Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1620fig1.ps} \end{figure}$ Figure 1: Distribution of measured redshifts for the sample by Dallacasa et al. (2000).
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{1620spc1.epsi} \end{figure}$ Figure 2: Radio spectra of sources [ $S_\nu$ (Jy) vs. $\nu$ (GHz)]. Stars and filled circles represent the first and the second epoch of simultaneous multifrequency VLA data respectively; the dashed and solid lines show the corresponding polynomial fits.
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In the text

$\begin{figure}\par\includegraphics[width=17.5cm,clip]{1620spc2.epsi} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17.5cm,clip]{1620spc3.epsi} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{1620fig3.ps} \end{figure}$ Figure 3: Histogram of observed turnover frequencies for the HFPsample at the two epochs.
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In the text

$\begin{figure} \par\includegraphics[height=6.15cm,width=6.2cm,clip]{1620f4_1.ps}... ...1cm} \includegraphics[height=6.05cm,width=5.8cm,clip]{1620f4_2.ps} \end{figure}$ Figure 4: Observed ( left) and rest frame ( right) turnover frequency distributions for galaxies and quasars.
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In the text

$\begin{figure} \par\includegraphics[height=5.6cm,width=5.9cm,clip]{1620f5_1.ps}\... ....2cm} \includegraphics[height=5.7cm,width=5.9cm,clip]{1620f5_2.ps} \end{figure}$ Figure 5: Differential ( left) and cumulative ( right) distribution of V, compared with the corresponding $\chi ^2$ distributions for 2 degrees of freedom (dashed lines). The bins of the differential distribution correspond to $\Delta \chi ^2 =1$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1620fig6.ps} \end{figure}$ Figure 6: Peak luminosity versus peak frequency for all objects with measured redshift. Circles: quasars, squares: galaxies. Open symbols refer to sources with $V\le 9$ , filled symbols to sources with V>9. The solid line shows the distribution in the $L_{\rm p}$ - $\nu _{\rm p}$ plane of sources with equal observed $S_{\rm p}=300$ mJy and $\nu _{\rm p}=5$ GHz at different redshifts.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f1.epsi} \end{figure}$ Figure A.1: J0111+3906; the restoring beam is in the Bottom Left Corner of each figure, the conturn levels are $\pm$ 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024, 2048, 4096 times the first conturn (f.c.) corresponding to 3 times the rms noise of the image.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f2.epsi} \end{figure}$ Figure A.2: J0217+0144.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f3.epsi} \end{figure}$ Figure A.3: J0329+3510.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f4.epsi} \end{figure}$ Figure A.4: J0428+3259.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f5.epsi} \end{figure}$ Figure A.5: J0519+0848.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f6.epsi} \end{figure}$ Figure A.6: J1457+0749.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f7.epsi} \end{figure}$ Figure A.7: J1603+1105.

In the text

$\begin{figure} \par\includegraphics[width=15.85cm,clip]{1620A_f8.epsi} \end{figure}$ Figure A.8: J1800+3848 ( left) at 1.465 GHz and J1811+1704 ( right) at 1.665 GHz.

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1620A_f9.epsi} \end{figure}$ Figure A.9: J2024+1718 ( left) at 1.465 GHz and J2101+0341 ( right) at 1.465 GHz.

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{1620Af10.epsi} \end{figure}$ Figure A.10: J2123+0535.

In the text

$\begin{figure} \par\includegraphics[width=15.35cm,clip]{1620Af11.epsi} \end{figure}$ Figure A.11: J2207+1652.

In the text

$\begin{figure} \par\includegraphics[width=15.3cm,clip]{1620Af12.epsi} \end{figure}$ Figure A.12: J2320+0513.

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1620fig1.ps} \end{figure}$	Figure 1: Distribution of measured redshifts for the sample by Dallacasa et al. (2000).
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{1620spc1.epsi} \end{figure}$	Figure 2: Radio spectra of sources [ $S_\nu$ (Jy) vs. $\nu$ (GHz)]. Stars and filled circles represent the first and the second epoch of simultaneous multifrequency VLA data respectively; the dashed and solid lines show the corresponding polynomial fits.
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$\begin{figure}\par\includegraphics[width=17.5cm,clip]{1620spc2.epsi} \end{figure}$	Figure 2: continued.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{1620fig3.ps} \end{figure}$	Figure 3: Histogram of observed turnover frequencies for the HFPsample at the two epochs.
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$\begin{figure} \par\includegraphics[height=6.15cm,width=6.2cm,clip]{1620f4_1.ps}... ...1cm} \includegraphics[height=6.05cm,width=5.8cm,clip]{1620f4_2.ps} \end{figure}$	Figure 4: Observed ( left) and rest frame ( right) turnover frequency distributions for galaxies and quasars.
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$\begin{figure} \par\includegraphics[height=5.6cm,width=5.9cm,clip]{1620f5_1.ps}\... ....2cm} \includegraphics[height=5.7cm,width=5.9cm,clip]{1620f5_2.ps} \end{figure}$	Figure 5: Differential ( left) and cumulative ( right) distribution of V, compared with the corresponding $\chi ^2$ distributions for 2 degrees of freedom (dashed lines). The bins of the differential distribution correspond to $\Delta \chi ^2 =1$ .
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1620fig6.ps} \end{figure}$	Figure 6: Peak luminosity versus peak frequency for all objects with measured redshift. Circles: quasars, squares: galaxies. Open symbols refer to sources with $V\le 9$ , filled symbols to sources with V>9. The solid line shows the distribution in the $L_{\rm p}$ - $\nu _{\rm p}$ plane of sources with equal observed $S_{\rm p}=300$ mJy and $\nu _{\rm p}=5$ GHz at different redshifts.
Open with DEXTER