Difference between revisions of "HFI detection chain"

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The heart of the HFI - the detectors - are bolometers, solid-state devices in which the
 
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
 
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
+
thermometer. The instrument Flight Model total number of bolometers is 52, split into six
−
channels at central frequencies of 100, 143, 217, 353, 545, and 857GHz.  
+
channels at central frequencies of 100, 143, 217, 353, 545, and 857 GHz.  
−
Two extra bolometers not optically coupled to the telescope are added to the focal plane
+
Two extra bolometers, not optically coupled to the telescope, are added to the focal plane
−
to monitor thermal noise (Dark Bolometers).  
+
to monitor thermal noise (dark bolometers).  
  
−
Thirty two of these bolometers are polarization sensitive allowing a map of the CMB polarisation to be built.
+
The bolometers consist of:
 +
* an absorber that transforms the in-coming radiation into heat;
 +
* a semi-conducting NTD thermistor that is thermally linked to the absorber and measures the temperature changes;
 +
* and a weak thermal link to a thermal sink, to which the bolometer is attached.
  
 +
There are two kinds of detector modules: polarization-sensitive bolometers (PSBs) and spider-web bolometers (SWBs).
  
−
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.
+
'''Spider-web bolometers''' {{BibCite|Bock1995}}{{BibCite|Mauskopf1997}}
  
−
 
+
In these bolometers, the absorber consists of a metallic grid deposited on a Si3 N4 substrate in the shape of a spider web.
−
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
 
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
+
adjusted to match vacuum impedance and maximize the absorption of millimetre waves, while minimizing the cross-section to
 
particles. The absorber is designed to offer equal impedance to
 
particles. The absorber is designed to offer equal impedance to
−
any linearly polarised radiation. Nevertheless, the thermometer
+
any linearly polarized radiation. Nevertheless, the thermometer
−
and its electrical leads define a privileged orientation (Fig. SWB) that
+
and its electrical leads define a privileged orientation that
−
makes the SWBs slightly sensitive to polarisation, as detailed in
+
makes the SWBs slightly sensitive to polarization, as detailed in
−
(Rosset et al. 2010). The thermometers are
+
{{PlanckPapers|rosset2010}}. The thermometers are
−
made of neutron transmuted doped (NTD) germanium (Haller
+
made of neutron transmutation doped (NTD) germanium {{BibCite|Haller1996}}, chosen to have an impedance of about 10 MΩ at
−
et al. 1996), chosen to have an impedance of about 10 MΩ at
 
 
their operating temperature.
 
their operating temperature.
  
 +
[[Image:HFI_2_4_1_FPiacentini_bolo1.png|thumb|500px|center|Picture of a spider-web bolometer. This a 143 GHz module. The temperature sensor is at the centre of the absorbing grid.]]
  
−
[[Image:HFI_2_4_1_FPiacentini_bolo1.png|thumb|500px|Picture of a spider web bolometer. This a 143 GHz module, The temperature sensor is at the center of the absorbing grid]]
+
'''Polarization-sensitive bolometers'''
−
 
 
  
−
The absorber of PSBs is a rectangular grid (Fig. PSB) with metallization in one direction (Jones et al.
+
The absorber of PSBs is a rectangular grid with metallization in one direction {{BibCite|Jones2003}}. Electrical fields parallel to this direction develop currents and then deposit some energy 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 polarization. Such a PSB pair measures two polarizations of radiation collected by the same horns and filtered by the same devices, which minimizes the systematic effects; differences between polarized
−
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
 
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
+
the peak. The differences in the spectral responses of a PSB pair have
 
also proved to be a few percent in the worst case. Each 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
 
of PSBs sharing the same horn is able to measure the intensity
−
Stokes parameter and the Q parameter associated with its local
+
Stokes parameter and the <I>Q</I> parameter associated with its local
−
frame. An associated pair of PSBs rotated by 45◦ scans exactly
+
frame. An associated pair of PSBs rotated by 45&deg; scans exactly
 
the same line (if the geometrical alignment is perfect), providing
 
the same line (if the geometrical alignment is perfect), providing
−
the U Stokes parameter.
+
the <I>U</I> Stokes parameter.
−
 
 
  
−
[[Image:HFI_2_4_1_FPiacentini_bolo2.png|thumb|500px|Picture of a polarization sensitive bolometer. This a 217 GHz module, The temperature sensor is at the an edge of the absorbing grid]]
+
[[Image:HFI_2_4_1_FPiacentini_bolo2.png|thumb|500px|center|Picture of a polarization-sensitive bolometer. This is a 217 GHz module. The temperature sensor is located at one edge of the absorbing grid.]]
  
−
 
+
The detectors operate at a temperature close to 100 mK, while the filters are distributed on the 100-mK, 1.6-K,
−
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
−
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
 
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 heat lift requirement and thus enhance the mission lifetime. The self-emission of the 4-K stage is minimized to limit the photon noise contribution on the detectors from the instrument.
−
The HFI Focal Plane Unit accommodates sub-millimiter absorbing
+
The HFI Focal Plane Unit accommodates sub-millimitre absorbing
 
material in order to decrease the scattering inside it.
 
material in order to decrease the scattering inside it.
  
  
−
[[Image:HFI_2_4_1_FPiacentini_table1.png|thumb|500px|to be change into a real table]]
+
[[Image:HFI_2_4_1_FPiacentini_table1.png|thumb|500px|center| ]]
  
 
==Focal plane layout==
 
==Focal plane layout==
  
−
The layout of the detectors in the focal plane is defined to cope with the
+
The layout of the detectors in the focal plane is defined in relation to the
 
scanning strategy. The HFI horns are positioned at the centre of the focal plane, where the optical
 
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
 
quality is good enough for the high frequencies. The curvature of
 
rows compensates for the distortion of images by the telescope.
 
rows compensates for the distortion of images by the telescope.
−
A pair of identical SWB will scan the same circle on the sky to
+
A pair of identical SWBs will scan the same circle on the sky to
−
provide additional redundancy. Similar horns feeding PSBs are
+
provide 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
+
also aligned so that two PSBs rotated by 45&deg; with respect to each other scan the same line. This will provide the <I>Q</I> and <I>U</I> Stokes parameters with minimal correction for the pointing {{PlanckPapers|rosset2010}}). 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
−
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. The focal plane layout is reported in the figures.  
−
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.  
 
  
−
[[Image:HFI_2_4_1_FPiacentini_FocalPlaneLayout.png|thumb|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
+
[[Image:HFI_2_4_1_FPiacentini_FocalPlaneGeo.png|thumb|500px|center|Focal plane layout as seen from outside the celestial sphere. PSB orientations are indicated, with a red rod for the "a" elements and a blue rod for the "b" elements. The scan direction is from left to right.]]
−
left to right.]]
 
−
 
 
−
[[Image:HFI_2_4_1_FPiacentini_FocalPlaneGeo.png|thumb|500px|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==
 
==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 AC bias readout electronics of the HFI instrument {{BibCite|Gaertner1997}} includes the following features:
−
 
+
* the cold load resistors were replaced by capacitors because they have no Johnson noise;
−
 
+
* the detectors are biased by applying a triangular voltage to the load capacitors, which produces a square current (I-bias) 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);
−
The particular features of the HFI AC bias readout are mainly
+
* a square offset compensation signal is subtracted from the bolometric signal to minimize the amplitude of the signal that has to be amplified and digitized;
−
 
+
* the electronic scheme is symmetrical and uses a differential amplification scheme to optimize the immunity to electromagnetic interference;
 +
* and finally every parameter of the REU can be set by commands, which is made possible by extensively using digital-to-analogue and analogue-to-digital converters.
  
−
* i)that the cold load resistors were replaced by capacitors because they have no Johnson noise;
+
The readout electronics consists of 72 channels designed to perform low noise measurements of the impedance of 52 bolometers, two blind bolometers, and 16 accurate low-temperature thermometers, all in the 10 MΩ range, together with one resistor of 10 MΩ and one capacitor of 100 pF. The semiconductor bolometers and thermometers of Planck-HFI operate at cryogenic temperatures around 100 mK on the focal plane, with impedance of about 10 MΩ when biased at the optimal current. The readout electronics, on the other hand, has to operate at “room” temperature (300 K). The distance between the two extremities of the readout chain is about 10 m and this could bring about an extreme susceptibility to electromagnetic interference. The readout electronics chain was therefore 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 1.8 m 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.  
−
* 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.
 
  
 +
[[Image:HFI_2_4_1_FPiacentini_HFIreadout.png|thumb|500px|center|Principles of readout electronics. The three modules of the chain are shown: JFET box; Pre-Amplifier Unit (PAU); and Readout Electronic Unit (REU)]]
  
−
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
+
[[Image:HFI_2_4_1_FPiacentini_table2.jpeg|thumb|500px|center|Organization of the HFI readout. Each row represents a belt. Each belt has six channels.]]
−
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).
 
−
 
 
−
[[Image:HFI_2_4_1_FPiacentini_HFIreadout.png|thumb|500px|Principles of readout electronics. The three modules of the chain are shown: JFet Box, Pre-Amplifier Unit (PAU) and Readout Electronic Unit (REU)]]
 
−
 
 
−
[[Image:HFI_2_4_1_FPiacentini_table2.jpeg|thumb|500px|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 ==
 
==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.
+
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 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 dynamics of the chain is controlled by the V-bal parameter.
−
 
 
−
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.
 
  
 +
The following parameters of the Readout Unit can be set to optimize the detector performance:
 +
* fmod, the modulation frequency of the square bias current, which was set to 90.18685;
 +
* Nsample, which defines the number of samples per half period of modulated, which signal was set to 40.
  
 
Each channel has its own settings for the following parameters:
 
Each channel has its own settings for the following parameters:
−
I-bias, amplitude of the triangular bias voltage;
+
* I-bias, the amplitude of the triangular bias voltage;
−
 
+
* T-bias, the amplitude of the transient bias voltage;
−
T-bias, amplitude of the transient bias voltage;
+
* V-bal, the amplitude of the square compensation voltage;
−
 
+
* G-amp, the value of the programmable gain of the REU [1/3, 1, 3, 7.6];
−
V-bal, amplitude of the square compensation voltage;
+
* N-blank, the number of blanked samples at the beginning of each half period not taken into account during integration of the signal;
−
 
+
* S-phase, the phase shift when computing the integrated signal.
−
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
 
All these parameters influence the effective response of the
 
detection chains, and were optimized during the calibration  
 
detection chains, and were optimized during the calibration  
 
campaigns and confirmed during the calibration and performance
 
campaigns and confirmed during the calibration and performance
−
verification (CPV) phase following the launch of
+
verification phase following the launch of
 
Planck. The scientific signal is provided by the integral of the
 
Planck. The scientific signal is provided by the integral of the
−
signal on each half-period, between limits fixed by the S-phase
+
signal over each half-period, between limits fixed by the S-phase
 
and N-blank parameters.
 
and N-blank parameters.
  
Line 141: Line 109:
 
The interaction of modulated readout electronics with semiconductor
 
The interaction of modulated readout electronics with semiconductor
 
bolometers is rather different from that of a classical
 
bolometers is rather different from that of a classical
−
DC bias readout (Jones 1953). The differences were seen during
+
DC bias readout {{BibCite|Jones1953}}. The differences were seen during
 
the calibration of the HFI, although the readout electronics
 
the calibration of the HFI, although the readout electronics
 
was designed to mimic the operation
 
was designed to mimic the operation
−
of a DC biased bolometric system as far as possible. With the
+
of a DC-biased bolometric system as far as possible. With the
 
AC readout the maximum of responsivity is lower and is obtained
 
AC readout the maximum of responsivity is lower and is obtained
 
for higher bias current in the bolometer with respect to the DC model.
 
for higher bias current in the bolometer with respect to the DC model.
 
This is caused by the stray capacitance in the
 
This is caused by the stray capacitance in the
−
wiring which has negligible effects for a DC bias and a major
+
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
 
effect for an AC bias. In our case, a stray capacitance of 150 pF
−
induces increases of NEP ranging from 4% (857 GHz bolometers)  
+
induces increases of NEP, ranging from 4% (857 GHz bolometers)  
−
to 10% (100 GHz bolometers) and also affects the HFI time
+
to 10% (100 GHz bolometers), and also affects the HFI time
−
response. Details of the effect of the HFI AC bias system into
+
response. Details of the effect of the HFI AC bias system on
 
the time response of the detectors are discussed in the  
 
the time response of the detectors are discussed in the  
−
[http://www.sciops.esa.int/wikiSI/planckpla/index.php?title=HFI_design,_qualification,_and_performance&instance=Planck_PLA_ES#Time_response| Time Response] Section.
+
[[HFI_detection_chain#Time_response| time response section]].
  
 
== JFETs==
 
== 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.  
+
Given the high impedance of the bolometers and the length of the connecting cables, it is  essential that the impedance of the signal is lowered as close as possible to that of the detectors. In our system this is accomplished by means of JFET source followers, located in boxes connected to the 50-K stage {{BibCite|Brienza2006}}. 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.
−
The JFET box has been designed, developed and tested in the Observational Cosmology group in the Physics Department of the University of Rome "La Sapienza" (Brienza D. et al 2006).
 
−
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%.
+
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 Hz<sup>1/2</sup> for the frequency range of interest. This increases the total noise of all bolometer channels by less than 5%.
  
 +
== Time response ==
  
−
==Data compression==
+
The HFI bolometers and readout electronics have a finite response-time to changes of the incident optical power, modelled as a Fourier domain transfer function, consisting of the product of a bolometer thermal response <I>F</I>(&omega;) and an electronics response <I>H'</I>(&omega;):
  
−
===Data compression scheme===
+
<math>\label{LFER4def}TF^{LFER}(\omega) = F(\omega) H'(\omega)</math>.
−
 
 
−
The output of the readout electronics unit (REU) consists of one
 
−
value for each of the 72 science channels (bolometers and thermometers) for each modulation half-period. This number, <math>S_{REU}</math>, is the sum
 
−
of the 40 16-bit ADC signal values measured within the given
 
−
half-period. The data processor unit (DPU) performs a lossy
 
−
quantization of <math>S_{REU}</math>.
 
  
−
We define a compression slice of 254 <math>S_{REU}</math> values, corresponding
+
The first part represents the bolometer thermal response, driven by its heat capacity, by the thermal link to the bolometer plate at 100 mK, and by the thermo-electrical feed-back {{BibCite|catalano2010}} resulting from the heat deposited in the bolometer by the readout electronics. This factor is empirically obtained from the observation of sources. The second factor is simply the time response of the part of the readout electronics that amplifies and digitizes the signal. It is obtained by modelling the electronics using only a very few free parameters.
−
to about 1.4 s of observation for each detector and to a
 
−
strip on the sky about 8 degrees long. The mean <math>\langle S_{REU} \rangle</math> of the data within
 
−
each compression slice is computed, and data are demodulated
 
−
using this mean:
 
  
−
<math>S_{demod,i} = (S_{REU,i} - \langle S_{REU} \rangle) \ast(-)^{i}</math>
+
Due to Planck's nearly constant scan rate, the time response is degenerate with the optical beam.  However, because of the long timescale 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]]).  <I>F</I>(&omega;) is tuned to optimize the "compactness" of the beams reconstructed with the deconvolved signal from planets.
  
−
where <math>1 < i < 254</math> is the running index within the compression slice.
+
The model developed and applied to the 2013 release data (PR1, see {{PlanckPapers|planck2013-p03c}}) is referred to as the LFER4 model.  
  
−
The mean <math>\langle S_{demod} \rangle</math> of the demodulated data <math>S_{demod,i}</math>
+
For the 2015 (PR2) release (see {{PlanckPapers|planck2014-a08}}), as well as for the 2018 (PR3) release, five time constants are used rather than four, and the values of the parameters have been measured from a different combination of data than used previously. The extra low-pass function and the consequent parameter updates are motivated by the discovery of a time delay between the measured CMB dipole and the expected one. In addition, new information comes from the stacking of glitches induced by high energy particles hits. As described in Planck Collaboration X (2014), short glitches are due to direct interaction of particles with the bolometer grid or thermistor. The time response of short events is then representative of the response to photons, and glitches can be stacked to determine time response constants. In summary, the values of the bolometer time transfer function parameters, ai and τi, are measured with the following logic:
−
is computed and subtracted, and the resulting slice data is quantized
+
* the two fastest time constants, τ1 and τ2, and the associated amplitudes a1 and a2, are unchanged with respect to the previous version, i.e., they are estimated from planet observations;
−
according to a step size Q that is fixed per detector:
+
* the two longest time constants, τ4 and τ5, are estimated from short glitch stacking, together with the a5/a4 ratio;
 +
* τ3, a3, and a4 are fitted from Jupiter scans, keeping τ1, a1, τ2, and a2 fixed, while the value of a5 is set to keep the same ratio a5/a4 as in the glitch data;
 +
* a5 is fitted from the CMB dipole time shift. It should be noted that the same dipole time shift can be obtained with different combinations of a5 and τ5 and for this reason, τ5 is recovered from the short glitches, and only a5 from the dipole time shift.
  
−
<math> S_{DPU,i} = \mbox{round} \left[( S_{demod,i} - \langle S_{demod} \rangle) /Q \right ] </math>
+
Details about the time response models of PR1 and PR2 can be found in [[HFI_time_response_model | this annex]].
  
−
This is the lossy part of the algorithm: the required compression
+
==Data compression==
−
factor, obtained through the tuning of the quantization step Q,
 
−
adds a noise of variance <math> \simeq 2\% </math> to the data. This will be discussed below.
 
  
−
The two means
+
The output of the readout electronics unit (REU) consists of one
−
<math>\langle S_{REU} \rangle</math>
+
value for each of the 72 science channels (bolometers and thermometers) for each modulation half-period. This number, <I>S</I><sub>REU</sub>, is the sum
−
and
+
of the 40 16-bit ADC signal values measured within the given
−
<math>\langle S_{demod} \rangle</math>
+
half-period. The data processor unit (DPU) performs a lossy
−
are computed as
+
quantization of <I>S</I><sub>REU</sub>.
−
32-bit words and sent through the telemetry, together with the
 
−
<math>S_{DPU,i}</math> values.
 
