Impact of beam deconvolution on noise properties in CMB measurements: Application to<i>Planck</i>LFI

Keihänen, E.; Kiiveri, K.; Lindholm, V.; Reinecke, M.; Suur-Uski, A.-S.

doi:10.1051/0004-6361/201526848

Cited by 4 publications

(4 citation statements)

References 18 publications

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“…Even after destriping, a small amount of residual correlated noise is still present; this adds to the signal power in the lowest multipoles. The properties of residual noise, and its effect on deconvolution, are addressed in Keihänen et al (2016). Deconvolution amplifies the noise in the high-multipole regime of the angular power spectrum, and creates correlation between neighbouring pixels.…”

Section: Input Toimentioning

confidence: 99%

Beam-deconvolved Planck LFI maps

Keihänen

Lindholm

López‐Caniego

et al. 2019

A&A

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The Planck Collaboration made its final data release in 2018. In this paper we describe beam-deconvolution map products made from Planck LFI data using the artDeco deconvolution code to symmetrize the effective beam. The deconvolution results are auxiliary data products, available through the Planck Legacy Archive. Analysis of these deconvolved survey difference maps reveals signs of residual signal in the 30-GHz and 44-GHz frequency channels. We produce low-resolution maps and corresponding noise covariance matrices (NCVMs). The NCVMs agree reasonably well with the half-ring noise estimates except for 44 GHz, where we observe an asymmetry between EE and BB noise spectra, possibly a sign of further unresolved systematics.

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Section: Input Toimentioning

confidence: 99%

Beam-deconvolved Planck LFI maps

Keihänen

Lindholm

López‐Caniego

et al. 2019

A&A

Self Cite

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“…For a perfectly circular beam profile, B(γ, γ ) ≡ B(γ • γ ), assumed in this work, it is easy to deconvolve the effect of the beam after inferring the power spectra. However, if the beam is not circular symmetric then the effect of the beam depends on the full scan pattern of the experiment and its deconvolution may be non-trivial [3,4,[27][28][29].…”

Section: A Brief Review Of Biposh Representationmentioning

confidence: 99%

Bayesian inference on the sphere beyond statistical isotropy

Das¹,

Wandelt²,

Souradeep³

2015

J. Cosmol. Astropart. Phys.

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Abstract. We present a general method for Bayesian inference of the underlying covariance structure of random fields on a sphere. We employ the Bipolar Spherical Harmonic (BipoSH) representation of general covariance structure on the sphere. We illustrate the efficacy of the method as a principled approach to assess violation of statistical isotropy (SI) in the sky maps of Cosmic Microwave Background (CMB) fluctuations. SI violation in observed CMB maps arise due to known physical effects such as Doppler boost and weak lensing; yet unknown theoretical possibilities like cosmic topology and subtle violations of the cosmological principle, as well as, expected observational artefacts of scanning the sky with a non-circular beam, masking, foreground residuals, anisotropic noise, etc. We explicitly demonstrate the recovery of the input SI violation signals with their full statistics in simulated CMB maps. Our formalism easily adapts to exploring parametric physical models with non-SI covariance, as we illustrate for the inference of the parameters of a Doppler boosted sky map. Our approach promises to provide a robust quantitative evaluation of the evidence for SI violation related anomalies in the CMB sky by estimating the BipoSH spectra along with their complete posterior.arXiv:1509.07137v1 [astro-ph.CO]

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Section: A Brief Review Of Biposh Representationmentioning

confidence: 99%

Bayesian inference on the sphere beyond statistical isotropy

Das,

Wandelt,

Souradeep

2015

Preprint

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We present a general method for Bayesian inference of the underlying covariance structure of random fields on a sphere. We employ the Bipolar Spherical Harmonic (BipoSH) representation of general covariance structure on the sphere. We illustrate the efficacy of the method as a principled approach to assess violation of statistical isotropy (SI) in the sky maps of Cosmic Microwave Background (CMB) fluctuations. SI violation in observed CMB maps arise due to known physical effects such as Doppler boost and weak lensing; yet unknown theoretical possibilities like cosmic topology and subtle violations of the cosmological principle, as well as, expected observational artefacts of scanning the sky with a non-circular beam, masking, foreground residuals, anisotropic noise, etc. We explicitly demonstrate the recovery of the input SI violation signals with their full statistics in simulated CMB maps. Our formalism easily adapts to exploring parametric physical models with non-SI covariance, as we illustrate for the inference of the parameters of a Doppler boosted sky map. Our approach promises to provide a robust quantitative evaluation of the evidence for SI violation related anomalies in the CMB sky by estimating the BipoSH spectra along with their complete posterior.

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Impact of beam deconvolution on noise properties in CMB measurements: Application toPlanckLFI

Cited by 4 publications

References 18 publications

Beam-deconvolved Planck LFI maps

Beam-deconvolved Planck LFI maps

Bayesian inference on the sphere beyond statistical isotropy

Bayesian inference on the sphere beyond statistical isotropy

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