Difference between revisions of "HFI design, qualification, and performance"

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[[Category:Instruments]]
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This section provides an overview of the High-Frequency Instrument and of its different sub-systems. Two papers that include and detail this information are available: {{PlanckPapers|lamarre2010}} and {{PlanckPapers|planck2011-1-5}}. Additional detailed information potentially useful for users of HFI data is included in this section or annexed to it.
  
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THIS SECTION IS CURRENTLY IN A VERY PRELIMINARY FORM. It is intended to provide an overview of the instrument and of its different sub-systems. Two papers that include and detail this information are available: LAMARRE, Jean-Michel, PUGET, Jean-Loup et 93 co-auteurs, " Planck pre-launch status: The HFI instrument, from specification to actual performance", Astronomy and Astrophysics, Volume 520, id.A9 (20 pages, A&A Homepage), 09/2010. and Planck-HFI Core Team and 165 co-authors. " Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance", Astronomy & Astrophysics, Volume 536, id.A4 (A&A Homepage) 12/2011." Additional detailed information potentially useful for the use of the HFI data will be included into this section or annexed to it.
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[[Image:HFI_2_4_1_JML_TheElectronicsAndServiceModule.png|thumb|500px|center|HFI electronics in the satellite]]
  
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==HFI high level description and Architecture==
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The HFI instrument is designed around 52 bolometers. Twenty of the bolometers (spider-web bolometers or SWBs) are sensitive to total power, and the remaining 32 units are arranged in pairs of orthogonally-oriented polarisation-sensitive bolometers (PSBs). All bolometers are operated at a temperature of ~0.1 K by means of a space qualified dilution cooler coupled to a high precision temperature control system. A 4He-JT system provides active cooling for 4 K stages using vibration controlled mechanical compressors to prevent excessive warming of the 100 mK stage and minimize microphonic effects in the bolometers. Bolometers and sensitive thermometers are read using an AC-bias scheme through JFET amplifiers operated at ~130 K that provide high sensitivity and low frequency stability. The HFI covers six bands centred at 100, 143, 217, 353, 545, and 857 GHz, thanks to a thermo-optical design consisting of three corrugated horns and a set of compact reflective filters and lenses at cryogenic temperatures.
  
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<span style="color:red">(Lamarre/Pajot)</span>
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[[Image:HFI_horns.jpg|thumb|500px|center|HFI focal plane optics and 4K thermo-mechanical stage.]]
  
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The HFI instrument is designed around 52 bolometers. Twenty of the bolometers (spider-web bolometers or SWBs) are sensitive to total power, and the remaining 32 units are arranged in pairs of orthogonally-oriented polarisation-sensitive bolometers (PSBs). All bolometers are operated at a temperature of ~0.1 K by mean of a space qualified dilution cooler coupled with a high precision temperature control system. A 4He-JT provides an active cooling for 4 K stages using vibration controlled mechanical compressors to prevent excessive warming of the 100 mK stage and minimize microphonic effects in the bolometers. Bolometers and sensitive thermometers are read using AC-bias scheme through JFET amplifiers operated at ~130 K that provide high sensitivity and low frequency stability. The HFI covers six bands centred at 100, 143, 217, 353, 545 and 857 GHz, thanks to a thermo-optical design consisting of three corrugated horns and a set of compact reflective filters and lenses at cryogenic temperatures.
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The whole satellite is organized to provide thermal transitions between its warm part exposed to radiation from the Sun and Earth, and the focal plane instruments that include the cold receivers (Sections [[HFI_cold_optics]] and [[HFI_detection_chain]]). The various parts of the HFI are distributed among three different stages of the satellite in order to provide each sub-system with an optimal operating temperature. The "warm" parts, including nearly all the electronics and the sources of fluids of the 4K and 0.1K coolers, are attached and thermally linked to the service module of the satellite. The first stage of the preamplifiers is attached to the back of the passively cooled telescope structure. The focal plane unit is attached to the 20K stage cooled by the sorption cooler. This is detailed in Section [[HFI_detection_chain]].  
  
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The whole satellite is organized to provide thermal transitions between its warm part exposed to the sun and earth radiation, and the focal plane instruments that include the cold receivers (Sections XXX1 and XXX2). The various parts of the HFI are distributed among three different stages of the satellite in order to provide each sub-system an optimal operating temperature. The "warm" parts, including nearly all the electronics and the sources of fluids of the 4K and 0.1K coolers, are attached and thermally linked to the service module of the satellite. The first stage of the preamplifiers is attached to the back of the passively cooled telescope structure. The focal plane unit is attached to the 20K stage cooled by the sorption cooler. This is detailed in (XXX2).  
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The telescope and horns select the geometrical origin of photons. They provide a high transmission efficiency to photons inside the main beam, while photons coming from the intermediate and far-side lobes have very low probability of being detected. The essential characteristics are determined by a complex process mixing ground measurements of components (horns, reflectors), modelling the shape of the far sidelobes, and measuring bright sources in-flight, especially planets.  
  
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The filters and bolometers define the spectral response and absolute optical efficiency, which are known mostly from ground-based measurements performed at component, sub-system, and system levels, reported in this document. The relationships between spectral response and geometrical response are also addressed.
  
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[[Image:HFI_2_4_1_JML_HFI_in_Planck.png|thumb|500px|FIGURE 2.4.1.1.a_HFI_parts_in_the_satellite]]
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Photons absorbed by a bolometer include the thermal radiation emitted by the various optical devices: telescope, horns, and filters. They are transformed into heat that propagates to the bolometer thermometer to influence its temperature, which is itself measured by the readout electronics. Temperatures of all these items must be stable enough not to contaminate the scientific signal delivered by the bolometers. How this stability is reached is described in Section [[HFI_cryogenics]].
  
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The bolometer temperature depends also on the temperature of the bolometer plate, on the intensity of the biasing current, and on any spurious inputs, such as cosmic rays and mechanical vibrations. Such systematics are included in a list discussed in Section [[HFI-Validation]].
  
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[[Image:HFI_2_4_1_JML_TheElectronicsAndServiceModule.png|thumb|500px|FIGURE 2.4.1.1.b_HFI_electronics_in_the_satellite]]
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Since the bolometer thermometer is part of an active circuit that also heats it, the response of this system is complex and has to be considered as a whole. In addition, due to the modulation of the bias current and to the sampling of the data, the response signal of the instrument when scanning a point source is more complex still. Item in Sub-Section [[HFI_detection_chain#Time_response|Time_response]] and Annex [[HFI_time_response_model]] are dedicated to the description of this time response.
  
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The telescope and horns selects the geometrical origin of photons. They provide a high transmission efficiency to photons inside the main beam, while photons coming from the intermediate and far-side lobes have very low probability of being detected. This essential characteristics is known by a complex process mixing ground measurements of components (horns, reflectors), modelling the shape of the far side lobes, and measuring in-flight bright sources, especially planets.  
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[[Image:HFI_2_4_1_JML_SignalFormation.png|thumb|500px|center|HFI signal formation.]]
  
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The filters and bolometers define the spectral responses and absolute optical efficiency, that will be known mostly from ground based measurements performed at component, sub-system and system levels reported in this document. The relations between spectral response and geometrical response will also be addressed.
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Logic of the formation of the signal in HFI. This is an idealized description of the physics that takes place in the instrument. The optical power that is absorbed by the bolometers comes from the observed sky and from the instrument itself. The bolometers and readout electronics, acting as a single and complex chain, transform this optical power into data that are compressed and transmitted for science data reduction.
  
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Photons absorbed by a bolometer include the thermal radiation emitted by the various optical devices: telescope, horns and filters. They are transformed in heat that propagates to the bolometer thermometer and influence its temperature which is itself measured by the readout electronics. Temperatures of all these items must stable enough not to contaminate the scientific signal delivered by the bolometers. How this stability is reached is described in section 2.4.1_cryogeny.
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<div style="clear: both"></div>
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== References ==
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<References />
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The bolometer temperature depends also on the temperature of the bolometer plate, on the intensity of the biasing current and on any spurious inputs, such as cosmic rays and mechanical vibrations. Such systematics are included in the list of section 2.4.1._systematics.
 
  
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Since the bolometer thermometer is part of an active circuitry that also heats it, the response of this system is complex and has to be considered as a whole. In addition, due to the modulation of the bias current and to the sampling of the data, a complex time response is expected, which modifies the beam shape resulting from the scanning of point sources. Section 2.4.1._time response is dedicated to the description of the time response.
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[[Category:HFI design, qualification and performance|000]]
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[[Image:HFI_2_4_1_JML_SignalFormation.png|thumb|500px|FIGURE 2.4.1.1.C_HFI signal formation]]
 
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Figure 2.4.1.1_HFI signal formation: Logic of the formation of the signal in HFI. This is an idealized description of the physics that takes place in the instrument. The optical power that is absorbed by the bolometers comes from the observed sky and from the instrument itself. The bolometers and readout electronics, acting as a single and complex chain, transform this optical power in data that is compressed and transmitted for science data reduction.
 
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==Cryogenics==
 
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<span style="color:red">(F .Pajot)</span>
 
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===Dilution===
 
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The HFI 3He-4He dilution cooler produces temperatures of 0.1 K for the bolometers through
 
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the dilution of 3He into 4He and 1.4 K through JT expansion of the 3He and 4He mixture. The
 
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dilution cooler is described in detail in section 2.3.3 of {{PEarly|2|page=7}}.
 
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The dilution was operated with flows set to the minimum available values, and provided a total
 
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lifetime of 30.5 months, exceeding the nominal lifetime of 16 months by 14.5 months. The
 
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dilution stage was stabilized by a PID control with a regulating power between 20 and 30 nW
 
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providing a temperature close to 101 mK. The bolometer plate was stabilized at 102.8 mK with a
 
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PID regulating power around 5 nW. The cooling power values were in very good agreement with those obtained during the ground tests and calibration.
 
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However, the cosmic particles interactions with the 100 mK stages induced temperature fluctuations and glitches on the thermometers measurements.
 
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The decorrelation of 100 mK bolometer stage temperatures fluctuations from the bolometers signals is described in section 4.4.2.
 
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[[Image:HFI_2_4_1_100mK_stability.png|thumb|500px|100 mK stages temperatures during the mission]]
 
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(here a few lines of 100 mK boloplate stability)
 
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[[Image:HFI_2_4_1_1_6K_stability.png|thumb|500px|1.6K stage temperatures during the mission]]
 
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Detailed analysis of the in-flight stability of the
 
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dilution cooler can be found in section
 
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5.4 of {{PEarly|2|page=23}}.
 
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=== 4K J-T cooler ===
 
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The HFI 4K J-T cooler produces a temperature of
 
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4K for the HFI 4K stage and optics and the
 
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precooling of the dilution gases. Full
 
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description of the 4K cooler can be found in
 
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in section 2.3.2 of {{PEarly|2|page=7}}.
 
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The 4K cooler was operated without interruption
 
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during all the survey phase of the mission. It is
 
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still in operation as it also provides the
 
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cooling of the optical reference loads of the
 
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LFI. The 4K PID stabilizing the temperature of
 
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the HFI optics is regulated at 4.81 K using a
 
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power around 1.8 mW.
 
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[[File:HFI_2_4_1_4K_stability.png|500px|4K stage temperatures during the mission]]
 
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(here a few lines of 4K stability, including compressors operation)
 
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Details on the in-flight performance of the
 
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4K J-T cooler can be found in in section
 
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5.3 of {{PEarly|2|page=21}}.
 
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== Cold optics ==
 
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<span style="color:red">(Lamarre)</span>
 
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=== Horns,lenses===
 
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links to Peter's paper
 
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=== filters, band===
 
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Includes Locke's very detailed document.
 
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Raw inclusion of Locke Spencer section following JML instructions (22-oct2012)
 
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http://www.sciops.esa.int/wikiSI/planckpla/index.php?title=HFI_Detector_Spectral_Response
 
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=== Abstract ===
 
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This section is comprised of excerpts from the ''HFI - Spectral Calibration report of the IAS measurements, v3.00,'' an internal report describing detailed pre-flight ground based measurements of the HFI focal plane.  The experimental setup, data collection, and related data processing are described.  The official version of the HFI detector spectral transmission profiles is available within the HFI instrument model and the RIMO files in the Planck Legacy archive  <span style="color:#000000; background:#FF0000"> [ref.] </span>.  This data is comprised of broadband Fourier transform spectrometer (FTS) measurements conducted with the HFI focal plane assembly as described above, and includes a waveguide model for the low frequency spectral region, and component-level filter spectra for the remaining out of band spectral regions. Specific attention is given to in-band and near-band spectral regions surrounding CO rotational transitions in order to support the CO extraction component separation effort <span style="color:#000000; background:#FF0000"> [ref.] </span>.  The spectral transmission profiles are evaluated with parameters such as cut-on, cut-off, centre frequency, effective frequency (including spectral index), and band-width are provided in the analysis.  Further evaluation yields band-average spectra (<span style="color:#000000; background:#FF0000"> [ref.] </span>) and unit conversion / colour correction coefficients (<span style="color:#000000; background:#FF0000"> [ref.] </span>) and software routines (<span style="color:#000000; background:#FF0000"> [ref.] </span>). 
 
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=== Objectives ===
 
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The main goal of the spectral transmission tests of the HFI instrument is to measure the spectral response of all HFI detectors to a known source of EM radiation individually. This was determined by measuring the interferometric output of all detection channels for radiation propagated through a continuously scanned polarising fourier transform spectrometer (FTS). The required accuracy to which the spectral transmission is to be recovered is 1<math>\%</math> (see §[[#Conformity with requirements|Req.]]).
 
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It is important to note that the absolute spectral calibration cannot be achieved solely from the analysis of the FTS data because of uncertainties in the coupling efficiency of the FTS source through the FTS, input optics, and integrating sphere. The relative FTS measurements must be combined with the optical efficiency tests  which used internal black-body sources (EFF Test – see §[[#Optical Efficiency|EFF]]).
 
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=== Description of setup ===
 
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<!-- [sec:setup] -->
 
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A brief description of the optical setup used for the spectral characterisation of the HFI instrument performed at the FPU level in the Saturne calibration facility at IAS is provided here. Further details are available from the pre-launch calibration papers . The spectrometer configuration is based on a polarizing Fourier transform interferometer, feeding an integrating sphere inside the Saturne tank (Figs. [fig:Optical-layout-of] &amp; and [fig:Top-view-of]). The output of the integrating sphere is conjugated by a mirror with the focal plane of the HFI. Therefore data are acquired simultaneously on all pixels while the moveable mirror in the external FTS is scanned.
 
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[[Image:fig3.png|thumb|600px|Internal optical layout of the FTS.]]
 
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<!-- |alt=Optical schematic of the FTS.]] -->
 
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[[Image:fig4.png|thumb|600px|FTS/ELS assembly with Saturne cryostat.]]
 
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[[Image:fig1.png|thumb|600px|Optical layout of the FTS with respect to the Saturne cryostat.]]
 
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[[Image:fig2.png|thumb|600px|Top view of 2K optical setup inside Saturne cryostat.]]
 
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An external light source system (ELS, see Fig.[fig:FTS/ELS-assembly-with]) is provided in addition to the FTS for time constant measurements. Selection between the FTS and the ELS is done by the M1 flip mirror.
 
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The polarising FTS was provided by Sciencetech Inc. (Canada) under contract with IAS and ESA (Fig.[fig:Internal-optical-layout]). The source can be selected from either a Hg vapour arc lamp or a globar. The 300 mm translation stage allows symmetric interferograms with a maximum theoretical (unapodized) Instrument Line Shape (ILS) Full-Width-at-Half-Maximum (FWHM) resolution of <math>0.020~\mbox{cm}^{-1}</math>. Filtering of short wavelength is done on the optical path entering the Saturne cryostat as follows:
 
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* Saturne vacuum window is polyethylene (6mm thick)
 
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* <math>1^{st}</math> thermal fiter at 300K
 
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* <math>2^{nd}</math> thermal filter at 77K
 
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* <math>46~\mbox{cm}^{-1}</math>filter at 77K
 
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* <math>3^{rd}</math> thermal filter at 20K
 
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* filter wheel at 2K (Fig. [fig:2K-filter-wheel]) with selection of: open, closed, <math>35~\mbox{cm}^{-1}</math> or <math>10~\mbox{cm}^{-1}</math>filter
 
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FIXME: typo in figure
 
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[[Image:fig5.png|thumb|600px|2K filter wheel on FTS optical path.]]
 
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FIXME: typo in figure
 
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[[Image:fig6.png|thumb|600px|Saturne integrating sphere and HFI focal plane.]]
 
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The optical flux from the FTS enters the integrating sphere through an 8mm diameter hole at its bottom (Fig. [fig:FTS-input-aperture]), which is the conjugate of the M1 mirror by M2.
 
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During scanning, encoder pulses from the translation stage are time stamped with a clock synchronized with the HFI signal acquisition clock (itself provided by the spacecraft simulator used during the calibration). In a similar way, a mechanical ZPD (Zero Path Difference) signal is stamped and stored in the database. After verification, the scanning speed was found to be sufficiently stable to be assumed as constant along the section of the interferogram needed for spectral processing. Therefore the data processing described below does not use the reference signal but relies instead on the data acquisition time line to derive the optical path difference.
 
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To provide a reference monitor for the interferometric flux, a dedicated bolometer is used within the integrating sphere. The flux recorded by this detector is directly related to the flux received by the HFI detectors on the focal plane which is coupled directly to the sphere output hole via mirror M1. The reference bolometer was provided by the team of N. Coron at IAS and has a predetermined absolute calibration between the flux measured and its output signal. It is fed by a modified Winston horn from Infrared Lab. Inc. (USA) and operated at 300 mK using a <math>^{3}He</math> fridge (Torre-Chanin). The reference spectra acquired during the calibration run with this bolometer are used to identify standing wave features in the FTS source and path (lamp, windows,...) and to check the shape of the source spectrum. The diffraction losses at low frequencies due to the horn exit aperture diameter (2.6 mm ) is a limitation taken into account in the data processing of the low frequency channels of HFI.
 
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=== Data Collection ===
 
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To allow for data sets that have the same instrumental effects the bulk of the sequences have been performed with the same parameters. Also, separate single tests have been performed in different configurations to understand instrument systematics. The following is a list of the sequences adopted for the final spectral calibration data.
 
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* Max OPD: The Maximum Optical Path Difference adopted during FTS testing is 30 cm. This relates to a nominal maximum resolution for the spectra of <math>\simeq 0.02~\mbox{cm}^{-1}</math>. This maximum resolution may then be deteriorated by the actual sample of data selected and by the apodization of the data (see §[sec:apod]).
 
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* Speed: The Speed of the scanning FTS is set to <math>0.1~\mbox{cm}/\mbox{s}</math> for all of the data. The sampling of the data given by the acquisition frequency allows knowledge of the spectrum up to <math> \simeq 430~\mbox{cm}^{-1}</math>. This is well above the optical filter cut-off frequency, so aliasing is not a concern. The independent filter measurements used in the spectral transmission outside of the optical pass-band (see §[sec:filter]) have a Nyquist frequency of <math>600~</math>cm<math>^{-1}</math>.
 
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* Source: two sources were used in separate measurements. The mercury arc lamp as the main source for the final data and also a GLOBAR<math>^{\circledR}</math> source to study any systematic effect present in the different measurements. (Although ratio with reference bolometer should remove such artifacts.) The spectra used to generate the Spectral Transmission data products in the IMO all originated from the mercury arc lamp as the optical source.
 
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* Spectral range: The spectral range of the radiation entering the Saturne cryostat is given by a fixed <math>46~\mbox{cm}^{-1}</math> LPE filter and a rotating filter wheel with the following positions (1- Open (no added filtering), 2- Dark (no radiation allowed), 3- LPE <math>=10~\mbox{cm}^{-1}</math>, 4- LPE <math>=36~\mbox{cm}^{-1}</math>). The last two positions have been adopted for the final data of the three lower spectral channels (100, 143, 217 GHz) and the higher three spectral channels (353, 545, 857 GHz), respectively.
 
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=== Additional Experiments ===
 
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There were two significant additional tests that are used in the derivation of the HFI detector spectral transmission profiles beyond the scope of the IAS HFI FTS measurements. Additional filter measurements were recorded in the AIG test facility at Cardiff during filter stack production. These measurements are used to extend the IAS FTS spectral meaurements beyond the HFI spectral passband. The EFF tests are used to obtain optical efficiency parameters for each detector. These parameters, when combined with the respective normalized spectral transmission profiles, provide an estimate of the absolute spectral transmission. The EFF tests are discussed briefly in §[[#Optical Efficiency|EFF]], with greater detail provided by A. Catalano . The filter measurements are described in §[[#Filter Measurements|filter]] below.
 
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==== Filter Measurements ====
 
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<!-- [sec:filter] -->
 
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Prior to the IAS measurements with the integrated HFI detectors and filter stacks, FTS measurements of the individual filters comprising the filter stacks for each band were conducted at Cardiff. As will be discussed in §[sec:OOB], the independent measure of the filter stack transmission is used for a portion of the HFI detector spectral transmission for regions of the spectrum where it is deemed to be of better quality then the IAS FTS measurements (i.e. for frequencies outside of the band edge filter cut-off(s)). The filter stacks for each of the frequency bands are comprised of 5 filters. There is an additional low frequency cut-on filter for the 545 and 857 GHz bands as the waveguide cut-on is too low. Figures [fig:Filt100] – [fig:Filt857] show the individual filter transmission measurements as well as the combined filter stack product.
 
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<gallery caption="Combined (bottom) and individual (top) filter transmission measurements for the 5 filters within the HFI band filter stacks (6 for 545 and 857 GHz)." widths="300px" heights="300px" perrow="3">
 
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File:HFI_FilterPlots_100GHz.png|100GHz
 
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File:HFI_FilterPlots_143GHz.png|143GHz
 
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File:HFI_FilterPlots_217GHz.png|217GHz
 
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File:HFI_FilterPlots_353GHz.png|353GHz
 
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File:HFI_FilterPlots_545GHz.png|545GHz
 
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File:HFI_FilterPlots_857GHz.png|857GHz
 
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</gallery>
 
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The uncertainty on the combined filter transmission measurement is determined as follows. Let <math>f_i(\sigma)</math> represent the individual filter transmission. The standard deviation of all values of <math>f_i(\sigma)</math> below a threshold of <math>0.001</math> is used as an approximate uncertainty for each individual filter measurement, i.e. <math>\varsigma_{i}</math>. The individual uncertainty estimates are combined to provide an estimate of the combined filter transmission spectral uncertainty through standard error propagation. For the combined filter transmission represented as <math>F(\sigma)</math>, the associated uncertainty estimate is given as
 
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<math>\label{eq:Ferror}
 
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\varsigma_F(\sigma) = \displaystyle\sqrt{[F(\sigma)]^2\Sigma_i [(\frac{\varsigma_i}{f_i(\sigma)})^2] } ~.</math>
 
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=== Raw Data ===
 
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<!-- [sec:RawData] -->
 
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Table [[#tab:RawData|1]] contains the details for the sets of data adopted for data analysis in the generation of the HFI detector spectral transmission profiles. The first two columns report the date and time of the starting point of the data set. The third column indicates the approximate scan length (in minutes). The fourth column is the maximum number of valid interferograms that are present in the data file. The column labeled RFP (Rotating Filter Wheel Position) indicates the filtering condition under which the data was taken: 1-Totally open (no filtering other than the ever present <math>46~\mbox{cm}^{-1}</math> LPE; 2-Closed (no radiation is allowed to pass into the cryostat from the FTS); 3-<math>10~\mbox{cm}^{-1}</math> LPE filter (for the low frequency channels); 4-<math>36~\mbox{cm}^{-1}</math> LPE filter (for the high frequency channels). The column immediately following indicates, within a milliKelvin, the average reading of the bolometer plate thermometers during the scan time. The data sets with the RFP set to <math>3</math> were used for the lower frequency channels, i.e. the 100, 143, and 217 GHz bands. The data corresponding to an RFP of <math>4</math> were used for the higher frequency channels, i.e. the 353, 545, and 857 GHz bands. Table [tab:BrefData] indicates the data sets used to obtain the reference bolometer spectra. In most instances the data were acquired synchronously, however, there were cases when the HFI data was of good quality and the reference bolometer data was not, and vice-versa. The recorded data corresponding to the entries in Tables [tab:RawData] &amp; [tab:BrefData] were used in the determination of the HFI spectral transmission profiles. There is also additional data that was recorded as part of the test campaign but not used in this specific work that is not listed here.
 
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{| border=1
 
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|+ <div id="tab:RawData"> Table n:</div> Summary of recorded data used to generate the spectral transmission profiles.
 
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|-
 
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| Date (DD/MM/YY) || Time || length (min) || #Ifgm. || RFP || Source || T(mK)
 
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|-
 
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| 25/06/06 || 07:52 || 25  ||  4 || 4 || Hg || 140
 
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|-
 
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| 25/06/06 || 08:33 || 25  ||  4 || 4 || Hg || 140
 
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|-
 
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| 25/06/06 || 09:02 || 65  || 12 || 4 || Hg || 140
 
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|-
 
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| 25/06/06 || 10:05 || 65  || 12 || 4 || Hg || 140
 
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|-
 
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| 25/06/06 || 11:15 || 65  || 12 || 4 || Hg || 140
 
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|-
 
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| 26/06/06 || 09:44 || 25  || 4  || 4 || Hg || 140
 
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|-
 
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| 27/06/06 || 17:48 || 148 || 28 || 3 || Hg || &lt;130
 
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|-
 
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| 27/06/06 || 20:20 || 335 || 50 || 3 || Hg || &lt;120
 
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|-
 
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| 28/06/06 || 21:39 || 163 || 28 || 3 || Hg || 95
 
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|-
 
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| 05/07/06 || 06:23 || 82  || 16 || 4 || Hg || 100
 
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|}
 
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{| border=1
 
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|+ Summary of recorded data used to generate the reference bolometer spectra.
 
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|-
 
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| Date (DD/MM/YY) || Time || length (min) || #Ifgm. || RFP || Source
 
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|-
 
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| 22/06/06 || 17:50 || 50 || 9  || 3 || Hg
 
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|-
 
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| 22/06/06 || 18:40 || 50 || 9  || 3 || Hg
 
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|-
 
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| 22/06/06 || 19:30 || 50 || 9  || 3 || Hg
 
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|-
 
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| 22/06/06 || 20:20 || 50 || 9  || 3 || Hg
 
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|-
 
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| 22/06/06 || 21:10 || 50 || 9  || 3 || Hg
 
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|-
 
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| 22/06/06 || 22:50 || 50 || 9  || 3 || Hg
 
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|-
 
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| 22/06/06 || 23:40 || 50 || 9  || 3 || Hg
 
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|-
 
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| 25/06/06 || 07:52 || 25 || 4  || 4 || Hg
 
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|-
 
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| 25/06/06 || 10:05 || 65 || 12  || 4 || Hg
 
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|-
 
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| 25/06/06 || 11:15 || 65 || 12  || 4 || Hg
 
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|-
 
−
| 26/06/06 || 09:44 || 25 || 4  || 4 || Hg
 
−
|-
 
−
| 26/06/06 || 17:04 || 38 || 7  || 3 || Hg
 
−
|-
 
−
| 26/06/06 || 22:23 || 41 || 8  || 3 || Hg
 
−
|-
 
−
| 27/06/06 || 00:04 || 86 || 16  || 3 || Hg
 
−
|-
 
−
| 27/06/06 || 17:48 || 148 || 28 || 3 || Hg
 
−
|-
 
−
| 27/06/06 || 20:20 || 335 || 50 || 3 || Hg
 
−
|-
 
−
| 28/06/06 || 21:39 || 163 || 28 || 3 || Hg
 
−
|-
 
−
| 05/07/06 || 06:23 || 82 || 16  || 4 || Hg
 
−
|}
 
−
 
 
−
=== Data Processing ===
 
−
<1-- [sec:DP] -->
 
−
 
 
−
Having identified the data sections that are of interest, here follows the data processing sequence used to obtain the resulting spectra. The processing steps taken are as follows:
 
−
 
 
−
# Selection and extraction of time sampled data sets
 
−
# Conversion of time sampled data to arrays of OPD sampled interferogram data sets
 
−
# Fourier transformation and averaging of interferogram data sets
 
−
# Discrimination of poor quality spectra by standard deviation comparison (see §[sec:FTavg])
 
−
# Division of detector spectra by reference bolometer spectra to obtain normalized spectral transmission profiles
 
−
# Combination of relative transmission spectra with filter measurements and waveguide models
 
−
# Determination of optical efficiency through evaluation of normalized spectral transmission in the context of the EFF experiments
 
−
# Addition of over-sampled data into spectrum for the CO transition regions (see §[sec:CO])
 
−
# Identification of common frequency sampling per channel and interpolation of spectra onto the common sampling
 
−
 
 
−
==== Selection and extraction of data sets ====
 
−
<!-- [sec:getData] -->
 
−
 
 
−
The selected arrays of data are imported into a KST client from the QLA server
 
−
 
 
−
<pre>plck-op-3.ias.u-psud.fr</pre>
 
−
and subsequently exported as text files. Separate files are generated for the various bolometer signals and sample times for each detector. The exported text files were transferred from the remote IAS machines to the dedicated Planck computer at Cardiff,
 
−
 
 
−
<pre>planck01.astro.cf.ac.uk, </pre>
 
−
for further processing and analysis. A sample bolometer signal timeline is shown in Fig. [fig:BolSig].
 
