Combining Faraday Tomography and Wavelet Analysis

Dmitry Sokoloff 1,2,*, Rainer Beck 3, Anton Chupin 4,5 , Peter Frick 4,6, George Heald 7 and Rodion Stepanov 4 1 Department of Physics, Moscow University, 119992 Moscow, Russia 2 Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Kaluzhskoe Hwy 4, Troitsk, 108840 Moscow, Russia 3 MPI für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany; rbeck@mpifr-bonn.mpg.de 4 Institute of Continuous Media Mechanics, Korolyov str. 1, 614061 Perm, Russia; chupin@icmm.ru (A.C.); frick@icmm.ru (P.F.); rodion@icmm.ru (R.S.) 5 Department of Mechanics and Mathematics, Perm State National Research University, Bukirev str. 15, 614990 Perm, Russia 6 Department of General Physics, Perm State National Research University, Bukirev str. 15, 614990 Perm, Russia 7 CSIRO Astronomy and Space Science, P.O. Box 1130, Bentley, WA 6102, Australia; George.Heald@csiro.au * Correspondence: sokoloff.dd@gmail.com


Introduction
The main bulk of contemporary knowledge concerning magnetic field configurations in spiral galaxies is obtained based on observations performed at a few wavelengths only. Modern progress in observational techniques allows us to observe galaxies at dozens and hundreds of wavelengths. It is however important to learn how to use this new tool. Some problems which arise in this way are illustrated at Fig. 1. The left panel gives the linearly polarized intensity distribution of NGC 6946 at λ = 6 cm from Beck et al. [1]. Magnetic spiral arms are clearly seen. Magnetic arms can be important because they possibly are magnetic reconnection regions [2] or may also be products of dynamo action [3]. However their origin remains unclear [4]. The middle panel shows the polarized intensity distribution obtained around λ = 20 cm in the modern multi-wavelength observations in the spectral range from 17 to 22 cm. The plot looks almost empty. It happens because of two reasons. On one hand, it is impractical to observe at each spectral channel as long as it was done in observations performed at just one wavelength. On the other hand, depolarization effects by Faraday rotation are much more pronounced at longer wavelengths rather at λ = 6 cm.
One can try resolve the problem in two ways. Firstly, it is possible to sum polarized intensities over all channels in the range λ = 17 ÷ 22 cm to emulate single-wavelength observations at λ ≈ 20 cm. This option, however, does not look attractive because it means that we emulate old-fashion results using modern observational technique. Another option is to use RM-synthesis which involves processing data at many wavelengths. Reconstruction of magnetic field even along a single line of the sight remains a challenging problem [5]. 3D RM-cube data (i.e. maps of polarized intensity at many wavelengths) can be processed in various ways. A straightforward approach is to pick up maximum values of Faraday spectra (i.e. the distribution of polarized intensity as a function of Faraday depth) [6]. The resulting distribution of F max is shown in Figure 1(c). The signals are much stronger than those shown in Figure 1(b). However, we do not see here the narrow magnetic arms visible in Figure 1    We face a difficult choice: to postpone multi-wavelength observations of magnetic arms in spiral galaxies until the forthcoming SKA telescope will be ready for observations in its full extent or to suggest a method which allows to recover magnetic arms from the available multi-wavelength data taken at long wavelengths. The second way looks more attractive. The desired method is described by Chupin et al. [7]. Technical details of the method are rather bulky. It is why here we present the idea of the method in a compressed form and illustrate it by an example of the NGC 6946 data obtained by Heald et al. [6] at λ = 17 ÷ 22 cm (Section 2) and by an artificial example (Section 3).

Idea of the method applied to the NGC 6946 data
The method under discussion [7] departs from the point that polarized observations performed at the wavelength λ * are most informative for magnetic structures of the scale l * for which λ 2 RM ∝ λBn e l is comparable with π. Indeed, contribution from the structures with l l * is strongly depolarized due to Faraday rotation while Faraday rotation from the structures with l l * is too weak to be useful. It means that using observations at λ 1 = 20 cm instead of that ones at λ 2 = 6 cm we deal with magnetic structures that are an order of magnitudes smaller ((λ 2 /λ 1 ) 2 ≈ 10). In other words, instead of detecting magnetic arms by large scales we have to do it by small-scale structures which arise by tangling and randomizing of large-scale structures, in addition to small-scale structures by small-scale turbulent magnetic fields predicted by dynamo theory.
Realization of the idea suggested in [7] is based on wavelet technique. Wavelet functions are used for an analysis of spatial and temporal data, also in astrophysics [8]. The wavelet transform can be used as an advance of RM-synthesis to structure analysis at different scales [9,10]. Here wavelets are used as a spatial-scale filtering tool. We decompose all all maps of polarized intensity at a given Faraday depth by wavelets of various scales (w l ) and then find a peak intensity w max along each line of sight. Results for various scales l measured in arcseconds are shown in the middle row of Figure 2. We recognize small-scale structures at the scalel = 16 arcsec that are ordered as arm-like structures. The structures at smaller and larger scales are less pronounced. In other words, we traced the structure of magnetic arms known from λ 1 = 6 cm using the data obtained at λ 2 = 20 cm. In a comparison the result of wavelet decomposition of polarized intensity at 6 cm (left row of Figure 2) and the peak Faraday spectra F max (right row of Figure 2) are much noisier. The technical details of the method are given in [7].

