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N Aghanim - One of the best experts on this subject based on the ideXlab platform.

  • planck 2018 results vi cosmological parameters
    Astronomy and Astrophysics, 2020
    Co-Authors: N Aghanim, L Polastri, J A Rubinomartin, X Dupac, M Liguori, Jaeyoung Kim, S Matarrese, R T Genovasantos, Z Huang
    Abstract:

    Author(s): 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; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, 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; Genova-Santos, RT; Gerbino, M; Ghosh, T; Gonzalez-Nuevo, J; Gorski, 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; Keihanen, E; Keskitalo, R; Kiiveri, K; Kim, J; Kisner, TS | Abstract: © ESO 2020. 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 l 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 l 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.

  • planck 2018 results v cmb power spectra and likelihoods
    Astronomy and Astrophysics, 2020
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, Yashar Akrami, M Ballardini, N Bartolo
    Abstract:

    Author(s): 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; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Finelli, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; 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; Lagache, G; Lamarre, JM | Abstract: © 2020 EDP Sciences. All rights reserved. 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 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 l 800 and l g 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.

  • planck 2018 results viii gravitational lensing
    arXiv: Cosmology and Nongalactic Astrophysics, 2018
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, N Bartolo, Yashar Akrami, M Ballardini, S Basak
    Abstract:

    Author(s): Collaboration, Planck; 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; Calabrese, E; Cardoso, J-F; Carron, J; Challinor, A; Chiang, HC; Colombo, LPL; Combet, C; Crill, BP; Cuttaia, F; Bernardis, P de; Zotti, G de; Delabrouille, J; Valentino, E Di; Diego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Forastieri, 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; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, 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, CR; Jeune, M Le | 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).

  • planck 2015 results xxii a map of the thermal sunyaev zeldovich effect
    Astronomy and Astrophysics, 2016
    Co-Authors: N Aghanim, M Arnaud, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, J G Bartlett, N Bartolo
    Abstract:

    Author(s): Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, AJ; Barreiro, RB; Bartlett, JG; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bonaldi, A; Bonavera, L; Bond, JR; Borrill, J; Bouchet, FR; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Catalano, A; Challinor, A; Chiang, HC; Christensen, PR; Churazov, E; Clements, DL; Colombo, LPL; Combet, C; Comis, B; Coulais, A; Crill, BP; Curto, A; Cuttaia, F; Danese, L; Davies, RD; Davis, RJ; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Desert, FX; Dickinson, C; Diego, JM; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Fraisse, AA; Franceschi, E; Frejsel, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Giard, M; Gonzalez-Nuevo, J; Gorski, KM; Gregorio, A; Gruppuso, A; Gudmundsson, JE; Hansen, FK; Harrison, DL; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, SR; Hivon, E | Abstract: © 2016 ESO. We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 l" l 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology.

N Bartolo - One of the best experts on this subject based on the ideXlab platform.

  • planck 2018 results v cmb power spectra and likelihoods
    Astronomy and Astrophysics, 2020
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, Yashar Akrami, M Ballardini, N Bartolo
    Abstract:

    Author(s): 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; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Finelli, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; 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; Lagache, G; Lamarre, JM | Abstract: © 2020 EDP Sciences. All rights reserved. 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 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 l 800 and l g 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.

  • planck 2018 results viii gravitational lensing
    arXiv: Cosmology and Nongalactic Astrophysics, 2018
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, N Bartolo, Yashar Akrami, M Ballardini, S Basak
    Abstract:

    Author(s): Collaboration, Planck; 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; Calabrese, E; Cardoso, J-F; Carron, J; Challinor, A; Chiang, HC; Colombo, LPL; Combet, C; Crill, BP; Cuttaia, F; Bernardis, P de; Zotti, G de; Delabrouille, J; Valentino, E Di; Diego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Forastieri, 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; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, 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, CR; Jeune, M Le | 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).

