Magnetic Fields in Galaxy Clusters and in the Large-Scale Structure of the Universe

Abstract

The formation and history of cosmic magnetism is still widely unknown. Significant progress can be made through the study of magnetic fields properties in the large-scale structure of the Universe: galaxy clusters, filaments, and voids of the cosmic web. A powerful tool to study magnetization of these environments is represented by radio observations of diffuse synchrotron sources and background or embedded radio galaxies. To draw a detailed picture of cosmic magnetism, high-quality data of these sources need to be used in conjunction with sophisticated tools of analysis.

1. Introduction

Evidence of magnetization has been found in a variety of environments up to the largest gravitationally bound systems of the Universe, clusters of galaxies. A fraction of galaxy clusters hosts diffuse and extended synchrotron sources that reveal the presence in these systems of ∼$\mathsf{\mu }$G magnetic fields and ultra-relativistic electrons ($\gamma \gtrsim {10}^4$) at their center (e.g., [1,2]). Despite the fact that these sources have been detected only in about 50 galaxy clusters, the presence of magnetic fields has been recognized in all galaxy clusters because they act as a birefringent medium for the signal traversing them (e.g., [3]). Magneto-hydro-dynamical simulations suggest that filaments connecting galaxy clusters should be magnetized with strengths ≳ nG (e.g., [4]). To date, only indications of the presence of magnetic fields have been found outside galaxy clusters [5] and upper limits on their strength of 0.03–2 $\mathsf{\mu }$G have been derived from the cross-correlation of radio images with magneto-hydro-dynamical simulations and data at other wavelengths [6,7]. Filaments should also host a large fraction of the thermal baryons that inhabit our Universe that should be visible at X-ray and millimeter/sub-millimeter wavelengths due to thermal bremsstrahlung and the Sunyaev-Zel’dovich effect. These signals are very hard to detect due to the low-densities involved. However, the mixing of magnetic fields and thermal particles could be observed at radio frequencies through the Faraday rotation of the signal of background radio sources up to a level of ∼1 rad/m${}^2$ [8].

Observations of radio galaxies and diffuse synchrotron radio sources in the large-scale structure of the Universe have the potential to shed light on the magnetic field properties in these environments and, therefore, give a precious contribution in the comprehension of genesis and history of cosmic magnetism. Presently, there is a general agreement on a primordial seed field modified in strength and geometry by structure formation processes. Galaxy clusters mergers, for example, can amplify magnetic fields and completely change their structure. Therefore, intracluster magnetic fields are thought to reflect the present level of turbulence in the environment and, consequently, the evolutionary processes. In the cluster outskirts, filaments, and voids of the cosmic web, the gas motion did not have enough time to affect magnetic field strength and structure and, therefore, they are deeply linked to those of the seed field. A detailed overview of magnetic field properties in these environments is essential for shedding light on cosmic magnetism but the detection and measurement of these magnetic fields are very challenging due to their extremely weak strengths. High-quality observations obtained with the new generation of radio telescopes in combination with advanced tools of analysis will play a key role in the study of magnetic fields from galaxy clusters to filaments and voids.

In the following, we report our recent works in the field. In Section 2, we describe the techniques that can be used for the study of magnetic fields in the large-scale structure of the Universe, with the help of the numerical simulations presented in Section 3. In Section 4 and Section 5 we respectively present and discuss our findings concerning the magnetization of galaxy clusters and the results and perspective beyond these systems. Finally, in Section 6 we draw our conclusions.

2. Methods

The presence of magnetic fields in the large-scale structure of the Universe can be investigated through the analysis of the emission of diffuse large-scale synchrotron sources and the Faraday effect on background radio galaxies with data of both individual objects and statistical samples. Diffuse synchrotron emission probes magnetic field properties on large-scales, while the depolarization of the radio galaxy signal witnesses the small-scale properties of magnetic fields.

