Issue 
A&A
Volume 532, August 2011



Article Number  A55  
Number of page(s)  12  
Section  Astronomical instrumentation  
DOI  https://doi.org/10.1051/00046361/201116986  
Published online  21 July 2011 
A deconvolution mapmaking method for experiments with circular scanning strategies
^{1}
Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK
email: dlh@ast.cam.ac.uk
^{2}
Astrophysics Group, Cavendish Laboratory, Madingley Road, Cambridge, CB3 0HE, UK
Received: 30 March 2011
Accepted: 9 June 2011
Aims. We investigate the performance of a deconvolution mapmaking algorithm for an experiment with a circular scanning strategy, specifically in this case for the analysis of Planckdata, and we quantify the effects of making maps using simplified approximations to the true beams.
Methods. We present an implementation of a mapmaking algorithm which allows the combined treatment of temperature and polarisation data, and removal of instrumental effects, such as detector time constants and finite sampling intervals, as well as the deconvolution of arbitrarily complex beams from the maps. This method may be applied to any experiment with a circular scanningstrategy.
Results. Lowresolution experiments were used to demonstrate the ability of this method to remove the effects of arbitrary beams from the maps and to demonstrate the effects on the maps of ignoring beam asymmetries. Additionally, results are presented of an analysis of a realistic fullscale simulated dataset for the Planck LFI 30 GHz channel.
Conclusions. Our method successfully removes the effects of the beams from the maps, and although it is computationally expensive, the analysis of the Planck LFI data should be feasible with this approach.
Key words: methods: data analysis / techniques: image processing / cosmic background radiation
© ESO, 2011
1. Introduction
Recently, there has been a lot of activity in the development of mapmaking methods for the European Space Agency satellite, Planck (Tauber et al. 2010; Planck Collaboration et al. 2011). Planck has been designed to produce highresolution temperature and polarisation maps of the cosmic microwave background (CMB). It has detectors divided between 9 frequency channels sensitive to the frequency range of 30 to 857 GHz. These frequency channels are split between two instruments the HFI and LFI, the High and Low Frequency Instruments, respectively.
Many of these mapmaking methods have been part of a coordinated development within the Planck collaboration, and have been tested using increasingly more sophisticated simulated data (Poutanen et al. 2006; Ashdown et al. 2007a,b). The method presented here was developed with Planck in mind, but is applicable to any experiment with a circular scanning strategy. It should be noted that this method is not, as of yet, part of the official data processing pipeline for the Planck project and has not been applied to the actual Planck data.
Planck spins about its axis once per minute, and as the line of sight (LOS) of the centre of the focal plane is almost perpendicular to this spin axis, the path of each detector describes an almost great circle on the sky. The spin axis is repositioned at least once every hour, with the sequence of spinaxis positions defining the scanning strategy. The nominal path of the LOS for each rotation of the satellite reobserves the same almostgreat circle on the sky, with the beams in the same orientations, for the duration of each pointing period. A pointing period is the period of time between two sequential repositionings of the satellite spinaxis. The nutation of the spin axis about its nominal position will produce variations in the LOS direction about the nominal path, changing the part of the sky which is observed. Provided the displacement of the LOS from its nominal path remains small with respect to the beam, the roughly 60 or so circles corresponding to a single pointing period may be thought of as a 1dimensional ring on the sky and may be analysed together with our method. It should be noted that the LFI with its larger beams is inherently more robust to this issue, than the HFI.
If the effects of beam asymmetries are not accounted for in the mapmaking process, then this will result in systematic errors in the maps and in the recovered power spectra. The systematic effects due to axisymmetric beams have been assessed by Carretti et al. (2004) and a completely general assessment of the asymmetries by O’Dea et al. (2007). The mapmaking method described in this paper provides a mechanism to account and correct for arbitrary beam asymmetries, hence the term deconvolution mapmaking. Our approach is not the only one to this problem; Armitage & Wandelt (2004) have developed a method to account for the effects of the asymmetries, which is less computationally expensive than our method in the case of simple beam asymmetries, but is effectively restricted in the detail of the beam description that can be implemented. Here we may account for any degree of beam complexity. Both methods may also remove from the data the instrumental effects due to detector time constants and the finite sampling interval, whereby each data point is formed from the signal integrated over a small time interval.
Removing the effects of the beam from the map could be extremely useful for the study of resolved objects, which would otherwise be distorted by the beam. Additionally, removing the distorting effects of the beam could aid in studies of the lensing of the CMB (Lewis & Challinor 2006; Perotto et al. 2010).
We have followed two approaches, to solving the mapmaking equations, in the development of our deconvolution mapmaking method: a direct approach from which the full noise covariance matrix may be recovered at low resolution and an iterative approach, which although still computationally expensive, will allow the resolutions required for the analysis of the LFI data to be reached. Both our approaches may be used to analyse polarised data with arbitrary beams, and recover the underlying multipoles on the sky without the need to pixelate the data.
We discuss the methods used and the implementation of our deconvolution mapmaking method in Sect. 2, from the preprocessing of the ring data in Sect. 2.1 to the reconstruction of the sky in Sect. 2.2. The simulations generated to fully test our method in the case of arbitrarily complex beams are described in Sect. 3 together with the results of this analysis. The results of the analysis of more realistic Planck data, used in a previous mapmaking comparison paper (Ashdown et al. 2007a), is described in Sect. 4.
2. Method and Implementation
Our method splits the data processing in a way which is natural in terms of how Planck acquires the data, allowing the timeordered data (TOD) from each pointing period to be processed separately. The TOD corresponding to each pointing period may be reduced, without loss of information, to Fourier coefficients on the rings as described below in Sect. 2.1. These Fourier coefficients together with the mean pointing information for each ring may then be analysed to recover the multipoles on the sphere, as outlined in Sect. 2.2.
2.1. TOD to Fourier coefficients on rings
The timeordered data for each pointing period is processed broadly as described in van Leeuwen et al. (2002). The implementation of this method to more realistic simulated data, however, has necessitated some modifications to the method presented in that paper. In this section we outline the processing required to extract the Fourier coefficients from the TOD, highlighting these modifications.
Fig. 1
Path described over a pointing period by the lineofsight of a detector for a given opening angle, α_{d} and spin axis position. The position of the instantaneous lineofsight may be described with the addition of another angle, ψ_{d}, the phase. The repositioning of the spin axis position over the course of the mission defines the scanning strategy; plotted here is the cycloidal scanning strategy which is used throughout this paper. 

