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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

QUIJOTE scientific results – XII. Characterization of the polarized synchrotron emission at the power spectrum level in the QUIJOTE-MFI wide survey

  • F Vansyngel1,2
  • J A Rubiño-Martín1,2
  • P de Ferra2
  • R B Barreiro3
  • R T Génova-Santos1,2
  • B Casaponsa3
  • M Fernández-Torreiro1,2
  • D Adak1,2
  • K Aryan1,2
  • M Ashdown4,5
  • J M Casas6,7
  • F J Casas3
10 more authors
  • R Cepeda-Arroita1,2
  • A Fasano1,2
  • D Herranz3
  • E Martínez-González3
  • F Poidevin1,2
  • R Rebolo1,2,8
  • B Ruiz-Granados9,1,2
  • D Tramonte10,1,2
  • P Vielva3
  • R A Watson11
11 affiliations
  1. 1Instituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife ,
  2. 2Universidad de La Laguna (ULL) Departamento de Astrofísica, , E-38206 La Laguna, Tenerife ,
  3. 3Instituto de Física de Cantabria (IFCA) , CSIC-Univ. de Cantabria, Avda. los Castros, s/n, E-39005 Santander ,
  4. 4Astrophysics Group, Cavendish Laboratory, University of Cambridge , J J Thomson Avenue, Cambridge CB3 0HE ,
  5. 5Kavli Institute for Cosmology, University of Cambridge , Madingley Road, Cambridge CB3 0HA ,
  6. 6Universidad de Oviedo , Departamento de Matemáticas, C. Federico García Lorca 18, 33007 Oviedo ,
  7. 7Instituto Universitario de Ciencias y Tecnologías Espaciales de Asturias (ICTEA) , C. Independencia 13, 33004 Oviedo ,
  8. 8Consejo Superior de Investigaciones Científicas , E-28006 Madrid ,
  9. 9Universidad de Córdoba Departamento de Física. Facultad de Ciencias. . Campus de Rabanales, Edif. C2. Planta Baja. E-14071 Córdoba ,
  10. 10Xi’an Jiaotong–Liverpool University, 111 Ren’ai Road, Suzhou Dushu Lake Science and Education Innovation District Department of Physics, , Suzhou Industrial Park, Suzhou 215123 ,
  11. 11School of Natural Sciences, The University of Manchester Jodrell Bank Centre for Astrophysics, Alan Turing Building, Department of Physics and Astronomy, , Oxford Road, Manchester M13 9PL, Manchester ,
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Abstract

We present an analysis of the polarized synchrotron emission at the power-spectrum level in the multipole range 30 ≤ ℓ < 130, using the recent QUIJOTE-MFI wide survey (10–20 GHz) in combination with Planck and WMAP data. The EE and BB power spectra are well described by a simple power-law model, with no evidence for the need of additional parameters. The best-fit slopes are αEE = −3.24 ± 0.12 and αEE = −3.81 ± 0.34 for |b| > 20○, hinting toward a steepening of the BB spectrum relative to EE at the ∼1.6σ level. The synchrotron frequency spectral indices are found to be β sEE = −3.26 ± 0.05 and β sBB = −3.25 ± 0.10 for the same cut, in agreement with earlier real-space analyses. We find no evidence for spatial variations of βs across different Galactic latitude cuts, within current uncertainties. The synchrotron BB/EE power ratio is approximately 0.2 over the considered multipole range, lower than typical values for thermal dust, and consistent with previous measurements. We also measure a dust-synchrotron spatial correlation in the range 0.1–0.25 over 30 ≤ ℓ < 130. Using these results, we estimate the level of synchrotron contamination in future CMB B-mode measurements, finding an average power in the considered sky masks equivalent to r ≃ 0.003 at 90 GHz and r ≃ 0.0002 at 150 GHz for the relevant angular scales.

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Cite

BibTeXRIS
BibTeX
@article{vansyngel2026quijote,
  title = {{QUIJOTE scientific results – XII. Characterization of the polarized synchrotron emission at the power spectrum level in the QUIJOTE-MFI wide survey}},
  author = {F Vansyngel and J A Rubiño-Martín and P de Ferra and R B Barreiro and R T Génova-Santos and B Casaponsa and M Fernández-Torreiro and D Adak and K Aryan and M Ashdown and J M Casas and F J Casas and R Cepeda-Arroita and A Fasano and D Herranz and E Martínez-González and F Poidevin and R Rebolo and B Ruiz-Granados and D Tramonte and P Vielva and R A Watson},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag2031},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2031/8997908},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - QUIJOTE scientific results – XII. Characterization of the polarized synchrotron emission at the power spectrum level in the QUIJOTE-MFI wide survey
AU  - F Vansyngel
AU  - J A Rubiño-Martín
AU  - P de Ferra
AU  - R B Barreiro
AU  - R T Génova-Santos
AU  - B Casaponsa
AU  - M Fernández-Torreiro
AU  - D Adak
AU  - K Aryan
AU  - M Ashdown
AU  - J M Casas
AU  - F J Casas
AU  - R Cepeda-Arroita
AU  - A Fasano
AU  - D Herranz
AU  - E Martínez-González
AU  - F Poidevin
AU  - R Rebolo
AU  - B Ruiz-Granados
AU  - D Tramonte
AU  - P Vielva
AU  - R A Watson
PY  - 2026
DA  - 2026/10/24
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag2031
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2031/8997908
AB  - We present an analysis of the polarized synchrotron emission at the power-spectrum level in the multipole range 30 ≤ ℓ < 130, using the recent QUIJOTE-MFI wide survey (10–20 GHz) in combination with Planck and WMAP data. The EE and BB power spectra are well described by a simple power-law model, with no evidence for the need of additional parameters. The best-fit slopes are αEE = −3.24 ± 0.12 and αEE = −3.81 ± 0.34 for |b| > 20○, hinting toward a steepening of the BB spectrum relative to EE at the ∼1.6σ level. The synchrotron frequency spectral indices are found to be β _s^EE = −3.26 ± 0.05 and β _s^BB = −3.25 ± 0.10 for the same cut, in agreement with earlier real-space analyses. We find no evidence for spatial variations of βs across different Galactic latitude cuts, within current uncertainties. The synchrotron BB/EE power ratio is approximately 0.2 over the considered multipole range, lower than typical values for thermal dust, and consistent with previous measurements. We also measure a dust-synchrotron spatial correlation in the range 0.1–0.25 over 30 ≤ ℓ < 130. Using these results, we estimate the level of synchrotron contamination in future CMB B-mode measurements, finding an average power in the considered sky masks equivalent to r ≃ 0.003 at 90 GHz and r ≃ 0.0002 at 150 GHz for the relevant angular scales.
SN  - 0035-8711
SN  - 1365-2966
ER  -