−
Variable-length encoding of the <math>S_{DPU,i}</math> values is
 
−
performed on board, and the inverse decoding is applied on
 
−
ground.
 
−
 
 
−
===Performance of the data compression during the mission===
 
−
 
 
−
Optimal use of the bandpass available for the downlink was obtained initially by using a value
 
−
of Q = <math>\sigma</math>/2.5 for all bolometer signals.
 
−
After the 12th of December 2009, and only for the 857 GHz detectors, the
 
−
value was reset to Q = <math>\sigma</math>/2.0 to avoid data loss
 
−
due to exceeding the limit of downlink rate.
 
−
With these settings the load during the mission never exceeded the
 
−
allowed band-pass width as is seen on the next figure.
 
−
 
 
−
[[Image:meankbits.png|500px|Evolution of the total load during the mission for the 72
 
−
    HFI channels. The variations are mainly due to
 
−
    the time spent by the high-frequency channels in the Galactic
 
−
    region, which has very large data gradients, and depends on the satellite scanning strategy.
 
−
    The bandpass-width limit was 80kb/s and was never
 
−
    reached during the mission.]]
 
−
 
 
−
 
 
−
===Setting the quantization step in flight===
 
−
 
 
−
 
 
−
The only parameter that enters the PLANCK-HFI compression algorithm is
 
−
the size of the quantization step, in units of <math>\sigma</math>, the white
 
−
noise standard deviation for each channel.
 
−
It has been adjusted during the mission by studying the mean frequency of
 
−
the central quantization bin [-Q/2,Q/2], <math>p_0</math> within each compression
 
−
slice (254 samples).
 
−
For a pure Gaussian noise, this frequency is related to the
 
−
step size (in units of <math>\sigma</math>) by
 
−
<math>
 
−
  \hat Q =2\sqrt{2} \text{Erf}^{-1}(p_0)\simeq 2.5 p_0
 
−
</math>
 
−
where the approximation is valid up to <math>p_0 <0.4</math>.
 
−
In PLANCK, however, the channel signal is not a pure Gaussian, since
 
−
glitches and the periodic crossing of the Galactic plane add some
 
−
strong outliers to the distribution.
 
−
By using the frequency of these outliers, <math>p_\text{out}</math>, above <math>5
 
−
\sigma</math>, simulations show that the following formula gives a valid
 
−
estimate:
 
−
<math>
 
−
  \hat Q_\text{cor}=2.5 \frac{p_0}{1-p_\text{out}}
 
−
</math>
 
−
 
 
−
The following figure shows an example of the <math>\hat Q</math> and
 
−
<math>\hat Q_\text{cor}</math> timelines that were used to monitor and adjust the
 
−
quantization setting.
 
−
 
 
−
[[Image:setting.png|500px|Example of the "bin0" frequency timeline (1 point per
 
−
      compression slice) <math>p_0</math> (labeled "ZERO") for one of the channels.
 
−
      The -1 ("NEG1") and +1 ("POS1") bin frequencies are also shown.  
 
−
      The lower plot shows
 
−
      the frequency timeline of outliers, where the glitches and
 
−
      periodic crossing of the Galaxy are visible. The estimated raw
 
−
      step size <math>\hat Q=0.47</math> and corrected value <math>\hat
 
−
      Q_\text{cor}=0.49</math> are automatically computed and the step size
 
−
      can be adjusted according to these control plots.]]
 
−
 
 
−
===Impact of data compression on science===
 
−
The effect of pure quantization process of step <math>Q</math> (in <math>\sigma</math>
 
−
units) onto the statistical moments of
 
−
a signal is well known (<cite>#widrow</cite>)
 
−
When the step is typically below the noise level (which is largely the PLANCK
 
−
case) one can apply the Quantization Theorem which states that the
 
−
process is equivalent to the addition of a uniform random noise in the
 
−
<math>[-Q/2,Q/2]</math> range.
 
−
The net effect of quantization is therefore to add quadratically to the
 
−
signal a <math>Q^2/12</math> variance. For <math>Q\simeq 0.5</math> this corresponds to a
 
−
2\% noise level increase.
 
−
The spectral effect of the non-linear process of quantization is theoretically much more
 
−
complicated and depends on the signal and noise details. As a rule of
 
−
thumb, a pure quantization adds some auto-correlation function that is
 
−
suppressed by a <math>\exp[-4\pi^2(\frac{\sigma}{Q})^2]</math> factor <cite>#banta</cite>.
 