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The position of the lineofsight of a detector for a pointing period may be described in terms of the mean spin axis position and two angles, as shown in Fig. 1. These angles are the opening angle, which is the angle between the spin axis position and the lineofsight of the detector, and the phase, which defines the position around the ring from a given reference point. By assessing the value of the phase for each sample in the TOD, these data may be binned in phase, which effectively compresses the data by a factor of 40 to 50. If a suitable number of phasebins is chosen, it is possible to recover the Fourier coefficients, which represent the TOD, from the phasebinned data with a negligible loss of accuracy as compared to evaluating them directly from the TOD, but with a significant reduction in the processing required.
It should be noted that our implementation differs from that in van Leeuwen et al. (2002) as to the number of phasebins required, and the number of moments which are included in Eqs. (4)–(8) in that paper. Our investigation showed that including the 3rd order terms of the phase improved the recovery of the Fourier coefficients and that there was no loss of accuracy in reducing the number of phasebins from 6n_{max} as used in van Leeuwen et al. (2002) to 4n_{max}, where n_{max} is the highest mode extracted. The value of n_{max} chosen should be such that n_{max} ≥ ℓ_{max}, where ℓ_{max} is the desired value to which the sky multipoles are to be recovered.
The above procedure successfully recovers the required Fourier coefficients with negligible loss of accuracy when the distribution of the TOD is relatively uniform in phase. If there is a resonance between the spin and sampling rates then the distribution of the data in phase will no longer be uniform, as samples from a previous rotation will occur at the same location in phase as the current rotation.
The performance of this method at recovering the Fourier coefficients from data with a nonuniform distribution in phase has been investigated. The degree of nonuniformity in phase, in terms of the maximum gap present between two subsequent phaseordered samples, which can be tolerated before the effect on the recovered values for the Fourier coefficients becomes significant with respect to the noise on the data, was assessed. Should this phasegap size be exceeded, the Fourier coefficients will be evaluated directly. In the case of the simulations, described in Sect. 4, this meant that 5% of the rings were not phasebinned, with the Fourier coefficients being evaluated directly from the TOD for these rings.
Although, when possible we phasebin the TOD to reduce the processing requirement, the effect of this binning is negligible, as the Fourier coefficients recovered from the phasebinned rings are of a negligible difference from those evaluated directly from the TOD. Therefore there can be no effects in our data analysis due to the binning or pixelisation of the data, which is one way in which our method differs from that of Armitage & Wandelt (2004).
2.2. Sky reconstruction
The data in terms of the Fourier coefficients for a single ring, d_{r}, may be expressed as (1)where n_{r} represents the noise on the Fourier coefficients, R_{r} is the coupling matrix which describes the connection between the multipole moments, a_{ℓm} on the sphere, represented by the vector a and the Fourier coefficients.
The data from all the rings may be combined and analysed together (2)where R is the equivalent of the pointing matrix in conventional pixelbased mapmaking. The maximum likelihood estimates for multipoles on the sky may then be found by solving the matrix equation (3) where N is the noise covariance matrix of the Fouriercoefficients, given by .
The coupling matrix is derived in Challinor et al. (2002) and requires information on the detector orientations, opening angles and beam profiles, together with the mean spin axis positions for each ring. The coupling matrix is constructed as in Challinor et al. (2002) with the exception of accounting for those effects on the data which occur around the rings such as those due to sampling intervals and the detector timeconstants, as removing these effects involves adjusting the Fourier coefficients for each pointing period, and is more naturally included in TOD to Fourier coefficient code, rather than in the sky reconstruction code.
As shown by Challinor et al. (2002) the correlations in the noise between different Fourier modes on the rings are expected to be negligible. This expectation was verified and we therefore treat the noise covariance matrix, N, for those data as diagonal. This method could use the full noise covariance for each ring, making N block diagonal, however this is not necessary as gaps in the data, due to glitches or otherwise, should not occur in any preferential location, hence the number of samples per phase bin should be on average the same. This will ensure the near stationarity of the noise at the ring level, and negligible level of noise correlations between Fourier modes. In the case of an experiment which does not have this redundancy, this method would still be applicable provided that a block diagonal N is used.
The presence of 1/f noise in the data results in striping in the maps, due to a different offset on each ring (Burigana et al. 1999; Delabrouille 1998). If the knee frequency is low then by removing the zerofrequency Fourier coefficients from our analysis we may “destripe” the maps, effectively removing the contribution of the 1/f noise, and projecting out correlated noise on timescales longer than a ring. Given that the noise covariance matrix is diagonal, the zerofrequency Fourier coefficients may be removed from the analysis by setting the diagonal elements of the inverse noise covariance matrix which correspond to these coefficients to zero. This is equivalent to increasing the noise on these coefficients to infinity and hence their contribution to the recovered signal is completely removed. An alternative approach is to introduce an additional parameter for every ring and solve for the offsets produced by the 1/f noise, as well as recovering the signal multipoles. As one would expect, there is no change in the recovered values of the signal multipoles using this approach, so this should only be used if the offsets themselves are required. If the knee frequency is not sufficiently low to isolate the 1/f noise in the zero frequency modes, then the approach presented here can be extended to deal with any arbitrary noise powerspectrum on the rings, by suitably weighting the higher frequency modes.
The matrix, , the inversion of which is required to obtain the solution for the spherical multipoles, unfortunately, is nonsparse and large with the order of elements. This effectively limits the maximum value of ℓ to which the analysis may proceed, as the computational requirements needed to produce a solution scale as for a direct method and for iterative methods such as the preconditioned conjugategradient method which we have implemented. It should be noted that there is an implicit assumption of fullsky coverage and a minimum of 4 × ℓ_{max} rings, should this not be the case the condition number of will increase and in practice not all multipoles will be recoverable.
Since the coupling matrix is already nonsparse there are no increases in the computational expense of our code if we choose to analyse the data with beams whose expansion in spherical multipoles contain arbitrary high values of m, in contrast to the method of Armitage & Wandelt (2004).
2.2.1. Iterative method
In order to reach the values of ℓ required for an analysis of Planck data, it was necessary to develop an iterative method for solving Eq. (3) for which a parallel implementation is possible. Due to its large requirement on memory, the coupling matrix, R, must be stored over multiple processors, as a copy on each processor would be prohibitively expensive in terms of memory used; even stored once the size of R becomes prohibitive for large values of ℓ_{max} for the full mission analysis.
In order to reduce the memory requirements, R is evaluated as needed and only the part which corresponds to a single ring is stored in memory at any one time. This reduces the memory requirement to . The division of the storage and calculation of R between the processors should be such that it minimises the amount of data which must be exchanged between them. This requirement may be met by storing and evaluating R in terms of the submatrices corresponding to individual ℓ values. This division of the processing has implications for the scaling of the code with the number of processors used, which is described in Appendix A.
We use a preconditioner, the purpose of which is to achieve a reduction in the number of iterations required at the expense of a small increase in the computational cost of each iteration in terms of an additional matrixvector multiplication (Golub & van Loan 1996). Our chosen preconditioner is the diagonal of the matrix R^{T}N^{1}R, which meets these criteria.
The implementation of the preconditioned conjugategradient method described here was parallelised using the MessagePassing Interface (MPI), and hence is capable of being run on both sharedmemory machines and clusters.
2.2.2. Direct method
Our direct method for solving Eq. (3) , takes advantage of the fact that in the case of a diagonal N, it is possible to prewhiten the data, d, and the coupling matrix, R, so that Eq. (3) reduces to a standard least squares equation, which may be solved by QR decomposition and backsubstitution. The direct method performs the QR decomposition using Householder transformations (van Leeuwen 2007) to reduce R to an upper triangular form, U. This method allows the processing of R to be split into sections in terms of rows, provided that the number of rows of R being processed together is larger than the number of columns of R. Our implementation uses this property to ensure that the subsection of data being processed together with its corresponding section of the coupling matrix will fit within the available memory. As each subsection of data is processed the upper triangular matrix, U, is further refined and updated.
Once U has been found the a_{ℓm} may be evaluated through backsubstitution. Additionally, U^{1} may also be found through backsubstition, and hence the full noise covariance matrix for the a_{ℓm} may be evaluated. This covariance matrix may be useful as an input to the hybrid approach of Efstathiou (2005) for power spectrum or parameter estimation, which uses a direct likelihood evaluation at low multipoles and pseudoC_{ℓ} estimators for high multipoles.
The direct approach was also parallelised using MPI, for reasons of code portability. Additionally, it makes use of the subroutines which calculate the submatrices of R for the individual values of ℓ, and hence the direct method will be subject to the same scaling conditions on the performance with the number of processors used, described in Appendix A, as the iterative method.
3. Complexbeam simulations
As a validation step, in order to demonstrate the ability of our method to remove the effects of any arbitrarilycomplex beam and to test it independently of the TOD to Fourier coefficient step, it was necessary to generate our own set of simulations.
The Fourier coefficients on the rings may be simulated directly by using Eq. (1). An arbitrary beam was generated based on the first author’s initials with the middle initial, l, being represented by an elliptical beam with major and minor fullwidth halfmaximums (FWHMs) of 3 and 1 degrees, respectively. The largest sidelobe is –15.8 dB relative to the peak, and located 5.9 degrees from it. The set of Fourier coefficients on the rings, generated using this arbitrary beam, shall be referred to from now on as the complexbeam simulation, and this beam shall be referred to as the true beam.
Fig. 2
T, Q and U maps, made using HEALPix^{1} (Górski et al. 2005), of the beams used in the complexbeam simulations. Top: the circularly symmetric beam; middle: the elliptic beam; bottom: the true beam for which the elliptic beam forms the main beam. 

