All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{7224f1.eps}\end{figure}$ Figure 1: 22.5 GHz images of the newly observed ULIRGs in our sample. Contour levels begin at $\pm$ $0.5~\rm mJy~beam^{-1}$ and are spaced by a factor of 2^1/2. The synthesised beam is shown in the bottom left of each panel.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[scale=0.26]{7224f2a.ps}\hskip-8mm \inc... ...6]{7224f2g.ps}\hskip-8mm \includegraphics[scale=0.26]{7224f2h.ps} } \end{figure}$ Figure 2: Contour maps for the new 8.4 GHz observations. The synthesised beam is shown in the bottom left of each panel. NGC 6285 is the companion of NGC 6286 and its radio map is included only for completeness.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{7224f6.ps}\end{figure}$ Figure 6: The relation between the near-infrared colour J-K and the radio spectral index between 1.4 and 4.8 GHz ( top) and 8.4 and 22.5 GHz ( bottom). Objects at the extremes of the distributions are labelled.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{7224f7.ps}\end{figure}$ Figure 7: Top: correlation between the radio spectral index between 1.4 and 4.8 GHz and IRAS 60/100 micron flux ratio. Bottom: same plot for the 8.4-22.5 GHz spectral index. Objects at the extremes of the distributions are labelled. Note that that UGC 8058 may have a radio loud AGN.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[scale=0.38]{maps/NGC34_C.ps}\includegr... ....ps}\includegraphics[scale=0.38]{maps/NGC7469_X.ps}\hspace*{2.5cm}} \end{figure}$ Figure 3: Contour maps for the archival VLA data. In brackets after the name of the source is the name of the radio frequency band; L (1.4 GHz), C (4.8 GHz), X (8.4 GHz), U (15 GHz), K (22.5 GHz). Contour levels are 2^-n x_i/2 where x = 0, 1, 2, ...The dotted contour has the same absolute value as the first contour but is negative. The value of n for each contour map is included in Table 3. The synthesised beam is shown at the bottom left of each panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{7224f4.ps}\end{figure}$ Figure 4: The radio spectra of the sample galaxies from 100 MHz to 100 GHz. The lower left panel shows the mean spectrum of all the sources scaled so that the 1.4 GHz flux is $0.1~\rm Jy$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.2cm,clip]{7224f5.ps}\end{figure}$ Figure 5: Relationship between radio spectral index at various frequencies and the logarithmic FIR-radio flux density ratio q, defined as $q = \log(FIR/3.75\times 10^{12}~{\rm Hz})/S$ , where S is the radio flux in units of $\rm W~m^{-2}~Hz^{-1}$ . The top panels show the radio spectral index as a function of q measured at $1.4~\rm GHz$ and the bottom panels show the radio spectral indices as a function of q measured at $8.4~\rm GHz$ . The left-most panels show the radio spectral index over the whole range from 1.4 to $22.5~\rm GHz$ while the remainder show the spectral indices over a more restricted range.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{7224f1.eps}\end{figure}$	Figure 1: 22.5 GHz images of the newly observed ULIRGs in our sample. Contour levels begin at $\pm$ $0.5~\rm mJy~beam^{-1}$ and are spaced by a factor of 2^1/2. The synthesised beam is shown in the bottom left of each panel.
Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[scale=0.26]{7224f2a.ps}\hskip-8mm \inc... ...6]{7224f2g.ps}\hskip-8mm \includegraphics[scale=0.26]{7224f2h.ps} } \end{figure}$	Figure 2: Contour maps for the new 8.4 GHz observations. The synthesised beam is shown in the bottom left of each panel. NGC 6285 is the companion of NGC 6286 and its radio map is included only for completeness.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{7224f6.ps}\end{figure}$	Figure 6: The relation between the near-infrared colour J-K and the radio spectral index between 1.4 and 4.8 GHz ( top) and 8.4 and 22.5 GHz ( bottom). Objects at the extremes of the distributions are labelled.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{7224f7.ps}\end{figure}$	Figure 7: Top: correlation between the radio spectral index between 1.4 and 4.8 GHz and IRAS 60/100 micron flux ratio. Bottom: same plot for the 8.4-22.5 GHz spectral index. Objects at the extremes of the distributions are labelled. Note that that UGC 8058 may have a radio loud AGN.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17cm,clip]{7224f4.ps}\end{figure}$	Figure 4: The radio spectra of the sample galaxies from 100 MHz to 100 GHz. The lower left panel shows the mean spectrum of all the sources scaled so that the 1.4 GHz flux is $0.1~\rm Jy$ .
Open with DEXTER