−
Note however that PLANCK does not perform a pure quantization
 
−
process. A baseline which
 
−
depends on the data (mean of each compression slice values),
 
−
is subtracted. Furthermore, for science data, circles
 
−
on the sky are coadded. Coaddition is again performed when
 
−
projecting the rings onto the sky (map-making).
 
−
To study the full effect of the PLANCK-HFI data compression
 
−
algorithm onto our main science observable, we have simulated a
 
−
realistic data timeline corresponding to the observation of a pure CMB
 
−
sky. The compressed/decompressed signal was then back-projected onto
 
−
the sky using PLANCK scanning strategy.
 
−
The two maps were analyzed using the \texttt{anafast} Healpix
 
−
procedure and both reconstructed <math>C_\ell</math> were compared. The result is
 
−
shown for a quantization step <math>Q=0.5</math>.
 
  
−
[[Image:cl_DPU_217unlensed.png|500px|Effect of the PLANCK compression algorithm onto the reconstructed
+
Details about the data compression scheme, performance of the data compression during the mission, setting the quantization step in flight, and the impact of the data compression on science, are given in [[HFI_data_compression | this annex]].
−
power spectrum (<math>C_\ell</math>) after data projection and map-making,
 
−
according to the simulation. The
 
−
upper plot shows the input reconstructed CMB power spectrum (black), the CMB+noise
 
−
spectrum for this channel (blue, barely noticeable) and the
 
−
reconstructed <math>C_\ell</math>)  when including in the chain data compression
 
−
(red).
 
−
The lower plot shows these last two
 
−
ratio and confirms the white nature of the final added noise at its
 
−
level that can still be computed by the Quantization Theorem
 
−
(2\% for <math>Q=0.5</math> used here).]]
 
  
 +
== References ==
 +
<References />
  
−
It is remarkable that the full procedure of
+
−
baseline-subtraction+quantization+ring-making+map-making still leads to the 2\% increase of the
 
−
variance that is predicted by the simple timeline quantization (for <math>Q/\sigma=2</math>).
 
−
Furthermore we check that the noise added by the compression algorithm is white.
 
  
−
It is not expected that the compression brings any non-gaussiannity,
 
−
since the pure quantization process does not add any skewness and less
 
−
than 0.001 kurtosis, and coaddition of circles and then rings erases
 
−
any non-gaussian contribution according to the Central Limit Theorem.
 
  
−
<biblio force=false>
+
[[Category:HFI design, qualification and performance|003]]
−
#[[References]]
 
−
</biblio>
 

Latest revision as of 21:36, 19 June 2018

Bolometers[edit]

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 six channels at central frequencies of 100, 143, 217, 353, 545, and 857 GHz. Two extra bolometers, not optically coupled to the telescope, are added to the focal plane to monitor thermal noise (dark bolometers).

The bolometers consist of:

  • an absorber that transforms the in-coming radiation into heat;
  • a semi-conducting NTD thermistor that is thermally linked to the absorber and measures the temperature changes;
  • and a weak thermal link to a thermal sink, to which the bolometer is attached.

There are two kinds of detector modules: polarization-sensitive bolometers (PSBs) and spider-web bolometers (SWBs).

Spider-web bolometers [1][2]

In these bolometers, the absorber consists of a metallic grid 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 millimetre waves, while minimizing the cross-section to particles. The absorber is designed to offer equal impedance to any linearly polarized radiation. Nevertheless, the thermometer and its electrical leads define a privileged orientation that makes the SWBs slightly sensitive to polarization, as detailed in Planck-PreLaunch-XIII[3]. The thermometers are made of neutron transmutation doped (NTD) germanium [4], chosen to have an impedance of about 10 MΩ at their operating temperature.

Picture of a spider-web bolometer. This a 143 GHz module. The temperature sensor is at the centre of the absorbing grid.

Polarization-sensitive bolometers

The absorber of PSBs is a rectangular grid with metallization in one direction [5]. Electrical fields parallel to this direction develop currents and then deposit some energy 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 polarization. Such a PSB pair measures two polarizations of radiation collected by the same horns and filtered by the same devices, which minimizes the systematic effects; differences between polarized 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 have 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.

Picture of a polarization-sensitive bolometer. This is a 217 GHz module. The temperature sensor is located at one edge of the absorbing grid.

The detectors operate at a temperature close to 100 mK, while the filters are distributed on the 100-mK, 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 4-K stage is minimized to limit the photon noise contribution on the detectors from the instrument. The HFI Focal Plane Unit accommodates sub-millimitre absorbing material in order to decrease the scattering inside it.


HFI 2 4 1 FPiacentini table1.png

Focal plane layout[edit]

The layout of the detectors in the focal plane is defined in relation to 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 SWBs will scan the same circle on the sky to provide redundancy. Similar horns feeding PSBs are also aligned so that two 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 Planck-PreLaunch-XIII[3]). 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. The focal plane layout is reported in the figures.

