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Table 2:

Observation parameters.

PKS 		Alias Date Dist. $F_{11.85~\mu{\rm m}}^{{\rm core}}$ Lit. Ref. $\log{\nu L_{11.85~\mu{\rm m}}^{{\rm core}}}$ $\log{\nu L_{5{\rm GHz}}^{{\rm core}}}$ $\log{\nu L_{12~\mu{\rm m}}^{{\rm total}}}$ R50 FWHM
                      Obj. St.
      Mpc (mJy) (mJy)   ( ${\rm erg}~{\rm s}^{-1}$) ( ${\rm erg}~{\rm s}^{-1}$) ( ${\rm erg}~{\rm s}^{-1}$) (pc) ( $\hbox{$^{\prime\prime}$ }$) ( $\hbox{$^{\prime\prime}$ }$)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
0007+12 4C12.03 2006-06-18 710 <3 $\dots$ $\dots$ <43.58 40.28 $\dots$ $\dots$ $\dots$ $\dots$
0034-01 3C 015 2006-06-18 310 <3 6 4 <42.93 41.21 $\dots$ $\dots$ $\dots$ $\dots$
0055-01 3C 029 2006-12-27 190 <4 2 4 <42.56 40.28 $\dots$ $\dots$ $\dots$ $\dots$
0123-01 3C 040 2006-12-27 70 <4 $\dots$ $\dots$ <41.76 39.51 <43.27 $\dots$ $\dots$ $\dots$
0305+03 3C 078 2006-12-27 120 <4 $\dots$ $\dots$ <42.18 40.78 <43.57 $\dots$ $\dots$ $\dots$
0320-37 Fornax A 2006-12-27 20 <9 $\dots$ $\dots$ <41.03 37.81 42.44 $\dots$ $\dots$ $\dots$
0340+04 3C 093 2006-12-27 1800 <5 $\dots$ $\dots$ <44.56 40.75 $\dots$ $\dots$ $\dots$ $\dots$
0356+10 3C 098 2005-12-18 130 20 $\pm$ 1.4 24 2 42.93 $\pm$ 0.04 38.91 <42.95 180 0.47 0.37
0404+03 3C 105 2005-12-18 390 <2 $\dots$ $\dots$ <42.93 40.06 $\dots$ $\dots$ $\dots$ $\dots$
0430+05 3C 120 2006-12-27 140 240 $\pm$ 15 109 1 44.10 $\pm$ 0.03 41.58 44.20 170 0.36 0.33
0511+00 3C 135 2006-12-27 570 <4 $\dots$ $\dots$ <43.51 39.89 $\dots$ $\dots$ $\dots$ $\dots$
0518-45 Pictor A 2006-12-27 150 68 $\pm$ 4.3 $\dots$ $\dots$ 43.59 $\pm$ 0.04 41.09 43.82 200 0.34 0.33
0819+06 3C 198 2006-12-27 350 <4 $\dots$ $\dots$ <43.13 39.13 $\dots$ $\dots$ $\dots$ $\dots$
0945+07 3C 227 2006-12-27 370 29 $\pm$ 3.1 $\dots$ $\dots$ 44.01 $\pm$ 0.05 40.38 <44.96 410 0.36 0.33
1216+06 3C 270 2006-06-18 30 <2 27 4 <40.72 39.17 <42.44 $\dots$ $\dots$ $\dots$
1322-42 Centaurus A 2006-12-27 3.8 1200 $\pm$ 47 1800 3 41.69 $\pm$ 0.03 38.79 42.69 5 0.37 0.33
1417-19 PKS1417-19 2006-12-27 530 26 $\pm$ 4.3 $\dots$ $\dots$ 44.27 $\pm$ 0.08 39.90 $\dots$ 770 0.44 0.33
1514+07 3C 317 2006-06-18 142 <3 3 4 <42.24 40.66 <43.67 $\dots$ $\dots$ $\dots$
1559+02 3C 327 2005-07-02 460 78 $\pm$ 7.5 $\dots$ $\dots$ 44.62 $\pm$ 0.05 40.50 <44.68 1300 1.25 0.42
1717-00 3C 353 2005-07-02 125 <4 $\dots$ $\dots$ <42.28 40.02 $\dots$ $\dots$ $\dots$ $\dots$
1839-48 PKS1839-48 2006-06-18 490 <4 $\dots$ $\dots$ <43.40 41.33 $\dots$ $\dots$ $\dots$ $\dots$
1949+02 3C 403 2006-06-18 250 89 $\pm$ 6.8 $\dots$ $\dots$ 44.17 $\pm$ 0.04 39.55 44.50 330 0.34 0.37
1949-01 3C 403.1 2006-06-18 230 <4 $\dots$ $\dots$ < 42.78 $\dots$ $\dots$ $\dots$ $\dots$ $\dots$
2045+06 3C 424 2006-06-18 560 <4 2 4 <43.46 40.48 $\dots$ $\dots$ $\dots$ $\dots$
2158-380 PKS2158-380 2006-06-18 140 17 $\pm$ 2.8 $\dots$ $\dots$ 42.94 $\pm$ 0.07 <38.88 <43.68 200 0.37 0.33
2221-02 3C 445 2005-07-02 240 190 $\pm$ 16 210 2 44.46 $\pm$ 0.04 40.44 44.44 390 0.42 0.42
2354-35 PKS2354-35 2006-06-18 210 <3 $\dots$ $\dots$ <42.55 39.08 $\dots$ $\dots$ $\dots$ $\dots$

Notes. Column (1) Parkes Radio catalogue reference. Column (3) Date of observation. Column (4) Distances under the chosen cosmology, determined from the redshifts. Columns (5-7) VISIR mid-infrared core flux and 3-$\sigma$ upper limits, at the SiC-band (11.9 $\mu$m), compared to literature values: 1 = Gorjian et al. (2004) (TIMMI, 1.5  $\hbox{$^{\prime\prime}$ }$, 10.8 $\mu$m), 2 = Siebenmorgen et al. (2004a) (ISOCAM, 5  $\hbox{$^{\prime\prime}$ }$, 14.3 $\mu$m), 3 = Whysong & Antonucci (2004) (Keck, 0.3 $\hbox{$^{\prime\prime}$ }$, 11.7 $\mu$m) and 4 = Leipski et al. (2009) (Spitzer IRS, 15 $\mu$m). Column (8) VISIR mid-infrared core luminosity at rest wavelength. Column (9) Radio (5 GHz) core luminosity at rest wavelength from fluxes tabulated in Table A.1. Column (10) IRAS mid-infrared galaxy luminosity at rest wavelength derived for most sources from flux from Golombek et al. (1988), for 3C 227 from Hes et al. (1995), and for PKS2158-380 from Moshir et al. (1990). Columns (11-13) The radius at $50\%$ of the flux, the full width half maximum (FWHM) of the flux of the source and of the standard star.


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