarization, magnetic fields, turbulence, dust, extinction, local insterstellar matter, submillimeter: ISM, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle ψ, and dispersion function of polarization angles «. The joint distribution (one-point statistics) of p and NH confirms that the mean and maximum polarization fractions decrease with increasing NH. The uncertainty on the maximum observed polarization fraction, pmax = 22.0-1.4+3.5% at 353 GHz and 80′ resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and « found earlier is seen to be present at high latitudes. This follows the «p-1 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, ψ, and « for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map « × p, looking for residual trends. While the polarization fraction p decreases by a factor of 3-4 between NH = 1020 cm-2 and NH = 2 × 1022 cm-2, out of the Galactic plane, this product « × p only decreases by about 25%. Because « is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with NH is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of « × p with the dust temperature Td, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion « tend, on the contrary, to have colder dust than lines of sight with low p and high «. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, RP/p and RS/V, which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, pV/E(B - V), of 13% at high Galactic latitude, compatible with the polarization fraction p ≈ 20% observed at 353 GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas.

Published
2020

25. Planck 2018 results: V. CMB power spectra and likelihoods

Author

Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, 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, JM, 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, JM, 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, YZ, Maciás-Pérez, JF, and Maggio, G

Subjects
cosmic background radiation, cosmology: observations, cosmological parameters, methods: data analysis, astro-ph.CO, Astronomy & Astrophysics, Astronomical and 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

26. 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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27. 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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28. 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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29. 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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30. 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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31. 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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32. 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

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2018
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33. Planck intermediate results. LIV. The Planck Multi-frequency Catalogue of Non-thermal Sources

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., Burigana, C., Butler, R. C., Calabrese, E., Carron, J., Chiang, H. C., 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., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., 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., 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., Lähteenmäki, A., 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., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., 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., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Pearson, T. J., 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., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Toffolatti, L., Tomasi, M., Trombetti, T., Tucci, M., 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

This paper presents the Planck Multi-frequency Catalogue of Non-thermal (i.e. synchrotron-dominated) Sources (PCNT) observed between 30 and 857 GHz by the ESA Planck mission. This catalogue was constructed by selecting objects detected in the full mission all-sky temperature maps at 30 and 143 GHz, with a signal-to-noise ratio (S/N)>3 in at least one of the two channels after filtering with a particular Mexican hat wavelet. As a result, 29400 source candidates were selected. Then, a multi-frequency analysis was performed using the Matrix Filters methodology at the position of these objects, and flux densities and errors were calculated for all of them in the nine Planck channels. The present catalogue is the first unbiased, full-sky catalogue of synchrotron-dominated sources published at millimetre and submillimetre wavelengths and constitutes a powerful database for statistical studies of non-thermal extragalactic sources, whose emission is dominated by the central active galactic nucleus. Together with the full multi-frequency catalogue, we also define the Bright Planck Multi-frequency Catalogue of Non-thermal Sources PCNTb, where only those objects with a S/N>4 at both 30 and 143 GHz were selected. In this catalogue 1146 compact sources are detected outside the adopted Planck GAL070 mask; thus, these sources constitute a highly reliable sample of extragalactic radio sources. We also flag the high-significance subsample PCNThs, a subset of 151 sources that are detected with S/N>4 in all nine Planck channels, 75 of which are found outside the Planck mask adopted here. The remaining 76 sources inside the Galactic mask are very likely Galactic objects., Comment: 24 pages, 15 figures. Accepted for publication in Astronomy & Astrophysics

Published
2018
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34. 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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35. Planck intermediate results LIV. The Planck multi-frequency catalogue of non-thermal sources

Author

Akrami, Y, Argueso, 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, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Butler, RC, Calabrese, E, Carron, J, Chiang, HC, Combet, C, Crill, BP, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Delouis, J-M, Di Valentino, E, Dickinson, C, Diego, JM, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Ensslin, TA, Eriksen, HK, Fantaye, Y, Finelli, F, Frailis, M, Fraisse, AA, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Genova-Santos, RT, Gerbino, M, Ghosh, T, Gonzalez-Nuevo, J, Gorski, KM, Gratton, S, Gruppuso, A, Gudmundsson, JE, Handley, W, Hansen, FK, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Keihanen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lahteenmaki, A, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, Lopez-Caniego, M, Ma, Y-Z, Macias-Perez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, PG, Martinez-Gonzalez, E, Matarrese, S, McEwen, JD, Meinhold, PR, Melchiorri, A, Mennella, A, Migliaccio, M, Miville-Deschenes, M-A, Molinari, D, and Moneti, A