  • planck 2015 results xxii a map of the thermal sunyaev zeldovich effect
    Astronomy and Astrophysics, 2016
    Co-Authors: N Aghanim, M Arnaud, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, J G Bartlett, N Bartolo
    Abstract:

    Author(s): Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, AJ; Barreiro, RB; Bartlett, JG; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bonaldi, A; Bonavera, L; Bond, JR; Borrill, J; Bouchet, FR; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Catalano, A; Challinor, A; Chiang, HC; Christensen, PR; Churazov, E; Clements, DL; Colombo, LPL; Combet, C; Comis, B; Coulais, A; Crill, BP; Curto, A; Cuttaia, F; Danese, L; Davies, RD; Davis, RJ; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Desert, FX; Dickinson, C; Diego, JM; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Fraisse, AA; Franceschi, E; Frejsel, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Giard, M; Gonzalez-Nuevo, J; Gorski, KM; Gregorio, A; Gruppuso, A; Gudmundsson, JE; Hansen, FK; Harrison, DL; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, SR; Hivon, E | Abstract: © 2016 ESO. We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 l" l 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology.

A J Banday - One of the best experts on this subject based on the ideXlab platform.

  • planck 2018 results v cmb power spectra and likelihoods
    Astronomy and Astrophysics, 2020
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, Yashar Akrami, M Ballardini, N Bartolo
    Abstract:

    Author(s): 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; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Finelli, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; 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; Lagache, G; Lamarre, JM | Abstract: © 2020 EDP Sciences. All rights reserved. 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 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 l 800 and l g 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.

  • planck 2018 results viii gravitational lensing
    arXiv: Cosmology and Nongalactic Astrophysics, 2018
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, N Bartolo, Yashar Akrami, M Ballardini, S Basak
    Abstract:

    Author(s): Collaboration, Planck; 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; Calabrese, E; Cardoso, J-F; Carron, J; Challinor, A; Chiang, HC; Colombo, LPL; Combet, C; Crill, BP; Cuttaia, F; Bernardis, P de; Zotti, G de; Delabrouille, J; Valentino, E Di; Diego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Forastieri, 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; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, 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, CR; Jeune, M Le | 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).

  • planck 2015 results xxii a map of the thermal sunyaev zeldovich effect
    Astronomy and Astrophysics, 2016
    Co-Authors: N Aghanim, M Arnaud, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, J G Bartlett, N Bartolo
    Abstract:

    Author(s): Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, AJ; Barreiro, RB; Bartlett, JG; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bonaldi, A; Bonavera, L; Bond, JR; Borrill, J; Bouchet, FR; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Catalano, A; Challinor, A; Chiang, HC; Christensen, PR; Churazov, E; Clements, DL; Colombo, LPL; Combet, C; Comis, B; Coulais, A; Crill, BP; Curto, A; Cuttaia, F; Danese, L; Davies, RD; Davis, RJ; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Desert, FX; Dickinson, C; Diego, JM; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Fraisse, AA; Franceschi, E; Frejsel, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Giard, M; Gonzalez-Nuevo, J; Gorski, KM; Gregorio, A; Gruppuso, A; Gudmundsson, JE; Hansen, FK; Harrison, DL; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, SR; Hivon, E | Abstract: © 2016 ESO. We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 l" l 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology.

R B Barreiro - One of the best experts on this subject based on the ideXlab platform.

  • planck 2018 results v cmb power spectra and likelihoods
    Astronomy and Astrophysics, 2020
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, Yashar Akrami, M Ballardini, N Bartolo
    Abstract:

    Author(s): 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; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Finelli, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; 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; Lagache, G; Lamarre, JM | Abstract: © 2020 EDP Sciences. All rights reserved. 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 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 l 800 and l g 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.

  • planck 2018 results viii gravitational lensing
    arXiv: Cosmology and Nongalactic Astrophysics, 2018
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, N Bartolo, Yashar Akrami, M Ballardini, S Basak
    Abstract:

    Author(s): Collaboration, Planck; 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; Calabrese, E; Cardoso, J-F; Carron, J; Challinor, A; Chiang, HC; Colombo, LPL; Combet, C; Crill, BP; Cuttaia, F; Bernardis, P de; Zotti, G de; Delabrouille, J; Valentino, E Di; Diego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Forastieri, 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; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, 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, CR; Jeune, M Le | 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).

