Swarm SCARF Dedicated Lithospheric Field Inversion chain
© The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Societyof Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB. 2013
Received: 31 March 2013
Accepted: 22 July 2013
Published: 22 November 2013
The forthcoming Swarm satellite mission is a constellation of three satellites dedicated to the study of the geomagnetic field. The orbital characteristics of the mission, which includes a pair of satellites flying side by side, has prompted new efforts in data processing and modeling. A consortium of several research institutions has been selected by the European Space Agency (ESA) to provide a number of Level-2 data products which will be made available to the scientific community. Within this framework, specific tools have been tailor-made to better recover the lithospheric magnetic field contribution. These tools take advantage of gradient properties measured by the lower pair of Swarm satellites and rely on a regional modeling scheme designed to better detect signatures of small spatial scales. We report on a processing chain specifically designed for the Swarm mission. Using an End-to-End simulation, we show that the tools developed are operational. The chain generates a model that meets the primary scientific objectives of the Swarm mission. We also discuss refinements that could also be implemented during the Swarm operational phase to further improve lithospheric field models and reach unprecedented spatial resolution.
Key wordsLithospheric magnetic field space magnetometry Swarm
Large magnetic anomaly field features with spatial dimensions of more than a few hundred kilometers can be inferred from Low Earth Orbiting (LEO) satellites. These length scales are typically dominated by the magnetic field created by the spatial variation in structure and composition of the Earth’s crust and upper mantle (Thébault et al., 2010 for a review). The previous CHAMP (Reigber et al., 2002) satellite mission allowed impressive progress towards mapping the Earth’s lithospheric magnetic field (e.g., Maus et al., 2008), understanding their geological sources (e.g., Hemant and Maus, 2005), and inferring other physical quantities such as the equivalent global Curie depth (Purucker et al., 2002) or the heat flow anomalies of the Earth’s crust in remote regions (e.g., FoxMaule et al., 2005). The Earth’s lithospheric field at large wavelengths (>400 km) is conceptually simple because mostly static in time (e.g., Thébault et al., 2009). Unfortunately, it is also one of the weakest detectable sources at satellite altitudes and is masked by all other constituents of the total Earth’s magnetic field (e.g., Hulot et al., 2007). For instance, it represents about 0.01% of the total Earth’s magnetic field strength at 400 km height (with a root mean square of about 3.8 nT using the NGDC-720 model; Maus, 2010) and its magnitude rarely exceeds 20 nT.
Planetary magnetic fields are often expressed in terms of a finite series of spherical harmonics (SH) to a maximum expansion degree. After ten years of the CHAMP mission, the most recent models describing the magnetic field of the lithosphere, such as the MF7 model (an upgrade of Maus et al., 2008; http://geomag.org/models/MF7.html) expanded to SH degree 133, and the CHAOS-4 model (an upgrade of Olsen et al., 2010a) expanded to SH degree 100, agree reasonably well up to degree 85, thus providing a robust bound of about 470 km on the maximum horizontal spatial resolution. The geometrical attenuation with altitude and the prominence of external fields at satellite level are the two main factors limiting our ability to reach higher SH degrees and thus to detect smaller scale structures. However, for equivalent altitude datasets, the differences between MF7 and CHAOS-4 mainly lie in the way the different models deal with source field separation and, more specifically, with the rapidly time-varying external fields.
Two approaches can indeed be followed for the analysis of magnetic field measurements from space. The first one, referred to as the comprehensive inversion (CI) approach, attempts to solve for all known magnetic field contributions through a grand inversion (e.g., Sabaka and Olsen, 2006; Sabaka et al., 2013; Olsen et al., 2010a). This approach requires some assumptions about the geometry of the dominant source fields to guide the model parameterization. Because of the time needed to properly sample the Earth’s surface and because of the satellite orbital precession through local time (LT), the CI approach relies on mathematical models describing the sources only on average in space and time. For the recent CHAMP mission, the complete coverage in space and LT was achieved after about 130 days (Olsen et al., 2010b, figure 8). As a result, in such models the external magnetic fields with higher time frequencies may overlap with the small scale and weak lithospheric fields so that both contributions can be difficult to identify without ambiguity (e.g., Olsen et al., 2010c).