−
 
 
−
[[Image:figures/LSfigs/BolSig_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
The bolometer signal is stored within the initial database in several formats: raw ADU, signal voltage, resistance, current, temperature, total power, electrical power, and radiant power, all of which may be exported to a KST session as a function of sample time. Although all of the above formats originated from the recorded detector ADU signal and instrument model parameters, it was not possible to trace these refined database vectors to the specific bolometer parameters used in their conversion. Also exported from a KST session were the set balance voltages and bias currents for each detector so that a bolometer model using the current IMO parameters (IMO ver. 2_50) could be applied to the raw data as well. The motivation for the application of a bolometer model to the data was to reduce the in-band effects of detector nonlinearities as evidence of detector operation in a non-linear regime was identified within the raw data.
 
−
 
 
−
For the interferograms within each of the data sets in the above tables (Tab. [tab:RawData] &amp; [tab:BrefData]), a course estimate of the temporal location of each position of Zero Optical-Path Difference (ZPD) was determined using the characteristic local maxima associated with a broad-band fringe for detectors with good S/N. This course ZPD location was then used as a starting point to identify a unique ZPD location within each interferogram through the fitting of a low order polynomial to the ZPD fringe.
 
−
 
 
−
The interferogram boundaries are determined as the mid-points between subsequent interferograms, less a small number of buffer points (<math>\sim</math>10) to ensure that the extracted interferograms include regions associated with the FTS stage travel having constant velocity while excluding the acceleration regions.
 
−
 
 
−
Visual verification of the extracted interferograms is performed to ensure that each ZPD was identified correctly and to remove any low-quality interferograms. The overlap of the extracted interferograms is also verified visually, with any anomolies either corrected (through a revised ZPD location) or removed. These interferograms are then saved to separate files, to be combined as a large dataset further on in the processing.
 
−
 
 
−
Once interferograms have been extracted from each data set, they are combined into a single array for each detector. The Maximum Optical Path Difference (MPD) is determined for each interferogram, and the minimum for each detector within a combined data set is used to generate an evenly sampled Optical Path Difference (OPD) grid onto which each interferogram in the combined data is then interpolated. This ensures that each individual interferogram is sampled at ZPD and that each spectrum has identical frequency sampling and can thus be averaged together. An example of a combined interferogram data set is illustrated in Figure [fig:CombinedIFGMex] where the central portions of the recorded interferograms are shown. A similar plot for each HFI detector is included in the Appendices (see §[sec:allIFGMs]). The MPD value for each detector, and corresponding spectral resolution, is shown in Fig. [fig:MPD].
 
−
 
 
−
[[Image:figures/LSfigs/PreRatioIFGMs/PreRatioIFGM_bc00_Prad_Apod5_v300_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/IFGM_Ls_ds|frame|none|alt=image]]
 
−
 
 
−
/figures/LSfigs/
 
−
 
 
−
==== Fourier Transformation and Averaging of Interferogram Data Sets ====
 
−
<!-- [sec:FTavg] -->
 
−
 
 
−
In preparation for Fourier transformation, a low-order polynomial baseline removal is performed on the individual interferograms. Consequently, no information can be recovered from the spectrum below <math>\sim 0.1~\mbox{cm}^{-1}</math>, but this is of no concern as this region of the spectrum is replaced by a waveguide fit in the final data product (see §[sec:WG]). An average interferogram is determined and used to identify glitches for removal from the interferogram data. If possible, the exponentially decaying tail of a glitch is identified, fit, removed, and replaced by the average of the remainder of the data set (which does not contain a glitch). If this is not possible then the entire interferogram is removed from the data set.
 
−
 
 
−
Although an average interferogram is determined, it is not directly used in obtaining the average spectrum. Once the data set has been deglitched, individual interferograms may be apodized (see §[sec:apod]), and then undergo Fourier transformation and phase correction . To allow phase correction to take place at the individual interferogram level, data averaging is then performed in the spectral domain. The uncertainty for every spectral data point is determined statistically through the standard deviation at a given frequency. A check for poor quality spectra is performed by comparing the overall standard deviation including and excluding any given spectrum. An example of the individual spectra and uncertainty for bc00 is shown in Fig. [fig:CombinedSpecEx]; similar plots for all of the detectors are shown in §[sec:allSpecs].
 
−
 
 
−
[[Image:figures/LSfigs/PreRatioSpecs/PreRatioSpec_bc00_Prad_Apod5_v300_avgSpec_SN_sm|frame|none|alt=image]]
 
−
 
 
−
Table [tab:Igstats] contains information on the individual detector data sets for each of the HFI detectors. Columns three and four contain the number of interferograms and spectra, respectively, used in the generation of subsequent data. These numbers may disagree due to the discrimination of poor quality data discussed above. There will never be more spectra than interferograms for a given data set. The fifth column indicates the minimum MPD for the detector data set. The FTS Instrument Line Shape (ILS) Full-Width-at-Half-Maximum (FWHM) for the data set is provided in the sixth column. An estimate of the S/N is obtained using the average spectrum and its statistical uncertainty, averaged across the in-band region of the spectrum.
 
−
 
 
−
The averaged spectra are then normalized and divided by a (normalized) reference bolometer spectrum (see §[sec:setup] &amp; §[sec:Bref]). This is done to remove spectral features from the data beyond those due to the HFI optics and detectors. The terminology ‘pre-ratio’ is used to refer to the spectra before division by the reference bolometer spectra.
 
−
 
 
−
{| border=1
 
−
|+ Properties of HFI Detector Spectra
 
−
|-
 
−
| Band (GHz) || bc || # Ifgm. || # Spec. || MPD (cm) || ILS<math>_{\mbox{FWHM}}</math> (cm<math>^{-1}</math>) || avg. S/N
 
−
|-
 
−
| 100 || 00 || 96 || 93 || 29.648639 || 0.020355066 || 104.70555
 
−
|-
 
−
| 100 || 01 || 96 || 95 || 29.648639 || 0.020355066 || 203.34226
 
−
|-
 
−
| 100 || 20 || 96 || 96 || 29.649801 || 0.020354268 || 271.38262
 
−
|-
 
−
| 100 || 21 || 95 || 94 || 29.650962 || 0.020353471 || 264.65385
 
−
|-
 
−
| 100 || 40 || 96 || 94 || 29.652124 || 0.020352674 || 432.40921
 
−
|-
 
−
| 100 || 41 || 96 || 96 || 29.652124 || 0.020352674 || 962.98064
 
−
|-
 
−
| 100 || 80 || 95 || 95 || 29.650962 || 0.020353471 || 262.71036
 
−
|-
 
−
| 100 || 81 || 96 || 96 || 29.650962 || 0.020353471 || 227.35782
 
−
|-
 
−
| 143 || 02 || 96 || 95 || 29.652124 || 0.020352674 || 434.93136
 
−
|-
 
−
| 143 || 03 || 96 || 96 || 29.652124 || 0.020352674 || 458.86741
 
−
|-
 
−
| 143 || 10 || 95 || 95 || 29.652124 || 0.020352674 || 565.21311
 
−
|-
 
−
| 143 || 30 || 92 || 92 || 29.653286 || 0.020351876 || 424.53824
 
−
|-
 
−
| 143 || 31 || 92 || 92 || 29.652124 || 0.020352674 || 447.50343
 
−
|-
 
−
| 143 || 42 || 92 || 92 || 29.652124 || 0.020352674 || 536.23423
 
−
|-
 
−
| 143 || 50 || 96 || 96 || 29.652124 || 0.020352674 || 441.68983
 
−
|-
 
−
| 143 || 51 || 96 || 96 || 29.652124 || 0.020352674 || 476.22684
 
−
|-
 
−
| 143 || 60 || 96 || 96 || 29.652124 || 0.020352674 || 517.43269
 
−
|-
 
−
| 143 || 70 || 95 || 94 || 29.652124 || 0.020352674 || 326.06542
 
−
|-
 
−
| 143 || 82 || 96 || 96 || 29.652124 || 0.020352674 || 454.23293
 
−
|-
 
−
| 143 || 83 || 96 || 96 || 29.652124 || 0.020352674 || 439.50612
 
−
|-
 
−
| 217 || 04 || 96 || 96 || 29.652124 || 0.020352674 || 625.92713
 
−
|-
 
−
| 217 || 11 || 96 || 96 || 29.652124 || 0.020352674 || 580.32904
 
−
|-
 
−
| 217 || 12 || 67 || 67 || 29.663741 || 0.020344703 || 549.24264
 
−
|-
 
−
| 217 || 22 || 96 || 96 || 29.652124 || 0.020352674 || 550.65242
 
−
|-
 
−
| 217 || 43 || 95 || 95 || 29.652124 || 0.020352674 || 616.57750
 
−
|-
 
−
| 217 || 44 || 96 || 96 || 29.652124 || 0.020352674 || 543.78288
 
−
|-
 
−
| 217 || 52 || 95 || 94 || 29.652124 || 0.020352674 || 684.91039
 
−
|-
 
−
| 217 || 61 || 92 || 92 || 29.652124 || 0.020352674 || 594.70296
 
−
|-
 
−
| 217 || 62 || 95 || 95 || 29.652124 || 0.020352674 || 579.69385
 
−
|-
 
−
| 217 || 71 || 96 || 96 || 29.652124 || 0.020352674 || 631.30065
 
−
|-
 
−
| 217 || 72 || 96 || 96 || 29.652124 || 0.020352674 || 687.10844
 
−
|-
 
−
| 217 || 84 || 92 || 92 || 29.652124 || 0.020352674 || 636.36790
 
−
|-
 
−
| 353 || 05 || 55 || 55 || 29.651916 || 0.020352816 || 354.15815
 
−
|-
 
−
| 353 || 13 || 57 || 57 || 29.651916 || 0.020352816 || 319.09858
 
−
|-
 
−
| 353 || 23 || 55 || 55 || 29.651916 || 0.020352816 || 218.05772
 
−
|-
 
−
| 353 || 24 || 64 || 64 || 29.651916 || 0.020352816 || 236.44464
 
−
|-
 
−
| 353 || 32 || 56 || 56 || 29.651916 || 0.020352816 || 238.40018
 
−
|-
 
−
| 353 || 33 || 55 || 55 || 29.651916 || 0.020352816 || 219.60443
 
−
|-
 
−
| 353 || 45 || 64 || 64 || 29.653078 || 0.020352019 || 246.97889
 
−
|-
 
−
| 353 || 53 || 57 || 57 || 29.651916 || 0.020352816 || 225.27621
 
−
|-
 
−
| 353 || 54 || 57 || 57 || 29.651916 || 0.020352816 || 228.47058
 
−
|-
 
−
| 353 || 63 || 57 || 56 || 29.651916 || 0.020352816 || 140.16991
 
−
|-
 
−
| 353 || 64 || 55 || 55 || 29.651916 || 0.020352816 || 158.85037
 
−
|-
 
−
| 353 || 85 || 57 || 57 || 29.653078 || 0.020352019 || 246.18460
 
−
|-
 
−
| 545 || 14 || 63 || 63 || 29.654240 || 0.020351221 || 448.67624
 
−
|-
 
−
| 545 || 34 || 64 || 64 || 29.654240 || 0.020351221 || 481.87111
 
−
|-
 
−
| 545 || 55 || 57 || 57 || 29.654240 || 0.020351221 || 328.07835
 
−
|-
 
−
| 545 || 73 || 57 || 57 || 29.654240 || 0.020351221 || 447.49901
 
−
|-
 
−
| 857 || 25 || 64 || 64 || 29.653078 || 0.020352019 || 501.25106
 
−
|-
 
−
| 857 || 35 || 64 || 64 || 29.654240 || 0.020351221 || 567.55125
 
−
|-
 
−
| 857 || 65 || 42 || 42 || 29.653078 || 0.020352019 || 482.41906
 
−
|-
 
−
| 857 || 74 || 64 || 64 || 29.654240 || 0.020351221 || 491.89133
 
−
|}
 
−
 
 
−
 
 
−
==== Apodization ====
 
−
<!-- [sec:apod] -->
 
−
 
 
−
Apodization of FTS interferograms results in reduced sidelobes of the FTS spectral ILS, at the cost of broadening the central feature of the ILS itself. Another perspective is that the interferogram is prefferentially weighted at certain OPD regions (i.e. ZPD) over others prior to Fourier transformation. This also, ideally, results in an improvement in the spectral S/N for a broad-spectrum source, again at the cost of reduced spectral resolution. Figure [fig:apodKernel] illustrates a variety of interferogram apodization kernels that have been used in this work . The modified Norton-Beer 1.5 apodization function has been selected to be used for the final spectral transmission profile data set as it represents a good compromise between the desired ILS sidelobe reduction and improved S/N with marginal reduction in spectral resolution. Figure [fig:ApodCompare] illustrates the difference between apodizations on the same sample data.
 
−
 
 
−
[[Image:figures/LSfigs/ApodFcns_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/ApodILS|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/ApodCompare|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
==== Reference Bolometer Spectra ====
 
−
<!-- [sec:Bref] -->
 
−
 
 
−
The reference bolometer spectra are obtained in a fashion similar to that used for the HFI detectors. Wherever possible, the same data processing is applied to the reference bolometer data as was applied to the HFI detector data, including RFP setting, scan speed, scan length, source intensity, apodization, phase correction, etc. Table [tab:Brefstats] contains the reference bolometer data set properties corresponding those listed for the HFI detectors in Table [tab:Igstats]. Figures [fig:BrefL] - [fig:Bref857] illustrate the resultant spectra and S/N from the reference bolometer data sets. Figure [fig:SNall] compares the approximate S/N of the average spectrum for each detector against the reference bolometer average spectrum S/N over the same spectral region.
 
