Sorption coolers using a continuous cycle to produce 20 K for the Planck flight mission

Bhandari, Pradeep; Prina, M.; Bowman, Robert C.; Paine, C.; Pearson, D.; Nash, Alfred

doi:10.1016/j.cryogenics.2004.02.022

Cited by 53 publications

(45 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…1) and the three bands of the LFI (Mennella et al 2011). The instrument uses a ∼20 K sorption cooler common to the HFI and the LFI (Planck Collaboration 2011b; Bhandari et al 2000Bhandari et al , 2004. The HFI focal plane unit is integrated inside the mechanical structure of the LFI, centered on the focal surface of a common off-axis Gregorian telescope (Tauber et al 2010a).…”

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

View full text Add to dashboard Cite

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.

show abstract

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

View full text Add to dashboard Cite

show abstract

“…In our work, we simulated a realistic periodic effect starting from the expected stability behaviour of the Planck sorption cooler (Bhandari et al 2004;Morgante et al 2009), which is the main cryogenic system on board the Planck satellite providing a 20 K stage for the LFI receivers and a 18 K precooling stage for the HFI 4 K cooler. The main frequencies of the temperature fluctuations depend on the (programmable) absorptiondesorption period of both each single compressor and the whole 6-compressor assembly.…”

Section: Periodic Systematic Effectmentioning

confidence: 99%

Effect of Fourier filters in removing periodic systematic effects from CMB data

Gasperin

Mennella

Maino

et al. 2011

A&A

View full text Add to dashboard Cite

We consider the application of high-pass Fourier filters to remove periodic systematic fluctuations from full-sky survey CMB datasets. We compare the filter performance with destriping codes commonly used to remove the effect of residual 1/f noise from timelines. As a realistic working case, we use simulations of the typical Planck scanning strategy and Planck Low Frequency Instrument noise performance, with spurious periodic fluctuations that mimic a typical thermal disturbance. We show that the application of Fourier high-pass filters in chunks always requires subsequent normalisation of induced offsets by means of destriping. For a complex signal containing all the astrophysical and instrumental components, the result obtained by applying filter and destriping in series is comparable to the result obtained by destriping only, which makes the usefulness of Fourier filters questionable for removing this kind of effects.

show abstract

“…The hydrogen sorption cooler was designed and built expressly for Planck at NASA's Jet Propulsion Laboratory (USA) (Bhandari et al 2004;Pearson et al 2006); it directly cools the LFI low-noise amplifiers to their operating temperature while providing pre-cooling for the HFI cooler chain. The sorption cooler consists of two cold redundant units, each including a six-element sorption compressor and a Joule-Thomson (JT) expansion valve.…”

Section: Thermal Design and The Cryo-chainmentioning

confidence: 99%

Planckpre-launch status: ThePlanckmission

Tauber¹,

Mandolesi

Puget

et al. 2010

A&A

Self Cite

290

119

View full text Add to dashboard Cite

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.

show abstract

Sorption coolers using a continuous cycle to produce 20 K for the Planck flight mission

Cited by 53 publications

References 4 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

Effect of Fourier filters in removing periodic systematic effects from CMB data

Planckpre-launch status: ThePlanckmission

Contact Info

Product

Resources

About