Initial test results on bolometers for the Planck high frequency instrument

Holmes, W. A.; Bock, J. J.; Crill, B. P.; Koch, T.; Jones, W. C.; Lange, A. E.; Paine, C.

doi:10.1364/ao.47.005996

Cited by 35 publications

(28 citation statements)

References 25 publications

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“…Other elements that composes a bolometer module have no impact on the goals of this paper so they are not discussed here. Details can be found in Holmes et al, 2008 10 .…”

Section: Hfi Bolometersmentioning

confidence: 99%

Characterization and Physical Explanation of Energetic Particles on Planck HFI Instrument

et al. 2014

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The Planck High Frequency Instrument (HFI) has been surveying the sky continuously from the second Lagrangian point (L2) between August 2009 and January 2012. It operates with 52 high impedance bolometers cooled at 100mK in a range of frequency between 100 GHz and 1THz with unprecedented sensivity, but strong coupling with cosmic radiation. At L2, the particle flux is about 5 cm −2 s −1 and is dominated by protons incident on the spacecraft. Protons with an energy above 40MeV can penetrate the focal plane unit box causing two different effects: glitches in the raw data from direct interaction of cosmic rays with detectors (producing a data loss of about 15% at the end of the mission) and thermal drifts in the bolometer plate at 100mK adding non-gaussian noise at frequencies below 0.1Hz. The HFI consortium has made strong efforts in order to correct for this effect on the time ordered data and final Planck maps. This work intends to give a view of the physical explanation of the glitches observed in the HFI instrument in-flight. To reach this goal, we performed several ground-based experiments using protons and α particles to test the impact of particles on the HFI spare bolometers with a better control of the environmental conditions with respect to the in-flight data. We have shown that the dominant part of glitches observed in the data comes from the impact of cosmic rays in the silicon die frame supporting the micro-machinced bolometric detectors propagating energy mainly by ballistic phonons and by thermal diffusion. The implications of these results for future satellite missions will be discussed.

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“…Other elements that composes a bolometer module have no impact on the goals of this paper so they are not discussed here. Details can be found in Holmes et al, 2008 10 .…”

Section: Hfi Bolometersmentioning

confidence: 99%

Characterization and Physical Explanation of Energetic Particles on Planck HFI Instrument

et al. 2014

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“…-Spider web bolometers (SWBs) (Bock et al 1995;Holmes et al 2008) and polarization sensitive bolometers (PSBs) (Jones et al 2003), which can reach the photon noise limit with sufficient bandwidth to enable scanning great circles on the sky at roughly 1 rpm. They offer a very low cross-section to cosmic rays that proves to be essential in this environment and with this sensitivity.…”

Section: Designmentioning

confidence: 99%

“…For the HFI bolometers, the thermal cutoff frequency is 20−50 Hz (Holmes et al 2008;Lamarre et al 2010;Pajot et al 2010). However, the time response of the HFI exhibits a slight low frequency excess response (LFER) that is typically less than one percent in excess of the response at 1 Hz.…”

Section: Low Frequency Excess Responsementioning

confidence: 99%

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

Ade¹,

Aghanim²,

Ansari³

et al. 2011

A&A

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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“…The bolometric detectors used in HFI (Holmes et al 2008) are located in a λ/4 cavity at the exit of the detector horn waveguide. For the spider-web bolometers (SWB − Bock et al 1995;Yun et al 2004), used for the unpolarised channels, crosspolarisation is not an issue and efficiency optimisation of the radiation coupling between the horn and the detector is the main concern.…”

Section: Detector Horn Coupling To Bolometermentioning

confidence: 99%

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

Maffei¹,

Noviello

Murphy

et al. 2010

A&A

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Planck is a European Space Agency (ESA) satellite, launched in May 2009, which will map the cosmic microwave background anisotropies in intensity and polarisation with unprecedented detail and sensitivity. It will also provide full-sky maps of astrophysical foregrounds. An accurate knowledge of the telescope beam patterns is an essential element for a correct analysis of the acquired astrophysical data. We present a detailed description of the optical design of the High Frequency Instrument (HFI) together with some of the optical performances measured during the calibration campaigns. We report on the evolution of the knowledge of the pre-launch HFI beam patterns when coupled to ideal telescope elements, and on their significance for the HFI data analysis procedure.

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Initial test results on bolometers for the Planck high frequency instrument

Cited by 35 publications

References 25 publications

Characterization and Physical Explanation of Energetic Particles on Planck HFI Instrument

Characterization and Physical Explanation of Energetic Particles on Planck HFI Instrument

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

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

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