Focal plane layout as seen from outside the celestial sphere. PSB orientations are indicated, with a red rod for the "a" elements and a blue rod for the "b" elements. The scan direction is from left to right.

Readout[edit]

The AC bias readout electronics of the HFI instrument [6] includes the following features:

  • the cold load resistors were replaced by capacitors because they have no Johnson noise;
  • the detectors are biased by applying a triangular voltage to the load capacitors, which produces a square current (I-bias) 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);
  • a square offset compensation signal is subtracted from the bolometric signal to minimize the amplitude of the signal that has to be amplified and digitized;
  • the electronic scheme is symmetrical and uses a differential amplification scheme to optimize the immunity to electromagnetic interference;
  • and finally every parameter of the REU can be set by commands, which is made possible by extensively using digital-to-analogue and analogue-to-digital converters.

The readout electronics consists of 72 channels designed to perform low noise measurements of the impedance of 52 bolometers, two blind bolometers, and 16 accurate low-temperature thermometers, all in the 10 MΩ range, together with one resistor of 10 MΩ and one capacitor of 100 pF. The semiconductor bolometers and thermometers of Planck-HFI operate at cryogenic temperatures around 100 mK on the focal plane, with impedance of about 10 MΩ when biased at the optimal current. The readout electronics, on the other hand, has to operate at “room” temperature (300 K). The distance between the two extremities of the readout chain is about 10 m and this could bring about an extreme susceptibility to electromagnetic interference. The readout electronics chain was therefore 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 1.8 m 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.

Principles of readout electronics. The three modules of the chain are shown: JFET box; Pre-Amplifier Unit (PAU); and Readout Electronic Unit (REU)
Organization of the HFI readout. Each row represents a belt. Each belt has six channels.

Principles of the readout electronics[edit]

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 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 dynamics of the chain is controlled by the V-bal parameter.

The following parameters of the Readout Unit can be set to optimize the detector performance:

  • fmod, the modulation frequency of the square bias current, which was set to 90.18685;
  • Nsample, which defines the number of samples per half period of modulated, which signal was set to 40.

Each channel has its own settings for the following parameters:

  • I-bias, the amplitude of the triangular bias voltage;
  • T-bias, the amplitude of the transient bias voltage;
  • V-bal, the amplitude of the square compensation voltage;
  • G-amp, the value of the programmable gain of the REU [1/3, 1, 3, 7.6];
  • N-blank, the number of blanked samples at the beginning of each half period not taken into account during integration of the signal;
  • S-phase, the 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 phase following the launch of Planck. The scientific signal is provided by the integral of the signal over 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 [7]. 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 on the time response of the detectors are discussed in the time response section.

JFETs[edit]

Given the high impedance of the bolometers and the length of the connecting cables, it is essential that the impedance of the signal is lowered as close as possible to that of the detectors. In our system this is accomplished by means of JFET source followers, located in boxes connected to the 50-K stage [8]. 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 of all bolometer channels by less than 5%.

Time response[edit]

The HFI bolometers and readout electronics have a finite response-time to changes of the incident optical power, modelled as a Fourier domain transfer function, consisting of the product of a bolometer thermal response F(ω) and an electronics response H'(ω):

[math]\label{LFER4def}TF^{LFER}(\omega) = F(\omega) H'(\omega)[/math].

The first part represents the bolometer thermal response, driven by its heat capacity, by the thermal link to the bolometer plate at 100 mK, and by the thermo-electrical feed-back [9] resulting from the heat deposited in the bolometer by the readout electronics. This factor is empirically obtained from the observation of sources. The second factor is simply the time response of the part of the readout electronics that amplifies and digitizes the signal. It is obtained by modelling the electronics using only a very few free parameters.

Due to Planck's nearly constant scan rate, the time response is degenerate with the optical beam. However, because of the long timescale effects present in the time response, the time response is deconvolved from the data in the processing of the HFI data (see TOI processing). F(ω) is tuned to optimize the "compactness" of the beams reconstructed with the deconvolved signal from planets.

The model developed and applied to the 2013 release data (PR1, see Planck-2013-VII[10]) is referred to as the LFER4 model.