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The data for the complexbeam simulation consists of 800 rings, for two polarised detector pairs, containing Fourier coefficients up to an ℓ_{max} of 200. These simulations are noise free; no noise is added to the coefficients, and a suitably lowlevel of noise is used to produce the noise covariance matrix, N.
To complete the set of beams with which to analyse the complexbeam simulation, the spherical multipoles for an elliptical and a circular beam were produced. The elliptical beam corresponds to the elliptical main lobe of the true beam, and a circular beam has a FWHM corresponding to the geometric mean of the two FWHMs of the elliptical beam. All the beams are defined by their spherical multipoles. However, for visualisation purposes, T, Q and U maps for these beams were produced. These maps, synthesised at the north pole of the coordinate system, may be seen in Fig. 2.
3.1. Analysis of complexbeam simulations
The complexbeam simulation was analysed, using the iterative approach described in Sect. 2.2.1, using the three different beams described in Sect. 3 and visually represented in Fig. 2. The residual multipoles of these analyses have been synthesised onto T, Q and U maps shown in Figs. 3–5, respectively. In each of these figures the inputsky multipoles, which are the same as those used in the Trieste simulations described in Sect. 4, are convolved with a circularly symmetric beam with a FWHM of 1° and synthesised onto a map for comparison with the structures seen in the residual maps.
An alternate assessment of the performance of the analyses is shown in Fig. 6. This figure shows the fractional reconstruction errors in the power spectra, for T, E, and B, in the cases where the true, elliptical or circular beams are used in the deconvolution. It should be noted that, these power spectra do not correspond to the CMB power spectrum, but to a combination of the CMB and all the simulated foregrounds, including point sources.
In Figs. 3 through 5, the maps synthesised from the residual multipoles from the analysis of the complexbeam simulation with the true beams may be seen to contain little power. Additionally, the low level of the fractional errors in the power spectra in Fig. 6, produced from the analysis using the true beams, also confirms the successful removal of the beam effects from the data.
Figures 3 through 5, also show how ignoring beam asymmetries may affect the maps. This is seen in the analyses using the elliptical and circular beams, where the residual maps show structure along the galactic plane and regions near compact objects.
Fig. 3
Top panel shows the input temperature multipoles, synthesised onto a HEALPix map of N_{side} = 64. The lower panels show the residuals between the input and the recovered temperature multipoles, in the cases of the three different beams, from top to bottom the residuals maps are from the analysis with the true, elliptical and circular beams. Note that each residual map has a different colour scale. 