Subjects
catalogs, cosmology: observations, radio continuum: general, submillimeter: general, Astronomical And Space Sciences, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

Context. The European Space Agency (ESA) Rosetta mission was the most comprehensive study of a comet ever performed. In particular, the Rosetta orbiter, which carried many instruments for monitoring the evolution of the dusty gas emitted by the cometary nucleus, returned an enormous volume of observational data collected from the close vicinity of the nucleus of comet 67P/Churyumov-Gerasimenko.Aims. Such data are expected to yield unique information on the physical processes of gas and dust emission, using current physical model fits to the data. We present such a model (the RZC model) and our procedure of adjustment of this model to the data.Methods. The RZC model consists of two components: (1) a numerical three-dimensional time-dependent code solving the Eulerian/Navier-Stokes equations governing the gas outflow, and a direct simulation Monte Carlo (DSMC) gaskinetic code with the same objective; and (2) an iterative procedure to adjust the assumed model parameters to best-fit the observational data at all times.Results. We demonstrate that our model is able to reproduce the overall features of the local neutral number density and composition measurements of Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) Comet Pressure Sensor (COPS) and Double Focusing Mass Spectrometer (DFMS) instruments in the period August 1–November 30, 2014. The results of numerical simulations show that illumination conditions on the nucleus are the main driver for the gas activity of the comet. We present the distribution of surface inhomogeneity best-fitted to the ROSINA COPS and DFMS in situ measurements.

Published
2018

36. Planck intermediate results

Author

Akrami, Y, Argüeso, 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, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Butler, RC, Calabrese, E, Carron, J, Chiang, HC, Combet, C, Crill, BP, Cuttaia, F, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Delouis, J-M, Di Valentino, E, Dickinson, C, Diego, JM, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, Finelli, 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, 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, Lähteenmäki, A, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Levrier, F, Liguori, M, Lilje, PB, Lindholm, V, López-Caniego, M, Ma, Y-Z, Macías-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, PG, Martínez-González, E, Matarrese, S, McEwen, JD, Meinhold, PR, Melchiorri, A, Mennella, A, Migliaccio, M, Miville-Deschênes, M-A, Molinari, D, and Moneti, A

Subjects
Space Sciences, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

This paper presents the Planck Multi-frequency Catalogue of Non-thermal (i.e. synchrotron-dominated) Sources (PCNT) observed between 30 and 857 GHz by the ESA Planck mission. This catalogue was constructed by selecting objects detected in the full mission all-sky temperature maps at 30 and 143 GHz, with a signal-to-noise ratio (S/N)> 3 in at least one of the two channels after filtering with a particular Mexican hat wavelet. As a result, 29 400 source candidates were selected. Then, a multi-frequency analysis was performed using the Matrix Filters methodology at the position of these objects, and flux densities and errors were calculated for all of them in the nine Planck channels. This catalogue was built using a different methodology than the one adopted for the Planck Catalogue of Compact Sources (PCCS) and the Second Planck Catalogue of Compact Sources (PCCS2), although the initial detection was done with the same pipeline that was used to produce them. The present catalogue is the first unbiased, full-sky catalogue of synchrotron-dominated sources published at millimetre and submillimetre wavelengths and constitutes a powerful database for statistical studies of non-thermal extragalactic sources, whose emission is dominated by the central active galactic nucleus. Together with the full multi-frequency catalogue, we also define the Bright Planck Multi-frequency Catalogue of Non-thermal Sources (PCNTb), where only those objects with a S/N > 4 at both 30 and 143 GHz were selected. In this catalogue 1146 compact sources are detected outside the adopted Planck GAL070 mask; thus, these sources constitute a highly reliable sample of extragalactic radio sources. We also flag the high-significance subsample (PCNThs), a subset of 151 sources that are detected with S/Na, >, 4 in all nine Planck channels, 75 of which are found outside the Planck mask adopted here. The remaining 76 sources inside the Galactic mask are very likely Galactic objects.

