Introduction and Summary
The overall geometry of the Planck focal plane is shown here:
In order to take full advantage of the HFI beams, we must know the individual detector positions to a precision of better than several arcseconds, over the course of the entire mission.
Spacecraft pointing comes from the on-board star tracker at 8 Hz between repointings. This is translated via a series of three-dimensional rotations to a pointing for the centre of the focal plane and resampled to the HFI TOI data rate for convenience. We must then further translate this focal-plane boresight pointing to the individual detector locations. Because neither the rotations from the star tracker to the boresight nor those from the boresight to the individual detectors are known exactly a priori, we must calibrate using flight data.
Specifically, measurements of HFI Detector pointing are based largely on observations of individual planets, with information from the much more frequent observation of lower-flux galactic and extragalactic high-frequency sources used to monitor and build a model of overall pointing drift. This long-term drift of the spacecraft attitude is due to changes in the moment of inertia and includes specific events which may induce sudden changes, essentially random as far as our ability to predict the effects thereof.
Note that the resulting pointing model cannot easily be directly compared to a physical/optical model: in particular, it includes a phase shift in the scan direction from the convolution and deconvolution of the detector transfer function, which is complex in the Fourier domain (see planck2013-p03c Planck-2013-VII ). This phase shift was not measured during normal operations, but a short campaign during which the spacecraft was spun at a higher rate will be used to determine these offsets in future date releases. Comparison with the initial optical model indicates that the in-scan change due to this phase shift is of the order of 1 arcminute. Note also that aberration is corrected in all observations.
The final pointing model is measured to be better than 2 arcsecond rms in the co-scan and cross-scan directions averaged over ten-day periods, as shown below. Note that there are larger hourly drifts of up to 10 arcseconds due to interference from the radiometer electronics box assembly (REBA) as discussed more fully in planck2013-p03 Planck-2013-VI ).
Initial measurements: Mars 1 and other planets
The first observation of Mars, which occured around 180 days from launch, is the baseline against which other objects are compared. Here, we show the relative pointing of Mars 1 to the pre-launch RFFM.
Focal plane drift: map-based measurement of detector positions
Prior to modeling of systematic changes in the Planck pointing, we find secular drifts of order one arcminute over the course of the nominal mission. We monitor this by making point-source catalogs based on single Planck surveys, only counting those objects which are observed over the course of less than seven days (this limits us to observations away from the ecliptic poles where Planck's observing strategy is highly cross-linked). We cross-match these catalog positions to the known IRAS point-source catalog Lingyu2009 and average the deviations in ten-day blocks (the individual measurements are shown as lighter points; error bars assume equal weighting for all points, but the results are not sensitive to any imposed S/N cutoff):
An analysis performed directly in the timestream gives similar results, below (evaluated until the end of HFI operations in January 2012).
A model for Planck Pointing
These analyses allow us to build a model for the pointing drift.
The correction is based on the measurement of pointing offset directly from the timeline, on a small sample of known and bright radio sources and planets. First the beam shape of each detector is measured by stacking individual timeline observation of bright planets. This process is of course contaminated by pointing error, but this is reduced by allowing each pass on the planet to be slightly displaced in order to correct for the observed location of the planet. This process yield a very clean estimate of the beam of each detector.
Then those beam are used to determine the offset of observed location of planets (Mars, Saturn & Jupiter) as well as a few (~10) bright radio sources.
This offset are estimated for all detectors for the planet, and only for 100Ghz to 217Ghz one for the radio sources.
From the planet observations, one can recover the alignment of each detector in the focal plane, as well as a first pointing correction at the time of planet observations. This pointing correction is obtained by fitting splines on the planet observation from each detector. We further allow this correction to have a sharp jump between the second and third survey (SCS switchover).
