Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[height=11.1cm,width=8.8cm,clip]{0908fig1.eps} \end{figure}$ Figure 1: Top: histogram of the distribution of the 178 MHz radio fluxes in the 3CR catalogue. The filled part represents the objects detected by ISOCAM. Bottom: radio fluxes of 3CR sources at 178 MHz plotted as a function of redshift. The filled squares are objects of this paper.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0908fig2.eps} \end{figure}$ Figure 2: Detection rate of 3CR sources in our survey as a function of redshift. The filled part part of the columns refers to 3CR sources detected with ISOCAM where the MIR emission can be attributed to dust (see Sect. 4). The shaded part represents all ISOCAM detections of the 3CR catalogue and the upper (blank) histogram shows the redshift distribution of 3CR sources sampled by ISOCAM.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{0908fig3a.ps} \end{figure}$ Figure 3: Observed spectral energy distributions of the sources of the ISOCAM survey: ISOCAM photometry (filled squares), NED data (triangles), submillimeter data (pentagons), radio core fluxes (asterisks). Error bars are 1 $\sigma$ and upper limits 3 $\sigma$ rms. Solid lines represent the addition of the photospheric component (dashed lines) and the dust emission resulting from the AGN models.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{0908fig3b.ps}\end{figure}$ Figure 3: continued.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{0908fig3c.ps}\end{figure}$ Figure 3: continued.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{0908fig3d.ps}\end{figure}$ Figure 3: continued.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{0908fig4.ps} \end{figure}$ Figure 4: The influence of the dust population on the infrared spectrum of the AGN. Model parameters are: visual extinction $A_{\rm {V}} = 8$ mag, radius R = 1 kpc, luminosity L = 10^12.5 $L_\odot$ at distance of 50 Mpc. Model with large grains only (dashed), with large grains and small graphites (dotted), full model with large grains, small graphites and PAH (solid line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0908fig5.ps} \end{figure}$ Figure 5: Comparison of radiative transfer computations of dusty starbursts (solid) and AGNs (dashed). In both models we applied a visual extinction of $A_{\rm {V}} = 32$ mag, luminosity of L = 10¹² $L_\odot$ at distance of 50 Mpc, and radius of R = 1 kpc.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0908fig6.ps} \end{figure}$ Figure 6: AGN model spectra are shown for visual extinctions of $A_{\rm {V}} = 1$ , 2, 4, 8, 16, 32 and 64 mag and luminosities of L = 10^10.5, 10^11.5 and 10^12.5 $L_\odot$ at a distance of 50 Mpc. The radius is fixed at R = 1 kpc.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.7cm,width=8.4cm,angle=90,clip]{0908fig7.ps} \end{figure}$ Figure 7: The influence of the radius on the AGN model spectra. We apply a distance of 50 Mpc. Top: for luminosity of L = 10¹² $L_\odot$ and extinction of $A_{\rm {V}} = 32$ mag we present models with R = 0.125, 0.25, 0.5, 1, 2, 4, 8 and 16 kpc. Bottom: for luminosity of L = 10¹¹ $L_\odot$ and extinction of $A_{\rm {V}} = 8$ mag we show models with R = 0.125 and 16 kpc.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=13.5cm,width=7.7cm,clip]{0908fig8.ps} \end{figure}$ Figure 8: Top: the intrinsic AGN luminosity of the model, $L_{\rm dust}$ , as function of redshift. Solid symbols are type 1 AGNs: triangles QSOs and squares BLRGs. Open squares are NLRGs and upper limits as of Table 4. Asteriks are unclassified radio galaxies. Bottom: luminosity ratio of AGN and stellar components as a function of redshift. Symbols as in top panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0908fig9.ps} \end{figure}$ Figure 9: The best fit model parameters, radius and dust extinction, for 27 galaxies with well determined SEDs. The objects are grouped according to their luminosity (high or low) and spectral type (1 or 2). There are QSOs (type 1, high L, filled triangles), BLRGs (type 1, low L, filled squares), NLRGs (type 2, high L, open triangles) and NLRGs (type 2, low L, open squares). For each type, logarithmic means are marked by crosses.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{aa0908f10a.eps} \end{figure}$ Figure B.1: ISOCAM contours overlayed on DSS grey scale images centered on NED position of the object marked in bold. For each object we specify the ISOCAM filter and contour levels in $\mu$ mJy/arcsec². Negative contours at -3 $\sigma$ , - $\sigma$ are shown dashed. 3C 006.1 at 12.0 $\mu$ m (LW10): $\pm$ 4.4, $\pm$ 8.7, 15.7, 102.5, 153.8. 3C 017 at 12.0 $\mu$ m (LW10): $\pm$ 22.2, $\pm$ 44.3, 79.7, 521.9, 782.8. 3C 018 at 12.0 $\mu$ m (LW10): $\pm$ 50.9, $\pm$ 101.7, 152.6, 183.1, 204.0. 3C 020 at 12.0 $\mu$ m (LW10) $\pm$ 25.1, $\pm$ 50.2, 90.4, 108.8, 163.2. 3C 022 at 12.0 $\mu$ m (LW10): $\pm$ 41.4, $\pm$ 82.8, 124.2, 149.0, 161.1. 3C 031 at 12.0 $\mu$ m (LW10): $\pm$ 65.6, $\pm$ 131.3, 196.9, 236.3, 260.1. 3C 033.1 at 12.0 $\mu$ m (LW10): $\pm$ 77.1, $\pm$ 96.4, 154.2, 231.3, 277.6. 3C 048 at 14.3 $\mu$ m (LW3): $\pm$ 342.5, $\pm$ 228.4, 342.5, 749.9, 1124.9, 1349.9. 3C 061.1 at 12.0 $\mu$ m (LW10): $\pm$ 30, $\pm$ 70, 157, 314, 471, 566. 3C 66B at 6.7 $\mu$ m (LW2): $\pm$ 22.2, $\pm$ 44.3, 66.5, 79.7, 95.1. 3C 076.1 at 4.5 $\mu$ m (LW1): $\pm$ 11.9, $\pm$ 23.8, 35.7, 42.8, 53.1. 3C 079 at 12.0 $\mu$ m (LW10): $\pm$ 89.6, $\pm$ 106.7, 213.5, 320.2, 384.3.