2.1. Diffuse Synchrotron Emission

To date, diffuse synchrotron sources called radio halos have been detected in about 50 galaxy clusters characterized by ongoing violent mergers (Figure 1, left panel). Radio halos directly prove the coexistence of magnetic fields and ultra-relativistic electrons at the center of galaxy clusters. Their emission in total intensity and polarization is deeply linked to the properties of intraclutser magnetic fields in strength and structure: total intensity is primarily related to the magnetic field strength, while polarization to its degree of order. Therefore, the analysis of their properties is capable to put solid constraints on the intracluster magnetic field power spectrum. Radio halos are characterized by a brightness of about 0.1–1 $\mathsf{\mu }$Jy/arcsec${}^2$ at 1.4 GHz, are ∼Mpc in size, show a radio emissivity of ≈${10}^{-42}$ erg/s/cm${}^3$/Hz and, unfortunately, are typically unpolarized at the present sensitivity limits (see [9] and references therein). In the periphery of a fraction of galaxy clusters, diffuse low-surface-brightness (∼0.1–1 $\mathsf{\mu }$Jy/arcsec${}^2$ at 1.4 GHz), extended (≳1 Mpc) and strongly polarized (≈20–30%) sources have been observed. They indicate the presence of ≈$\mathsf{\mu }$G magnetic fields and $\gamma \gtrsim {10}^4$ relativistic particles at the location of shock fronts in disturbed systems (e.g., [10]). Beyond galaxy clusters, only hints of diffuse synchrotron sources have been reported in the literature, corresponding to a surface brightness ∼0.01–0.1$\mathsf{\mu }$Jy/arcsec${}^2$ at 1.4 GHz (e.g., [11,12]).

2.2. Polarimetric Properties of Radio Galaxies

An alternative and complementary instrument to study magnetic fields in the cosmic web is given by the Faraday effect on embedded or background radio galaxies (e.g., [14]). The linearly polarized signal of a radio galaxy suffers a rotation of the polarization angle while crossing a magneto-ionic medium as a galaxy cluster. For a completely foreground Faraday screen, the rotation is given by

$${\mathsf{\Psi }}_{\mathrm{obs}}={\mathsf{\Psi }}_{\mathrm{int}}+RM{\lambda }^2$$

(1)

where ${\mathsf{\Psi }}_{\mathrm{int}}$ and ${\mathsf{\Psi }}_{\mathrm{obs}}$ are respectively the intrinsic and observed polarization angle, $\lambda$ is the wavelength of observation, and $RM$ is the rotation measure,

$$RM=812{\int }_0^l{n}_{\mathrm{e}}{B}_{\left|\right|}dl\mathrm{rad}/{\mathrm{m}}^2,$$

(2)

related to the magnetic field component parallel to the line of sight $B_{\left|\right|}$ ($\mathsf{\mu }$G) and to the thermal gas density $n_{\mathrm{e}}$ (cm${}^{-3}$) of the magneto-ionic medium along a physical depth of l (kpc). A linear fit of the observed polarization angle ${\mathsf{\Psi }}_{\mathrm{obs}}$ versus ${\lambda }^2$ at three or more different wavelengths permits the derivation of the intrinsic polarization angle and the rotation measure. Detailed rotation measure images can be obtained with a pixel-by-pixel fit of high-quality and extended polarization images of a radio galaxy at multiple frequencies. If the source is embedded or in the background of a galaxy cluster and the cluster is the only or the predominant contribution to the Faraday rotation, this image represents a two-dimensional projection of the intracluster magnetic field: the mean value of the rotation measure image probes the magnetic field fluctuations on large spatial scale, while its dispersion reflects the turbulent behavior of the field on small scales. Unresolved rotation measure structures in the foreground screen cause a depolarization of the signal of the radio galaxies. Therefore, depolarization of the radio galaxy signal can be used in conjunction with the analysis of the rotation measure images to constrain the intracluster magnetic field [15,16].

3. Simulations

A detailed evaluation of the magnetic field power spectrum from radio observations of diffuse synchrotron sources and polarized emission of radio galaxies is not an easy task (e.g., [17,18]). Following [19], we look for the best magnetic field that describes the data by using a numerical approach based on the comparison of the observations with synthetic images corresponding to different configurations of the magnetic field. Numerical simulations of diffuse synchrotron sources and of radio galaxies require a model of the thermal and non-thermal components: images of diffuse synchrotron sources in total intensity can be produced based on a model for the magnetic field and for the relativistic electrons, while polarization intensity and radio galaxy rotation measure images additionally require a thermal gas model. We assume:

• a Gaussian intracluster magnetic field with a power law power spectrum

  $$|B_k{|}^2\propto k^{-\mathrm{n}}$$

  (3)

  fluctuating between a minimum ${\mathsf{\Lambda }}_{\min }=2\pi /k_{\max }$ and a maximum ${\mathsf{\Lambda }}_{\max }=2\pi /k_{\min }$ spatial scale, where k is the wave-number and n the slope of the power spectrum $|B_k{|}^2\propto k^{-\mathrm{n}}$. The normalization of the power spectrum is fixed by imposing an average magnetic field radial profile $\langle B\left(r\right)\rangle$ proportional to a function of the thermal gas density $n_{\mathrm{e}}$,

  $$\langle B\left(r\right)\rangle =\langle B_0\rangle {\left(\frac{n_{\mathrm{e}}\left(r\right)}{n_0}\right)}^{\eta },$$

  (4)

  where $\langle B_0\rangle$ and $n_0$ are respectively the magnetic field strength and the thermal gas density at the center of the cluster and $\eta$ describes the radial profile;
• a population of relativistic electrons with a power law energy spectrum

  $$N(ϵ,\theta )=N_0{ϵ}^{-\delta }\frac{sin\theta }{2}$$

  (5)

  with energy $ϵ$ between ${\gamma }_{\min }{m}_{\mathrm{e}}{c}^2$ and ${\gamma }_{\max }{m}_{\mathrm{e}}{c}^2$, index $\delta$ related to the spectral index $\alpha$ of the radio halo emission through $\delta =2\alpha +1$, isotropic distribution of the pitch angle $\theta$ between the direction of the magnetic field and of their velocity and normalization $N_0$;
• a single $\beta$-model

  $$n_{\mathrm{e}}\left(r\right)=n_0{\left(1+\frac{r^2}{r_{\mathrm{c}}^2}\right)}^{-\frac{3}{2}\beta }$$

  (6)

  for the thermal gas in merging galaxy clusters [20], where $n_0$ is the central thermal gas density, $r_{\mathrm{c}}$ the core radius, an $\beta$ the parameter that describes the radial decrease. A combination of two $\beta$-models is more suitable in relaxed systems [21].

4. Magnetic Fields in Galaxy Clusters

We investigated the magnetic field properties in galaxy clusters characterized by different dynamical and thermal properties by comparing the observations of radio halos and powerful and extended radio galaxies with the expectation from numerical simulations. In

Table 1. Summary of all the clusters for which either a numerical or analytic study of the intracluster magnetic field is available.

Clusters	Observable(s)	Frequency Band(s)	Instrument(s)	Reference
A400	Radio galaxies	C, X band	VLA	[22]
A2634	Radio galaxies	C, X band	VLA	[22]
Hydra A	Radio galaxies	X band	VLA	[17,22,23,24]
A119	Radio galaxies	L, C, X band	VLA	[19]
A2382	Radio galaxies	L, C band	VLA	[25]
3C 31	Radio Galaxies	L, C, X band	VLA	[17]
3C 449	Radio galaxies	L, C, X band	VLA	[26]
A2199	Radio galaxies	L, C, X band	VLA	[27]
A1656 (center)	Radio galaxies	L, C, X band	VLA	[28]
A1656 (outskirts)	Radio Galaxies	L, C band	VLA	[29]
A194	Radio galaxies	L, C band	VLA, SRT	[30]
A2255	Radio galaxies and radio halo	C, X band	VLA	[31]
A665	Radio halo	L band	VLA	[13]
A523	Radio halo	L band	VLA	[32]

is given a summary of all the clusters for which a detailed study of the magnetic field has been done either with a numerical or an analytic approach. Column 1 reports the name of the cluster, Column 2 the observable(s) used to carry out the analysis, Column 3 the frequency band(s) of the observations, Column 4 the instrument(s) used for the observations (VLA = Very Large Array, SRT = Sardinia Radio Telescope), and Column 5: Reference of the corresponding work.

We studied the magnetic field strength and structure in a galaxy cluster suffering strong merger events, i.e., A665 [13], by exploiting the spatial fluctuations in total intensity and the upper limits in the polarized emission of the radio halo at its center. Radio halo emission is a simultaneous expression of magnetic fields and relativistic electrons. To discriminate among the two contributions from radio observations only is not possible. Approaches based on multiwavelength observations as, e.g., the combination of the synchrotron radio and inverse Compton X-ray emission from galaxy clusters could be applied (see e.g., [33]). However, difficulties may derive by the fact that the population of electrons responsible for the radio and X-ray emission must be the same and that to discern between the thermal and non-thermal X-ray emission of the source may be not trivial. We carried out our analysis with radio data only and for this reason we assumed an equipartition condition between the relativistic electrons and the magnetic field. To constraint the intracluster magnetic field, we compared the observations with synthetic radio halo images corresponding to different magnetic field strengths and structures. By varying the magnetic field outer scale of fluctuation from 102.4 kpc to 1024 kpc, we found that if the intracluster magnetic field fluctuates on spatial scales comparable with the resolution of the radio observation, the halo emission appears smooth and regular, while if it is ordered on spatial scales larger than the observing beam, the radio halo morphology is much more distorted and the offset of the radio halo peak from the cluster X-ray center is significant (Figure 1, right panel). A key tool to directly constrain the magnetic field properties is represented by the polarized emission of radio halos. The ratio of the total and polarized emission is indeed only marginally dependent on the relativistic electron energy spectrum and permits the placing of strong constraints on the magnetic field properties. Unfortunately, the polarized emission has been detected only in three radio halos to date as, e.g., A523 [32], where we could use this signal to investigate the magnetic field properties.

In galaxy clusters not showing diffuse synchrotron radio emission, we investigated the intracluster magnetic field power spectrum with the analysis of polarimetric properties of powerful and extended radio galaxies over a wide frequency range, as for example in A2199 [27] and A194 [30] where the Faraday effect is dominated by the intracluster contribution. By using radio observations respectively from 1.4 to 8 GHz and from 1.4 to 5 GHz, we derived rotation measure images for the radio galaxies in these clusters that appear patchy and reveal turbulent central intracluster magnetic fields, see Figure 2. We characterized these rotation measures images by means of their structure function

$$S_{\mathrm{RM}}\left(r_{\perp }\right)={\langle {[RM(x,y)-RM(x+\Delta x,y+\Delta y)]}^2\rangle }_{x,y}$$

(7)

obtained by averaging the difference in rotation measure values in pixels at the scale distance $r_{\perp }=\sqrt{\Delta x^2+\Delta y^2}$. To derive the power spectrum of the intracluster magnetic field, we produced synthetic images corresponding to different configurations of intracluster magnetic field and we compared the observed and synthetic rotation measure structure functions with advanced Bayesian algorithms of inference (Figure 3).

According to magneto-hydro-dynamical simulations, the dynamical state of the system plays an important role in the intracluster magnetic field evolution [34]. Young merging galaxy clusters are expected to be less magnetized than old relaxed systems since the amplification of the magnetic field strength requires long timescales. During the formation of galaxy clusters, significant amount of energy is released in the intracluster medium. The energy is injected on large spatial scales and then decades on smaller and smaller scales through turbulent cascades. This expectation is confirmed by present radio observations. Indeed, overall, we find magnetic fields characterized by central strengths of ∼$\mathsf{\mu }$G and fluctuation scales up to a few hundreds of kpc in merging systems, while in relaxed systems we derive magnetic field central strengths up to ∼10 $\mathsf{\mu }$G and fluctuation scales from a few tens of kpc down to a few kpc or less.

Present and next generation radio telescopes will supply sensitive and detailed observations both of diffuse synchrotron sources and of radio galaxies in total intensity and polarization, essential to derive stronger constraints on intracluster magnetic fields. Radio halos are steep spectrum sources brighter at frequencies ≲1 GHz. Their polarized signal is affected by Faraday rotation that is less important at higher frequencies. Overall, total intensity and polarized emission of radio halos can be therefore studied simultaneously at best at frequencies ∼1 GHz. Our numerical three-dimensional simulations [35] indicate that radio halos are intrinsically polarized with central fractional polarization at full resolution of 15–35% at 1.4 GHz and higher levels toward the cluster periphery. However, this polarization is hard to detect due to instrumental limitations of present radio telescopes. The sensitivity and resolution imposed by the Jansky Very Large Array (JVLA) and Meerkat and by the polarimetric surveys planned with APERTIF (Westerbork Observations of the Deep APERTIF Northern-Sky, [36]) and ASKAP (Polarization Sky Survey of the Universe’s Magnetism [37]) allow for the detection of polarized emission in high-luminosity ($L_{1.4\mathrm{GHz}}\gtrsim {10}^{25}$ W/Hz) radio halos, while for intermediate-luminosity ($L_{1.4\mathrm{GHz}}\approx {10}^{24}$ W/Hz) the advanced capabilities of the Square Kilometer Array (SKA) during Phase 1 are necessary. Instead, polarized emission from faint-luminosity ($L_{1.4\mathrm{GHz}}\lesssim {10}^{23}$ W/Hz) radio halos will be very hard to detect even with the SKA during Phase 2.

