The QUIJOTE Experiment: Prospects for CMB B-MODE polarization detection and foregrounds characterization

Poidevin, F.; Rubiño-Martín, J. A.; Génova-Santos, R. T.; Реболо, Р.; Aguiar, M.; Gómez-Reñasco, F.; Guidi, F.; Gutiérrez, Carlos M.; Hoyland, R. J.; López-Caraballo, C. H.; Carreras, A. Oria; Peláez-Santos, A.; Pérez-de-Taoro, M. R.; Ruiz-Granados, B.; Tramonte, D.; Vega-Moreno, A.; Viera-Curbelo, T.; Vignaga, R.; Martínez-González, E.; Barreiro, R. B.; Casaponsa, B.; Casas, F. J.; Diego, J. M.; Fernández-Cobos, R.; Herranz, D.; López‐Caniego, M.; Ortiz, D.; Vielva, P.; Artal, E.; Aja, B.; Cagigas, J.; Cano, Juan Luis; Fuente, L. de la; Mediavilla, A.; Terán, J. V.; Villa, Enrique; Piccirillo, L.; Dickinson, C.; Grainge, K.; Harper, Simon; McCulloch, M.; Melhuish, S. J.; Pisano, G.; Watson, R. A.; Lasenby, A. N.; Ashdown, M.; Perrott, Y. C.; Razavi-Ghods, N.; Titterington, D.; Scott, Paul F.

doi:10.48550/arxiv.1802.04594

Cited by 7 publications

(9 citation statements)

References 3 publications

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“…Although no synchrotron EB has been found so far [53], more evidence is needed to rule out synchrotron EB as one of the culprits. The C-BASS and QUIJOTE experiments will give us a better understanding of synchrotron in the near future [55,56]. Finally, we show the average of the observed EB power spectra ("stacked observed EB power spectrum") with the uncertainty in Fig.…”

Section: Resultsmentioning

confidence: 99%

Improved constraints on cosmic birefringence from the WMAP and Planck cosmic microwave background polarization data

Eskilt

Komatsu

2022

Phys. Rev. D

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The observed pattern of linear polarization of the cosmic microwave background photons is a sensitive probe of physics violating parity symmetry under inversion of spatial coordinates. A new parity-violating interaction might have rotated the plane of linear polarization by an angle β as the cosmic microwave background photons have been traveling for more than 13 billion years. This effect is known as "cosmic birefringence." In this paper, we present new measurements of cosmic birefringence from a joint analysis of polarization data from two space missions, Planck and WMAP. This dataset covers a wide range of frequencies from 23 to 353 GHz. We measure β ¼ 0.342°þ 0.094°− 0.091°[ 68% confidence level (CL)] for nearly full-sky data, which excludes β ¼ 0 at 99.987% CL. This corresponds to the statistical significance of 3.6σ. There is no evidence for frequency dependence of β. We find a similar result, albeit with a larger uncertainty, when removing the Galactic plane from the analysis.

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Section: Resultsmentioning

confidence: 99%

Improved constraints on cosmic birefringence from the WMAP and Planck cosmic microwave background polarization data

Eskilt

Komatsu

2022

Phys. Rev. D

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“…Martire et al (2022) found that the EB of A10, page 7 of 11 synchrotron emission is compatible with zero at 1σ using the 30 GHz band of Planck and the WMAP K-band for different sky fractions. The low signal-to-noise of these instruments puts weak constraints on it, but QUIJOTE and C-BASS aim to get a better understanding of the polarized synchrotron emission (Poidevin et al 2018;Jones et al 2018). Hence, we treat the full analysis of all Planck polarized maps with the inclusion of the 30 and 44 GHz channels separately, and we do not include any modeling of the intrinsic EB of either dust or synchrotron emission.…”

Section: Including All the Planck Polarized Frequency Mapsmentioning

confidence: 99%

Frequency-dependent constraints on cosmic birefringence from the LFI and HFI Planck Data Release 4