This first pointing correction is further refined using the point sources observations in order to fill the period between planet observations. The radio sources offsets require further treatment than the planet based offsets. First, the brightness of the sources being much smaller than planets, the offset on individual detector observation are very noisy, and we filter out the noise by building median offsets for each point source observation. Second, since the sources can be slightly extended we still observe systematic offset above and below the planet based pointing correction in a regular alternating pattern. This is due to the fact that we are observing those extended objects scanning in alternating directions, and our fit of those extended sources to our beam translate into this systematic alternating pattern. We thus allow for a small, arcsec correction of those offsets : i.e. each object is allowed a single offset displacement of order arc seconds in order to minimize the offset between different observations of the same object at different time.
The resulting list of point source offsets is then merged with the planet offsets. Again a spline based correction is built fitting all of this data, and allowing rupture of continuity at the time of the SCS switchover and other major onboard event (typically between each surveys).
Once we assume the full Planck pointing model and re-measure the position of Mars for this observation, we see sub-arcsecond deviations (as expected); this gives an indication of the purely numerical limitations of the method. Further planet observations show the small remaining uncorrected drift present in the pointing model (note that cross-scan positions are measured with considerably less data than in-scan positions due to the scan strategy):
Redoing the single-survey map- and catalog-based computation with the corrected pointing shows that Planck has achieved the arcsecond-scale goal of pointing rms:
Wobble angles are the angles which defines the relationship between the Principal Axis Reference Frame of Planck and the Body Reference Frame of Planck, both of which have their origin in the Planck Baricenter (ACMS, AHF-ICD).
Pointings are determined by a set of rotations converting coordinates in the STR reference frame to ecliptical reference frame, i.e. defining the rotation matrix . The matrix can be decomposend in a sequence of matrix mutiplications:
here we usedto denote transformation from Rerference Frame RFA to Reference Frame RFB, and .
The STR coordinates to Body Reference Frame coordinates, it is a constant matrix.converts from
where STR boresight angle assumed to be constant and aligned with the telescope LOS, but this is not the case. The STR is located on the SVM, at about 1.5 m from the origin of the Body reference frame, a change in its position of 0.15 mm will result in a change of its orientation of about radiants about 20 arcsec.is the
There is no way to measure directly those changes. So the effect is that to have an apparent change in the AHF) and (azimuth angle as defined in the AHF) angles: the reason is apparent immediately when looking at the way a perturbation in STR reference frame orientation propagates., (tilt angles as defined in the
AHF provides wobble angle measures at 1 minute ( , ) and one OD ( ) rate. Indeed is provided at each pointing period but measures within each given OD are constant.
Assuming to have quaternions represented by rotation matrixat a time , and assuming to have representative values of true wobble angles , , and a way to estimate the apparent , , it is possible to remove the apparent effect.
With the available information it can be done forand .
The correction algorithm initializes two rotation matrices as references usingand from the first pointing period of the nominal mission:
Then, for each pointing period, builds two correction matrices using AHF in the Observation section:and as provided by the
From these matrices the correction matrix is build:
Each quaternion of the AHF is finally corrected using .
The corrected quaternions are interpolated using Spherical Linear Interpolation algorithm and transformed in cartesian vector, which we call. For each sample the stellar aberration correction is applied:
whereis the satellite velocity and is the speed of light. After this operation the vector is normalized.
Finally the cartesian vetor is converted in Ecliptic Coordinates, the detector pointing.
The rotation of the beam with respect the north direction is theangle and is computed rotating the corrected quaternions using:
The resulting rotation matrix represents the rotation of the beam, the \psi angle is then:
(Planck) High Frequency Instrument
LFI Radiometer Electronics Box Assembly
Operation Day definition is geometric visibility driven as it runs from the start of a DTCP (satellite Acquisition Of Signal) to the start of the next DTCP. Given the different ground stations and spacecraft will takes which station for how long, the OD duration varies but it is basically once a day.
sudden change of the baseline level inside a ring
Sorption Cooler Subsystem (Planck)
Attitude Control & Measurement Subsystem (AOCS)
Attitude History File
Interface Control Document
Line Of Sight