One may follow a second approach, referred to as the sequential approach, and focus on one specific constituent such as the lithospheric magnetic field (e.g., Maus et al., 2008). The ambiguity with respect to internal and external field separation can then be partly removed by adding prior information or by selecting measurements in a way that is more optimum. This is a complex and subjective procedure where the investigator’s decisions are needed all along the way to isolate the corresponding contributions. This approach successfully led to a suite of lithospheric field models with unprecedented spatial resolution (SH degree 133 for the MF7 model). Even though specific problems related to spectral leakage can arise (Sabaka and Olsen, 2006; Thébault et al., 2012), implying that all SH coefficients are not necessarily well resolved, these models clearly revealed striking regional correlations between magnetic anomalies and continental geological bodies at small spatial scales.
One of the primary goals of the European Swarm satellite mission (Friis-Christensen et al., 2006) is to unveil the lithospheric field signal to the highest possible horizontal spatial resolution. We therefore decided to develop a processing chain dedicated to the production of a lithospheric field model. This so-called ‘Dedicated Lithospheric Field Inversion Chain’ was proposed within the Swarm SCARF (Satellite Constellation Application and Research Facility, see Olsen et al., 2013) set up by a consortium of several research institutions and selected for implementation by ESA. It will be operated during the mission as one of more than a dozen Level 2 processing chains, which will also include a Comprehensive Inversion chain (producing an independent lithospheric field model, see Sabaka et al., 2013) and two other chains: the Swarm SCARF Dedicated Ionospheric Field Inversion chain (Chulliat et al., 2013) and the Swarm SCARF equatorial electric field inversion chain (Alken et al., 2013) developed by IPGP or in collaboration with NOAA.
Whichever the chosen modeling approach, the general idea is to carefully represent the selected and corrected data by a single set of parameters that allows computing the lithospheric magnetic field values outside the dominion of data. The common approach relies on the SH series expansion that is the most natural solution of the Laplace’s equation in the geocentric reference frame. Here we favor a regional modeling scheme which has several advantages. First, it makes it possible to bypass the problem of truncated spherical harmonics that can arguably be suboptimal for the purpose of highlighting small magnetic field wavelengths. Indeed, splitting the global problem into subre-gions allows high regional spatial resolution to be reached with a manageable number of parameters. Second, correction errors result mostly from transient external magnetic fields that contaminate the data in a different way depending on the location. Regional modeling can adjust to this by treating the noise regionally; it also offers the possibility of constraining the inverse problem depending on how well the regional model parameters are resolved (e.g., Lesur and Maus, 2006). Finally, computing regionally the covariance matrices of the errors for a better understanding of their correlation in space and in time is also possible, something that is demanding in terms of computer resources when building high degree SH models.
We report below on the Dedicated Lithospheric Field Chain as it was implemented during the preparation phase of the Swarm satellite mission. The block processes were duly tested in the course of the development and we do not discuss the details of the closed-loop simulations that were successfully completed. Rather, we focus on the end-to-end simulation and describe in some details the algorithm, its advantages but also its shortcomings. Because the dedicated techniques rely on the operator’s judgment rather than unequivocal scientific observations (which often raises some contentious issues), we describe the difficulties we met and the compromises we decided to make. We finally show that the chain is able to produce a lithospheric field model that reaches the Swarm performance criteria (Swarm Level 2 Processing System Consortium, 2013).
2. Theoretical Background
Different regional modelling techniques are currently used or under development in the field of geomagnetism (see Schott and Thébault, 2011, for a review). These are based, for instance, on frames of Poisson wavelets (e.g., Maier and Mayer, 2003), slepian functions (e.g., Beggan et al., 2013), combination of band-limited spherical harmonics (e.g., Lesur, 2006), spherical tesselation (e.g., Stockman et al., 2009), or equivalent dipole source distributions (e.g., Langlais et al., 2004). We choose to rely on the Revised Spherical Cap Harmonic Analysis (R-SCHA, Thebault et al., 2006) technique as this approach was successfully used with the CHAMP magnetic data to build a global model of the Earth’s lithospheric field (Thébault, 2006). We briefly restate the basic properties of the modelling strategy we follow. A complete description of the Revised Spherical Cap Harmonic Analysis technique can otherwise be found in (Thébault et al. 2004, 2006).