  • planck 2015 results xxii a map of the thermal sunyaev zeldovich effect
    Astronomy and Astrophysics, 2016
    Co-Authors: N Aghanim, M Arnaud, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, J G Bartlett, N Bartolo
    Abstract:

    Author(s): Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, AJ; Barreiro, RB; Bartlett, JG; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bonaldi, A; Bonavera, L; Bond, JR; Borrill, J; Bouchet, FR; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Catalano, A; Challinor, A; Chiang, HC; Christensen, PR; Churazov, E; Clements, DL; Colombo, LPL; Combet, C; Comis, B; Coulais, A; Crill, BP; Curto, A; Cuttaia, F; Danese, L; Davies, RD; Davis, RJ; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Desert, FX; Dickinson, C; Diego, JM; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Fraisse, AA; Franceschi, E; Frejsel, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Giard, M; Gonzalez-Nuevo, J; Gorski, KM; Gregorio, A; Gruppuso, A; Gudmundsson, JE; Hansen, FK; Harrison, DL; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, SR; Hivon, E | Abstract: © 2016 ESO. We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 l" l 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology.

C Baccigalupi - One of the best experts on this subject based on the ideXlab platform.

  • planck 2018 results v cmb power spectra and likelihoods
    Astronomy and Astrophysics, 2020
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, Yashar Akrami, M Ballardini, N Bartolo
    Abstract:

    Author(s): 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; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Finelli, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Giraud-Heraud, Y; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; 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; Lagache, G; Lamarre, JM | Abstract: © 2020 EDP Sciences. All rights reserved. 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 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 l 800 and l g 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.

  • planck 2018 results viii gravitational lensing
    arXiv: Cosmology and Nongalactic Astrophysics, 2018
    Co-Authors: N Aghanim, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, N Bartolo, Yashar Akrami, M Ballardini, S Basak
    Abstract:

    Author(s): Collaboration, Planck; 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; Calabrese, E; Cardoso, J-F; Carron, J; Challinor, A; Chiang, HC; Colombo, LPL; Combet, C; Crill, BP; Cuttaia, F; Bernardis, P de; Zotti, G de; Delabrouille, J; Valentino, E Di; Diego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Fernandez-Cobos, R; Forastieri, 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; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, 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, CR; Jeune, M Le | 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).

  • planck 2015 results xxii a map of the thermal sunyaev zeldovich effect
    Astronomy and Astrophysics, 2016
    Co-Authors: N Aghanim, M Arnaud, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, J G Bartlett, N Bartolo
    Abstract:

    Author(s): Aghanim, N; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, AJ; Barreiro, RB; Bartlett, JG; Bartolo, N; Battaner, E; Battye, R; Benabed, K; Benoit, A; Benoit-Levy, A; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bonaldi, A; Bonavera, L; Bond, JR; Borrill, J; Bouchet, FR; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Catalano, A; Challinor, A; Chiang, HC; Christensen, PR; Churazov, E; Clements, DL; Colombo, LPL; Combet, C; Comis, B; Coulais, A; Crill, BP; Curto, A; Cuttaia, F; Danese, L; Davies, RD; Davis, RJ; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Desert, FX; Dickinson, C; Diego, JM; Dolag, K; Dole, H; Donzelli, S; Dore, O; Douspis, M; Ducout, A; Dupac, X; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fergusson, J; Finelli, F; Forni, O; Frailis, M; Fraisse, AA; Franceschi, E; Frejsel, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Giard, M; Gonzalez-Nuevo, J; Gorski, KM; Gregorio, A; Gruppuso, A; Gudmundsson, JE; Hansen, FK; Harrison, DL; Henrot-Versille, S; Hernandez-Monteagudo, C; Herranz, D; Hildebrandt, SR; Hivon, E | Abstract: © 2016 ESO. We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 l" l 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology.