FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W4288097673> ?p ?o ?g. }

• W4288097673 endingPage "A149" @default.
• W4288097673 startingPage "A149" @default.
• W4288097673 abstract "Magnetized plasmas within haloes of galaxies leave their footprint on the polarized anisotropies of the cosmic microwave background. The two dominant effects of astrophysical haloes are Faraday rotation, which generates rotation of the plane of linear polarization, and Faraday conversion, which induces a leakage from linear polarization to circular polarization. We revisit these sources of secondary anisotropies by computing the angular power spectra of the Faraday rotation angle and the Faraday conversion rate by the large-scale structures. To this end, we use the halo model and we pay special attention to the impact of magnetic field projections. Assuming magnetic fields of haloes to be uncorrelated, we found a vanishing two-halo term, and angular power spectra peaking at multipoles ℓ ∼ 10 4 . The Faraday rotation angle is dominated by the contribution of thermal electrons. For the Faraday conversion rate, we found that both thermal electrons and relativistic, non-thermal electrons contribute equally in the most optimistic case for the density and Lorentz factor of relativistic electrons, while in more pessimistic cases the thermal electrons give the dominant contribution. Assuming the magnetic field to be independent of the halo mass, the angular power spectra for both effects roughly scale with the amplitude of matter perturbations as ∼ σ 3 8 , and with a very mild dependence with the density of cold dark matter. Introducing a dependence of the magnetic field strength with the halo mass leads to an increase of the scaling at large angular scales (above a degree) with the amplitude of matter fluctuations up to ∼ σ 9.5 8 for Faraday rotation and ∼ σ 15 8 for Faraday conversion for a magnetic field strength scaling linearly with the halo mass. Introducing higher values of the magnetic field for galaxies, as compared to clusters, instead leads to a decrease of such a scaling at arcminute scales down to ∼ σ 0.9 8 for Faraday rotation." @default.
• W4288097673 created "2022-07-28" @default.
• W4288097673 creator A5013738329 @default.
• W4288097673 creator A5036155936 @default.
• W4288097673 creator A5071565194 @default.
• W4288097673 creator A5072852806 @default.
• W4288097673 creator A5089417448 @default.
• W4288097673 date "2019-10-01" @default.
• W4288097673 modified "2023-10-14" @default.
• W4288097673 title "Secondary CMB anisotropies from magnetized haloes" @default.
• W4288097673 cites W1550168878 @default.
• W4288097673 cites W1647293269 @default.
• W4288097673 cites W1758282328 @default.
• W4288097673 cites W1966550139 @default.
• W4288097673 cites W1970053916 @default.
• W4288097673 cites W1970488901 @default.
• W4288097673 cites W1971778344 @default.
• W4288097673 cites W1978469662 @default.
• W4288097673 cites W1983091630 @default.
• W4288097673 cites W1991509509 @default.
• W4288097673 cites W1998610499 @default.
• W4288097673 cites W2001823370 @default.
• W4288097673 cites W2007030757 @default.
• W4288097673 cites W2017935404 @default.
• W4288097673 cites W2018719255 @default.
• W4288097673 cites W2020266637 @default.
• W4288097673 cites W2034111526 @default.
• W4288097673 cites W2044345588 @default.
• W4288097673 cites W2044647983 @default.
• W4288097673 cites W2047171730 @default.
• W4288097673 cites W2047525308 @default.
• W4288097673 cites W2048956221 @default.
• W4288097673 cites W2049537569 @default.
• W4288097673 cites W2057539390 @default.
• W4288097673 cites W2067083584 @default.
• W4288097673 cites W2082561828 @default.
• W4288097673 cites W2083910651 @default.
• W4288097673 cites W2085068386 @default.
• W4288097673 cites W2100198528 @default.
• W4288097673 cites W2106062944 @default.
• W4288097673 cites W2110640130 @default.
• W4288097673 cites W2114870168 @default.
• W4288097673 cites W2115324751 @default.
• W4288097673 cites W2118413445 @default.
• W4288097673 cites W2137392515 @default.
• W4288097673 cites W2156337336 @default.
• W4288097673 cites W2164261152 @default.
• W4288097673 cites W2170470847 @default.
• W4288097673 cites W2317415105 @default.
• W4288097673 cites W2486893148 @default.
• W4288097673 cites W2583367587 @default.
• W4288097673 cites W2741656519 @default.
• W4288097673 cites W2785017848 @default.
• W4288097673 cites W2796662909 @default.
• W4288097673 cites W2888259247 @default.
• W4288097673 cites W3098657930 @default.
• W4288097673 cites W3098818776 @default.
• W4288097673 cites W3099150453 @default.
• W4288097673 cites W3101196377 @default.
• W4288097673 cites W3101658590 @default.
• W4288097673 cites W3102368526 @default.
• W4288097673 cites W3102887027 @default.
• W4288097673 cites W3102887613 @default.
• W4288097673 cites W3103278742 @default.
• W4288097673 cites W3103467909 @default.
• W4288097673 cites W3103491448 @default.
• W4288097673 cites W3103618759 @default.
• W4288097673 cites W3104708647 @default.
• W4288097673 cites W3105180953 @default.
• W4288097673 cites W3105609887 @default.
• W4288097673 cites W3105790017 @default.
• W4288097673 cites W3106054260 @default.
• W4288097673 cites W3124310639 @default.
• W4288097673 cites W3124695462 @default.
• W4288097673 cites W4213223317 @default.
• W4288097673 cites W4297676541 @default.
• W4288097673 cites W991013512 @default.
• W4288097673 doi "https://doi.org/10.1051/0004-6361/201834485" @default.
• W4288097673 hasPublicationYear "2019" @default.
• W4288097673 type Work @default.
• W4288097673 citedByCount "3" @default.
• W4288097673 countsByYear W42880976732021 @default.
• W4288097673 countsByYear W42880976732022 @default.
• W4288097673 countsByYear W42880976732023 @default.
• W4288097673 crossrefType "journal-article" @default.
• W4288097673 hasAuthorship W4288097673A5013738329 @default.
• W4288097673 hasAuthorship W4288097673A5036155936 @default.
• W4288097673 hasAuthorship W4288097673A5071565194 @default.
• W4288097673 hasAuthorship W4288097673A5072852806 @default.
• W4288097673 hasAuthorship W4288097673A5089417448 @default.
• W4288097673 hasBestOaLocation W42880976731 @default.
• W4288097673 hasConcept C107190969 @default.
• W4288097673 hasConcept C115260700 @default.
• W4288097673 hasConcept C120665830 @default.
• W4288097673 hasConcept C121332964 @default.
• W4288097673 hasConcept C147120987 @default.
• W4288097673 hasConcept C147789679 @default.
• W4288097673 hasConcept C184665706 @default.

• next