Empirically, we observe that a solution defined by the Neumann boundary conditions converges fast for the vector magnetic field components. This is a desired property when dealing with anomaly fields still possibly containing large spatial scales magnetic field contaminations, which is usually the case when processing real satellite measurements or realistic synthetic Swarm datasets built from SH models. The spherical and spherical cap harmonics both allow an exact representation of any poloidal magnetic field so that the two solutions converge in norm to each other. However, some representation errors invariably occur when the infinite series (Eqs. (1) and (2)) are truncated to finite expansion indices. A regional solution converging fast can represent the magnetic field B with fewer parameters than a slow converging series expansion. It guarantees a better comparison with the benchmark model during the synthetic validation of the algorithm as it mitigates the problem of truncation errors. There are some disadvantages, though, of combining the Eq. (1) with (2). In particular, the basis functions are not mutually orthogonal within the conical domain (Thébault et al., 2004). This leads to a non-diagonal design matrix where cross-talking between parameters implies some reorganization of their estimated values when changing the series truncation. In general, this is not ideal for carrying out spectral analysis of the magnetic field signal or for isolating a single model parameter. For the purpose of this work, this is a minor issue because we do not aim at interpreting the values of each regional parameter independently and because we only deal with high spatial density satellite data. In such a case, the design matrix, although not diagonal, is never dense. The inverse problem is numerically stable.
3. The Dedicated Lithospheric Field Inversion (DLFI) Chain
3.1 Data selection
For this simulation, we use only the vector Level 1b data simulated for the lowest pair of satellites Swarm A and Swarm B (Olsen et al., 2013) since the third satellite, Swarm C, is expected to be too high to detect the fine lithospheric field structures. Nevertheless, its data could prove useful for the chain in case of a failure of Swarm A or B and all data selection and correction procedures described below were also made operational for processing Swarm C magnetic field measurements. Considering that vector magnetometers may suffer from malfunctions, the chain was also adapted to ingest scalar magnetic measurements if required.
More than four years of simulated vector Swarm A and B data are selected between a simulated time period extending from July 1998 to December 2002. These data are sub-sampled every 10 seconds, corresponding to a spacing of about 70 km along the satellite track at 400 km altitude. This ensures that no aliasing occurs because of magnetic field contributions at small wavelengths (recall that the minimum spatial wavelength detected by the regional model is 130 km with the current setting). Although the synthetic data do not contain toroidal external fields from field aligned currents, we account for the different behavior of the external field with latitudes by separating the vector data in two sets, one for mid-latitudes (−52° to 52° magnetic latitudes), and one for polar regions (>52° and <−52°). In addition, we allow an overlap of 10° between mid and polar latitude regions (see also Maus et al., 2008, for instance) so that the provisional selected data for both sets range between −57° to 57° magnetic latitude for the mid-latitude set and above ǀ±47ǀ for the polar set. As discussed below, this overlap is introduced to reduce correction errors caused by dedicated corrections applied along the satellite tracks. The mid-latitude data are further selected at 21:00 to 5:00 local time (LT) in order to minimize the contributions from the ionospheric S q field. All LT are considered for the polar data, provided they are outside the sunlit area (−10° below horizon). We use the DSt index to lower the effect of the magnetic field generated by the ring current and select the data corresponding to DSt values lower than ±20 nT and to Dst variations smaller than 10 nT over the previous three hours. We also apply a selection criterion based on the Kp index to keep data corresponding to a global low level of geomagnetic activity. The data corresponding to a Kp index larger than 2, and to Kp variations larger than 2 over the previous three hours, are rejected. For this study, the selected Dst threshold is relatively large. We argue that rejecting many satellite data because of a high level of magnetic activity does not necessarily reduce the noise in the final model, as the data error variance is proportional to the ratio v/M, where v is the variance of the external field and M the number of available orbits over a given longitude (e.g., Lesur et al., 2013). It is important to define an acceptable trade-off between the number of available satellite tracks and the level of external field activity, more particularly when processing the data on regional scales because the local functions require a dense data coverage in space.
The selection procedure we applied is not exhaustive. The process 1.2 (see Fig. 2) contains more data selection modules than the ones activated for this simulation. Among other selection criteria we included a processing block based on the measure of the Interplanetary Magnetic Field (IMF), whose value is related to the solar wind activity. We included also a selection block based on the ap index, which measures the general magnetic activity at the planetary scale, and a selection block based on quality flags such as the on/off status of the star camera. Other selection blocks are likely to be added as more and more experience is gained on the Swarm satellite data during the calibration/validation and operational phases.
3.2 Data correction for the main and external fields
We developed two families of magnetic field corrections for the selected vector data. The first family relies on explicit models for the main field, its secular variation, and the magnetospheric field, (processes 2 and 3 in Fig. 2), all expanded in spherical harmonics. These input models are provided by the other Swarm processing chains (see Olsen et al., 2013). Note that the data are not corrected for the ionospheric field, which is assumed minimum at night-times (see Chulliat et al., 2013). The second family of correction is based on more empirical processes, performed either at the global scale, or along the satellite orbits (process 4). The settings of this suite of corrections depend on the analysis of the data residual after the completion of processes 2 and 3.
Within the overall process proposed by the consortium (see Olsen et al., 2013), the dedicated lithospheric field chain is initiated as soon as the models for other source fields are available for use. The main field correction can be performed using either the output of the comprehensive inversion chain (Sabaka et al., 2013) or that of the dedicated core field chain (Rother et al., 2013). In principle, there is a better consistency between the data selection detailed in the previous section and the data selection applied in the dedicated chain for the core field (Lesur et al., 2010; Rother et al., 2013), particularly at night times. This consistency is important if one keeps in mind that differences in data selection are acknowledged to be one of the major sources of discrepancies between main field models yet parameterized in similar ways (e.g., Finlay et al., 2010). In the course of the Swarm preparation phase, we tested the influence of each of the input main field models and the results were similar. In this paper, the solution is obtained with the vector data corrected with the MCO SHAi2D (the output of the core field dedicated inversion, see Fig. 2) for the main field model and its secular variation up to SH degree 15. Since the synthetic Swarm vector measurements were generated using a secular variation model up to SH degree 20 (Olsen et al., 2013), the secular variation is only partly corrected for. The corrections for the external magnetospheric sources are made using the MMA SHAi2C model (Sabaka et al., 2013; see also Fig. 2). This model provides coefficients for the primary magnetospheric field to SH degree 3 and a maximum order 1 with a time step of 1.5 hours. The induced counterpart is also defined every 1.5 hours but to maximum degree and order 5. This space and time resolution is lower compared to the benchmark magnetospheric field model used to generate the synthetic data. This represents another source of significant correction error.
We next identify the Swarm A and B data with the common reading times and built up a set of so-called gradient data. The terminology of gradient is misleading here as it refers to a point to point difference between the measured data across the two orbits of the lowest pair of satellites (Swarm A and B). This difference is expressed in the same units as the vector measurements (in nT), which avoids the unnecessarily complication of solving the inverse problem with different data types (the true gradients are in nT/km or nT/degree). Considering the nature of the residuals, and their variations in space and in time, taking the difference between the data from the lower pair of satellites in the East-West direction, spaced about 1.4 degree apart (at the geographic equator, see Friis-Christensen et al., 2006), appears to be an efficient way to mitigate the contributions of large-scale non-lithospheric fields. This gradient however is incomplete since the across difference between the two satellite measurements approximates only the three gradient components along the East-West direction. There is no redundancy with the vector measurements that are still needed to recover the lithospheric field and to stabilize the inverse problem.
The first additional block process aims at correcting globally for the large spatial scale error of reduction, be it of internal or external origin. The internal and external Gauss coefficients are estimated to SH degree 8 in the inclined dipole reference frame with a one year knot-spacing over the full simulated mission duration. We also scale the measurements by the F10.7 solar radio flux values in order to account for the dependence of the ionospheric field on the solar activity. The improvement brought by this scaling is rather marginal but reduces the offsets between close satellite encounters. Note that the internal and external Gauss coefficients estimated by the dedicated corrections have little scientific value as they contain numerous sources of magnetic fields. They are not intended to be interpreted but they remain useful for better understanding the origin of the large scale field residuals. There is no major technical limit for this processing block to accept more sophisticated parameterization or improved time resolution. For instance, it could be fine-tuned to absorb most of the remaining large scale magnetic fields in case we lack the explicit models for the main and the magnetospheric fields described above.
The final dedicated correction is performed via a Fast Fourier Transform along the satellite tracks. The technique of high-pass filtering along the tracks dates back to the 1980’s (Langel and Hinze, 1998, section 4.4). The inconvenience of this procedure is that there is no clear cutoff frequency in the signal to isolate the contributions of the lithospheric field without ambiguities (see for instance Wang, 1987 for a discussion). Also, it can only be applied independently on the three magnetic field components. This has much less physical justification than methods based on SH representation. However, the along-track Fourier filtering has interesting convergence properties. When the data are properly tapered, it significantly filters the remaining intermediate wavelengths while producing little edge effect. We use this processing block to further reduce the magnetic field contributions with length-scales larger than 10° in arc-length along the satellite orbit using a Butterworth filter with a sharp cutoff (filter of order 20). The overlapping data at the junction between mid and polar areas are then used to confine possible edge effects outside the effective data geographic intervals. It is worth stressing that this processing block must be used with extreme care as it cannot discriminate between perturbation and lithospheric fields. In particular, the cut-off frequency must be adjusted depending on how well the AUX_LIT_2 model values temporarily removed from the data agree with the measurements in the filtered waveband.
Finally, the redundant data that were kept to improve the continuity between the processing in mid and polar latitudes (see Subsection 3.1) are removed from the dataset. Then, the standard deviation and the mean of the residuals are computed for each vector component. All values outside the 3σ range are considered as outliers and thus rejected and the auxiliary lithospheric field model values subtracted before the series of dedicated corrections are added back.
Figure 4 shows the residual map for the vertical component after all corrections (where, again, the lithospheric field contributions have been subtracted for the purpose of illustration). The processing applied to the vector data is heavy but successful (compare Figs. 3 and 4). However, the corrected measurements now contain a certain amount of artifacts caused by the ad hoc corrections we applied. This shows how important the gradient data are to balance the correction errors made when correcting the vector data for other contributions than those from the lithospheric field. Still, the corrected data can be assumed to reflect mainly the lithospheric field contributions and are now ready to be used for modelling purposes.
3.3 Regional iterative modelling of the pre-processed data
The selected and corrected vector data, with their East-West gradients, are processed regionally (Processes 5 and 6 in Fig. 1). The first step consists in distributing the data within each of the 600 spherical cones that patch the Earth at the Swarm A and B altitudes. Then, the inverse problem is solved for each region. The cones have 8° aperture, are centered on the nodes of an equal area grid (Saff and Kuijlaars, 1997) about 8.5° spaced apart, and therefore overlap with each other. The lower and upper radii are automatically defined by the minimum and maximum altitudes of the available data within each cap. The estimated maximum likelihood regional parameters of each type (see Eqs. (1) and (2)) are stored for each region. The maximum horizontal spatial resolution is about 130 km (see Eq. (5) with kmax = 15).
The R-SCHA technique, initially set up for processing the CHAMP satellite data (Thebault, 2006), was further developed to ingest the Swarm satellite vector and scalar data. This required the implementation of specific tools to deal also with the magnetic field satellite track differences (referred to as gradient data), with the inversion procedure, its weighting, and its regularization.