In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{aa0908f10b.eps}\end{figure}$ Figure B.1: continued. 3C 079 at 12.0 $\mu$ m (LW10): $\pm$ 89.6, $\pm$ 106.7, 213.5, 320.2, 384.3. 3C 083.1 at 4.5 $\mu$ m (LW1): $\pm$ 61.1, $\pm$ 91.6, 227.6, 341.5, 409.8. 3C 084 at 6.7 $\mu$ m (LW2): $\pm$ 129.4, $\pm$ 194.1, 759.9, 1139.9, 1367.9. 3C 098 at 14.3 $\mu$ m (LW3): $\pm$ 10.0, $\pm$ 14.2, 21.3, 30.0, 35.9. 3C 265 at 12.0 $\mu$ m (LW10): $\pm$ 34.7, $\pm$ 69.4, 124.9, 477.0, 715.6. 3C 270 at 14.3 $\mu$ m (LW3): $\pm$ 27.7, $\pm$ 38.0, 76.1, 114.1, 137.0. 3C 272.1 at 14.3 $\mu$ m (LW3): $\pm$ 95.2, $\pm$ 95.2, 142.7, 306.4, 459.5, 551.4. 3C 274 (M 87) at 12.0 $\mu$ m (LW10): $\pm$ 55.6, $\pm$ 111.2, 166.8, 185.2, 200.1. 3C 277.3 at 14.3 $\mu$ m (LW3): $\pm$ 3.2, $\pm$ 6.5, 11.6, 62.0, 93.0. 3C 288.1 at 12.0 $\mu$ m (LW10): $\pm$ 18.5, $\pm$ 36.9, 62.6, 66.5, 93.9. 3C 293 at 12.0 $\mu$ m (LW10): $\pm$ 47.4, $\pm$ 94.9, 170.8, 184.3, 276.4. 3C 295 at 6.7 $\mu$ m (LW2): $\pm$ 2.5, $\pm$ 5.0, 9.1, 9.6, 13.6. 3C 296 at 4.5 $\mu$ m (LW1): $\pm$ 37.8, $\pm$ 40.0, 79.9, 119.9, 143.9.

