QUIJOTE scientific results – VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI

Hoz, E. de la; Barreiro, R. B.; Vielva, P.; Martínez-González, E.; Rubiño-Martín, J. A.; Casaponsa, B.; Guidi, F.; Ashdown, M.; Génova-Santos, R. T.; Artal, E.; Casas, F. J.; Fernández-Cobos, R.; Fernández-Torreiro, M.; Herranz, D.; Hoyland, R. J.; Lasenby, A.; López‐Caniego, M.; López-Caraballo, C. H.; Peel, M.; Piccirillo, L.; Poidevin, F.; Реболо, Р.; Ruiz-Granados, B.; Tramonte, D.; Vansyngel, F.; Watson, R. A.

doi:10.1093/mnras/stac3020

Cited by 9 publications

(6 citation statements)

References 55 publications

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“…where ν s = 30 GHz and A s < 1000 Jy/sr. In accordance with the results of [53], β s can vary from 0.9 to 1.4.…”

Section: Methods Comparison and Prospects For Measuring Spectral Dist...supporting

confidence: 87%

Least response method to separate CMB spectral distortions from foregrounds

Maillard,

Mihalchenko,

Novikov

et al. 2024

Phys. Rev. D

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We present a signal-foreground separation algorithm for filtering observational data to extract spectral distortions of the cosmic microwave background (CMB). Our linear method, called the least response method (LRM), is based on the idea of simultaneously minimizing the response to all possible foregrounds with poorly defined spectral shapes and random noise while maintaining a constant response to the signal of interest. This idea was introduced in detail in our previous paper. Here, we have expanded our analysis by taking into consideration all the main foregrounds. We draw a detailed comparison between our approach and the moment internal linear combination method, which is a modification of the internal linear combination technique previously used for CMB anisotropy maps. We demonstrate advantages of LRM and evaluate the prospects for measuring various types of spectral distortions.Besides, we show that LRM suggests the possibility of its improvements if we use an iterative approach with sequential separation and partial subtraction of foreground components from the observed signal.In addition, we estimate the optimal temperature that the telescope's optical system should have in order to detect the chemical type µ distortions. We present a design of an instrument where, according to our estimates, the optimal contrast between its thermal emission and the CMB allows us to measure such distortions.

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“…where ν s = 30 GHz and A s < 1000 Jy/sr. In accordance with the results of [53], β s can vary from 0.9 to 1.4.…”

Section: Methods Comparison and Prospects For Measuring Spectral Dist...supporting

confidence: 87%

Least response method to separate CMB spectral distortions from foregrounds

Maillard,

Mihalchenko,

Novikov

et al. 2024

Phys. Rev. D

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“…We are aware that, locally, β can assume values over a very broad range. However, we compute the polarization fraction averaging over extended areas, so it is reasonable to assume that in these areas σ β = 0.1 as found in previous works on partial-sky analysis [10,13,50]. We report good agreement between the WMAP and Planck results, the largest discrepancies arising for the more diffuse filaments, e.g., filament XII.…”

Section: Jcap04(2023)049supporting

confidence: 64%

“…Typical values around -3 have been reported for spectral index both in intensity [6,7] and polarization [8][9][10]. More recent analyses seem to indicate the presence of spatial variations in the spectral index [11][12][13], with a tendency to steeper values moving from low to high Galactic latitudes [5].…”

Section: Jcap04(2023)049 1 Introductionmentioning

confidence: 82%

“…The synchrotron spectral energy distribution (SED) is generally approximated by a power law 6 S ν ∝ ν β where β is the energy spectral index. Spatial variations of β have been reported in the literature [11][12][13]. In this section, we measure the spectral index of each filament described in 4.1 employing a method based on the Q and U Stokes parameters [5,51].…”

Section: Spectral Indexmentioning

confidence: 97%

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Morphological analysis of the polarized synchrotron emission with WMAP and Planck

