A new readout system for bolometers with improved low frequency
stability

Gaertner, S.; Benoı̂t, A.; Lamarre, J.-M.; Giard, M.; Bret, J. L.; Chabaud, J. P.; Désert, F.‐X.; Faure, J.-P.; Jegoudez, G.; Lande, J.; Leblanc, J.; Lepeltier, J. P.; Narbonne, J.; Piat, M.; Pons, R.; Serra, G.; Simiand, G.

doi:10.1051/aas:1997256

Cited by 25 publications

(25 citation statements)

References 9 publications

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“…-The 4 He-JT cooler, an active cooler for 4 K (Bradshaw & Orlowska 1997) using vibration controlled mechanical compressors to prevent excessive warming of the 100 mK stage and minimize microphonic effects in the bolometers. -AC biased readout electronics that provide high sensitivity and low frequency stability (Rieke et al 1989;Gaertner et al 1997). -A thermo-optical design consisting of three corrugated horns and a set of compact reflective filters and lenses at cryogenic temperatures (Church et al 1996).…”

Section: Designmentioning

confidence: 99%

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

Ade¹,

Aghanim²,

Ansari³

et al. 2011

A&A

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139

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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: Designmentioning

confidence: 99%

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

Ade¹,

Aghanim²,

Ansari³

et al. 2011

A&A

Self Cite

139

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“…The planets Mars, Jupiter, and Saturn are expected to be extremely bright compared to the ambient optical background and will drive the bolometers nonlinear. In the case of HFI's readout electronics (Gaertner et al 1997), a drop in bolometer resistance always leads to a state of "overcompensation" for the transient compensation. The average signal over a readout cycle will not drop as much as in a DC biasing scheme, mitigating the effect of bolometer nonlinearity.…”

Section: Detector Propertiesmentioning

confidence: 99%

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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“…A specially developed amplifier [11] using tunable AC bias and cold J-FET preamplifier shows a 5 nVHz" 172 noise down to 10" 2 Hz.…”

Section: Requirements and Design Of Hfi Detection Systemmentioning

confidence: 99%

Use of high sensitivity bolometers for astronomy: Planck high frequency instrument

Lamarre

Piat

Bock

et al. 2002

AIP Conference Proceedings

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Abstract. The Planck satellite is dedicated to the measurement of the anisotropy of the Cosmic Microwave Background (CMB) with unprecedented sensitivity and angular resolution. It is a project of the European Space Agency based on a wide international collaboration, including United States and Canadian laboratories. The detectors of its High Frequency Instrument (HFI) are bolometers cooled down to 100 mK. Their sensitivity will be limited by the photon noise of the CMB itself at low frequencies, and of the instrument background at high frequencies. The requirements on the measurement chain are directly related to the strategy of observation used for the satellite. This impacts the bolometer design as well as other elements: The cooling system must present outstanding temperature stability, and the amplification chain must show a flat noise spectrum down to very low frequencies.

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A new readout system for bolometers with improved low frequency stability

Cited by 25 publications

References 9 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

Measuring Planck beams with planets

Use of high sensitivity bolometers for astronomy: Planck high frequency instrument

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