3.4 Conversion to a SH model and assessment
We finally convert the regional models into a set of Gauss SH coefficients. The most efficient way to do this is to exploit the sampling theorem on the Earth’s sphere (see for instance Schaeffer, 2013 and references therein). We first compute the forward problem for each regional model on the nodes of a Gauss-Legendre grid in the geocentric reference frame (see process 7 in Fig. 1) at 400 km altitude (this corresponds to the median altitude of the considered dataset). This grid satisfies the sampling theorem to SH degree 300. To ensure that the numerical solution is not affected too much by the lack of measurements in the polar gap, we rely on a final module. Indeed, large errors, or lack of data, near the geographic pole have a clear adverse effect on the recovery of some constituents of the lithospheric field. The zonal SH coefficients (of order m = 0) are mostly constrained by the magnetic field vector components (mostly the horizontal ones) at high latitudes. The Swarm orbital configuration tested in this study has a polar gap of about 5.2°. This represents a diameter of about 615 km at 400 km altitude. Discontinuities caused by the polar gaps introduce ringing when local functions are used. This problem is addressed using a post-processing based on an iterative regional modelling of the vector values computed on the Gauss-Legendre grid above the two polar gaps. The vector data outside the Northern (respectively the Southern) polar gap are first used to derive a low spatial resolution regional model (i.e., with a minimum spatial wavelength larger than the size of the polar gap). Synthetic data are then generated from this low resolution model on the Gauss-Legendre points located within the Northern (respectively the Southern) polar gap areas and a new set of model parameters is estimated at the next iteration to a higher spatial resolution. The process stops when the spatial resolution of the model over the polar gaps reaches the same resolution as in other regions. This iterative procedure could have been implemented directly in the block dedicated to the regional inversions (Fig. 1). However, implementing it as a post-processing step offers a better control because the ratio between the number of gridded data inside and outside the polar gaps is then the same from one simulation to the other.
Finally, we cast the spatial vector data computed on the Gauss-Legendre grid into the SH using a fast spherical transform of the vertical component (process 8 in Fig. 1). This is generally done up to SH degree 300 to provide a theoretical spatial resolution for the model in agreement with the one provided by the local basis functions. The transformation into SH Gauss coefficients could also be done by a slower module that computes the problem in a least-squares sense. This process would allow considering the three vector field components, some global scale regularization to be introduced if needed, and to double check the model obtained by the fast spherical transform. The official and final results will then be provided as a set of Gauss coefficients up to SH degree 150 (MLI_SHA_2D, see Fig. 1). However, recognizing that some regions are better represented than others (see Fig. 6), a similar set up to SH 200 (MLI SHA 2E) will also be provided. This latter model, however, should not be downward continued to the Earth’s surface unless otherwise stated (for this reason, we call it a map in Fig. 1).
In this paper we presented the Swarm SCARF Dedicated Lithospheric Field Inversion chain, which will be used to process the magnetic data of the forthcoming Swarm satellite mission and to produce a model for the Earth’s lithospheric field. This approach differs significantly from the comprehensive approach (Sabaka et al., 2013) as it heavily relies on data selection, corrections, and visual inspections. It also uses a modeling scheme based on local functions that were designed to better detect the small scales of the lithospheric field. During the operational phase, the criteria discussed in this paper will be subject to changes and will therefore be described in a companion report of the Swarm SCARF dedicated lithospheric field model. With the current setting, the algorithm provides a model that meets the required performance at least up to SH degree 133 when considering and the synthetic data provided to us for the full mission duration. This is a better spatial resolution than achieved so far by single satellite missions at comparable altitudes. This result confirms that we are able to develop strategies for recovering the lithospheric magnetic field to a high spatial resolution in a favorable situation when high quality vector magnetic field measurements are available for the two lower Swarm A and B satellites. This simulation was realistic in the sense that it was realized with a mathematical method different from the one used to synthesize the simulated data, with a separation into regions that inevitably introduces discontinuities, with imperfect main and external field models for correcting the synthetic measurements for non-lithospheric magnetic fields, and with real proxies for selecting the data for quiet magnetic days along the entire simulated mission duration. However, in the operational phase, the performance of this chain will depend on our ability to estimate the real quality of the input magnetic field measurements and the accuracy of the scientific products used to correct for the main and the external fields. For instance, complementary simulations (not shown) performed with the same parameters as the ones described in this paper suggest that a small bias of 0.3 nT affecting intermittently Swarm A or B vector measurements, would degrade the overall performance down to about SH degree 110–120. It is worth stressing that even this degraded performance remains impressive compared to those achieved by single satellite missions, which based on the experience with CHAMP are of the order of SH degree 85 (this it the maximum SH degree for which models start being in significant disagreement). An improvement from n = 85 to n = 120 means that twice as many SH Gauss coefficients would be recovered (the number of Gauss coefficients is n(n + 2)). This spatial resolution limit may not be a hard bound but it shows that the recipe we followed may need to be revised and fine-tuned when real data will become available.