−
 
 
−
{| border=1
 
−
|+ Properties of Ref. Bolometer Spectra
 
−
|-
 
−
| Band (GHz) || RFP || # Ifgm. || # Spec. || MPD (cm) || ILS<math>_{\mbox{FWHM}}</math> (cm<math>^{-1}</math>) || avg. S/N
 
−
|-
 
−
| 100  ||  3  ||  164  ||  164  ||  29.644698  ||  0.020357772  ||  11.478057
 
−
|-
 
−
| 143  ||  3  ||  164  ||  164  ||  29.644698  ||  0.020357772  ||  37.361317
 
−
|-
 
−
| 217  ||  3  ||  164  ||  164  ||  29.644698  ||  0.020357772  ||  126.14280
 
−
|-
 
−
| 353  ||  4  ||  24  ||  24  ||  29.652306  ||  0.020352549  ||  136.06159
 
−
|-
 
−
| 545  ||  4  ||  24  ||  24  ||  29.652306  ||  0.020352549  ||  314.58093
 
−
|-
 
−
| 857  ||  4  ||  24  ||  24  ||  29.652306  ||  0.020352549  ||  388.23050
 
−
|}
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_LowF_Apod5_avgSpec_SN_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_HighF_Apod5_avgSpec_SN_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/Bref_LowF_HighF_SN_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_LowF_Apod5_avgSpec_SN_100_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_LowF_Apod5_avgSpec_SN_143_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_LowF_Apod5_avgSpec_SN_217_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_HighF_Apod5_avgSpec_SN_353_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_HighF_Apod5_avgSpec_SN_545_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/BREF_HighF_Apod5_avgSpec_SN_857_sm|frame|none|alt=image]]
 
−
 
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/SNall|frame|none|alt=image]]
 
−
 
 
−
==== Out-of-Band Spectral Transmission Content ====
 
−
<!-- [sec:OOB] -->
 
−
 
 
−
The HFI detector spectral transmission profiles have been extended beyond the optical pass-band of the detectors. This is done by using a combination of a waveguide model and external filter measurements for the out-of-band regions of the detector spectral response. An uncertainty estimate for these additional spectral regions is also provided, however, it should be noted that the spectral uncertainty for the waveguide and filter spectra are determined indirectly (as described above/below).
 
−
 
 
−
There is a transition from IAS FTS data to filter data for every band edge which is defined by an optical filter. For the 100, 143, 217, and 353 GHz bands this is the high frequency cut-off band edge. For the 545 and 857 GHz bands a separate filter is used to define each of the high and low frequency band edges. For the spectral regions outside of the HFI detector optical bands, first the IAS FTS data is used to qualitatively verify that there are no spectral leaks or features, and then the external filter measurements are grafted into the ratioed spectra where they better represent the relative spectral transmission. The spectral transmission profiles switch from the ratioed IAS FTS data to the filtered data as follows:
 
−
 
 
−
# The normalized ratioed spectrum is scaled by the optical efficiency (see §[sec:EFF]) whereas the filter spectrum remains normalized. This results in a conservative over-estimation of the out-of-band transmission.
 
−
# A lower threshold frequency, <math>\nu_{l}</math>, is defined for each band, below which the FTS data must be used.
 
−
# An upper threshold frequency, <math>\nu_{u}</math>, is defined for each band, above which the filter data must be used. The <math>\nu_{u}</math> is defined to be twice the band cut-on frequency. This is done to avoid introducing any detector nonlinearity residuals into the final spectral transmission data products.
 
−
# The region between the lower and upper threshold frequencies is defined as the transition region.
 
−
# The transition point is defined as the first data point in the transition region where the ratioed FTS spectrum is greater in amplitude than the filter spectrum.
 
−
# If no such transition point exists, the filter spectrum is temporarily scaled to be smaller until a transition point is identified, after which the filter spectrum is restored to its original amplitude. If the temporary filter data scaling becomes less than 0.01 then the upper threshold frequency is defined as the transition point.
 
−
# The filter spectrum is used for the transmission profile for all frequencies greater than and equal to the transition frequency.
 
−
# The above method resulted in a mild distortion to the spectrum within the transition region for the 143 and 857 GHz spectra. This was a result of nonlinearity features in the FTS spectra just before the transition region cut-off. In these cases, a comparison between the FTS data derivative and filter data derivative was used to determine the transition point, instead of using the spectral amplitudes.
 
−
 
 
−
Additionally, a similar technique is used, with decreasing frequency instead of increasing, for the 545 and 857 GHz bands with a filter-induced frequency cut-on. Figure [fig:OOBex] illustrates an example of both the FTS and filter spectra used in extending the transmission profiles beyond the HFI optical bands. Similar plots for every detector are shown in §[sec:stitch].
 
−
 
 
−
==== Waveguide Model ====
 
−
<!-- [sec:WG] -->
 
−
 
 
−
A waveguide model is used to provide the data for the lowest frequency portion of the HFI detector spectral transmission. For the 100, 143, 217, and 353 GHz bands the waveguide model is transitioned (with increasing frequency) to the FTS ratioed spectra directly. There is an intermediate transition to the filter data, and then the ratioed spectra for the 545 and 857 GHz bands. For each detector, the waveguide transmission, <math>W(\sigma)</math>, is given by the following relation
 
−
 
 
−
<math>\label{eq:WGmodel}
 
−
W(\sigma) = \left\{ \begin{array}{lcl}
 
−
\exp{\left[ -\displaystyle\left(\sqrt{(c_{nm}/r_{w})^2 - (2\pi\sigma)^2}\right) \left( l_w \right) \right]} & , & \mbox{ for }\sigma \leq c_{nm}/(2\pi r_w) \\
 
−
1 & , & \mbox{ for }\sigma > c_{nm}/(2\pi r_w)
 
−
\end{array}\right.~,</math>
 
−
 
 
−
where <math>\sigma</math> is the frequency in cm<math>^{-1}</math>, <math>r_w</math> is the waveguide radius in cm, <math>l_w</math> is the waveguide length in cm, and <math>c_{nm}</math> is a waveguide specific constant; 1.841 for the TE<math>_{11}</math>/TM<math>_{11}</math> (HE<math>_{11}</math>) hybrid mode in this case . Table [tab:WG] lists the waveguide radii and lengths resultant from the waveguide model fit to the ratioed spectra. As all of the feedhorns for a given band are meant to be identical (i.e. within mechanical manufacturing tolerances) the uncertainty of the waveguide transmission is estimated statistically using all of the waveguide models for each band. I.e. for <math>n</math> bands, the uncertainty at each spectral data point is determined by the standard deviation of <math>n</math> transmission values at that frequency. As a result of each detector in a given band having a unique cut-on frequency, this method begins to over-estimate the uncertainty for frequencies approaching the cut-on; for regions very near the waveguide cut-on, the uncertainty is extrapolated from the ratioed spectrum as a more accurate representation.
 
−
 
 
−
{| border=1
 
−
|+ Waveguide model parameters for the HFI detectors.
 
−
|-
 
−
| Band (GHz) || bc || Det. || r<math>_{\mbox{w}}</math> (mm) || r<math>_{\mbox{w}}</math> (mm)
 
−
|-
 
−
| 100  ||  00  ||  1a  ||  1.039705  ||  12.| 1000
 
−
|-
 
−
| 100  ||  01  ||  1b  ||  1.038040  ||  12.5813
 
−
|-
 
−
| 100  ||  20  ||  2a  ||  1.038375  ||  14.3000
 
−
|-
 
−
| 100  ||  21  ||  2b  ||  1.041035  ||  12.3750
 
−
|-
 
−
| 100  ||  40  ||  3a  ||  1.042370  ||  12.9250
 
−
|-
 
−
| 100  ||  41  ||  3b  ||  1.042370  ||  12.5125
 
−
|-
 
−
| 100  ||  80  ||  4a  ||  1.033050  ||  13.2000
 
−
|-
 
−
| 100  ||  81  ||  4b  ||  1.033050  ||  12.6500
 
−
|-
 
−
| 143  ||  02  ||  1a  ||  0.740345  ||  9.4500
 
−
|-
 
−
| 143  ||  03  ||  1b  ||  0.737550  ||  9.5625
 
−
|-
 
−
| 143  ||  10  ||  5  ||  0.736155  ||  9.4500
 
−
|-
 
−
| 143  ||  30  ||  2a  ||  0.740345  ||  9.4500
 
−
|-
 
−
| 143  ||  31  ||  2b  ||  0.739880  ||  9.2250
 
−
|-
 
−
| 143  ||  42  ||  6  ||  0.741275  ||  9.4500
 
−
|-
 
−
| 143  ||  50  ||  3a  ||  0.741275  ||  9.4500
 
−
|-
 
−
| 143  ||  51  ||  3b  ||  0.741275  ||  9.4500
 
−
|-
 
−
| 143  ||  60  ||  7  ||  0.729635  ||  9.7875
 
−
|-
 
−
| 143  ||  70  ||  8  ||  0.739415  ||  9.4500
 
−
|-
 
−
| 143  ||  82  ||  4a  ||  0.739415  ||  9.4500
 
−
|-
 
−
| 143  ||  83  ||  4b  ||  0.738480  ||  9.4500
 
−
|-
 
−
| 217  ||  04  ||  1  ||  0.4740750  ||  7.8000
 
−
|-
 
−
| 217  ||  11  ||  5a  ||  0.4814250  ||  7.8000
 
−
|-
 
−
| 217  ||  12  ||  5b  ||  0.4817310  ||  8.0000
 
−
|-
 
−
| 217  ||  22  ||  2  ||  0.4749935  ||  7.8000
 
−
|-
 
−
| 217  ||  43  ||  6a  ||  0.4832625  ||  8.0000
 
−
|-
 
−
| 217  ||  44  ||  6b  ||  0.4832625  ||  8.0000
 
−
|-
 
−
| 217  ||  52  ||  3  ||  0.4753000  ||  8.0000
 
−
|-
 
−
| 217  ||  61  ||  7a  ||  0.4820375  ||  8.0000
 
−
|-
 
−
| 217  ||  62  ||  7b  ||  0.4820375  ||  8.0000
 
−
|-
 
−
| 217  ||  71  ||  8a  ||  0.4838750  ||  8.0000
 
−
|-
 
−
| 217  ||  72  ||  8b  ||  0.4838750  ||  8.| 1000
 
−
|-
 
−
| 217  ||  84  ||  4  ||  0.4740750  ||  7.6000
 
−
|-
 
−
| 353  ||  05  ||  1  ||  0.2921850  ||  6.47500
 
−
|-
 
−
| 353  ||  13  ||  2  ||  0.29| 14300  ||  7.00000
 
−
|-
 
−
| 353  ||  23  ||  3a  ||  0.2891650  ||  7.70000
 
−
|-
 
−
| 353  ||  24  ||  3b  ||  0.289| 3535  ||  7.52500
 
−
|-
 
−
| 353  ||  32  ||  4a  ||  0.2869000  ||  7.35000
 
−
|-
 
−
| 353  ||  33  ||  4b  ||  0.2870890  ||  7.39375
 
−
|-
 
−
| 353  ||  45  ||  7  ||  0.2876550  ||  6.12500
 
−
|-
 
−
| 353  ||  53  ||  5a  ||  0.2936950  ||  7.35000
 
−
|-
 
−
| 353  ||  54  ||  5b  ||  0.2936950  ||  7.61250
 
−
|-
 
−
| 353  ||  63  ||  6a  ||  0.2929400  ||  6.73750
 
−
|-
 
−
| 353  ||  64  ||  6b  ||  0.2925625  ||  6.62500
 
−
|-
 
−
| 353  ||  85  ||  8  ||  0.2889765  ||  6.73750
 
−
|-
 
−
| 545  ||  14  ||  1  ||  0.386| 1000  ||  3.600
 
−
|-
 
−
| 545  ||  34  ||  2  ||  0.3865875  ||  3.525
 
−
|-
 
−
| 545  ||  55  ||  3  ||  0.3800065  ||  3.525
 
−
|-
 
−
| 545  ||  73  ||  4  ||  0.3787875  ||  3.525
 
−
|-
 
−
| 857  ||  25  ||  1  ||  0.2985  ||  2.4
 
−
|-
 
−
| 857  ||  35  ||  2  ||  0.2985  ||  2.4
 
−
|-
 
−
| 857  ||  65  ||  3  ||  0.2985  ||  2.4
 
−
|-
 
−
| 857  ||  74  ||  4  ||  0.2985  ||  2.4
 
−
|}
 
−
 
 
−
 
 
−
[[Image:figures/LSfigs/FinalSpecs/OOBstitch_bc00_Prad_Apod5_v300|frame|none|alt=image]]
 
−
 
 
−
==== Optical Efficiency ====
 
−
<!-- [sec:EFF] -->
 
−
 
 
−
The EFF tests involved exposing the HFI detectors to a known blackbody source and observing the response. Sufficient details for the HFI detector spectral transmission profiles are provided here while full details of the EFF experiments and results are provided in a separate technical report . A blackbody source internal to the Saturne cryostat was set to a variety of temperatures (<math>\sim</math>1 – 6 K) and the bolometer detector response was recorded. A bolometer model was applied to the recorded response in order to obtain the radiative optical power absorbed by the detector, in units of W, i.e. <math>P_{\mbox{abs}}(T_i)</math> where <math>T_i</math> represents the blackbody source temperature. Using the measured source temperature, the theoretical radiative optical power incident on the detector is also calculated using the Planck function. The ratio of the received power and the theoretical power provides the optical efficiency term. To remove any offsets in the measurement, a ratio of differences between unique temperature settings is used. The measured absorbed optical power difference is given by
 
−
 
 
−
<math>\label{eq:EFFdPabs}
 
−
\Delta P_{\mbox{abs}} = P_{\mbox{abs}}(T_j) - P_{\mbox{abs}}(T_i) ~,</math>
 
−
 
 
−
where <math>T_j</math> and <math>T_i</math> represent two unique source temperature settings. The theoretical incident power is determined using the HFI detector spectral transmission profiles. Let <math>\tau(\nu)</math> represent the normalized detector transmission spectrum (i.e. it has been ratioed and had the waveguide model and filter data appropriately grafted). The spectral transmission is scaled for <math>\lambda^2</math> throughput and then re-normalized as follows
 
−
 
 
−
<math>\label{eq:EFFrenorm}
 
−
\tau'(\nu) = \mbox{Norm}\left[ \tau(\nu) \left( \frac{\nu}{c}\right)^2 \right]~,</math>
 
−
 
 
−
where <math>\mbox{Norm}\left(f(x)\right)</math> is the division of <math>f(x)</math> by its maximum value, and <math>c</math> is the speed of light. The normalized spectral transmission is then used with the Planck function at the temperature setting to determine the theoretical power, <math>P_{\mbox{th}}(T_i)</math> , as follows
 
−
 
 
−
<math>\label{eq:EFFPth}
 
−
P_{\mbox{th}}(T_i) = \displaystyle \int_{\nu_1}^{\nu_2}{
 
−
    \left\{ 
 
−
        \tau'(\nu)
 
−
        \left[
 
−
            \displaystyle \frac{2 h \nu^3}{c^2 (\exp{(\frac{h\nu}{k T_i})} - 1)}
 
−
        \right]
 
−
        \left(
 
−
            \displaystyle \frac{c^2}{\nu^2}n_m
 
−
        \right)
 
−
        d\nu
 
−
    \right\}} ~,</math>
 
−
 
 
−
where <math>h</math> is the Planck constant, <math>k</math> is the Boltzmann constant, the integration limits are given by <math>\nu_1</math> and <math>\nu_2</math>, and <math>n_m</math> is the expected mode content of the frequency band. Table [tab:modes] lists the <math>n_m</math> values used for each band . In this case the integration is performed over the range <math>\nu \in [67~\mbox{GHz},1142~\mbox{GHz}]</math>. The difference between the theoretical power loading is given by
 
−
 
 
−
<math>\label{eq:EFFdPth}
 
−
\Delta P_{\mbox{th}} = P_{\mbox{th}}(T_j) - P_{\mbox{th}}(T_i) ~,</math>
 
−
 
 
−
which allows the optical efficiency term to be determined as follows
 
−
 
 
−
<math>\label{eq:EFFoptEff}
 
−
\epsilon = \displaystyle \frac{\Delta P_{\mbox{abs}}}{\Delta P_{\mbox{th}}} ~.</math>
 
−
 
 
−
Thus, if <math>\epsilon \tau'(\nu)</math> were used in Equation [eq:EFFPth] in place of <math>\tau'(\nu)</math>, the resultant optical efficiency would be unity, indicating that the transmission losses have already been taken into account.
 