Published
2018

37. Towards including super-sample covariance in the unbinned likelihood for cluster abundance cosmology.

Author

Payerne, C, Murray, C, Combet, C, and Penna-Lima, M

Subjects
PHYSICAL cosmology, GALAXY clusters, DARK matter, CLUSTER analysis (Statistics), REDSHIFT, UNIVERSE, NOISE measurement, NOISE
Abstract

The measurement of the abundance of galaxy clusters in the Universe is a sensitive probe of cosmology, which depends on both the expansion history of the Universe and the growth of structure. Density fluctuations across the finite survey volume add noise to this measurement, this is often referred to as super-sample covariance (SSC). For an unbinned cluster analysis, such noise has not been included in the cluster likelihood, since the effect of SSC was small compared to the Poisson shot-noise for samples of a few hundred clusters. For upcoming large cluster surveys such as the Rubin LSST, which will deliver catalogues of tens of thousands of clusters, this effect will no longer be negligible. In this paper, we propose a new hybrid likelihood based on the Gauss-Poisson Compound model (GPC), by using infinitesimal mass bins and standard redshift bins. This likelihood has the advantages of an unbinned Poisson likelihood while successfully incorporating the effects of SSC. Using a simulated dark matter halo catalogue, we find that the hybrid likelihood, accounting for both Poisson noise and SSC, increases the dispersion of the parameter posteriors by 20 per cent when using 100 000 clusters compared to the standard unbinned likelihood, based on Poisson statistics only. [ABSTRACT FROM AUTHOR]

Published
2024
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38. 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

39. Planck intermediate results: LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters

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, JF, 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, JM, 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, YZ, 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
cosmology: observations, cosmic background radiation, cosmological parameters, cosmology: theory, astro-ph.CO, Astronomy & Astrophysics, Astronomical and 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

40. 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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41. 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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42. 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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43. 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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44. 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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45. 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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46. 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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47. 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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48. 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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49. 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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50. Planck intermediate results: L. Evidence of spatial variation of the polarized thermal dust spectral energy distribution and implications for CMB B-mode analysis

Author

Aghanim, N, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Burigana, C, Calabrese, E, Cardoso, JF, Chiang, HC, Colombo, LPL, Combet, C, Comis, B, Crill, BP, Curto, A, Cuttaia, F, Davis, RJ, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, JM, Di Valentino, E, Dickinson, C, Diego, JM, Doré, O, Douspis, M, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, 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, Ghosh, T, Giard, M, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Gudmundsson, JE, Hansen, FK, Helou, G, Herranz, D, Hivon, E, Huang, Z, Jaffe, AH, Jones, WC, Keihänen, E, Keskitalo, R, Kisner, TS, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, JM, Lasenby, A, Lattanzi, M, Lawrence, CR, Le Jeune, M, Levrier, F, Liguori, M, Lilje, PB, López-Caniego, M, Lubin, PM, MacIás-Pérez, JF, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, PG, and Martínez-González, E

Subjects
cosmic background radiation, cosmology, observations, submillimeter, ISM - dust, extinction, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

The characterization of the Galactic foregrounds has been shown to be the main obstacle in thechallenging quest to detect primordial B-modes in the polarized microwave sky. We make use of the Planck-HFI 2015 data release at high frequencies to place new constraints on the properties of the polarized thermal dust emission at high Galactic latitudes. Here, we specifically study the spatial variability of the dust polarized spectral energy distribution (SED), and its potential impact on the determination of the tensor-to-scalar ratio, r. We use the correlation ratio of the angular power spectra between the 217 and 353 GHz channels as a tracer of these potential variations, computed on different high Galactic latitude regions, ranging from 80% to 20% of the sky. The new insight from Planck data is a departure of the correlation ratio from unity that cannot be attributed to a spurious decorrelation due to the cosmic microwave background, instrumental noise, or instrumental systematics. The effect is marginally detected on each region, but the statistical combination of all the regions gives more than 99% confidence for this variation in polarized dust properties. In addition, we show that the decorrelation increases when there is a decrease in the mean column density of the region of the sky being considered, and we propose a simple power-law empirical model for this dependence, which matches what is seen in the Planck data. We explore the effect that this measured decorrelation has on simulations of the BICEP2-Keck Array/Planck analysis and show that the 2015 constraints from these data still allow a decorrelation between the dust at 150 and 353 GHz that is compatible with our measured value. Finally, using simplified models, we show that either spatial variation of the dust SED or of the dust polarization angle are able to produce decorrelations between 217 and 353 GHz data similar to the values we observe in the data.

Published
2017

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