The Swarm calibration/validation phase will be a valuable learning experience to better control the intrinsically different information content and contamination errors of the vector and the gradient data. Some tools have been developed to account for the statistical differences between these two types of datasets. In this paper, we did not try to optimize the weights or to regularize the inverse problem but this possibility was left open on both the regional (Process 6.2) and the global scales (Process 8). More theoretical work will be needed to define the most relevant physical norms to be used for the lithospheric field and fully benefit from this possibility. We may also select the spectral band corresponding to the highest information content for each type of data to constrain the model with vector data at the low SH degrees and with gradient data at high SH degrees (see Kotsiaros and Olsen, 2012 for a discussion). This is an option we did not consider at present because the gradient estimated from the Swarm lower pair of satellites is not complete. Its implementation is not necessarily complex but it adds another level of subjectivity concerning the respective spectral bands that are better constrained by each data type.
A major issue we did not address is that of the impact on the East-West gradient of undesired magnetic signals due to electric currents that would cross the two orbits of the lower pair of satellites. At present, the R-SCHA technique is efficient for processing poloidal magnetic field measurements but cannot handle toroidal fields without some significant amount of development. This is the main shortcoming of the Dedicated Lithospheric Field Inversion chain in its present form. But we may still exploit the information provided by the East-West gradient to at least estimate the amount of current crossing the Swarm A and B mesocenter (see Kotsiaros and Olsen, 2012, equation (3.8); or Shen et al., 2012, for instance) and to use this as a selection criterion. We could then use the gradient at times (and location) of negligible estimated currents. We note that, as it stands, the chain could also readily be used with scalar gradient data only that are in general less affected by toroidal fields.
One key advantage of the Dedicated Lithospheric Field Inversion chain is that it is based on a regional modeling approach. This allows the inverse problem to be solved independently for each region. Depending on the available computer resources, the process divided in as many independent jobs is intrinsically fast. For the present simulation, a few hours were necessary to select and process more than five million out of more than 250.106 available vector synthetic measurements of the Swarm A and B satellites. A fast algorithm is advantageous considering the chosen philosophy. Isolating the lithospheric field relies on a careful selection of data and on compromises made in correcting the data more or less empirically. Therefore, fast processes open an avenue for computing parades of statistically equivalent models in order to estimate the variability of each SH degree part depending on the applied selections and corrections. An immediate application of this principle would be to play with the boundary separating mid and polar regions as it introduces one of the largest source of errors in this simulation (see Fig. 8).
The algorithm is also highly modular. Complementary processing blocks could be included as more and more experience is gained with the real Swarm satellite measurements. Preprocessing blocks based on quality indicators, flags, and star camera switches could be useful to account for instrumental failures or malfunctions. The algorithm is therefore not frozen and will benefit from the scientific advances prompted by the Swarm mission along its entire duration. Finally, we note that the median altitude of Swarm A and B measurements was about 400 km for the simulations we discussed. An extension of the mission to lower altitudes would amplify the small-scale signals, which are currently strongly attenuated at 400 km altitude, and would possibly allow us to derive lithospheric field models to even higher resolution.
The authors gratefully acknowledge support from the Centre National des Etudes Spatiales (CNES) within the context of the “Travaux préparatoires et exploitation de la mission Swarm” project and from the European Space Agency (ESA) through the ESTEC contract No. 4000102140/10/NL/JA “Development of the Swarm Level2 Algorithms and Associated Level2 Processing Facility”. We also acknowledge the comments of two anonymous referees that helped to improve the manuscript. This is IPGP contribution number 3410.
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