<i>Planck</i>pre-launch status: HFI beam expectations from the optical optimisation of the focal plane

Maffei, B.; Noviello, F.; Murphy, John A.; Ade, Peter A. R.; Lamarre, J.-M.; Bouchet, F. R.; Brossard, J.; Catalano, A.; Colgan, R.; Gispert, R.; Gleeson, Emily; Haynes, C. V.; Jones, W. C.; Lange, A. E.; Longval, Y.; McAuley, Ian; Pajot, F.; Peacocke, T.; Pisano, G.; Puget, J.‐L.; Ristorcelli, I.; Savini, G.; Sudiwala, R.; Wylde, Richard; Yurchenko, V.B.

doi:10.1051/0004-6361/200912999

Cited by 37 publications

(45 citation statements)

References 29 publications

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“…As reported in Maffei et al (2010), the 545 GHz and 857 GHz channels are multimoded (more than one electromagnetic mode propagating through the horn antennas) and their optical beams are markedly non-Gaussian. Multimoded horns collect photons from the whole primary mirror but make a beam on the sky large enough to match the scanning strategy and the data rate of the CMB channels at lower frequency.…”

Section: Optical Beamsmentioning

confidence: 93%

Planckearly results. IV. First assessment of the High Frequency Instrument in-flight performance

Ade¹,

Aghanim²,

Ansari³

et al. 2011

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The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ∼30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10 (100 GHz), 7 (143 GHz), and 5 (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, the removal of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6−2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.

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Section: Optical Beamsmentioning

confidence: 93%

Planckearly results. IV. First assessment of the High Frequency Instrument in-flight performance

Ade¹,

Aghanim²,

Ansari³

et al. 2011

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139

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“…The corrugated feed horns exhibit some internal cross-polar response (Maffei et al 2010). GRASP simulations show that this cross-polar response is at the level of 0.1-0.5%, considerably smaller than the detector cross-polar response (2-5%).…”

Section: Cross-polar Response and Temperature-to-polarization Leakagementioning

confidence: 89%

“…This is of particular concern, because we measure the beam on a source with a roughly Rayleigh-Jeans SED, yet we use the effective beam window function to correct the CMB. Planck Collaboration VII (2014) described possible levels of this bias derived using GRASP calculations with the prelaunch telescope model (Maffei et al 2010;Tauber et al 2010). The pre-launch calculations did not agree well enough with the data to allow a direct application of the colour correction.…”

Section: Colour Correction Of the Beam Shapementioning

confidence: 99%

Planck2015 results

Adam

Ade

Aghanim

et al. 2016

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The Planck High Frequency Instrument (HFI) has observed the full sky at six frequencies (100, 143, 217, 353, 545, and 857 GHz) in intensity and at four frequencies in linear polarization (100, 143, 217, and 353 GHz). In order to obtain sky maps, the time-ordered information (TOI) containing the detector and pointing samples must be processed and the angular response must be assessed. The full mission TOI is included in the Planck 2015 release. This paper describes the HFI TOI and beam processing for the 2015 release. HFI calibration and map making are described in a companion paper. The main pipeline has been modified since the last release (2013 nominal mission in intensity only), by including a correction for the nonlinearity of the warm readout and by improving the model of the bolometer time response. The beam processing is an essential tool that derives the angular response used in all the Planck science papers and we report an improvement in the effective beam window function uncertainty of more than a factor of 10 relative to the 2013 release. Noise correlations introduced by pipeline filtering function are assessed using dedicated simulations. Angular cross-power spectra using data sets that are decorrelated in time are immune to the main systematic effects.

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“…A detailed description of the Planck telescope and the instrument optics is provided in Tauber et al (2010), Sandri et al (2010) and Maffei et al (2010). The LFI horns are situated in a ring around the HFI, see Fig.…”

Section: Opticsmentioning

confidence: 99%

“…telescope plus instruments; - Mandolesi et al (2010), describing programmatic aspects of the LFI and its development; - Bersanelli et al (2010), describing in detail the design of the LFI; - Mennella et al (2010), describing the test and calibration programme of the LFI at instrument and system levels prior to launch; - , describing the test and calibration of the LFI radiometer chains; - Sandri et al (2010), describing the design and test of the LFI optics; - Leahy et al (2010), describing the polarisation aspects of the LFI, and its expected performance in orbit; - Lamarre et al (2010), describing in detail the on-ground design, manufacture, test and performance of the HFI; - Pajot et al (2010), describing the test and calibration programme of the HFI prior to launch; - Ade et al (2010), describing the design, test and performance of the cryogenic elements of the HFI focal plane; - Holmes et al (2008), describing the design, manufacture and test of the HFI bolometers; - Maffei et al (2010), describing the design and test of the HFI optics; - Rosset et al (2010), describing the polarisation aspects of the HFI.…”

Section: Introductionmentioning

confidence: 99%

Planckpre-launch status: ThePlanckmission

Tauber¹,

Mandolesi

Puget

et al. 2010

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The European Space Agency's Planck satellite, launched on 14 May 2009, is the third-generation space experiment in the field of cosmic microwave background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity ( ΔT T ∼ 2 × 10 −6 ) and angular resolution (∼5 arcmin). Planck will provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the Universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the Milky Way as well as external galaxies and clusters of galaxies. The ability of Planck to measure polarization across a wide frequency range (30−350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight, not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a series which describes the technical capabilities of the Planck scientific payload. It is based on the knowledge gathered during the on-ground calibration campaigns of the major subsystems, principally its telescope and its two scientific instruments, and of tests at fully integrated satellite level. It represents the best estimate before launch of the technical performance that the satellite and its payload will achieve in flight. In this paper, we summarise the main elements of the payload performance, which is described in detail in the accompanying papers. In addition, we describe the satellite performance elements which are most relevant for science, and provide an overview of the plans for scientific operations and data analysis.

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Planckpre-launch status: HFI beam expectations from the optical optimisation of the focal plane

Cited by 37 publications

References 29 publications

Planckearly results. IV. First assessment of the High Frequency Instrument in-flight performance

Planckearly results. IV. First assessment of the High Frequency Instrument in-flight performance

Planck2015 results

Planckpre-launch status: ThePlanckmission

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