All Figures

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig1.eps}\end{figure}$ Figure 1: VLA 1.49 GHz radio continuum image overlaid on our H ${\alpha }$ image of NGC 4700. Contours represent flux density levels -0.2, -0.14, 0.14 (2.5- $\sigma$ ), 0.2, 0.28, ..., 1.6 mJy beam^-1, spaced by factors of $\sqrt {2}$ , while the logarithmic H ${\alpha }$ grey scales range from 0 to the maximum observed surface brightness. The resolution (full width at half maximum) of the radio image is 13'' (1.6 kpc).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig2.eps}\end{figure}$ Figure 2: Placement of a 12''-wide cut through the H ${\alpha }$ emission distribution of NGC 4666 along the disk plane, indicating the area over which the cut displayed in Fig. 3 was determined. See Table 2 for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig3.eps}\end{figure}$ Figure 3: 12'' wide cut through our H ${\alpha }$ image (dotted line) and through the 1.49 GHz emission distribution of NGC 4666 (solid line) along the disk plane (cf. Fig. 2), demonstrating the measurements of $r_{\rm SF}$ and $r_{\rm CR}$ . Arrows mark the positions at which radii were measured; upwards arrows at the $r_{\rm CR}$ measurements (at the intersection of the solid line with the dotted 5- $\sigma$ threshold value), downwards arrows at the $r_{\rm SF}$ points (at the intersection of the dotted data graph with the dashed horizontal threshold line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig4.eps}\end{figure}$ Figure 4: Overlay of rectangular boxes with widths of 12'' for the measurements of $r_{\rm CR}$ and $r_{\rm halo}$ in NGC 4666 on our 1.49 GHz radio continuum image. The central cut is the same as in Fig. 2, the properties of the two parallel cuts through the halo are listed in Table 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig5.eps}\end{figure}$ Figure 5: Cuts through the 1.49 GHz emission distribution of NGC 4666 through the radio halo, parallel to the disk plane, at z-offsets of $\pm 32''$ (see Table 2). The cut through the halo north-west of the plane is shown as a dashed line, the south-eastern cut is represented by a solid line. For comparison the cut through the H ${\alpha }$ image along the disk plane is shown again as a dotted line. Arrows mark the positions at which radii were measured; upwards arrows at the $r_{\rm halo}$ measurements, downwards arrows at the $r_{\rm SF}$ points (same as in Fig. 3).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fg6a.ps}\hspace*{3mm} \includegraphics[width=9cm,clip]{4787fg6b.ps}\end{figure}$ Figure 6: Left: radial extent of the star-forming part of the galaxy disks, $r_{\rm SF}$ , against the radial extent of the associated halos, $r_{\rm halo}$ ; see Sect. 4.1 for details. Right: radial extent of the optical disk, r₂₅, against $r_{\rm halo}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4787fg7a.ps}\includegraphics[width=9cm,clip]{4787fg7b.ps}\end{figure}$ Figure 7: Left: energy input per unit star-forming area, $A_{\rm SF}$ , as a function of stellar mass surface density, as derived from K-band imagery. Filled symbols indicate galaxies with radio halos, open symbols are galaxies without radio halo detections. The dashed line roughly indicates the transition zone between galaxies with and without radio halos. Right: the same as on the left, but using A₂₅ instead of $A_{\rm SF}$ as an approximation of the area over which energy is deposited into the disk ISM.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fg8a.ps}\includegraphics[width=8.8cm,clip]{4787fg8b.ps}\end{figure}$ Figure 8: Left: $A_{\rm SF}/A_{25}$ plotted against the far-infrared luminosity, $L_{\rm FIR}$ . Right: $A_{\rm SF}/A_{25}$ now plotted against the far-infrared vs. optical blue luminosity ratio, $L_{\rm FIR}$ /L_B. NGC 1808 is not shown, because the contributions of its AGN and starburst to the FIR flux densities could not be separated.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fg9a.ps}\hspace*{4mm} \includegraphics[width=8.7cm,clip]{4787fg9b.ps}\end{figure}$ Figure 9: Left: $A_{\rm SF}/A_{25}$ plotted vs. the IRAS 60 $\mu$ m to 100 $\mu$ m flux ratio, which is a measure of the average warm dust temperature. Right: energy input rates per unit surface area, $\dot E^{\rm tot}_{\rm A}$ , plotted vs. f₆₀/f₁₀₀. NGC 1808 is not shown, because the contributions of its AGN and starburst to the FIR flux densities could not be separated.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig2.eps}\end{figure}$	Figure 2: Placement of a 12''-wide cut through the H ${\alpha }$ emission distribution of NGC 4666 along the disk plane, indicating the area over which the cut displayed in Fig. 3 was determined. See Table 2 for details.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fig4.eps}\end{figure}$	Figure 4: Overlay of rectangular boxes with widths of 12'' for the measurements of $r_{\rm CR}$ and $r_{\rm halo}$ in NGC 4666 on our 1.49 GHz radio continuum image. The central cut is the same as in Fig. 2, the properties of the two parallel cuts through the halo are listed in Table 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fg6a.ps}\hspace*{3mm} \includegraphics[width=9cm,clip]{4787fg6b.ps}\end{figure}$	Figure 6: Left: radial extent of the star-forming part of the galaxy disks, $r_{\rm SF}$ , against the radial extent of the associated halos, $r_{\rm halo}$ ; see Sect. 4.1 for details. Right: radial extent of the optical disk, r₂₅, against $r_{\rm halo}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fg8a.ps}\includegraphics[width=8.8cm,clip]{4787fg8b.ps}\end{figure}$	Figure 8: Left: $A_{\rm SF}/A_{25}$ plotted against the far-infrared luminosity, $L_{\rm FIR}$ . Right: $A_{\rm SF}/A_{25}$ now plotted against the far-infrared vs. optical blue luminosity ratio, $L_{\rm FIR}$ /L_B. NGC 1808 is not shown, because the contributions of its AGN and starburst to the FIR flux densities could not be separated.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{4787fg9a.ps}\hspace*{4mm} \includegraphics[width=8.7cm,clip]{4787fg9b.ps}\end{figure}$	Figure 9: Left: $A_{\rm SF}/A_{25}$ plotted vs. the IRAS 60 $\mu$ m to 100 $\mu$ m flux ratio, which is a measure of the average warm dust temperature. Right: energy input rates per unit surface area, $\dot E^{\rm tot}_{\rm A}$ , plotted vs. f₆₀/f₁₀₀. NGC 1808 is not shown, because the contributions of its AGN and starburst to the FIR flux densities could not be separated.
Open with DEXTER