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Fig. 4
As for Fig. 3 but with the and multipoles sythesised onto a HEALPix map for the Stokes parameter Q. 

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Fig. 5
As for Fig. 3 but with the and multipoles sythesised onto a HEALPix map for the Stokes parameter U. 

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Fig. 6
Power spectra of the residuals in T (top), E, (middle) and B (bottom) divided by the power spectrum of the input sky. Shown here are the results of the analysis of the complexbeam simulation, by the three different beams. The red, green and blue points show these different analyses using the true, elliptical and circular beams, respectively. As the true beam, including its sidelobes, spans some 15° all scales are effected by the beam; as seen in the figures in the large difference between the fractional errors of the analysis performed using the true beam and the analyses using the elliptical and circular beams. The fractional errors of the analyses using the elliptical and circular beams, are seen to diverge from the scale at which the difference between these two beams becomes important. 

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Fig. 7
Top: temperature multipoles, , as input to the Trieste simulations, curtailed at ℓ = 400, and synthesised onto a HEALPix map of N_{side} = 128. These a_{ℓm} include contributions from the CMB, synchrotron, freefree, and dust. Middle: recovered from the analysis, up to ℓ_{max} = 400, of the corresponding Trieste simulations which included the effects of sampling, elliptical beams and 1/f noise. These are again synthesised onto a HEALPix map of N_{side} = 128. It should be noted that the simulations analysed here contain power above ℓ = 400 and it is only for comparison purposes that we curtail the input temperature multipoles to the value of ℓ_{max} to which the recovery proceeded. Bottom: Residuals between the inputsky and the recovered . These residuals are consistent with noise, the visible pattern is due to the scanning strategy. 

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Fig. 8
As for Fig. 7 but with the and multipole sythesised onto a HEALPix map for the Stokes parameter Q. 

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Fig. 9
As for Fig. 8 but for the Stokes parameter U. 

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Fig. 10
Top: residuals between the inputsky, including SZ and point sources, and the recovered map, plotted over the same range as the residuals found when SZ and point sources were not included in the inputsky. Middle: residuals between the inputsky, including SZ and point sources, and the map recovered using the circular beams, plotted over the same range as the top panel. Bottom: absolute differences between the maps recovered using the elliptical and circular beams, in the case when SZ and point sources are included. 

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Fig. 11
Top: residuals, for the Stokes Q parameter, between the inputsky including SZ and point sources and the map recovered using the circular beams, plotted over the same range as the residuals found for this parameter when the inputsky does not include SZ and point sources. Bottom: absolute differences between the maps recovered using elliptical and circular beams. 

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Fig. 12
As Fig. 11 but for the Stokes U parameter. 