In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{aa0908f10c.eps}\end{figure}$ Figure B.1: continued. 3C 303.1 at 12.0 $\mu$ m (LW10): $\pm$ 5.0, $\pm$ 10.0, 17.9, 117.5, 176.3 3C 305.0 at 12.0 $\mu$ m (LW10): $\pm$ 50.5, $\pm$ 101.0, 151.5, 181.8, 185.0. 3C 305.1 at 12.0 $\mu$ m (LW10): $\pm$ 7.3, $\pm$ 14.7, 26.4, 73.4, 110.2. 3C 309.1 at 12.0 $\mu$ m (LW10): $\pm$ 39.8, $\pm$ 79.3, 118.9, 119.4, 143.3. 3C 319 at 12.0 $\mu$ m (LW10): $\pm$ 2.5, $\pm$ 4.9, 8.9, 109.5, 164.2. 3C 324 at 12.0 $\mu$ m (LW10): $\pm$ 7.8, $\pm$ 15.7, 28.3, 355.4, 533.1. 3C 330 at 14.3 $\mu$ m (LW3): $\pm$ 2.1, $\pm$ 4.3, 6.4, 7.7, 8.5. 3C 332 at 12.0 $\mu$ m (LW10): $\pm$ 45.0, $\pm$ 89.9, 134.9, 161.8, 175.2. 3C 336 at 12.0 $\mu$ m (LW10): $\pm$ 9.7, $\pm$ 19.4, 34.9, 74.3, 111.4. 3C 338 at 6.7 $\mu$ m (LW2): $\pm$ 4.3, $\pm$ 7.9, 11.9, 13.0, 15.6. 3C 341 at 12.0 $\mu$ m (LW10): $\pm$ 14.4, $\pm$ 21.7, 73.4, 110.1, 132.2. 3C 343 at 12.0 $\mu$ m (LW10): $\pm$ 6.9, $\pm$ 13.8, 24.8, 101.4, 152.1.

In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{aa0908f10d.eps}\end{figure}$ Figure B.1: continued. 3C 343.1 at 12.0 $\mu$ m (LW10): $\pm$ 2.9, $\pm$ 5.7, 10.3, 58.9, 88.3. 3C 345 at 12.0 $\mu$ m (LW10): $\pm$ 118.1, $\pm$ 177.1, 362.8, 544.2, 653.0. 3C 346 at 12.0 $\mu$ m (LW10): $\pm$ 20.2, $\pm$ 40.5, 72.9, 132.2, 198.3. 3C 349 at 12.0 $\mu$ m (LW10): $\pm$ 15.8, $\pm$ 31.6, 56.8, 106.2, 159.3. 3C 351 at 12.0 $\mu$ m (LW10): $\pm$ 13.2, $\pm$ 19.8, 349.5, 524.3, 629.2 . 3C 356 at 12.0 $\mu$ m (LW10): $\pm$ 4.6, $\pm$ 9.2, 16.6, 113.8, 170.7 . 3C 371 at 12.0 $\mu$ m (LW10): $\pm$ 118.8, $\pm$ 178.2, 757.4, 1136.1, 1363.3. 3C 379.1 at 12.0 $\mu$ m (LW10): $\pm$ 9.7, $\pm$ 14.5, 31.3, 47.0, 56.3. 3C 380.0 at 12.0 $\mu$ m (LW10): $\pm$ 78.4, $\pm$ 101.1, 156.8, 235.2, 282.3. 3C 381 at 12.0 $\mu$ m (LW10): $\pm$ 91.0, $\pm$ 132.1, 198.2, 272.9, 327.4. 3C 382 at 12.0 $\mu$ m (LW10) : $\pm$ 138.8, $\pm$ 208.1, 992.6, 1488.9, 1786.7. 3C 386 at 12.0 $\mu$ m (LW10): $\pm$ 8.8, $\pm$ 17.6, 31.7, 144.5, 216.7.

In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{aa0908f10e.eps}\end{figure}$ Figure B.1: continued. 3C 388 at 12.0 $\mu$ m (LW10): $\pm$ 3.4, $\pm$ 6.8, 12.3, 110.0, 165.0. 3C 390.3 at 12.0 $\mu$ m (LW10): $\pm$ 119.1, $\pm$ 178.7, 1031.4, 1547.1, 1856.5. 3C 402 at 12.0 $\mu$ m (LW10): $\pm$ 12.1, $\pm$ 24.2, 43.6, 173.5, 260.3. 3C 410 at 12.0 $\mu$ m (LW10): $\pm$ 114.9, $\pm$ 143.2, 229.8, 344.6, 413.6. 3C 418 at 12.0 $\mu$ m (LW10): $\pm$ 16.0, $\pm$ 32.0, 57.6, 174.8, 262.2. 3C 430 at 12.0 $\mu$ m (LW10): $\pm$ 30, $\pm$ 50, 60, 100, 150, 180. 3C 433 at 12.0 $\mu$ m (LW10): $\pm$ 230.4, $\pm$ 232.0, 463.9, 695.9, 835.1. 3C 442, NGC 7236 and NGC 7237 at 12.0 $\mu$ m (LW10): $\pm$ 8.2, $\pm$ 16.4, 29.4, 178.2, 267.3. 3C 445 at 14.3 $\mu$ m (LW3): $\pm$ 258.5, $\pm$ 387.7, 1678.3, 2517.4, 3020.9. 3C 449 at 12.0 $\mu$ m (LW10): $\pm$ 32.3, $\pm$ 64.7, 116.4, 164.6, 246.9. 3C 452 at 12.0 $\mu$ m (LW10): $\pm$ 101.4, $\pm$ 202.8, 304.2, 314.6, 365.1. 3C 456 at 12.0 $\mu$ m (LW10): $\pm$ 20.4, $\pm$ 30.7, 73.7, 110.5, 132.6.