For the 2015 (PR2) release (see Planck-2015-A07[11]), as well as for the 2018 (PR3) release, five time constants are used rather than four, and the values of the parameters have been measured from a different combination of data than used previously. The extra low-pass function and the consequent parameter updates are motivated by the discovery of a time delay between the measured CMB dipole and the expected one. In addition, new information comes from the stacking of glitches induced by high energy particles hits. As described in Planck Collaboration X (2014), short glitches are due to direct interaction of particles with the bolometer grid or thermistor. The time response of short events is then representative of the response to photons, and glitches can be stacked to determine time response constants. In summary, the values of the bolometer time transfer function parameters, ai and τi, are measured with the following logic:

  • the two fastest time constants, τ1 and τ2, and the associated amplitudes a1 and a2, are unchanged with respect to the previous version, i.e., they are estimated from planet observations;
  • the two longest time constants, τ4 and τ5, are estimated from short glitch stacking, together with the a5/a4 ratio;
  • τ3, a3, and a4 are fitted from Jupiter scans, keeping τ1, a1, τ2, and a2 fixed, while the value of a5 is set to keep the same ratio a5/a4 as in the glitch data;
  • a5 is fitted from the CMB dipole time shift. It should be noted that the same dipole time shift can be obtained with different combinations of a5 and τ5 and for this reason, τ5 is recovered from the short glitches, and only a5 from the dipole time shift.

Details about the time response models of PR1 and PR2 can be found in this annex.

Data compression[edit]

The output of the readout electronics unit (REU) consists of one value for each of the 72 science channels (bolometers and thermometers) for each modulation half-period. This number, SREU, is the sum of the 40 16-bit ADC signal values measured within the given half-period. The data processor unit (DPU) performs a lossy quantization of SREU.

Details about the data compression scheme, performance of the data compression during the mission, setting the quantization step in flight, and the impact of the data compression on science, are given in this annex.

References[edit]

  1. ↑ A Novel Bolometer for Infrared and Millimeter-Wave Astrophysics, J. J. Bock, D. Chen, P. D. Mauskopf, A. E. Lange, Space Science Reviews, 74, 229-235, (1995).
  2. ↑ Composite infrared bolometers with Si 3 N 4 micromesh absorbers, P. D. Mauskopf, J. J. Bock, H. del Castillo, W. L. Holzapfel, A. E. Lange, Appl. Opt, 36, 765-771, (1997).
  3. ↑ 3.03.1 Planck pre-launch status: High Frequency Instrument polarization calibration, C. Rosset, M. Tristram, N. Ponthieu, et al. , A&A, 520, A13+, (2010).
  4. ↑ Neutron Transmutation Depot (NTD) Germanium Thermistors for Submillimetre Bolometer Applications, E. E. Haller, K. M. Itoh, J. W. Beeman, in Submillimetre and Far-Infrared Space Instrumentation E. J. Rolfe, G. Pilbratt (Ed.), ESA Special Publication, 388, 115-+, (1996).
  5. ↑ A Polarization Sensitive Bolometric Receiver for Observations of the Cosmic Microwave Background, W. C. Jones, R. Bhatia, J. J. Bock, A. E. Lange, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series T. G. Phillips, J. Zmuidzinas (Ed.), Presented at the Society of Photo-Optical Instrumentation Engineers (SPIE) Conference, 4855, 227-238, (2003).
  6. ↑ A new readout system for bolometers with improved low frequency stability, S. Gaertner, A. Benoît, J.-M. Lamarre, M. Giard, J.-L. Bret, J.-P. Chabaud, F.-X. Desert, J.-P. Faure, G. Jegoudez, J. Lande, J. Leblanc, J.-P. Lepeltier, J. Narbonne, M. Piat, R. Pons, G. Serra, G. Simiand, A&As, 126, 151-160, (1997).
  7. ↑ The general theory of bolometer performance, R. C. Jones, Journal of the Optical Society of America (1917-1983), 43, 1-+, (1953).
  8. ↑ Cryogenic pre-amplifiers for high resistance bolometers, D., de Angelis, L., de Bernardis, P., et al., Brienza, in Seventh International Workshop on Low Temperature Electronics WOLTE-7, ESA-WPP-264283, (2006).
  9. ↑ Analytical approach to optimizing alternating current biasing of bolometers, A. Catalano, A. Coulais, J.-M. Lamarre, Appl. Opt., 49, 5938--5946, (2010).
  10. ↑ Planck 2013 results. VII. HFI time response and beams, Planck Collaboration, 2014, A&A, 571, A7.
  11. ↑ Planck 2015 results. VII. High Frequency Instrument data processing: Time-ordered information and beam processing, Planck Collaboration, 2016, A&A, 594, A7.

(Planck) High Frequency Instrument

Readout Electronic Unit

Junction Field Elect Transistor

Pre_Amplification Unit

Noise Equivalent Power

low frequency excess response

Cosmic Microwave background

analog to digital converter

Data Processing Unit

European Space Agency

Retrieved from ‘https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=HFI_detection_chain&oldid=13701’