−
 
 
−
The uncertainty estimate of the optical efficiency is statistically based on the results from the multiple temperature settings used in the EFF test sequences.
 
−
 
 
−
 
 
−
 
 
−
{| border=1
 
−
|+ Mode Content for the HFI detector bands.
 
−
|-
 
−
| Band (GHz) || 100 || 143 || 217 || 353 || 545 || 857
 
−
|-
 
−
| <math>n_m</math> || 1 || 1 || 1 || 1 || 3.4 || 8.3
 
−
|}
 
−
 
 
−
==== CO interpolation ====
 
−
<!-- [sec:CO] -->
 
−
 
 
−
The IAS FTS/Saturne data taken with the HFI detectors is limited to a spectral resolution of <math>\sim0.017~\mbox{cm}^{-1}~(\sim0.5~\mbox{GHz})</math> by the mechanical travel of the FTS translation stage. This corresponds to an unapodized FTS ILS FWHM of <math>\sim0.020~\mbox{cm}^{-1}~(\sim0.61~\mbox{GHz})</math>. The previous iteration of the spectral transmission (IMO ver. 2_28), in addition to a triangular apodization kernel, has a factor of 3 sub-sampled spectral resolution to improve the signal-to-noise ratio (S/N) of the output spectra. In light of the CO contribution to the 100 GHz spectra, the spectral transmission has been reprocessed at the original full spectral resolution with a different apodization function which provides better noise reduction and less spectral resolution degradation, as discussed above.
 
−
 
 
−
In order to provide an improved estimate of the spectral transmission near the CO features, an interpolation of the spectra by a factor of <math>\sim</math>10 has been performed. This over-sampling was accomplished by zero-padding the FTS interferograms prior to Fourier transformation , and subsequently incorporated into the Nyquist-sampled spectral data near the CO transitions (see Table [tab:CO]). Although the data are presented at higher resolution, the resolution of independent data points is not improved, i.e. the ILS line-width remains the same. A flag column has been added to the spectral transmission profile data files to indicate whether a given data point originates from the actual data, or is a result of the ILS-based interpolation. The region of the over-sampled, interpolated, data has been extended to also include other CO isotopes; the COJ1-0 – J9-8 transitions should be oversampled for CO, C<math>^{13}</math>O, CO<math>^{17}</math>, and CO<math>^{18}</math>. The original data points within the over-sampled region have been preserved (i.e. every tenth data point – the data point that is not an interpolated one – is flagged with a zero rather than a one), as is indicated by the data flag, so a flag filter on the data will restore the independent data points easily. Figure [fig:COflag] illustrates the regions where the over-sampling has been incorporated into the spectral transmission profiles. An example of the over-sampled spectra is shown in Figure [fig:COzoom100] for the 100 GHz detectors. Examples for the other detector bands are shown in §[sec:COappend]
 
−
 
 
−
 
 
−
 
 
−
{| border=1
 
−
|+ Regions of HFI spectral transmission profiles near CO transitions.
 
−
|-
 
−
| Band (GHz) || CO transition (<math>J_{Upper}</math> - <math>J_{Lower}</math>) || <math>\nu_o</math> (GHz) || over-sampled region (GHz)
 
−
|-
 
−
| 100  ||  1 – 0  ||  115.2712018  ||  109.67 – 115.39
 
−
|-
 
−
| 143  ||  1 – 0  ||  115.2712018  ||  109.67 – 115.39
 
−
|-
 
−
| 143  ||  2 – 1  ||  230.5380000  ||  219.34 – 230.77
 
−
|-
 
−
| 217  ||  2 – 1  ||  230.5380000  ||  219.34 – 230.77
 
−
|-
 
−
| 353  ||  3 – 2  ||  345.7959899  ||  329.00 – 346.15
 
−
|-
 
−
| 545  ||  4 – 3  ||  461.0407682  ||  438.64 – 461.51
 
−
|-
 
−
| 545  ||  5 – 4  ||  576.2679305  ||  548.28 – 576.85
 
−
|-
 
−
| 857  ||  6 – 5  ||  691.4730763  ||  657.89 – 692.17
 
−
|-
 
−
| 857  ||  7 – 6  ||  806.6518060  ||  767.48 – 807.46
 
−
|-
 
−
| 857  ||  8 – 7  ||  921.7997000  ||  877.04 – 922.73
 
−
|-
 
−
| 857  ||  9 – 8  || 1036.9123930  ||  986.57 – 1037.95
 
−
|}
 
−
 
 
−
[[Image:figures/LSfigs/COflags|frame|none|alt=image]]
 
−
 
 
−
[[Image:figures/LSfigs/COJ10_HFI100_SpecTrans_v300_Apod5|frame|none|alt=image]]
 
−
 
 
−
 
 
−
{| border=1
 
−
|+ Spectral transmission for CO transitions for HFI detectors.
 
−
|-
 
−
|  BC  ||  Det.  ||  CO transition (<math>J_{\mbox{upper}} - J_{\mbox{lower}}</math>)  ||  Transmission
 
−
|-
 
−
| 100  ||  00  ||  1a  ||  1 – 0  ||  0.1495 <math>\pm</math> 0.0054
 
−
|-
 
−
| 100  ||  01  ||  1b  ||  1 – 0  ||  0.1812 <math>\pm</math> 0.0052
 
−
|-
 
−
| 100  ||  20  ||  2a  ||  1 – 0  ||  0.2577 <math>\pm</math> 0.0119
 
−
|-
 
−
| 100  ||  21  ||  2b  ||  1 – 0  ||  0.1944 <math>\pm</math> 0.0086
 
−
|-
 
−
| 100  ||  40  ||  3a  ||  1 – 0  ||  0.2798 <math>\pm</math> 0.0133
 
−
|-
 
−
| 100  ||  41  ||  3b  ||  1 – 0  ||  0.1660 <math>\pm</math> 0.0093
 
−
|-
 
−
| 100  ||  80  ||  4a  ||  1 – 0  ||  0.2538 <math>\pm</math> 0.0114
 
−
|-
 
−
| 100  ||  81  ||  4b  ||  1 – 0  ||  0.| 2173 <math>\pm</math> 0.0105
 
−
|-
 
−
| 217  ||  04  ||  1  ||  2 – 1  ||  0.3781 <math>\pm</math> 0.0026
 
−
|-
 
−
| 217  ||  11  ||  5a  ||  2 – 1  ||  0.4530 <math>\pm</math> 0.0029
 
−
|-
 
−
| 217  ||  12  ||  5b  ||  2 – 1  ||  0.4174 <math>\pm</math> 0.0030
 
−
|-
 
−
| 217  ||  22  ||  2  ||  2 – 1  ||  0.3773 <math>\pm</math> 0.0026
 
−
|-
 
−
| 217  ||  43  ||  6a  ||  2 – 1  ||  0.3149 <math>\pm</math> 0.0023
 
−
|-
 
−
| 217  ||  44  ||  6b  ||  2 – 1  ||  0.3609 <math>\pm</math> 0.0030
 
−
|-
 
−
| 217  ||  52  ||  3  ||  2 – 1  ||  0.3924 <math>\pm</math> 0.0025
 
−
|-
 
−
| 217  ||  61  ||  7a  ||  2 – 1  ||  0.3428 <math>\pm</math> 0.0022
 
−
|-
 
−
| 217  ||  62  ||  7b  ||  2 – 1  ||  0.2770 <math>\pm</math> 0.0017
 
−
|-
 
−
| 217  ||  71  ||  8a  ||  2 – 1  ||  0.4623 <math>\pm</math> 0.0031
 
−
|-
 
−
| 217  ||  72  ||  8b  ||  2 – 1  ||  0.4340 <math>\pm</math> 0.0031
 
−
|-
 
−
| 217  ||  84  ||  4  ||  2 – 1  ||  0.3506 <math>\pm</math> 0.0025
 
−
|-
 
−
353  ||  05  ||  1  ||  3 – 2  ||  0.4487 <math>\pm</math> 0.0036
 
−
|-
 
−
| 353  ||  13  ||  2  ||  3 – 2  ||  0.5461 <math>\pm</math> 0.0044
 
−
|-
 
−
| 353  ||  23  ||  3a  ||  3 – 2  ||  0.3443 <math>\pm</math> 0.0030
 
−
|-
 
−
| 353  ||  24  ||  3b  ||  3 – 2  ||  0.4706 <math>\pm</math> 0.0037
 
−
|-
 
−
| 353  ||  32  ||  4a  ||  3 – 2  ||  0.3099 <math>\pm</math> 0.0024
 
−
|-
 
−
| 353  ||  33  ||  4b  ||  3 – 2  ||  0.2801 <math>\pm</math> 0.0027
 
−
|-
 
−
| 353  ||  45  ||  7  ||  3 – 2  ||  0.2923 <math>\pm</math> 0.0022
 
−
|-
 
−
| 353  ||  53  ||  5a  ||  3 – 2  ||  0.3150 <math>\pm</math> 0.0024
 
−
|-
 
−
| 353  ||  54  ||  5b  ||  3 – 2  ||  0.3181 <math>\pm</math> 0.0023
 
−
|-
 
−
| 353  ||  63  ||  6a  ||  3 – 2  ||  0.2059 <math>\pm</math> 0.0014
 
−
|-
 
−
| 353  ||  64  ||  6b  ||  3 – 2  ||  0.2113 <math>\pm</math> 0.0017
 
−
|-
 
−
| 353  ||  85  ||  8  ||  3 – 2  ||  0.3509 <math>\pm</math> 0.0028
 
−
|-
 
−
| 545  ||  14  ||  1  ||  4 – 3  ||  0.0747 <math>\pm</math> 0.0003
 
−
|-
 
−
| 545  ||  34  ||  2  ||  4 – 3  ||  0.0731 <math>\pm</math> 0.0003
 
−
|-
 
−
| 545  ||  55  ||  3  ||  4 – 3  ||  0.0521 <math>\pm</math> 0.0002
 
−
|-
 
−
| 545  ||  73  ||  4  ||  4 – 3  ||  0.0473 <math>\pm</math> 0.0002
 
−
|-
 
−
| 545  ||  14  ||  1  ||  5 – 4  ||  0.3306 <math>\pm</math> 0.0012
 
−
|-
 
−
| 545  ||  34  ||  2  ||  5 – 4  ||  0.3183 <math>\pm</math> 0.0011
 
−
|-
 
−
| 545  ||  55  ||  3  ||  5 – 4  ||  0.2428 <math>\pm</math> 0.0009
 
−
|-
 
−
| 545  ||  73  ||  4  ||  5 – 4  ||  0.2597 <math>\pm</math> 0.0009
 
−
|-
 
−
| 857  ||  25  ||  1  ||  6 – 5  ||  0.0280 <math>\pm</math> 0.0001
 
−
|-
 
−
| 857  ||  35  ||  2  ||  6 – 5  ||  0.0241 <math>\pm</math> 0.0001
 
−
|-
 
−
| 857  ||  65  ||  3  ||  6 – 5  ||  0.0292 <math>\pm</math> 0.0001
 
−
|-
 
−
| 857  ||  74  ||  4  ||  6 – 5  ||  0.0159 <math>\pm</math> 0.0001
 
−
|-
 
−
| 857  ||  25  ||  1  ||  7 – 6  ||  0.1636 <math>\pm</math> 0.0005
 
−
|-
 
−
| 857  ||  35  ||  2  ||  7 – 6  ||  0.1427 <math>\pm</math> 0.0004
 
−
|-
 
−
| 857  ||  65  ||  3  ||  7 – 6  ||  0.| 2176 <math>\pm</math> 0.0007
 
−
|-
 
−
| 857  ||  74  ||  4  ||  7 – 6  ||  0.1168 <math>\pm</math> 0.0003
 
−
|-
 
−
| 857  ||  25  ||  1  ||  8 – 7  ||  0.2554 <math>\pm</math> 0.0009
 
−
|-
 
−
| 857  ||  35  ||  2  ||  8 – 7  ||  0.2218 <math>\pm</math> 0.0007
 
−
|-
 
−
| 857  ||  65  ||  3  ||  8 – 7  ||  0.2744 <math>\pm</math> 0.0009
 
−
|-
 
−
| 857  ||  74  ||  4  ||  8 – 7  ||  0.1119 <math>\pm</math> 0.0004
 
−
|-
 
−
| 857  ||  25  ||  1  ||  9 – 8  ||  0.0053 <math>\pm</math> 0.0000
 
−
|-
 
−
| 857  ||  35  ||  2  ||  9 – 8  ||  0.0060 <math>\pm</math> 0.0000
 
−
|-
 
−
| 857  ||  65  ||  3  ||  9 – 8  ||  0.0085 <math>\pm</math> 0.0000
 
−
|-
 
−
| 857  ||  74  ||  4  ||  9 – 8  ||  0.0001 <math>\pm</math> 0.0000
 
−
|}
 
−
 
 
−
=== Conformity with requirements ===
 
−
<!-- [sec:req] -->
 
−
The two defining requirements indicated in the HFI calibration plan are the acquisition of the spectral transmission of the single pixels with a prescribed accuracy and spectral resolution. The desired accuracy is 3% for the low frequency channels (CMB – 100, 143, and 217 GHz) and 1% for the high frequency channels (353, 545, 857 GHz). The spectral resolution requirement is for a resolution superior to 0.1 cm<math>^{-1}</math>.
 
−
 
 
−
The spectral resolution requirement has been exceeded by more than a factor of five. It is also possible to degrade the spectral resolution to the 0.1 cm<math>^{-1}</math> requirement to gain an improvement in the S/N.
 