Martire

Banday

Martínez-González

et al. 2023

J. Cosmol. Astropart. Phys.

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The bright polarized synchrotron emission, away from the Galactic plane, originates mostly from filamentary structures. We implement a filament finder algorithm which allows the detection of bright elongated structures in polarized intensity maps. We analyse the sky at 23 and 30 GHz as observed respectively by WMAP and Planck. We identify 19 filaments, 13 of which have been previously observed. For each filament, we study the polarization fraction, finding values typically larger than for the areas outside the filaments, excluding the Galactic plane, and a fraction of about 30% is reached in two filaments. We study the polarization spectral indices of the filaments, and find a spectral index consistent with the values found in previous analysis (about -3.1) for more diffuse regions. Decomposing the polarization signals into the E and B families, we find that most of the filaments are detected in PE , but not in PB . We then focus on understanding the statistical properties of the diffuse regions of the synchrotron emission at 23 GHz. Using Minkowski functionals and tensors, we analyse the non-Gaussianity and statistical isotropy of the polarized intensity maps. For a sky coverage corresponding to 80% of the fainter emission, and on scales smaller than 6 degrees (ℓ > 30), the deviations from Gaussianity and isotropy are significantly higher than 3σ. The level of deviation decreases for smaller scales, however, it remains significantly high for the lowest analised scale (∼ 1.5°). When 60% sky coverage is analysed, we find that the deviations never exceed 3σ. Finally, we present a simple data-driven model to generate non-Gaussian and anisotropic simulations of the synchrotron polarized emission. The simulations are fitted in order to match the spectral and statistical properties of the faintest 80% sky coverage of the data maps.

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“…The polarized sky signal at 40 GHz is dominated by the Galactic synchrotron radiation at scales larger than degree level, with contributions from cosmic microwave background (CMB), Galactic thermal dust radiation, and potentially anomalous microwave emission (AME; Génova-Santos et al 2017;Planck Collaboration IV et al 2020;de la Hoz et al 2023;Herman et al 2023;Svalheim et al 2023;Watts et al 2024). Improved measurements at 40 GHz spanning scales larger than degree level are promising for advancing our understanding of the spatial variation and any steepening or flattening of the polarized synchrotron spectral index, as well as the polarization fraction (currently, there are only upper limits) of the AME (Abazajian et al 2016;Hensley et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Sensitivity-improved Polarization Maps at 40 GHz with CLASS and WMAP Data

Shi 时,

Appel,

Bennett

et al. 2024

ApJ

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Improved polarization measurements at frequencies below 70 GHz with degree-level angular resolution are crucial for advancing our understanding of the Galactic synchrotron radiation and the potential polarized anomalous microwave emission and ultimately benefiting the detection of primordial B modes. In this study, we present sensitivity-improved 40 GHz polarization maps obtained by combining the CLASS 40 GHz and Wilkinson Microwave Anisotropy Probe (WMAP) Q-band data through a weighted average in the harmonic domain. The decision to include WMAP Q-band data stems from similarities in the bandpasses. Leveraging the accurate large-scale measurements from the WMAP Q band and the high-sensitivity information from the CLASS 40 GHz band at intermediate scales, the noise level at ℓ ∈ [30, 100] is reduced by a factor of 2–3 in the map space. A pixel domain analysis of the polarized synchrotron spectral index (β s ) using the WMAP K band and the combined maps (mean and 16th/84th percentiles across the β s map: − 3.08 − 0.20 + 0.20 ) reveals a stronger preference for spatial variation (probability to exceed for a uniform β s hypothesis smaller than 0.001) than the results obtained using WMAP K and Ka bands ( − 3.08 − 0.14 + 0.14 ). The cross-power spectra of the combined maps follow the same trend as other low-frequency data, and validation through simulations indicates negligible bias introduced by the combination method (subpercent level in the power spectra). The products of this work are publicly available on LAMBDA (https://lambda.gsfc.nasa.gov/product/class/class_prod_table.html).

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QUIJOTE scientific results – VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI

Cited by 9 publications

References 55 publications

Least response method to separate CMB spectral distortions from foregrounds

Least response method to separate CMB spectral distortions from foregrounds

Morphological analysis of the polarized synchrotron emission with WMAP and Planck

Sensitivity-improved Polarization Maps at 40 GHz with CLASS and WMAP Data

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