Moreover, the sensitivity and high-spatial and spectral resolution of the SKA during Phase 1 will permit the study of polarimetric properties for a large number of radio galaxies in the background of galaxy clusters. With the radio instruments presently available detailed rotation measure images can be typically produced only for one extended radio galaxy (either background or cluster) per cluster, the only exception being in A2255 (4 sources, [31]) and in the Coma cluster (7 sources, [28]), being the main limitations the sensitivity and resolution of the observations. With observations taken by SKA during Phase 1, detailed and extended rotation measure images will be produced for several sources between several tens and a few hundreds in nearby galaxy clusters ($z<0.1$) and at least for 1–2 radio galaxies for high redshift systems (up to $z=0.5$) [38], consequently enabling the trace of magnetic field strength and structure up to the cluster outskirts [39], a territory still largely unexplored.

5. Present Results and Perspectives Beyond Galaxy Clusters

With the aim of investigating the magnetization along the elusive regions connecting galaxy clusters, we recently observed an area of the sky of 8${}^{\circ }\times$ 8${}^{\circ }$ with the Sardinia Radio Telescope (SRT) at 1.4 GHz [40]. This field of view is very bright in radio (Figure 4) and is of particular interest because of the presence of several galaxy clusters among which nine are at a similar redshift ($z\approx 0.1$). Single-dish observations are very sensitive to faint surface brightness extended over large angular scale but are characterized by low-spatial resolution (in our case ∼13${}^{\prime }$). To discriminate between the presence of diffuse large-scale synchrotron emission and the radio emission from discrete sources, we combined these data with higher resolution observations from the NRAO VLA Sky Survey (NVSS, [41]). After the subtraction of point-like emission (not shown here, but see [40]), the combined image revealed a population of 28 new diffuse synchrotron radio sources whose properties differ from cluster sources, with X-ray luminosity and radio emissivity 10–100 lower. The comparison of these observations with magneto-hydro-dynamical simulations indicates that their properties are consistent with those expected for the brightest patches of the cosmic web and correspond to magnetic field strengths of ∼20–50 nG. Polarization analysis of these data is currently in progress and will be the subject of a future work.

Due to their weak strengths, the detection and study of magnetic fields along filaments and voids of the cosmic web is very challenging. Sensitive and high-spatial and spectral resolution polarization surveys of the sky are planned with the SKA, its pathfinders and precursors. These surveys will enable the study of polarimetric properties for several extra-galactic radio sources from a few thousands with low-frequency radio telescopes as the LOw-Frequency ARray (LOFAR, e.g., [42]) up to 7–14 million with the SKA during Phase 1 [38]. Typically, the linearly polarized signal from background radio sources is modified through the Faraday effect by different intervening media: our Galaxy, galaxy clusters, filaments, voids, sheets, the emitting source itself and any other source along the line of sight. Therefore, the upcoming data contain an enormous quantity of information, among which is the tiny signature of intergalactic magnetic field. This signal is very weak (≈1 rad/m${}^2$) and is easily buried by the Galactic rotation measure (up to several hundreds of rad/m${}^2$) and by the observing noise (up to ≈10–15 rad/m${}^2$, for the largest rotation measure catalog presently available [43]). To detect and investigate the magnetization of the cosmic web based on these data, it is crucial to develop statistical advanced tools of analysis capable of disentangling all the contributions to the Faraday rotation, properly taking into account the observing noise. We developed a sophisticate Bayesian tool to separate the Galactic contribution from the Faraday effect associated with extra-galactic environments and derived that the extra-galactic Faraday rotation is well described by a Gaussian distribution with zero-mean and standard deviation ${\sigma }_{\mathrm{e}}\approx 7$ rad/m${}^2$ [44]. As a further step, we built upon it an advanced Bayesian algorithm based on Gibbs sampling, to disentangle the contributions from different extra-galactic environments. As we described in [45], the overall extra-galactic Faraday rotation variance can be expressed as the sum of the intrinsic ${\sigma }_{\mathrm{int}}^2$ and environmental ${\sigma }_{\mathrm{env}}^2$ Faraday rotation

$${\sigma }_{\mathrm{e}}^2={\sigma }_{\mathrm{int}}^2+{\sigma }_{\mathrm{env}}^2={\left(\frac{L}{L_0}\right)}^{{\chi }_{\mathrm{lum}}}\frac{{\sigma }_{\mathrm{int},0}^2}{{(1+z)}^4}+\frac{D(z,{\chi }_{\mathrm{red}})}{D_0}{\sigma }_{\mathrm{env},0}^2$$