Synthetic data analysis
We constrain a model magnetic field to demonstrate qualitatively the applicability of our approach and to support an interpretation of the results. The galactic magnetic field B g is modelled as a superposition of a large-scale component B and a small-scale turbulent component b: where r is the radius vector in the cylindric coordinate system (r, φ, z). The regular part of magnetic field is assumed to be of bisymmetric form with two reversals along azimuthal angle: where B 0 is the field amplitude (strength) and φ 0 is the azimuthal phase of the mode m, p is a pitch angle, R 0 and h 0 are the Gaussian radius and vertical scales of the magnetic galactic disk. The tanh term is introduced to suppress a peculiarity near axis at characteristic radius r 0 [11]. Then components of regular magnetic field are evaluated by where a latter relation is a result of the incompressibility condition. The turbulent magnetic field is considered as a divergence-free, random fluctuating field with the given energy spectra Ψ and Gaussian spatial distribution with the radius R t and the vertical scale h t : where b 0 is the strength of the turbulent field. The spectral property of the random function Ψ are specified as follows: We adopt α = −5/3 (Kolmogorov scaling), β = 2, k 0 = 10h −1 t [12].  Figure 3 shows the distribution of galactic magnetic field in three-dimensional numerical domain 14 × 14 × 14 kpc 3 with resolution 0.4 kpc for a particular choice of parameters: m = 1, p = π/12, h 0 = 1 kpc, R 0 = 14 kpc, r 0 = 4 kpc, R t = 20 kpc, h t = 4 kpc and B 0 = b 0 = 1. Thermal electron and cosmic rays densities are adjusted to get qualitative correspondence with the observation. We use simulated magnetic field to calculate an artificial maps of polarized intensity and Fadaray rotation for λ in the observed range from 17 to 22 cm. Then synthetic RM-cube is analysed by the same approach as NGC 6946 data in the Section 2.
For the case of zero-noise contribution in polarized intensity the distribution of F max (see Figures 4(a)) is slightly affected by Faraday depolarization. We note the result does not differ from the initial distribution in Figure 3(a) because the rotation measures are rather moderate (a few tens rad/m 2 ) and the beam depolarization effect is not taken into account. However, the synchrotron emission is considerably scattered over the Faraday depths so that small-scale structures appear in distribution of w max (see Figures 4(b)). Nevertheless the large-scale structure of galactic magnetic arm is well traced by w max . The situation is substantially changed in the case if a white noise of level S/N = 20 is added to the ideal observations. Figure 5 shows resulting distribution of F max and w max in the presence of the noise. The galactic signal in F max representation is getting much weaker. At the same time the distribution of w max reveals the magnetic arms with a patchy structure.

Discussion
In this paper, we presented an idea how to use long-wavelength multi-wavelength observations to isolate magnetic structures which were previously accessible from short-wavelength observations only. Our understanding of the method is that we isolate small-scale structures in the RM-cube which are associated with a large-scale structures of magnetic field distorted by Faraday dispersion. We support this interpretation by an analysis of a synthetic observation obtained using a realistic model of a galactic magnetic field. The above results demonstrate that the method can be helpful in practice especially in the case of noisy polarization data at an individual wavelength. However, we keep in mind that small-scale structures of a magnetic field may contribute in wavelet coefficients. Existence of such structures was a general expectation from dynamo theory but the previous methods do not allow isolating this. We note that wavelet technique can be successfully combined with modern approaches like the Faraday tomography [13] and the method based on the synchrotron derivative polarization gradients [14]. Then one can probe the local interstellar medium in the Galactic foreground towards some galaxies [15]. Our model of galactic magnetic field may be also useful for validation of processing results.
Author Contributions: The idea of the method presented here belongs to R.S. and A.Ch., P.F. embedded the method in the general framework of wavelet methods, D.S. is responsible for the link with dynamo studies, R.B. elaborated the link with classical RM-synthesis, the observational data exploited was obtained by G.H.