Eskilt

2022

A&A

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We present new constraints on the frequency dependence of the cosmic birefringence angle from the Planck Data Release 4 polarization maps. An axion field coupled to electromagnetism predicts a nearly frequency-independent birefringence angle, βν = β, while Faraday rotation from local magnetic fields and Lorentz violating theories predict a cosmic birefringence angle that is proportional to the frequency, ν, to the power of some integer n, βν ∝ νn. In this work, we first sampled βν individually for each polarized HFI frequency band in addition to the 70 GHz channel from the LFI. We also constrained a power law formula for the birefringence angle, βν = β0(ν/ν0)n, with ν0 = 150 GHz. For a nearly full-sky measurement, fsky = 0.93, we find β0 = 0.26° ±0.11° (68% C.L.) and n = −0.45−0.82+0.61 when we ignore the intrinsic EB correlations of the polarized foreground emission, and β0 = 0.33° ±0.12° and n = −0.37−0.64+0.49 when we use a filamentary dust model for the foreground EB. Next, we used all the polarized Planck maps, including the 30 and 44 GHz frequency bands. These bands have a negligible foreground contribution from polarized dust emission and we thus treated them separately. Without any modeling of the intrinsic EB of the foreground, we generally find that the inclusion of the 30 and 44 GHz frequency bands raises the measured values of βν and tightens n. At nearly full-sky, we measure β0 = 0.29°−0.11°+0.10° and n = −0.35−0.47+0.48. Assuming no frequency dependence, we measure β = 0.33° ±0.10°. If our measurements have effectively mitigated the EB of the foreground, our constraints are consistent with a mostly frequency-independent signal of cosmic birefringence.

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“…The current optical design for BINGO is based on a two mirror, off-axis, crossed Dragonian design (Dragone 1978;Tran et al 2008), which is very common in CMB experiments because it minimizes cross polarization (e.g., Poidevin et al 2018), so that the focal plane is at right angles to the incoming light, preserving the polarization of light. The primary mirror is a parabolic mirror with a focal length ( f ) of 140 m; the mirror is symmetric around its z axis and is a cut out of this parabola in the (x, y) plane centered at 226.54 m away from the origin with a diameter (D) of 40 m in this same (x, y) plane.…”

Section: Optical Model Definitionmentioning

confidence: 99%

The BINGO Project

Abdalla

Marins

Motta

et al. 2022

A&A

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Context. The Baryon Acoustic Oscillations from Integrated Neutral Gas Observations (BINGO) telescope was designed to measure the fluctuations of the 21 cm radiation arising from the hyperfine transition of neutral hydrogen. It is also aimed at measuring the baryon acoustic oscillations (BAO) from such fluctuations, thereby serving as a pathfinder to future, deeper intensity mapping surveys. The requirements for the Phase 1 of the projects consider a large reflector system (two 40 m-class dishes in a crossed-Dragone configuration) illuminating a focal plane with 28 horns to measure the sky, with two circular polarizations in a drift scan mode to produce measurements of the radiation in intensity (I) as well as the circular (V) polarization. Aims. In this paper, we present the optical design for the instrument. We describe the optical arrangement of the horns in the focal plane to produce a homogeneous and well-sampled map after the end of Phase 1, as well as the intensity and polarization properties of the beams. Our analysis provides an optimal model for the location of the horns in the focal plane, producing a homogeneous and Nyquist-sampled map after the nominal survey time. Methods. We used the GRASP package to model the focal plane arrangement and performed several optimization tasks to arrive at the current configuration, including an estimation of the sidelobes corresponding to the diffraction patterns of the two mirrors. The final model for the focal plane was defined through a combination of neural network and other direct optimization methods. Results. We arrived at an optimal configuration for the optical system that includes the focal plane positioning and the beam behavior of the instrument. We present an estimate of the expected sidelobes both for intensity and polarization, as well as the effect of band averaging on the final sidelobes, as well as an estimation of the cross-polarization leakage for the final configuration. Conclusions. We conclude that the chosen optical design meets the requirements for the project in terms of polarization purity and area coverage as well as a homogeneity of coverage so that BINGO can perform a successful BAO experiment. We further conclude that the requirements on the placement and rms error on the mirrors are also achievable so that a successful experiment can be conducted.

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The QUIJOTE Experiment: Prospects for CMB B-MODE polarization detection and foregrounds characterization

Cited by 7 publications

References 3 publications

Improved constraints on cosmic birefringence from the WMAP and Planck cosmic microwave background polarization data

Improved constraints on cosmic birefringence from the WMAP and Planck cosmic microwave background polarization data

Frequency-dependent constraints on cosmic birefringence from the LFI and HFI Planck Data Release 4

The BINGO Project

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