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Fig. 13
Top: eesiduals between the inputsky and the recovered , plotted over the same range as the residuals, in Fig. 7. The inputsky, containing only the diffuse foregrounds, is the same as that shown in Fig. 7 whereas the were recovered using circular beams rather than the elliptical beams used in the simulations. Bottom: absolute difference between the maps recovered using elliptical and circular beams. 

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Fig. 14
Power spectra of the residuals in T (top), E, (middle) and B (bottom) divided by the power spectrum of the input sky. Shown here are the results of the analysis of two different sets of simulated data with two different beams. Both data set were simulated using the elliptical beams, and contain the CMB, diffuse Galactic foregrounds and 1/f and white noise. The second simulated data set additionally includes point and SZ sources. Each data set was analysed twice, once using the elliptical beams and once with the circular beams. The dark and light blue points are from the analysis of the first data set, with the circular and elliptical beams respectively. The green and red points correspond to the analysis of the second data set again with the circular and elliptical beams respectively. The differences between the recoveries due to the beams may easily be seen in the figures. In the temperature power spectra the differences are only apparent at intermediate ℓvalues, for the case where there are no point sources, as at higher ℓvalues the noise dominates. The upturn in the fractional residuals in all the figures at low ℓ is due to residual 1/f noise, that was not removed by discarding the zerofrequency Fourier coefficients from the analysis. 

