Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2007f1a.ps}\par\vspace*{3mm}... ...b.ps}\par\vspace*{3mm} \includegraphics[width=8cm,clip]{2007f1c.ps} \end{figure}$ Figure 1: Images of the radio source J1343+3758 at a) 327 and b), c) 1400 MHz from the WENSS and NVSS surveys, respectively. a) The contours, spaced by factors of $\sqrt {2}$ in brightness, are plotted starting with 9 mJy beam^-1. b) Total intensity contours, spaced by a factor of 2, are plotted starting with 1 mJy beam^-1. Superimposed are electric field E-vectors with their lengths proportional to the polarised intensity. c) Linearly polarised intensity contours of 0.8, 1.6, 3.2 mJy beam^-1 with the vectors of the fractional linear polarisation superimposed. The scales of the polarisation vectors are indicated by the bars, and the beam size by the ellipse in a) and circles in b), c) in the bottom left corners of the images; "x'' marks the position of the parent galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{2007f2.ps} \end{figure}$ Figure 2: VLA D-array map of J1343+3758 at 4860 MHz convolved to the angular resolution of $20\hbox {$^{\prime \prime }$ }\times 20\hbox {$^{\prime \prime }$ }$ and overlaid on the optical field from the Digital Sky Survey. The contour levels are spaced by factors of $\sqrt {2}$ ; the first contour is 40 $\mu$ Jy beam^-1. The compact 1.16 mJy radio core coincides with the parent galaxy position.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2007f3a.ps}\par\vspace*{3mm} \includegraphics[width=8.3cm,clip]{2007f3b.ps} \end{figure}$ Figure 3: The Effelsberg images of the source J1343+3758 at 8350 MHz. a) Total intensity contours spaced by a factor of $\sqrt {2}$ starting with 1.35 mJy beam^-1. Superimposed are E-vectors with their lengths proportional to the polarised intensity. b) Linearly polarised intensity contours spaced by a factor of $\sqrt {2}$ starting with 0.28 mJy beam^-1 with the vectors of the fractional linear polarisation superimposed. Otherwise the layout is the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2007f4a.ps}\par\vspace*{3mm} \includegraphics[width=8.5cm,clip]{2007f4b.ps} \end{figure}$ Figure 4: a) The map of the spectral index $\alpha ^{327}_{4860}$ across the radio galaxy; b) this index in 30 $\hbox {$^{\prime \prime }$ }$ wide strips perpendicular to the source axis vs. strip distance from the core.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{2007f5.ps} \end{figure}$ Figure 5: a)-c) Spectra observed in different strips across the NE lobe of J1343+3758 fitted with the JP model for $\alpha _{\rm inj}=0.57$ . d)-f) The same for the SW lobe. The values of the resultant $\nu _{\rm b}$ and $\chi ^{2}_{\rm red}$ are shown in the top-right corner of each panel, and the distance of each strip from the radio core is given its bottom-left corner.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2007f6.ps} \end{figure}$ Figure 6: Radiative age of relativistic particles in the lobes of J1343+3758 vs. distance from the radio core. Open circles: age corresponding to the equipartition magnetic field strengths; the filled circles: the age determined for the enhanced fields (cf. the text). The solid and dashed lines show the weighted least-squares fits to these ages. The extrapolations of the fits towards the core suggest maximum spectral ages of particles in both lobes.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2007f7.ps} \end{figure}$ Figure 7: a) Model energy density ( $u_{\rm c}$ ) in the NE and SW lobes of J1343+3758 vs. the ambient density at their peripheries ( $\rho _{\rm a}$ ) for different ages of the lobes with present values of their observational parameters (cf. the text); b) model jet power ( $Q_{\rm jet}$ ) vs. the central core density ( $\rho _{0}$ ) for the NE and SW lobes at different ages.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2007f4a.ps}\par\vspace*{3mm} \includegraphics[width=8.5cm,clip]{2007f4b.ps} \end{figure}$	Figure 4: a) The map of the spectral index $\alpha ^{327}_{4860}$ across the radio galaxy; b) this index in 30 $\hbox {$^{\prime \prime }$ }$ wide strips perpendicular to the source axis vs. strip distance from the core.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{2007f5.ps} \end{figure}$	Figure 5: a)-c) Spectra observed in different strips across the NE lobe of J1343+3758 fitted with the JP model for $\alpha _{\rm inj}=0.57$ . d)-f) The same for the SW lobe. The values of the resultant $\nu _{\rm b}$ and $\chi ^{2}_{\rm red}$ are shown in the top-right corner of each panel, and the distance of each strip from the radio core is given its bottom-left corner.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{2007f7.ps} \end{figure}$	Figure 7: a) Model energy density ( $u_{\rm c}$ ) in the NE and SW lobes of J1343+3758 vs. the ambient density at their peripheries ( $\rho _{\rm a}$ ) for different ages of the lobes with present values of their observational parameters (cf. the text); b) model jet power ( $Q_{\rm jet}$ ) vs. the central core density ( $\rho _{0}$ ) for the NE and SW lobes at different ages.
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