All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8688f1.ps}\end{figure}$ Figure 1: Optical DSS B image of NGC 4254 and polarized intensity at 4.86 GHz in $15\hbox {$^{\prime \prime }$ }$ resolution in contours. The contours are at $9.7\times (4, 9, 16, 25, 40)~\mu$ G. Three main optical spiral arms (SW, N and NE) are schematically marked. Letters a-e denote positions of contrast derivations in Sect. 3.5.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8688f2a.ps}\hspace*{3mm} \includegraphics[width=9cm,clip]{8688f2b.ps}\end{figure}$ Figure 2: a) Faraday rotation measure distribution in NGC 4254 in $15\hbox {$^{\prime \prime }$ }$ resolution in colors, computed between 8.46 GHz and 4.86 GHz with contours of total radio intensity at 4.86 GHz. The galaxy major axis is marked. b) Faraday depolarization distribution in colors and contours of soft X-ray emission from our XMM-Newton observations.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8688f3.ps} \end{figure}$ Figure 3: Distribution of rotation measures between 8.46 and 4.86 GHz along the azimuthal angle in 5 different rings of NGC 4254. The rings of 1.2 kpc width start from $30\hbox {$^{\prime \prime }$ }$ (2.4 kpc) distance from the galaxy center (ring 1, the most upper one). The last ring (bottom) ends at distance of 8.5 kpc. The best-fitted dynamo modes are also shown: for the ring 3 the bisymmetric m=1 mode (dashed) and superposition of axisymmetric and bisymmetric m=0/1 modes (dotted); and for ring 4 the axisymmetric m=0 mode (dashed), see Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8688f4.ps}\end{figure}$ Figure 4: Actual (Faraday-free) structure of magnetic field vectors in NGC 4254 obtained from the combined VLA and single-dish (Effelsberg) polarized data at 8.46 GHz and 4.86 GHz. The lengths of vectors are proportional to the degree of polarization at 4.86 GHz. The regions with inner and outer magnetic arms are designated. Overlaid (in colors) is the H $\alpha$ image (from Knapen et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8688f5.ps}\end{figure}$ Figure 5: Magnetic maps for NGC 4254 with a resolution of $15\hbox {$^{\prime \prime }$ }$ (in colors): total a), regular b), random c) magnetic field strength, and field regularity d) with contours of H I, H $\alpha$ , infrared (24 $\mu$ m), and UV emission, respectively. The method of the maps construction is given in Sect. 2.3.
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In the text

$\begin{figure} \par\includegraphics[width=18.4cm,clip]{8688f6.ps}\end{figure}$ Figure 6: A phase diagram of the regular component of magnetic fields in dependence of natural logarithm of distance and galactocentric azimuthal angle, as measured from the northern tip of the major axis counterclockwise. The vectors are proportional to the polarized intensity at 4.86 GHz, which is also presented in contours. In the frame of this representation, a logarithmic spiral arm would be a straight line inclined by the pitch angle. The galactic spiral structure is shown by the distribution of UV emission (in color) with additionally marked (the straight lines) approximate orientations of the main three optical spiral arms. All the presented values were averaged in sectors of $7\hbox {$^\circ $ }$ width in the azimuth.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8688f7a.ps}\hspace*{3.5mm} \... ...8f7c.ps}\hspace*{3.5mm} \includegraphics[width=9cm,clip]{8688f7d.ps}\end{figure}$ Figure 7: Total magnetic field strength a), field regularity b), random c), and regular d) magnetic field strengths versus IR-based SFR within NGC 4254. From among all regions (marked by diamond sign) magnetic arms are denoted separately: southern outer magnetic arm by crosses; western outer magnetic arm by rectangles; and northern inner magnetic arm by triangles. The lines fitted by bisector method to all regions are drawn (except d-panel, see Sect. 3.2).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8688f1.ps}\end{figure}$	Figure 1: Optical DSS B image of NGC 4254 and polarized intensity at 4.86 GHz in $15\hbox {$^{\prime \prime }$ }$ resolution in contours. The contours are at $9.7\times (4, 9, 16, 25, 40)~\mu$ G. Three main optical spiral arms (SW, N and NE) are schematically marked. Letters a-e denote positions of contrast derivations in Sect. 3.5.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{8688f2a.ps}\hspace*{3mm} \includegraphics[width=9cm,clip]{8688f2b.ps}\end{figure}$	Figure 2: a) Faraday rotation measure distribution in NGC 4254 in $15\hbox {$^{\prime \prime }$ }$ resolution in colors, computed between 8.46 GHz and 4.86 GHz with contours of total radio intensity at 4.86 GHz. The galaxy major axis is marked. b) Faraday depolarization distribution in colors and contours of soft X-ray emission from our XMM-Newton observations.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{8688f5.ps}\end{figure}$	Figure 5: Magnetic maps for NGC 4254 with a resolution of $15\hbox {$^{\prime \prime }$ }$ (in colors): total a), regular b), random c) magnetic field strength, and field regularity d) with contours of H I, H $\alpha$ , infrared (24 $\mu$ m), and UV emission, respectively. The method of the maps construction is given in Sect. 2.3.
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