−
 
 
−
No quantitative number is present on the document regarding the blocking of high frequency (near IR, visible, UV) radiation outside the range of the instrument. Checks in order to quantify the rejection have been performed at subsystem level and estimates of the out-of-band transmission profiles have been incorporated into the data products.
 
−
 
 
−
The requirement on the spectral transmission accuracy for the CMB channels is of <math>3\%</math>. There is also a requirement that the high frequency channels effective frequencies be known to within <math>1\%</math>; knowledge of the transmission to 1% accuracy should allow this.
 
−
 
 
−
Considering statistical fluctuations in the determination of the spectra, these goals have been achieved. There are, however, caveats regarding the nature of error bars when dealing with frequency space. The nature of uncertainties in spectra determination is less obvious than when dealing with timestream data. Systematic effects produced from instrumental setup, but also by data reduction can in some cases exceed the actual statistical oscillation in the determination of the final spectra. This is the case for the high-frequency data for instance where the statistical fluctuation of the different determinations of the spectra in some case are better than 1 part in <math>10^3</math>.
 
−
 
 
−
A second caveat regards the method of data analysis of the calibration test data, for which the ratio with the reference bolometer data (of which the relative error is a function of frequency) introduces an error that increase with wavelength. With the spectral resolution of the data provided being much higher that the stated 0.1 cm<math>^{-1}</math>, the transmission accuracy requirement is not met for the 100 GHz detectors. It is possible to degrade the spectral resolution to the 0.1cm<math>^{-1}</math> level to allow the accuracy to achieve the required level, but the higher spectral resolution data has been provided to better assist with the CO contamination removal from the 100 GHz signal.
 
−
 
 
−
 
 
−
== Detection chain ==
 
−
<span style="color:red">(Francesco Piacentini)</span>
 
−
=== Bolometers===
 
−
 
 
−
The heart of the HFI - the detectors - are bolometers, solid-state devices in which the
 
−
incoming radiation dissipates its energy as heat that increases the temperature of a
 
−
thermometer. The instrument Flight Model total number of bolometers is 52, split into 6
 
−
channels at central frequencies of 100, 143, 217, 353, 545, and 857GHz.
 
−
 
 
−
Thirty two of these bolometers are polarization sensitive allowing a map of the CMB polarisation to be built.
 
−
 
 
−
 
 
−
 
 
−
Bolometers consist of (i) an absorber that transforms the in-coming radiation into heat; (ii) a thermometer that is thermally linked to the absorber and measures the temperature changes; and (iii) a weak thermal link to a thermal sink, to which the bolometer is attached.
 
−
 
 
−
 
 
−
The detectors are semi-conducting NTD thermistor bolometers. There are two kinds of detector modules:
 
−
 
 
−
* SWB, spider web bolometers, are mounted on an absorbing spider-web of metallised silicon nitride
 
−
* PSB, polarization sensitive bolometers, are mounted or on a parallel absorbing grid of metallised silicon nitride.
 
−
 
 
−
 
 
−
In the spider-web bolometers, or SWBs (Bock et al. 1995; Mauskopf et al. 1997), the absorbers consist of metallic grids
 
−
deposited on a Si3 N4 substrate in the shape of a spider web.
 
−
The mesh design and the impedance of the metallic layer are
 
−
adjusted to match vacuum impedance and maximize the absorption of millimeter waves, while minimizing the cross section to
 
−
particles. The absorber is designed to offer equal impedance to
 
−
any linearly polarised radiation. Nevertheless, the thermometer
 
−
and its electrical leads define a privileged orientation (Fig. SWB) that
 
−
makes the SWBs slightly sensitive to polarisation, as detailed in
 
−
(Rosset et al. 2010). The thermometers are
 
−
made of neutron transmuted doped (NTD) germanium (Haller
 
−
et al. 1996), chosen to have an impedance of about 10 MΩ at
 
−
their operating temperature.
 
−
 
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_bolo1.png|500px|((Illustration 6)): Picture of a spider web bolometer. This a 143 GHz module, The temperature sensor is at the center of the absorbing grid]]
 
−
 
 
−
 
 
−
The absorber of PSBs is a rectangular grid (Fig. PSB) with metallization in one direction (Jones et al.
 
−
2003). Electrical fields parallel to this direction develop currents and then deposit some power in the grid, while perpendicular electrical fields propagate through the grid without significant interaction. A second PSB perpendicular to the first one absorbs the other polarisation. Such a PSB pair measures two polarisations of radiation collected by the same horns and filtered by the same devices, which minimises the systematic effects: differences between polarised
 
−
beams collected by a given horn are typically less than −30 dB of
 
−
the peak. The differences in the spectral responses of a PSB pair
 
−
also proved to be a few percent in the worst case. Each pair
 
−
of PSBs sharing the same horn is able to measure the intensity
 
−
Stokes parameter and the Q parameter associated with its local
 
−
frame. An associated pair of PSBs rotated by 45◦ scans exactly
 
−
the same line (if the geometrical alignment is perfect), providing
 
−
the U Stokes parameter.
 
−
 
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_bolo2.png|500px|Picture of a polarization sensitive bolometer. This a 217 GHz module, The temperature sensor is at the an edge  of the absorbing grid]]
 
−
 
 
−
 
 
−
The detectors operate at a temperature close to 100 mK, while the filters are distributed on the 100mK, 1.6 K,
 
−
and 4 K stages in such a way that the heat load on the coldest stages is minimized to
 
−
limit the heat load on the detectors and to decrease
 
−
the heat lift requirement and thus enhance the mission lifetime. The self-emission of the 4K stage is minimised to limit the photon noise contribution on the detectors from the instrument.
 
−
The HFI Focal Plane Unit accommodates sub-millimiter absorbing
 
−
material in order to decrease the scattering inside it.
 
−
 
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_table1.png|500px|to be change into a real table]]
 
−
 
 
−
===Focal plane layout===
 
−
 
 
−
The layout of the detectors in the focal plane is defined to cope with the
 
−
scanning strategy. The HFI horns are positioned at the centre of the focal plane, where the optical
 
−
quality is good enough for the high frequencies. The curvature of
 
−
rows compensates for the distortion of images by the telescope.
 
−
A pair of identical SWB will scan the same circle on the sky to
 
−
provide additional redundancy. Similar horns feeding PSBs are
 
−
also aligned so that two pairs of PSBs rotated by 45◦ with respect to each other scan the same line. This will provide the Q and U Stokes parameters with minimal correction for the pointing (Rosset et al. 2010). Residual systematics will come from the differences between the beam shapes of the two horns. In all
 
−
cases except for the 100 GHz horns, a measurement is also done
 
−
by a pair of similar channels shifted by 1.25 arcminutes in the cross-scan direction, to ensure adequate sampling. In the figures focal plane layout is reported.
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_FocalPlaneLayout.png|500px|Focal plane layout as seen from outside the celestial sphere. Each spot represents an horn in the focal plane. Coordinates are in pointing direction with respect to the telescope boresight. PSBs detectors are indicated with a cross oriented as the two polarimeters axes. Scan direction is from
 
−
left to right.]]
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_FocalPlaneGeo.png|500px|Illustration 4: Focal plane layout as seen from outside the celestial sphere. In this case PSBs orientations are reported. Red rod is for a elements of PSBs, blue rod is for b elements.]]
 
−
 
 
−
=== Readout===
 
−
 
 
−
The AC bias readout electronics of the HFI instrument (Gaertner et al. 1997) includes a number of original features proposed by several laboratories (CRTBT in Grenoble, CESR in Toulouse and IAS in Orsay), which were validated on the Diabolo experiment and on the balloon-borne Archeops experiment. It was developed for space by the CESR in Toulouse.
 
−
 
 
−
 
 
−
The particular features of the HFI AC bias readout are mainly
 
−
 
 
−
 
 
−
* i)that the cold load resistors were replaced by capacitors because they have no Johnson noise;
 
−
* ii)that the detectors are biased by applying a triangular voltage to the load capacitors
 
−
which produces a square current [Ibias ] in the capacitors, and a square voltage [T bias ] that compensates for the stray capacitance of the wiring (producing a nearly square bias current into the bolometer;
 
−
* iii)that a square offset com-pensation signal is subtracted to the bolometric signal to minimise the amplitude of the signal that has to be amplified and digitized;
 
−
* iv)that the electronic scheme is symmetrical and uses a differential amplification scheme to optimize the immunity to electromagnetic interferences;
 
−
* v)and finally that every parameter of the REU can be set by commands, which
 
−
is made possible by using digital-to-analog and analog-to-digital converters extensively.
 
−
 
 
−
 
 
−
The readout electronics consist of 72 channels designed to perform low noise measurements of the impedance of 52 bolometers, two blind bolometers, 16 accurate low temperature thermometers, all in the 10 MΩ range, one resistor of 10 MΩ and one capacitor of 100 pF. The semiconductor bolometers and thermometers of Planck-HFI operate at cryogenic temperature around 100 mK on the focal plane, with impedance of about 10 MΩ when biased at the optimal current. The readout electronics on the contrary have to operate at “room” temperature (300 K). The distance between the two extremities of the readout chain is about 10 m and could represent a point of extreme susceptibility to electromagnetic interference. The readout electronic chain was split into three boxes. These are the JFET box, located on the 50 K stage of the satellite at 2.2 m from the focal plane, the pre-amplifier unit (PAU), located 1.8m further at 300 K, and the REU, located on the opposite side of the satellite, 5 m away. Each of the three boxes (JFET, PAU and
 
−
REU) consists of 12 belts of six channels. The first nine belts are dedicated to the bolometers, and the three last ones to the accurate thermometers, the resistor and the capacitor (see figure Organization of the HFI readout).
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_HFIreadout.png|500px|Illustration 6: Organization of the HFI readout. Each row represents a belt. Each belt has 6 channels.]]
 
−
 
 
−
[[File:HFI_2_4_1_FPiacentini_table2.jpeg|500px|Illustration 5: Organization of the HFI readout. Each row represents a belt. Each belt has 6 channels. (to be change into a real table ?)]]
 
−
 
 
−
===Principles of the readout electronics. ===
 
−
 
 
−
See figure [Principles of readout electronics]. The bolometer is biased by a square wave AC current obtained by the differentiation of a triangular voltage through a load capacitance, in a completely differential architecture. The presence of the stray capacitance due to losses of charge in the wiring requires a correction of the shape of the square bias current by a transient voltage. Thus the bias voltage generation is controlled by the two parameters I-bias and T-bias that express the amplitude of the triangular and transient voltage. The compensation voltage added to the bolometric signal to optimize the dynamic of the chain is controlled by the V-bal parameter.
 
−
 
 
−
Illustration 6: Principles of readout electronics. The three modules of the chain are shown: JFet Box, Pre-Amplifier
 
−
Unit (PAU) and Readout Electronic Unit (REU).
 
−
 
 
−
 
 
−
Parameters of the Readout Unit can be set to optimize the detectors performance.
 
−
 
 
−
The modulation frequency of the AC bias system, fmod of the square bias current
 
−
can be tuned from 70 Hz to 112 Hz by the telecommand parameters:
 
−
Nsample, which defines the number of samples per half period of modulated signal,
 
−
fdiv which determines the sampling frequency of the ADC.
 
−
 
 
−
The optimal frequencies are around 90 Hz.
 
−
 
 
−
 
 
−
Each channel has its own settings for the following parameters:
 
−
I-bias, amplitude of the triangular bias voltage;
 
−
 
 
−
T-bias, amplitude of the transient bias voltage;
 
−
 
 
−
V-bal, amplitude of the square compensation voltage;
 
−
 
 
−
G-amp, value of the programmable gain of the REU [1/3, 1, 3, 7.6];
 
−
 
 
−
N-blank, number of blanked samples at the beginning of halfperiod not taken into account during integration of the signal;
 
−
 
 
−
S-phase, phase shift when computing the integrated signal.
 
−
 
 
−
All these parameters influence the effective response of the
 
−
detection chains, and were optimized during the calibration
 
−
campaigns and confirmed during the calibration and performance
 
−
verification (CPV) phase following the launch of
 
−
Planck. The scientific signal is provided by the integral of the
 
−
signal on each half-period, between limits fixed by the S-phase
 
−
and N-blank parameters.
 
−
 
 
−
 
 
−
The interaction of modulated readout electronics with semiconductor
 
−
bolometers is rather different from that of a classical
 
−
DC bias readout (Jones 1953). The differences were seen during
 
−
the calibration of the HFI, although the readout electronics
 
−
was designed to mimic the operation
 
−
of a DC biased bolometric system as far as possible. With the
 
−
AC readout the maximum of responsivity is lower and is obtained
 
−
for higher bias current in the bolometer with respect to the DC model.
 
−
This is caused by the stray capacitance in the
 
−
wiring which has negligible effects for a DC bias and a major
 
−
effect for an AC bias. In our case, a stray capacitance of 150 pF
 
−
induces increases of NEP ranging from 4% (857 GHz bolometers)
 
−
to 10% (100 GHz bolometers) and also affects the HFI time
 
−
response. Details of the effect of the HFI AC bias system into
 
−
the time response of the detectors are discussed in the Time Response Section [link].
 
−
 
 
−
=== JFETs===
 
−
 
 
−
Given the high impedance of the bolometers and the length of the connecting cables, it it is  essential that the impedance of the signal is lowered as close as possible to the detectors. In our system this is accomplished by means of JFET source followers, located in boxes connected to the 50 K stage. There are two JFETs per channel, since the readout is fully differential, and they provide a current amplification of the signal while keeping the voltage amplification very close to unity.
 
−
 
 
−
Inside the box, the JFETs are mounted on a thermally insulated plate with an active temperature control to keep them at the optimal temperature of 110 K. With a dissipated power lower than 240 mW, mainly produced by the JFETs and the source resistors, we obtained a noise power spectral density of less than 3 nV Hz1/2 for the frequency range of interest. This increases the total noise ofall bolometer channels by less than 5%.
 
−
 
 
−
 
 
−
=== Data compression===
 
−
=== Time response.===
 
−
 
 
−
 
 
−
 
 
−
The HFI bolometers and readout electronics have a finite response time to changes in incident optical power.  The bolometers are thermal detectors of radiation whose response time is determined by the thermal circuit defined by the heat capacity of the detector and thermal conductivity.
 
−
 
 
−
Due to Planck's nearly constant scan rate, the time response is degenerate with the optical beam.  However, because of the long time scale effects present in the time response, the  time response is deconvolved from the data in the processing of the HFI data (see [[TOI processing|TOI processing]]).
 
−
 
 
−
The time response of the HFI bolometers and readout electronics is modeled as a Fourier domain transfer function (called the LFER4 model) consisting of the product of an bolometer thermal response <math>F(\omega)</math> and an electronics response <math>H'(\omega)</math>.
 