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4. Trieste simulations
As well as testing our method on the complexbeam simulations, as described in Sect. 3, we also used a set of simulations produced by the Planck CTP Working Group, which is concerned with the evaluation of mapmaking, powerspectrum and likelihood methods for Planck data. The CTP simulations were produced to enable the comparison of a number of mapmaking algorithms, (Ashdown et al. 2007a) and they will be referred to throughout this paper as the Trieste simulations. They were generated using a simulations pipeline developed by the Planck collaboration with the purpose of providing simulated Planck data, (Reinecke et al. 2006) .
One year of pointing and signal data for the LFI 30 GHz channel, which corresponds to 8784 rings of TOD, was generated. Each repositioning of the spin axis, corresponds to one hour of data and to one ring of TOD, and this repositioning follows a cycloidal scanning strategy. The data were simulated for the two polarised detector pairs of which the LFI 30 GHz channel is comprised. Two different sets of beams, circular and elliptical, were used with these simulations allowing the effects of different beams to be investigated. The circular beams are Gaussian beams with a fullwidth halfmaximum (FWHM) of 32.5′, which is the geometric mean of the two FWHMs of the elliptical beams. These elliptical beams are the bestfit elliptical approximation to the prelaunch LFI 30 GHz beams (Sandri et al. 2010), for each of the two detectors corresponding to each of the two horns.
These data include the effects of variable spin velocity and nutation. There is also the option of including sampling effects, where the effects of the finite sampling period of the detectors are taken into account. Here we use the most realistic data, which is, in this case, the TOD simulated using the elliptical beams, in which the effects of sampling are included. The following components of the signal are included in the simulations: the CMB, the diffuse Galactic foregrounds, including the synchrotron, freefree and dust, compact objects, such as SunyaevZel’dovich (SZ) clusters and point sources, and both white noise and 1/f noise. The models and templates used for these foregrounds are described in Reinecke et al. (2006) and references therein; it should be noted that the templates used for the diffuse Galactic emission are extrapolations to Planck frequencies.
4.1. Analysis of Trieste data
In this section we present the results of the analysis, using the iterative approach of Sect. 2.2.1, of the most realistic subset of Trieste simulations; which were created using the cycloidal scanning strategy, the elliptical beams and included the effects of sampling. The 8784 simulated pointing periods, corresponding to one year of data were processed and the sky multipoles were reconstructed up to ℓ_{max} = 400. It should be noted that the simulations contain signals at ℓ values greater than ℓ_{max}. Given the beam sizes of the LFI 30 GHz detectors, and hence their much reduced sensitivity to power above ℓ = 400, this value for ℓ_{max} should be sufficient at least in the case of diffuse signals. Indeed, curtailing the reconstruction acts like a lowpass filter preventing the highfrequency noise from dominating the maps, due to the deconvolution.
The first set of simulated data to be analysed included contributions from the CMB, diffuse Galactic foregrounds, 1/f and white noise. The results of the analysis of these data may be seen in Figs. 7–9. In these figures the a_{ℓm} corresponding to the signals input to the simulations were used to generate a map of the inputsky for comparison with the map produced from the recovered a_{ℓm}. In order to perform this comparison the input a_{ℓm} were curtailed to the same value of ℓ_{max} that was used in the recovery of the a_{ℓm} from the simulated data. The differences between these two sets of a_{ℓm} were used to generate residual maps, in order to illustrate the differences between the recovered and the input sky. In Figs. 7–9 it is seen that there has been a successful reconstruction of the input sky, with the only features visible in the residual maps being due to the noise modulated by the hitcount. The hitcount is determined by the scanning strategy and this is the cause of the lower level of the residuals seen at the ecliptic poles, where the coverage is very much enhanced over that of the rest of the sky. These residuals maps also demonstrate that the remaining unrecovered power at higher multipoles has not interfered with the recovery of the lower multipoles.
The second set of data was the same as the first except that the contributions from SZ and point sources were also included. These simulations were first analysed using the elliptical beams they were produced with and then they were reanalysed assuming circular beams. The recovery of the a_{ℓm} when using the elliptical beams results in residuals maps indistinguishable from the residual maps for Q and U from the analysis of the first data set (shown in Figs. 8 and 9). The residuals for the T map, however, show that the recovery is not ideal in the region of bright point sources. The top panel of Fig. 10 shows these residuals plotted over the same colour range as the residual map for T from the analysis of the first data set. This sensitivity to pointlike objects is due to the resultant extra power at small scales, and the fact the recovery is limited in ℓ. The contribution of the point sources to the polarisation signal is small, so the Q and U maps remain unaffected. Increasing the value of ℓ_{max} used in the recovery of the a_{ℓm} will remove these effects from the residual map. This sensitivity was not seen in the complexbeam simulations, with their relatively higher value of l_{max} in comparison to the beam size.
The residuals from the analysis of this simulated data set with the circular beams, equivalent to a standard pixelbased mapmaking analysis, are shown in Figs. 10–12. These residual maps are again plotted over the same colour range as the residual maps produced from the analysis of the first data set, shown in Figs. 7–9. Recalling that the residual maps produced from the recovery using the elliptical beams were indistinguishable from the residual maps produced from the analysis of the first data set for the Q and U maps, it is seen that for all the maps there is an increase in the magnitude of the residuals along the Galactic plane and in the vicinity of beamsized or smaller objects when circular beams are assumed. Figure 13 shows the residual T map found from the analysis of the first data set with the circular beams; this also shows an increase in the level of the residuals.
The bottom panels of Figs. 10–13 show maps of the absolute difference between the maps recovered using the elliptical beams and the maps recovered using the circular beams. Given that the same set of simulated data is used in each case, all the differences must be due to the difference between the elliptical and circular beams. The smallest differences between these recovered maps are observed to be at the ecliptic poles. This is due to the properties of the sky coverage in these regions, with multiple intersecting scans at many different orientations, and the fact that the circular beams used have FWHMs which are the geometric mean of the two FWHMs which describe each elliptical beam.
It is noticeable that the magnitude of the additional errors in the recovery due to using the circular, and in this case incorrect, beams is typically larger than the residuals due to the noise in the data. The differences between the recoveries due to the different beams may easily be seen in Fig. 14 which shows the fractional errors in the power spectrum of both data sets with both the elliptical and circular beams. This figure shows the ratio of the power spectra of the residual a_{ℓm}, which are formed from the difference between the input and recovered a_{ℓm}, and the input power spectra. These power spectra are seen to increase with increasing ℓ. This increase is observed as the beams have been deconvolved and is due to the fact that the signal is suppressed by the beams whereas the noise is not. The dark blue (green) and light blue (red) points are from the analysis of the first (second) data set, with the circular and elliptical beams respectively. The first data set does not contain point or SZ sources whereas the second data set does, the input power spectra for the second data set will therefore have more power at smaller scales, especially in T, than that of the first data set. This leads to the smaller fractional errors seen for the analysis of the second data set, at higher multipoles in the T power spectra. For the E and B power spectra the figure shows virtually no differences between the two different data sets, for each beam. The B power spectra for the different beams are very similar, whereas there are clear differences between the E power spectra formed using the different beams, as may be expected from Carretti et al. (2004), who showed that the E power spectrum is coupled to the unpolarised sky through the beam, with the contamination peaking on the scale corresponding to the FWHM of the beam. In the case of the temperature power spectra the differences are only apparent at intermediate ℓvalues, for the case where there are no point sources, as at higher ℓvalues the noise dominates. Whereas the differences between the the power spectra formed from the different beams using the second data set, which contained point sources, are visible for all ℓ values higher than ℓ ~ 70.
5. Conclusions
We have described a successful implementation of the mapmaking methodology developed in Challinor et al. (2002) and van Leeuwen et al. (2002). While the computational costs of our implementation are far from trivial, the ability to deconvolve any arbitrarily complex beam from the data may prove to be worth the computational expense, at least for an analysis of the Planck LFI channels. Due to their position at the edges of the focal plane the LFI detectors are anticipated to have more elongated beams than their HFI counterparts.
We have demonstrated that this method may successfully be applied in the presence of compact and point sources provided that recovery proceeds to a value of ℓ_{max} at which there is little remaining unresolved signal. We have also shown how ignoring beam asymmetries affects the recovery of the Planck maps, both for temperature and polarisation. These effects are most noticeable in the Galactic plane region and near the locations of compact or point source objects.
We have shown that our method can produce maps without the distorting influence of the beams. This property may be especially useful for producing the best possible maps for Galactic science where we have shown that ignoring beam asymmetries will results in larger distortions.
As the attractiveness of this method increases with increasing beam complexities, it may also be of use for proposed future experiments, which are likely to consist of many more detectors, hence there will be detectors further from the centre of the focal plane resulting in the beams being more distorted. Additionally, the analysis of data from any future experiment would benefit from increases in computing performance, likely to occur in the interim.
Acknowledgments
This work was supported by STFC at the Cambridge Planck Analysis Centre, and utilised COSMOS VI, an Altix 3700 supercomputer, funded by SGI/Intel, HEFCE and PPARC. This research also used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DEAC0205CH11231. Some of the results in this paper have been derived using the HEALPix (Górski et al. 2005) package. This paper has made use of simulated data produced by the CTP Working Group.
References
 Armitage, C., & Wandelt, B. D. 2004, Phys. Rev. D, 70, 123007 [NASA ADS] [CrossRef] [Google Scholar]
 Ashdown, M. A. J., Baccigalupi, C., Balbi, A., et al. 2007a, A&A, 471, 361 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ashdown, M. A. J., Baccigalupi, C., Balbi, A., et al. 2007b, A&A, 467, 761 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Burigana, C., Malaspina, M., Mandolesi, N., et al. 1999 [arXiv:astroph/9906360] [Google Scholar]
 Carretti, E., Cortiglioni, S., Sbarra, C., & Tascone, R. 2004, A&A, 420, 437 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Challinor, A. D., Mortlock, D. J., van Leeuwen, F., et al. 2002, MNRAS, 331, 994 [NASA ADS] [CrossRef] [Google Scholar]
 Delabrouille, J. 1998, A&AS, 127, 555 [NASA ADS] [CrossRef] [EDP Sciences] [PubMed] [Google Scholar]
 Efstathiou, G. 2005, MNRAS, 356, 1549 [NASA ADS] [CrossRef] [Google Scholar]
 Golub, G. H., & van Loan, C. F. 1996, Matrix computations, 3rd ed. (London: The Johns Hopkins University Press) [Google Scholar]
 Górski, K. M., Hivon, E., Banday, A. J., et al. 2005, ApJ, 622, 759 [NASA ADS] [CrossRef] [Google Scholar]
 Lewis, A., & Challinor, A. 2006, Phys. Rep., 429, 1 [NASA ADS] [CrossRef] [Google Scholar]
 O’Dea, D., Challinor, A., & Johnson, B. R. 2007, MNRAS, 292 [Google Scholar]
 Perotto, L., Bobin, J., Plaszczynski, S., Starck, J., & Lavabre, A. 2010, A&A, 519, A4 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2011 [arXiv:1101.2022] [Google Scholar]
 Poutanen, T., de Gasperis, G., Hivon, E., et al. 2006, A&A, 449, 1311 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Reinecke, M., Dolag, K., Hell, R., Bartelmann, M., & Enßlin, T. A. 2006, A&A, 445, 373 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Sandri, M., Villa, F., Bersanelli, M., et al. 2010, A&A, 520, A7 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tauber, J. A., Mandolesi, N., Puget, J., et al. 2010, A&A, 520, A1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 van Leeuwen, F. 2007, Hipparcos, the New Reduction of the Raw Data, Astrophysics and Space Science Library (Springer), 350 [Google Scholar]
 van Leeuwen, F., Challinor, A. D., Mortlock, D. J., et al. 2002, MNRAS, 331, 975 [NASA ADS] [CrossRef] [Google Scholar]
Appendix A: Implementation details
A.1. Scaling with number of processors
This appendix describes the effect, due to the method used to evaluate R, on the scaling with the number of processers used in the parallel implementations of both the iterative and direct methods.
Fig. A.1
Scaling of the mapmaking algorithm with the number of processors used. Since each processor is assigned a number of different values of ℓ, the number of processors to which the code will successfully scale will depend on the value of ℓ_{max} to which the analysis is to be performed. For a given ℓ_{max} there will be a number of processors above which it is not possible to balance the load between them. This is shown in the top plot for ℓ_{max} = 400. The black crosses show the load on the processor with the heaviest workload, normalised by the equivalent value for 32 processors. The red curve shows the reduction in the workload assuming perfect load balancing. It is seen that there is no reduction in the maximum load once the number of processors is increased beyond 142. The bottom plot shows the relationship between the maximum load and the time required per iteration of the code, where the dashed line shows the expected relationship and the black points, labeled with the number of processor used, show the observed behaviour. 

