<i>Planck</i>pre-launch status: High Frequency Instrument polarization calibration

Rosset, C.; Tristram, M.; Ponthieu, N.; Ade, Peter A. R.; Aumont, J.; Catalano, A.; Conversi, L.; Couchot, F.; Crill, B. P.; Désert, F.‐X.; Ganga, K.; Giard, M.; Giraud‐Héraud, Y.; Haïssinski, J.; Henrot-Versillé, S.; Holmes, W. A.; Jones, W. C.; Lamarre, J.-M.; Lange, A. E.; Leroy, C.; Macías-Pérez, J. F.; Maffei, B.; Marcillac, P. de; Miville-Deschênes, M.-A.; Montier, L.; Noviello, F.; Pajot, F.; Perdereau, O.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, É.; Puget, J.‐L.; Ristorcelli, I.; Savini, G.; Sudiwala, R.; Veneziani, M.; Yvon, D.

doi:10.1051/0004-6361/200913054

Cited by 90 publications

(49 citation statements)

References 34 publications

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“…This analysis confirms that such an instrumental angle is compatible with zero but unfortunately does not favor an update of the ground-based parameters given in Ref. 17. Therefore, currently how to go beyond Ref.…”

Section: Conclusion and Discussionsupporting

confidence: 70%

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Cosmological birefringence constraints from the Planck 2015 CMB likelihood

Gruppuso

2016

Int. J. Mod. Phys. D

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The Planck 2015 cosmic microwave background (CMB) likelihood is employed to constrain the cosmological birefringence angle, i.e. the in vacuo rotation of the linear polarization that CMB photons would experience during propagation in case of parity violating coupling within the electromagnetic sector of the Standard Model of particle physics. We find α = 0.0 • ± 1.3 • (stat) ± 1 • (sys) which is well compatible with no parity violation mechanism in action from recombination epoch to present.

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Section: Conclusion and Discussionsupporting

confidence: 70%

“…Therefore, currently how to go beyond Ref. 17 remains an open question and it is possible that the systematic uncertainty in the polarization angle will dominate the error budget of future Planck data releases.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Cosmological birefringence constraints from the Planck 2015 CMB likelihood

Gruppuso

2016

Int. J. Mod. Phys. D

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“…where the quantities F i are the total flux density measured for bolometer i, and ψ i and ρ i are the angles of polarization sensitivity and polarization efficiencies of the bolometers, respectively (Rosset et al 2010). For the majority of the planet observations, the degree of polarization (defined as p ≡ Q 2 + U 2 /I) is consistent with zero to within the errors in the total flux measurements.…”

Section: Polarized Flux Density Of Planetsmentioning

confidence: 92%

Planckintermediate results

Akrami

Ashdown

Aumont

et al. 2017

A&A

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Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of β ring = 2.30 ± 0.03 over the 30-1000 GHz frequency range. Estimates of the polarization amplitude of the planets have also been made in the four bands that have polarizationsensitive detectors (100-353 GHz); this analysis provides a 95 % confidence level upper limit on Mars's polarization of 1.8, 1.7, 1.2, and 1.7 % at 100, 143, 217, and 353 GHz, respectively. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 0.997, 0.997, 1.018, and 1.032 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent-level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2 %. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.

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“…For Planck-HFI, we consider several uncertainties associated to the measurement of the Crab polarisation angle. We refer to the pre-flight errors on the absolute calibration of the polarisation angle [13] as the ground calibration error. These absolute calibration errors were later refined at 100, 143 and 217 GHz in [14] using C T B and C EB minimisation, for which no cosmological signal is expected in the abscence of parity violating processes.…”

Section: Crab Polarisation Angle Measurementsmentioning

confidence: 99%

Absolute calibration of the polarisation angle for future CMB B-mode experiments from current and future measurements of the Crab nebula

Aumont

Macías-Pérez

Ritacco

et al. 2020

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A tremendous international effort is currently dedicated to observing the so-called primordial B modes of the Cosmic Microwave Background (CMB) polarisation. If measured, this faint signal imprinted by the primordial gravitational wave background, would be an evidence of the inflation epoch and quantify its energy scale, providing a rigorous test of fundamental physics far beyond the reach of accelerators. At the unprecedented sensitivity level that the new generation of CMB experiments aims to reach, every uncontrolled instrumental systematic effect will potentially result in an analysis bias that is larger than the much sought-after CMB B-mode signal. The absolute calibration of the polarisation angle is particularly important in this sense, as any associated error will end up in a leakage from the much larger E modes into B modes. The Crab nebula (Tau A), with its bright microwave synchrotron emission, is one of the few objects in the sky that can be used as absolute polarisation calibrators. In this communication, we review the best current constraints on its polarisation angle from 23 to 353 GHz, at typical angular scales for CMB observations, from WMAP, IRAM XPOL, Planck and NIKA data. We will show that these polarisation angle measurements are compatible with a constant angle and we will present a study of the uncertainty on this mean angle, making different considerations on how to combine the individual measurement errors. For each of the cases, the potential impact on the CMB B-mode spectrum will be explored. *

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Planckpre-launch status: High Frequency Instrument polarization calibration

Cited by 90 publications

References 34 publications

Cosmological birefringence constraints from the Planck 2015 CMB likelihood

Cosmological birefringence constraints from the Planck 2015 CMB likelihood

Planckintermediate results

Absolute calibration of the polarisation angle for future CMB B-mode experiments from current and future measurements of the Crab nebula

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