Free Access
Issue
A&A
Volume 551, March 2013
Article Number A97
Number of page(s) 39
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201220374
Published online 04 March 2013

Online material

Table 6

Data of the 217 sources which were in principle detectable (SVLA > 6 × rms).

Table 7

Multi-wavelength data for the VLBI-detected sources.

thumbnail Fig. 21

Contour plots of the VLBA images of the 65 detected sources. The plots show regions of 216 mas × 216 mas, centred on the sources, except for the plot of L0703, which shows a region of 360 mas × 360 mas. Black contours indicate the full-resolution, naturally-weighted images, whereas grey, dashed contours indicate images made with a 10 Mλ taper. The black and grey ellipses in the lower left corners indicate the size and orientation of the restoring beams used with full resolution and a 10 Mλ taper, respectively. In both cases contours start at the 3 times the naturally-weighted image noise and increase by factors of . The noise levels of the naturally weighted images have been added to the plots. Note that the flux densities listed in Table 6 have been extracted from uniformly-weighted images (not shown), to reduce the effect of the point spread function (see Sect. 4 and Fig. 10).

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thumbnail Fig. 22

Left column: UV to mid-infrared SED fits. Black points: photometric observations, red line: best-fitting model, cyan line: stellar template, black line (where applicable): galaxy template of second photometric redshift solution. The inset shows the probability distribution function of the best-fit model. Right column: RGB cutouts made from Subaru RcIcz′ images, with a single VLA contour overlaid and the VLBA position indicated with red crosses. These images show regions 28.8 arcsec × 28.8 arcsec in size.

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thumbnail Fig. 23

RGB images of sources with uncatalogued, blended, or otherwise unavailable counterparts, made using the same settings as used for Fig. 22. In L0199, L0251, L0386 and L0708 very faint, but uncatalogued counterparts can be seen in the images; in L0506 and L1148 the VLBA detection is offset from the foreground object by so much that an association was deemed unlikely.

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thumbnail Fig. 24

RGB images of sources with no visible counterparts, made using the same settings as used for Fig. 22.

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© ESO, 2013

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