−
 
 
−
<math>\label{LFER4def}TF^{LFER4}(\omega) = F(\omega) H'(\omega)</math>
 
−
 
 
−
=== LFER4 model ===
 
−
 
 
−
If we write the input signal (power) on a bolometer as <math>\label{bol_in}
 
−
s_0(t)=e^{i\omega t}
 
−
</math> the bolometer physical impedance can be written as: <math>\label{bol_out}
 
−
s(t)=e^{i\omega t}F(\omega)
 
−
</math> where <math>\omega</math> is the angular frequency of the signal and <math>F(\omega)</math> is the complex intrinsic bolometer transfer function. For HFI the bolometer transfer function is modelled as the sum of 4 single pole low pass filters: <math>\label{bol_tf}
 
−
F(\omega) = \sum_{i=0,4} \frac{a_i}{1 + i\omega\tau_i}
 
−
</math> The modulation of the signal is done with a square wave, written here as a composition of sine waves of decreasing amplitude: <math>\label{sigmod}
 
−
s'(t)=e^{i\omega t}F(\omega)\sum_{k=0}^{\infty} \frac{e^{i\omega_r(2k+1)t}-e^{-i\omega_r(2k+1)t}}{2i(2k+1)}
 
−
</math> where we have used the Euler relation <math>\sin x=(e^{ix}-e^{-ix})/2i</math> and <math>\omega_r</math> is the angular frequency of the square wave. The modulation frequency is <math>f_{mod} = \omega_r/2\pi</math> and was set to <math>f_{mod} = 90.18759 </math>Hz in flight. This signal is then filtered by the complex electronic transfer function <math>H(\omega)</math>. Setting: <math>\omega_k^+=\omega+(2k+1)\omega_r</math> <math>\omega_k^-=\omega-(2k+1)\omega_r</math> we have: <math>\label{sigele}
 
−
\Sigma(t)=\sum_{k=0}^\infty\frac{F(\omega)}{2i(2k+1)}\left[H(\omega_k^+)e^{i\omega_k^+t}-H(\omega_k^-)e^{i\omega_k^-t}\right]
 
−
</math> This signal is then sampled at high frequency (<math>2 f_{mod} NS</math>). <math>NS</math> is one of the parameters of the HFI electronics and corresponds to the number of high frequency samples in each modulation semi-period. In order to obtain an output signal sampled every <math>\pi/\omega_r</math> seconds, we must integrate on a semiperiod, as done in the HFI readout. To also include a time shift <math>\Delta t</math>, the integral is calculated between <math>n\pi/\omega_r+\Delta t</math> and <math>(n+1)\pi/\omega_r+\Delta t</math> (with <math>T=2 \pi/\omega_r</math> period of the modulation). The time shift <math>\Delta t</math> is encoded in the HFI electronics by the parameter <math>S_{phase}</math>, with the relation <math>\Delta t = S_{phase}/NS/f_{mod} </math>.
 
−
 
 
−
After integration, the <math>n</math>-sample of a bolometer can be written as <math>\label{eqn:output}
 
−
Y(t_n) = (-1)^n F(\omega) H'(\omega) e^{i t_n \omega}
 
−
</math> where <math>\label{tfele}
 
−
H'(\omega) = \frac 12 \sum_{k=0}^\infty
 
−
e^{-i(\frac{\pi\omega}{2\omega_r}+\omega\Delta t)} \Bigg[
 
−
\frac{H(\omega_k^+)e^{i\omega_k^+ \Delta t}}{(2k+1)\omega_k^+}
 
−
\left(1-e^{\frac{i\omega_k^+\pi}{\omega_r}}\right)
 
−
\\ - \frac{H(\omega_k^-)e^{i\omega_k^- \Delta t}}{(2k+1)\omega_k^-}  \left(1-e^{\frac{i\omega_k^-\pi}{\omega_r}}\right)
 
−
\Bigg]
 
−
</math>
 
−
 
 
−
The output signal in equation eqn:output can be demodulated (thus removing the <math>(-1)^n</math>) and compared to the input signal in equation bol_in. The overall transfer function is composed of the bolometer transfer function and the effective electronics transfer function, <math>H'(\omega)</math>: <math>TF(\omega) = F(\omega) H'(\omega)
 
−
</math>
 
−
 
 
−
The shape of <math>H(\omega)</math> is obtained combining low and high-pass filters with Sallen Key topologies (with their respective time constants) and accounting also for the stray capacitance low pass filter given by the bolometer impedance combined with the stray capacitance of the cables. The sequence of filters that define the electronic band-pass function <math>H(\omega) = h_0*h_1*h_2*h_3*h_4*h_{5}</math> are listed in table table:readout_electronics_filters.
 
−
 
 
−
=== Parameters of LFER4 model ===
 
−
 
 
−
The LFER4 model has are a total of 10 parameters(<math>A_1</math>,<math>A_2</math>,<math>A_3</math>,<math>A_4</math>,<math>\tau_1</math>,<math>\tau_2</math>,<math>\tau_3</math>,<math>\tau_4</math>,<math>S_{phase}</math>,<math>\tau_{stray}</math>) 9 of which are independent, for each bolometer. The free parameters of the LFER4 model are determined using in-flight data in the following ways:
 
−
 
 
−
* <math>S_{phase}</math> is fixed at the value of the REU setting.
 
−
* <math>\tau_{stray}</math> is measured during the QEC test during CPV.
 
−
* <math>A_1</math>, <math>\tau_1</math>, <math>A_2</math>, <math>\tau_2</math> are fit forcing the compactness of the scanning beam.
 
−
* <math>A_3</math>, <math>\tau_3</math>, <math>A_{4}</math> <math>\tau_4</math> are fit by forcing agreement of survey 2 and survey 1 maps.
 
−
* The overall normalization of the LFER4 model is forced to be 1.0 at the signal frequency of the dipole. 
 
−
 
 
−
The details of determining the model parameters are given in (reference P03c paper) and the best-fit parameters listed here in table table:LFER4pars.
 
−
 
 
−
 
 
−
===HFI electronics filter sequence ===
 
−
 
 
−
{| class="wikitable" style="text-align: left; border-collapse: collapse; border-width: 1px; border-style: solid; border-color: #000"
 
−
|+HFI electronics filter sequence. We define $s = i \omega$
 
−
|-
 
−
! style="border-style: solid; border-width: 1px"|Filter
 
−
! style="border-style: solid; border-width: 1px"|Parameters
 
−
! style="border-style: solid; border-width: 1px"|Function
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|0. Stray capacitance low pass filter
 
−
|style="border-style: solid; border-width: 1px"|<math>\tau_{stray}= R_{bolo} C_{stray}</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>h_0 = \frac{1}{1.0+\tau_{stray}*s}</math>
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|1. Low pass filter
 
−
|style="border-style: solid; border-width: 1px"|<math>R_1=1</math>k<math>\Omega</math> <br /> <math>C_1=100</math>nF
 
−
|style="border-style: solid; border-width: 1px"|<math>h_1 = \frac{2.0+R_1*C_1*s}{2.0*(1.0+R_1*C_1*s)}</math>
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|2. Sallen Key high pass filter
 
−
|style="border-style: solid; border-width: 1px"|<math>R_2=51</math>k<math>\Omega</math><br /> <math>C_2=1\mu</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>h_2= \frac{(R_2*C_2*s)^2}{(1.0+R_2*C_2*s)^2}</math>3
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|3. Sign reverse with gain
 
−
|style="border-style: solid; border-width: 1px"|
 
−
|style="border-style: solid; border-width: 1px"|<math>h_3=-5.1</math>
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|4. Single pole low pass filter with gain
 
−
|style="border-style: solid; border-width: 1px"|<math>R_4=10</math>k<math>\Omega</math><br /> <math>C_4=10</math>nF
 
−
|style="border-style: solid; border-width: 1px"|<math>h_4= \frac{1.5}{1.0+R_4*C_4*s}</math>
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|5. Single pole high pass filter coupled to a Sallen Key low pass filter
 
−
|style="border-style: solid; border-width: 1px"|<math>R_9=18.7</math>k<math>\Omega</math><br /><math>R_{12}=37.4</math>k<math>\Omega</math><br /> <math>C=10.0</math>nF<br /><math>R_{78}=510</math>k<math>\Omega</math><br /> <math>C_{18}=1.0\mu</math>F<br /><math>K_3 = R_9^2*R_{78}*R_{12}^2*C^2*C_{18}</math><br /> <math>K_2 = R_9*R_{12}^2*R_{78}*C^2+R_{9}^2*R_{12}^2*C^2+R_9*R_{12}^2*R_{78}*C_{18}*C</math><br /> <math>K_1 =R_9*R_{12}^2*C+R_{12}*R_{78}*R_9*C_{18}</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>h_{5} = \frac{2.0*R_{12}*R_9*R_{78}*C_{18}*s}{s^3*K_3 +
 
−
      s^2*K_2+
 
−
      s*K_1 + R_{12}*R_9 } </math>
 
−
 
 
−
|}
 
−
 
 
−
 
 
−
 
 
−
{| class="wikitable" style="text-align: left; align: center; border-collapse: collapse; border-width: 1px; border-style: solid; border-color: #000"
 
−
|+ Parameters for LFER4 model.
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|Bolometer
 
−
|style="border-style: solid; border-width: 1px"|<math>A_1</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>\tau_1</math> (s)
 
−
|style="border-style: solid; border-width: 1px"|<math>A_2</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>\tau_2</math> (s)
 
−
|style="border-style: solid; border-width: 1px"|<math>A_3</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>\tau_3</math> (s)
 
−
|style="border-style: solid; border-width: 1px"|<math>A_4</math>
 
−
|style="border-style: solid; border-width: 1px"|<math>\tau_4</math> (s)
 
−
|style="border-style: solid; border-width: 1px"|<math>\tau_{stray}</math> (s)
 
−
|style="border-style: solid; border-width: 1px"|<math>S_{phase}</math>
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|100-1a
 
−
|style="border-style: solid; border-width: 1px"|0.392
 
−
|style="border-style: solid; border-width: 1px"|0.01
 
−
|style="border-style: solid; border-width: 1px"|0.534
 
−
|style="border-style: solid; border-width: 1px"|0.0209
 
−
|style="border-style: solid; border-width: 1px"|0.0656
 
−
|style="border-style: solid; border-width: 1px"|0.0513
 
−
|style="border-style: solid; border-width: 1px"|0.00833
 
−
|style="border-style: solid; border-width: 1px"|0.572
 
−
|style="border-style: solid; border-width: 1px"|0.00159
 
−
|style="border-style: solid; border-width: 1px"|0.00139
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|100-1b
 
−
|style="border-style: solid; border-width: 1px"|0.484
 
−
|style="border-style: solid; border-width: 1px"|0.0103
 
−
|style="border-style: solid; border-width: 1px"|0.463
 
−
|style="border-style: solid; border-width: 1px"|0.0192
 
−
|style="border-style: solid; border-width: 1px"|0.0451
 
−
|style="border-style: solid; border-width: 1px"|0.0714
 
−
|style="border-style: solid; border-width: 1px"|0.00808
 
−
|style="border-style: solid; border-width: 1px"|0.594
 
−
|style="border-style: solid; border-width: 1px"|0.00149
 
−
|style="border-style: solid; border-width: 1px"|0.00139
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|100-2a
 
−
|style="border-style: solid; border-width: 1px"|0.474
 
−
|style="border-style: solid; border-width: 1px"|0.00684
 
−
|style="border-style: solid; border-width: 1px"|0.421
 
−
|style="border-style: solid; border-width: 1px"|0.0136
 
−
|style="border-style: solid; border-width: 1px"|0.0942
 
−
|style="border-style: solid; border-width: 1px"|0.0376
 
−
|style="border-style: solid; border-width: 1px"|0.0106
 
−
|style="border-style: solid; border-width: 1px"|0.346
 
−
|style="border-style: solid; border-width: 1px"|0.00132
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|100-2b
 
−
|style="border-style: solid; border-width: 1px"|0.126
 
−
|style="border-style: solid; border-width: 1px"|0.00584
 
−
|style="border-style: solid; border-width: 1px"|0.717
 
−
|style="border-style: solid; border-width: 1px"|0.0151
 
−
|style="border-style: solid; border-width: 1px"|0.142
 
−
|style="border-style: solid; border-width: 1px"|0.0351
 
−
|style="border-style: solid; border-width: 1px"|0.0145
 
−
|style="border-style: solid; border-width: 1px"|0.293
 
−
|style="border-style: solid; border-width: 1px"|0.00138
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|100-3a
 
−
|style="border-style: solid; border-width: 1px"|0.744
 
−
|style="border-style: solid; border-width: 1px"|0.00539
 
−
|style="border-style: solid; border-width: 1px"|0.223
 
−
|style="border-style: solid; border-width: 1px"|0.0147
 
−
|style="border-style: solid; border-width: 1px"|0.0262
 
−
|style="border-style: solid; border-width: 1px"|0.0586
 
−
|style="border-style: solid; border-width: 1px"|0.00636
 
−
|style="border-style: solid; border-width: 1px"|0.907
 
−
|style="border-style: solid; border-width: 1px"|0.00142
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|100-3b
 
−
|style="border-style: solid; border-width: 1px"|0.608
 
−
|style="border-style: solid; border-width: 1px"|0.00548
 
−
|style="border-style: solid; border-width: 1px"|0.352
 
−
|style="border-style: solid; border-width: 1px"|0.0155
 
−
|style="border-style: solid; border-width: 1px"|0.0321
 
−
|style="border-style: solid; border-width: 1px"|0.0636
 
−
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|style="border-style: solid; border-width: 1px"|0.00181
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-4b
 
−
|style="border-style: solid; border-width: 1px"|0.684
 
−
|style="border-style: solid; border-width: 1px"|0.00454
 
−
|style="border-style: solid; border-width: 1px"|0.224
 
−
|style="border-style: solid; border-width: 1px"|0.0108
 
−
|style="border-style: solid; border-width: 1px"|0.0774
 
−
|style="border-style: solid; border-width: 1px"|0.08
 
−
|style="border-style: solid; border-width: 1px"|0.0149
 
−
|style="border-style: solid; border-width: 1px"|0.267
 
−
|style="border-style: solid; border-width: 1px"|0.00166
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-5a
 
−
|style="border-style: solid; border-width: 1px"|0.767
 
−
|style="border-style: solid; border-width: 1px"|0.00596
 
−
|style="border-style: solid; border-width: 1px"|0.159
 
−
|style="border-style: solid; border-width: 1px"|0.0124
 
−
|style="border-style: solid; border-width: 1px"|0.0628
 
−
|style="border-style: solid; border-width: 1px"|0.0303
 
−
|style="border-style: solid; border-width: 1px"|0.0109
 
−
|style="border-style: solid; border-width: 1px"|0.357
 
−
|style="border-style: solid; border-width: 1px"|0.00156
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-5b
 