Open with DEXTER 
The time taken per iteration of the code will be determined by the processor with the largest workload. It is therefore important that the load is balanced as equally as possible over the number of processors being used. As the code is parallelised by dividing the individual values of ℓ between the various processes, there must come a point at which using additional processors will no longer produce a decrease in the time required, as it becomes impossible to share the workload between the different processors. This situation is shown in the top panel in Fig. A.1, for an analysis up to an ℓ_{max} = 400. In this figure the black crosses represent the load on the processor with the maximum load, relative to the processor with the maximum load in the case when 32 processors are used. The red curve shows, for comparison, the reduction in the workload, with increasing numbers of processors, assuming perfect load balancing. The bottom panel in Fig. A.1 shows the relationship between the maximum load and the time taken per iteration. Doubling the number of processors used halves the workload per processor which in turn halves the time taken per iteration, up until the point at which the load balancing breaks down. The number of processors at which this occurs may be easily evaluated and is found to be equal to ℓ_{max}/2.8.
All Figures
Fig. 1
Path described over a pointing period by the lineofsight of a detector for a given opening angle, α_{d} and spin axis position. The position of the instantaneous lineofsight may be described with the addition of another angle, ψ_{d}, the phase. The repositioning of the spin axis position over the course of the mission defines the scanning strategy; plotted here is the cycloidal scanning strategy which is used throughout this paper. 

Open with DEXTER  
In the text 
Fig. 2
T, Q and U maps, made using HEALPix^{1} (Górski et al. 2005), of the beams used in the complexbeam simulations. Top: the circularly symmetric beam; middle: the elliptic beam; bottom: the true beam for which the elliptic beam forms the main beam. 

Open with DEXTER  
In the text 
Fig. 3
Top panel shows the input temperature multipoles, synthesised onto a HEALPix map of N_{side} = 64. The lower panels show the residuals between the input and the recovered temperature multipoles, in the cases of the three different beams, from top to bottom the residuals maps are from the analysis with the true, elliptical and circular beams. Note that each residual map has a different colour scale. 