In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{aa0908f10f.eps}\end{figure}$ Figure B.1: continued. 3C 465 at 6.7 $\mu$ m (LW2): $\pm$ 9.2, $\pm$ 9.9, 19.7, 29.6, 35.5. 3C 469.1 at 12.0 $\mu$ m (LW10): $\pm$ 10.3, $\pm$ 20.7, 37.2, 181.7, 272.5. 4C+72.26 at 12.0 $\mu$ m (LW10): $\pm$ 0.4, $\pm$ 0.7, 1.3, 114.0, 171.1. NGC 382 at 12.0 $\mu$ m (LW10): $\pm$ 27.3, $\pm$ 54.6, 98.3, 173.4, 260.1. PMNJ0214-11582 at 12.0 $\mu$ m (LW10): $\pm$ 4.6, $\pm$ 9.1, 16.4, 250.0, 375.0. PCd91212130.83+245139.2 at 6.7 $\mu$ m (LW2): $\pm$ 48.2, $\pm$ 72.3, 235.9, 353.9, 424.6.

In the text

$\begin{figure} \par\includegraphics[height=11.1cm,width=8.8cm,clip]{0908fig1.eps} \end{figure}$	Figure 1: Top: histogram of the distribution of the 178 MHz radio fluxes in the 3CR catalogue. The filled part represents the objects detected by ISOCAM. Bottom: radio fluxes of 3CR sources at 178 MHz plotted as a function of redshift. The filled squares are objects of this paper.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0908fig2.eps} \end{figure}$	Figure 2: Detection rate of 3CR sources in our survey as a function of redshift. The filled part part of the columns refers to 3CR sources detected with ISOCAM where the MIR emission can be attributed to dust (see Sect. 4). The shaded part represents all ISOCAM detections of the 3CR catalogue and the upper (blank) histogram shows the redshift distribution of 3CR sources sampled by ISOCAM.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{0908fig3b.ps}\end{figure}$	Figure 3: continued.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{0908fig4.ps} \end{figure}$	Figure 4: The influence of the dust population on the infrared spectrum of the AGN. Model parameters are: visual extinction $A_{\rm {V}} = 8$ mag, radius R = 1 kpc, luminosity L = 10^12.5 $L_\odot$ at distance of 50 Mpc. Model with large grains only (dashed), with large grains and small graphites (dotted), full model with large grains, small graphites and PAH (solid line).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0908fig5.ps} \end{figure}$	Figure 5: Comparison of radiative transfer computations of dusty starbursts (solid) and AGNs (dashed). In both models we applied a visual extinction of $A_{\rm {V}} = 32$ mag, luminosity of L = 10¹² $L_\odot$ at distance of 50 Mpc, and radius of R = 1 kpc.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0908fig6.ps} \end{figure}$	Figure 6: AGN model spectra are shown for visual extinctions of $A_{\rm {V}} = 1$ , 2, 4, 8, 16, 32 and 64 mag and luminosities of L = 10^10.5, 10^11.5 and 10^12.5 $L_\odot$ at a distance of 50 Mpc. The radius is fixed at R = 1 kpc.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=8.7cm,width=8.4cm,angle=90,clip]{0908fig7.ps} \end{figure}$	Figure 7: The influence of the radius on the AGN model spectra. We apply a distance of 50 Mpc. Top: for luminosity of L = 10¹² $L_\odot$ and extinction of $A_{\rm {V}} = 32$ mag we present models with R = 0.125, 0.25, 0.5, 1, 2, 4, 8 and 16 kpc. Bottom: for luminosity of L = 10¹¹ $L_\odot$ and extinction of $A_{\rm {V}} = 8$ mag we show models with R = 0.125 and 16 kpc.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=13.5cm,width=7.7cm,clip]{0908fig8.ps} \end{figure}$	Figure 8: Top: the intrinsic AGN luminosity of the model, $L_{\rm dust}$ , as function of redshift. Solid symbols are type 1 AGNs: triangles QSOs and squares BLRGs. Open squares are NLRGs and upper limits as of Table 4. Asteriks are unclassified radio galaxies. Bottom: luminosity ratio of AGN and stellar components as a function of redshift. Symbols as in top panel.
Open with DEXTER