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Burigana, C.; Natoli, P.; Vittorio, N.; Mandolesi, N.; Bersanelli, M.

doi:10.1023/a:1016338603042

Cited by 43 publications

(71 citation statements)

References 3 publications

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“…The code developed by Burigana et al (1997b) and Maino et al (1999) has been used to generate maps from TODs. With this code it is also possible to significantly reduce correlated systematic effects as the 1/ f α noise stripes from the data before generating the final maps.…”

Section: Simulation Toolsmentioning

confidence: 99%

The effect of signal digitisation in CMB experiments

Maris

Maino

Burigana

et al. 2004

A&A

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Abstract. Signal digitisation may produce significant effects in balloon -borne or space CMB experiments, when the limited bandwidth for downlink of data requires loss-less data compression. In fact, the data compressibility depends on the quantization step q applied on board by the instrument acquisition chain. In this paper we present a study of the impact of the quantization error in CMB experiments using, as a working case, simulated data from the P/LFI 30 and 100 GHz channels. At TOD level, the effect of the quantization can be approximated as a source of nearly normally distributed noise, with RMS q/ √ 12N s , with deviations from normality becoming relevant for a relatively small number of repeated measures N s < ∼ 20. At map level, the data quantization alters the noise distribution and the expectation of some higher order moments. We find a constant ratio, 1/( √ 12σ/q), between the RMS of the quantization noise and RMS of the instrumental noise, σ over the map ( 0.14 for σ/q 2), while, for σ/q ∼ 2, the bias on the expectation for higher order moments is comparable to their sampling variances. Finally, we find that the quantization introduces a power excess, C ex , that, although related to the instrument and mission parameters, is weakly dependent on the multipole at middle and large and can be quite accurately subtracted. For σ/q 2, the residual uncertainty, ∆C ex , implied by this subtraction is only 1-2% of the RMS uncertainty, ∆C noise , on C sky reconstruction due to the noise power, C noise . Only for < ∼ 30 the quantization removal is less accurate; in fact, the 1/ f noise features, although efficiently removed, increase C noise , ∆C noise , C ex and then ∆C ex ; anyway, at low multipoles C sky ∆C noise > ∆C ex . This work is based on P LFI activities.

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Section: Simulation Toolsmentioning

confidence: 99%

The effect of signal digitisation in CMB experiments

Maris

Maino

Burigana

et al. 2004

A&A

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“…The normalized sensitivity per pixel in the sky (i.e., the sensitivity divided by the averaged sensitivity of the observed pixels in the sky) for a typical Planck Planck sensitivity relevant for moving bodies and variable sources can be found in (Burigana 2000) and . For the LFI sensitivities we take into account the most recent computations of the LFI beam positions of the telescope field of view (Sandri & Villa 2001).…”

Section: Planck Performancesmentioning

confidence: 99%

Asteroid detection at millimetric wavelengths with the PLANCK survey

Cremonese

Marzari

Burigana³

et al. 2002

New Astronomy

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“…successfully by Burigana et al 2000). This approach also proves convenient for studying some effects (e.g.…”

Section: Beam Fitting Methodsmentioning

confidence: 93%

Measuring Planck beams with planets

Huffenberger

Crill

Lange

et al. 2010

A&A

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Aims. Accurate measurement of the cosmic microwave background (CMB) anisotropy requires precise knowledge of the instrument beam. We explore how well the Planck beams will be determined from observations of planets, developing techniques that are also appropriate for other experiments. Methods. We simulate planet observations with a Planck-like scanning strategy, telescope beams, noise, and detector properties. Then we employ both parametric and non-parametric techniques, reconstructing beams directly from the time-ordered data. With a faithful parameterization of the beam shape, we can constrain certain detector properties, such as the time constants of the detectors, to high precision. Alternatively, we decompose the beam using an orthogonal basis. For both techniques, we characterize the errors in the beam reconstruction with Monte Carlo realizations. For a simplified scanning strategy, we study the impact on estimation of the CMB power spectrum. Finally, we explore the consequences for measuring cosmological parameters, focusing on the spectral index of primordial scalar perturbations, n s .Results. The quality of the power spectrum measurement will be significantly influenced by the optical modeling of the telescope. In our most conservative case, using no information about the optics except the measurement of planets, we find that a single transit of Jupiter across the focal plane will measure the beam window functions to better than 0.3% for the channels at 100-217 GHz that are the most sensitive to the CMB. Constraining the beam with optical modeling can lead to much higher quality reconstruction. Conclusions. Depending on the optical modeling, the beam errors may be a significant contribution to the measurement systematics for n s .

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Untitled

Cited by 43 publications

References 3 publications

The effect of signal digitisation in CMB experiments

The effect of signal digitisation in CMB experiments

Asteroid detection at millimetric wavelengths with the PLANCK survey

Measuring Planck beams with planets

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