(8)

where ${\sigma }_{\mathrm{int},0}^2$ is the pure variance in Faraday rotation intrinsic to the emitting radio source, L is the total luminosity of the source, $L_0={10}^{27}$ W/Hz, ${\chi }_{\mathrm{lum}}$ absorbs possible dependencies on the luminosity of the source, ${\sigma }_{\mathrm{env},0}^2$ is the variance in the pure environmental Faraday rotation, $D_0$ = 1 Gpc, and $D(z,{\chi }_{\mathrm{red}})$ is defined as

$$D(z,{\chi }_{\mathrm{red}})={\int }_0^z\frac{c}{H\left(z\right)}{(1+z)}^{4+{\chi }_{\mathrm{red}}}dz$$

(9)

to capture the redshift dependence. Our studies indicate that low-frequency (≈150 MHz) data can provide useful constraints on the presence of ≲$\mathsf{\mu }$G magnetic fields in the cosmic web already with rotation measures for a few thousands of sources thanks to the small observational uncertainty (∼0.05–0.1 rad/m${}^2$), see Figure 5. However, difficulties in calibration of low-frequency observations (e.g., due to the ionosphere and to the wide fields of view) as well as limited number density of polarized sources due to the depolarization of the signal, makes the use of higher frequency observations (≈1.4 GHz) easier. The larger uncertainties in rotation measures (≈1–10 rad/m${}^2$) at these frequencies require the use of wider catalogs of sources [46].

The overall environmental extra-galactic Faraday rotation is the result of several magneto-ionic media along the line of sight as, e.g., galaxy clusters, filaments, voids, sheets,

$${\sigma }_{\mathrm{env}}^2=\sum _{j=1}^{N_{\mathrm{env}}}{l}_j{\sigma }_j^2$$

(10)

where ${\sigma }_1$, ${\sigma }_2$, …, ${\sigma }_{{\mathrm{N}}_{\mathrm{env}}}$ is the standard deviation of the Faraday rotation from each of the $N_{\mathrm{env}}$ different environments and $l_j$ is the length of the path covered by the signal through each environment j. Detailed knowledge of the redshift of the emitting sources and of the large-scale structure of the Universe ($l_j$, e.g., [47]) is therefore essential to further disentangle the contribution to Faraday rotation from the environments of the large-scale structure of the Universe.

6. Conclusions

The detection and investigation of magnetic fields in the large-scale structure of the Universe, from galaxy clusters to filaments and voids, have the potential to put strong constraints on cosmic magnetism genesis and evolution. To date, detailed investigation of magnetic fields in galaxy clusters have been possible only in a few systems. These studies suggest magnetic field properties strongly related to the dynamical and thermal state of the cluster. Magnetic fields at the center of merging galaxy cluster show ≈$\mathsf{\mu }$G strengths and are ordered up to scales of ≈500 kpc, while in relaxed systems we measure magnetic fields with ∼10 $\mathsf{\mu }$G central strengths and turbulence down to scales of a few kpc or less. The comparison of thermal and non-thermal properties in galaxy clusters for which a detailed study is available suggests that at the center of the cluster the magnetic field energy is deeply related to the thermal gas density. Thanks to instruments with high-sensitivity to surface brightness and capable of sampling large angular scales in the sky, we are now starting to observe the magnetization also beyond galaxy clusters, along the brightest patches of the cosmic web, where we observe large-scale diffuse synchrotron sources with radio emissivity 10–100 lower than in clusters, corresponding to magnetic fields strengths ∼20–50 nG.

The coexistence of large and small scales of turbulence can be well studied by combining total and polarized brightness fluctuations of diffuse synchrotron sources and polarimetric data of background radio galaxies. The advent of sensitive high-spatial and spectral resolution observations will enable to exploit the information from radio halo polarized emission in a larger number of systems and to produce extended and high-quality rotation measure images for several sources both at the center and in the periphery of close-by galaxy clusters. To investigate the properties of the magnetic field in a detailed way from the center of galaxy clusters to their periphery and beyond galaxy clusters, along filaments and voids of the cosmic web, where our knowledge of the non-thermal component is still limited, it is crucial to combine these data with advanced tools of analysis.