−
|style="border-style: solid; border-width: 1px"|0.832
 
−
|style="border-style: solid; border-width: 1px"|0.00619
 
−
|style="border-style: solid; border-width: 1px"|0.126
 
−
|style="border-style: solid; border-width: 1px"|0.0111
 
−
|style="border-style: solid; border-width: 1px"|0.0324
 
−
|style="border-style: solid; border-width: 1px"|0.035
 
−
|style="border-style: solid; border-width: 1px"|0.0096
 
−
|style="border-style: solid; border-width: 1px"|0.397
 
−
|style="border-style: solid; border-width: 1px"|0.00166
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-6a
 
−
|style="border-style: solid; border-width: 1px"|0.0487
 
−
|style="border-style: solid; border-width: 1px"|0.00176
 
−
|style="border-style: solid; border-width: 1px"|0.855
 
−
|style="border-style: solid; border-width: 1px"|0.006
 
−
|style="border-style: solid; border-width: 1px"|0.0856
 
−
|style="border-style: solid; border-width: 1px"|0.0216
 
−
|style="border-style: solid; border-width: 1px"|0.0105
 
−
|style="border-style: solid; border-width: 1px"|0.222
 
−
|style="border-style: solid; border-width: 1px"|0.00199
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-6b
 
−
|style="border-style: solid; border-width: 1px"|0.829
 
−
|style="border-style: solid; border-width: 1px"|0.00561
 
−
|style="border-style: solid; border-width: 1px"|0.127
 
−
|style="border-style: solid; border-width: 1px"|0.00561
 
−
|style="border-style: solid; border-width: 1px"|0.0373
 
−
|style="border-style: solid; border-width: 1px"|0.0252
 
−
|style="border-style: solid; border-width: 1px"|0.00696
 
−
|style="border-style: solid; border-width: 1px"|0.36
 
−
|style="border-style: solid; border-width: 1px"|0.00228
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-1
 
−
|style="border-style: solid; border-width: 1px"|0.41
 
−
|style="border-style: solid; border-width: 1px"|0.000743
 
−
|style="border-style: solid; border-width: 1px"|0.502
 
−
|style="border-style: solid; border-width: 1px"|0.00422
 
−
|style="border-style: solid; border-width: 1px"|0.0811
 
−
|style="border-style: solid; border-width: 1px"|0.0177
 
−
|style="border-style: solid; border-width: 1px"|0.0063
 
−
|style="border-style: solid; border-width: 1px"|0.329
 
−
|style="border-style: solid; border-width: 1px"|0.00132
 
−
|style="border-style: solid; border-width: 1px"|0.00097
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-2
 
−
|style="border-style: solid; border-width: 1px"|0.747
 
−
|style="border-style: solid; border-width: 1px"|0.00309
 
−
|style="border-style: solid; border-width: 1px"|0.225
 
−
|style="border-style: solid; border-width: 1px"|0.00726
 
−
|style="border-style: solid; border-width: 1px"|0.0252
 
−
|style="border-style: solid; border-width: 1px"|0.0447
 
−
|style="border-style: solid; border-width: 1px"|0.00267
 
−
|style="border-style: solid; border-width: 1px"|0.513
 
−
|style="border-style: solid; border-width: 1px"|0.00154
 
−
|style="border-style: solid; border-width: 1px"|0.00097
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-7
 
−
|style="border-style: solid; border-width: 1px"|0.448
 
−
|style="border-style: solid; border-width: 1px"|0.0009
 
−
|style="border-style: solid; border-width: 1px"|0.537
 
−
|style="border-style: solid; border-width: 1px"|0.0041
 
−
|style="border-style: solid; border-width: 1px"|0.0122
 
−
|style="border-style: solid; border-width: 1px"|0.0273
 
−
|style="border-style: solid; border-width: 1px"|0.00346
 
−
|style="border-style: solid; border-width: 1px"|0.433
 
−
|style="border-style: solid; border-width: 1px"|0.00178
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|353-8
 
−
|style="border-style: solid; border-width: 1px"|0.718
 
−
|style="border-style: solid; border-width: 1px"|0.00223
 
−
|style="border-style: solid; border-width: 1px"|0.261
 
−
|style="border-style: solid; border-width: 1px"|0.00608
 
−
|style="border-style: solid; border-width: 1px"|0.0165
 
−
|style="border-style: solid; border-width: 1px"|0.038
 
−
|style="border-style: solid; border-width: 1px"|0.00408
 
−
|style="border-style: solid; border-width: 1px"|0.268
 
−
|style="border-style: solid; border-width: 1px"|0.00177
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|545-1
 
−
|style="border-style: solid; border-width: 1px"|0.991
 
−
|style="border-style: solid; border-width: 1px"|0.00293
 
−
|style="border-style: solid; border-width: 1px"|0.00743
 
−
|style="border-style: solid; border-width: 1px"|0.026
 
−
|style="border-style: solid; border-width: 1px"|0.00139
 
−
|style="border-style: solid; border-width: 1px"| 2.6
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|0.00216
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|545-2
 
−
|style="border-style: solid; border-width: 1px"|0.985
 
−
|style="border-style: solid; border-width: 1px"|0.00277
 
−
|style="border-style: solid; border-width: 1px"|0.0128
 
−
|style="border-style: solid; border-width: 1px"|0.024
 
−
|style="border-style: solid; border-width: 1px"|0.00246
 
−
|style="border-style: solid; border-width: 1px"| 2.8
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|0.00187
 
−
|style="border-style: solid; border-width: 1px"|0.00097
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|545-4
 
−
|style="border-style: solid; border-width: 1px"|0.972
 
−
|style="border-style: solid; border-width: 1px"|0.003
 
−
|style="border-style: solid; border-width: 1px"|0.0277
 
−
|style="border-style: solid; border-width: 1px"|0.025
 
−
|style="border-style: solid; border-width: 1px"|0.000777
 
−
|style="border-style: solid; border-width: 1px"| 2.5
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|0.00222
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|857-1
 
−
|style="border-style: solid; border-width: 1px"|0.974
 
−
|style="border-style: solid; border-width: 1px"|0.00338
 
−
|style="border-style: solid; border-width: 1px"|0.0229
 
−
|style="border-style: solid; border-width: 1px"|0.025
 
−
|style="border-style: solid; border-width: 1px"|0.00349
 
−
|style="border-style: solid; border-width: 1px"| 2.2
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|0.00176
 
−
|style="border-style: solid; border-width: 1px"|0.00111
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|857-2
 
−
|style="border-style: solid; border-width: 1px"|0.84
 
−
|style="border-style: solid; border-width: 1px"|0.00148
 
−
|style="border-style: solid; border-width: 1px"|0.158
 
−
|style="border-style: solid; border-width: 1px"|0.00656
 
−
|style="border-style: solid; border-width: 1px"|0.00249
 
−
|style="border-style: solid; border-width: 1px"| 3.2
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|  0
 
−
|style="border-style: solid; border-width: 1px"|0.0022
 
−
|style="border-style: solid; border-width: 1px"|0.00125
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|857-3
 
−
|style="border-style: solid; border-width: 1px"|0.36
 
−
|style="border-style: solid; border-width: 1px"|4.22e-05
 
−
|style="border-style: solid; border-width: 1px"|0.627
 
−
|style="border-style: solid; border-width: 1px"|0.0024
 
−
|style="border-style: solid; border-width: 1px"|0.0111
 
−
|style="border-style: solid; border-width: 1px"|0.017
 
−
|style="border-style: solid; border-width: 1px"|0.002
 
−
|style="border-style: solid; border-width: 1px"| 1.9
 
−
|style="border-style: solid; border-width: 1px"|0.00152
 
−
|style="border-style: solid; border-width: 1px"|0.00126
 
−
|-
 
−
|style="border-style: solid; border-width: 1px"|857-4
 
−
|style="border-style: solid; border-width: 1px"|0.278
 
−
|style="border-style: solid; border-width: 1px"|0.0004
 
−
|style="border-style: solid; border-width: 1px"|0.719
 
−
|style="border-style: solid; border-width: 1px"|0.00392
 
−
|style="border-style: solid; border-width: 1px"|0.00162
 
−
|style="border-style: solid; border-width: 1px"|0.09
 
−
|style="border-style: solid; border-width: 1px"|0.00152
 
−
|style="border-style: solid; border-width: 1px"| 0.8
 
−
|style="border-style: solid; border-width: 1px"|0.00149
 
−
|style="border-style: solid; border-width: 1px"|0.000558
 
−
|}
 
−
 
 
−
 
 
−
 
 
−
 
 
−
== System (Ken) ==
 
−
===List of systematics===
 
−
 
 
−
{{:HFI-bottom_up}}
 
−
 
 
−
==Summary==
 
−
<span style="color:red">(Lamarre)</span>
 
−
here remind worse sytematics and point to DPC
 
−
Summary of sucess and limitations. JML. Link to early HFI in flight perf.
 

Latest revision as of 09:41, 3 February 2015

This section provides an overview of the High-Frequency Instrument and of its different sub-systems. Two papers that include and detail this information are available: Planck-PreLaunch-III[1] and Planck-Early-IV[2]. Additional detailed information potentially useful for users of HFI data is included in this section or annexed to it.

HFI electronics in the satellite

The HFI instrument is designed around 52 bolometers. Twenty of the bolometers (spider-web bolometers or SWBs) are sensitive to total power, and the remaining 32 units are arranged in pairs of orthogonally-oriented polarisation-sensitive bolometers (PSBs). All bolometers are operated at a temperature of ~0.1 K by means of a space qualified dilution cooler coupled to a high precision temperature control system. A 4He-JT system provides active cooling for 4 K stages using vibration controlled mechanical compressors to prevent excessive warming of the 100 mK stage and minimize microphonic effects in the bolometers. Bolometers and sensitive thermometers are read using an AC-bias scheme through JFET amplifiers operated at ~130 K that provide high sensitivity and low frequency stability. The HFI covers six bands centred at 100, 143, 217, 353, 545, and 857 GHz, thanks to a thermo-optical design consisting of three corrugated horns and a set of compact reflective filters and lenses at cryogenic temperatures.

HFI focal plane optics and 4K thermo-mechanical stage.

The whole satellite is organized to provide thermal transitions between its warm part exposed to radiation from the Sun and Earth, and the focal plane instruments that include the cold receivers (Sections HFI_cold_optics and HFI_detection_chain). The various parts of the HFI are distributed among three different stages of the satellite in order to provide each sub-system with an optimal operating temperature. The "warm" parts, including nearly all the electronics and the sources of fluids of the 4K and 0.1K coolers, are attached and thermally linked to the service module of the satellite. The first stage of the preamplifiers is attached to the back of the passively cooled telescope structure. The focal plane unit is attached to the 20K stage cooled by the sorption cooler. This is detailed in Section HFI_detection_chain.

The telescope and horns select the geometrical origin of photons. They provide a high transmission efficiency to photons inside the main beam, while photons coming from the intermediate and far-side lobes have very low probability of being detected. The essential characteristics are determined by a complex process mixing ground measurements of components (horns, reflectors), modelling the shape of the far sidelobes, and measuring bright sources in-flight, especially planets.

The filters and bolometers define the spectral response and absolute optical efficiency, which are known mostly from ground-based measurements performed at component, sub-system, and system levels, reported in this document. The relationships between spectral response and geometrical response are also addressed.

Photons absorbed by a bolometer include the thermal radiation emitted by the various optical devices: telescope, horns, and filters. They are transformed into heat that propagates to the bolometer thermometer to influence its temperature, which is itself measured by the readout electronics. Temperatures of all these items must be stable enough not to contaminate the scientific signal delivered by the bolometers. How this stability is reached is described in Section HFI_cryogenics.

The bolometer temperature depends also on the temperature of the bolometer plate, on the intensity of the biasing current, and on any spurious inputs, such as cosmic rays and mechanical vibrations. Such systematics are included in a list discussed in Section HFI-Validation.

Since the bolometer thermometer is part of an active circuit that also heats it, the response of this system is complex and has to be considered as a whole. In addition, due to the modulation of the bias current and to the sampling of the data, the response signal of the instrument when scanning a point source is more complex still. Item in Sub-Section Time_response and Annex HFI_time_response_model are dedicated to the description of this time response.

HFI signal formation.

Logic of the formation of the signal in HFI. This is an idealized description of the physics that takes place in the instrument. The optical power that is absorbed by the bolometers comes from the observed sky and from the instrument itself. The bolometers and readout electronics, acting as a single and complex chain, transform this optical power into data that are compressed and transmitted for science data reduction.

References[edit]

  1. ↑ Planck pre-launch status: The HFI instrument, from specification to actual performance, J.-M. Lamarre, J.-L. Puget, P. A. R. Ade, F. Bouchet, G. Guyot, A. E. Lange, F. Pajot, A. Arondel, K. Benabed, J.-L. Beney, A. Benoît, J.-P. Bernard, R. Bhatia, Y. Blanc, J. J. Bock, E. Bréelle, T. W. Bradshaw, P. Camus, A. Catalano, J. Charra, M. Charra, S. E. Church, F. Couchot, A. Coulais, B. P. Crill, M. R. Crook, K. Dassas, P. de Bernardis, J. Delabrouille, P. de Marcillac, J.-M. Delouis, F.-X. Désert, C. Dumesnil, X. Dupac, G. Efstathiou, P. Eng, C. Evesque, J.-J. Fourmond, K. Ganga, M. Giard, R. Gispert, L. Guglielmi, J. Haissinski, S. Henrot-Versillé, E. Hivon, W. A. Holmes, W. C. Jones, T. C. Koch, H. Lagardère, P. Lami, J. Landé, B. Leriche, C. Leroy, Y. Longval, J. F. Macías-Pérez, T. Maciaszek, B. Maffei, B. Mansoux, C. Marty, S. Masi, C. Mercier, M.-A. Miville-Deschênes, A. Moneti, L. Montier, J. A. Murphy, J. Narbonne, M. Nexon, C. G. Paine, J. Pahn, O. Perdereau, F. Piacentini, M. Piat, S. Plaszczynski, E. Pointecouteau, R. Pons, N. Ponthieu, S. Prunet, D. Rambaud, G. Recouvreur, C. Renault, I. Ristorcelli, C. Rosset, D. Santos, G. Savini, G. Serra, P. Stassi, R. V. Sudiwala, J.-F. Sygnet, J. A. Tauber, J.-P. Torre, M. Tristram, L. Vibert, A. Woodcraft, V. Yurchenko, D. Yvon, A&A, 520, A9+, (2010).
  2. ↑ Planck early results, IV. First assessment of the High Frequency Instrument in-flight performance, Planck HFI Core Team, A&A, 536, A4, (2011).

(Planck) High Frequency Instrument

Junction Field Elect Transistor

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