Open with DEXTER  
In the text 
Fig. 4
As for Fig. 3 but with the and multipoles sythesised onto a HEALPix map for the Stokes parameter Q. 

Open with DEXTER  
In the text 
Fig. 5
As for Fig. 3 but with the and multipoles sythesised onto a HEALPix map for the Stokes parameter U. 

Open with DEXTER  
In the text 
Fig. 6
Power spectra of the residuals in T (top), E, (middle) and B (bottom) divided by the power spectrum of the input sky. Shown here are the results of the analysis of the complexbeam simulation, by the three different beams. The red, green and blue points show these different analyses using the true, elliptical and circular beams, respectively. As the true beam, including its sidelobes, spans some 15° all scales are effected by the beam; as seen in the figures in the large difference between the fractional errors of the analysis performed using the true beam and the analyses using the elliptical and circular beams. The fractional errors of the analyses using the elliptical and circular beams, are seen to diverge from the scale at which the difference between these two beams becomes important. 

Open with DEXTER  
In the text 
Fig. 7
Top: temperature multipoles, , as input to the Trieste simulations, curtailed at ℓ = 400, and synthesised onto a HEALPix map of N_{side} = 128. These a_{ℓm} include contributions from the CMB, synchrotron, freefree, and dust. Middle: recovered from the analysis, up to ℓ_{max} = 400, of the corresponding Trieste simulations which included the effects of sampling, elliptical beams and 1/f noise. These are again synthesised onto a HEALPix map of N_{side} = 128. It should be noted that the simulations analysed here contain power above ℓ = 400 and it is only for comparison purposes that we curtail the input temperature multipoles to the value of ℓ_{max} to which the recovery proceeded. Bottom: Residuals between the inputsky and the recovered . These residuals are consistent with noise, the visible pattern is due to the scanning strategy. 

Open with DEXTER  
In the text 
Fig. 8
As for Fig. 7 but with the and multipole sythesised onto a HEALPix map for the Stokes parameter Q. 

Open with DEXTER  
In the text 
Fig. 9
As for Fig. 8 but for the Stokes parameter U. 

Open with DEXTER  
In the text 
Fig. 10
Top: residuals between the inputsky, including SZ and point sources, and the recovered map, plotted over the same range as the residuals found when SZ and point sources were not included in the inputsky. Middle: residuals between the inputsky, including SZ and point sources, and the map recovered using the circular beams, plotted over the same range as the top panel. Bottom: absolute differences between the maps recovered using the elliptical and circular beams, in the case when SZ and point sources are included. 

Open with DEXTER  
In the text 
Fig. 11
Top: residuals, for the Stokes Q parameter, between the inputsky including SZ and point sources and the map recovered using the circular beams, plotted over the same range as the residuals found for this parameter when the inputsky does not include SZ and point sources. Bottom: absolute differences between the maps recovered using elliptical and circular beams. 

Open with DEXTER  
In the text 
Fig. 12
As Fig. 11 but for the Stokes U parameter. 

Open with DEXTER  
In the text 
Fig. 13
Top: eesiduals between the inputsky and the recovered , plotted over the same range as the residuals, in Fig. 7. The inputsky, containing only the diffuse foregrounds, is the same as that shown in Fig. 7 whereas the were recovered using circular beams rather than the elliptical beams used in the simulations. Bottom: absolute difference between the maps recovered using elliptical and circular beams. 

Open with DEXTER  
In the text 
Fig. 14
Power spectra of the residuals in T (top), E, (middle) and B (bottom) divided by the power spectrum of the input sky. Shown here are the results of the analysis of two different sets of simulated data with two different beams. Both data set were simulated using the elliptical beams, and contain the CMB, diffuse Galactic foregrounds and 1/f and white noise. The second simulated data set additionally includes point and SZ sources. Each data set was analysed twice, once using the elliptical beams and once with the circular beams. The dark and light blue points are from the analysis of the first data set, with the circular and elliptical beams respectively. The green and red points correspond to the analysis of the second data set again with the circular and elliptical beams respectively. The differences between the recoveries due to the beams may easily be seen in the figures. In the temperature power spectra the differences are only apparent at intermediate ℓvalues, for the case where there are no point sources, as at higher ℓvalues the noise dominates. The upturn in the fractional residuals in all the figures at low ℓ is due to residual 1/f noise, that was not removed by discarding the zerofrequency Fourier coefficients from the analysis. 

Open with DEXTER  
In the text 
Fig. A.1
Scaling of the mapmaking algorithm with the number of processors used. Since each processor is assigned a number of different values of ℓ, the number of processors to which the code will successfully scale will depend on the value of ℓ_{max} to which the analysis is to be performed. For a given ℓ_{max} there will be a number of processors above which it is not possible to balance the load between them. This is shown in the top plot for ℓ_{max} = 400. The black crosses show the load on the processor with the heaviest workload, normalised by the equivalent value for 32 processors. The red curve shows the reduction in the workload assuming perfect load balancing. It is seen that there is no reduction in the maximum load once the number of processors is increased beyond 142. The bottom plot shows the relationship between the maximum load and the time required per iteration of the code, where the dashed line shows the expected relationship and the black points, labeled with the number of processor used, show the observed behaviour. 

Open with DEXTER  
In the text 
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