This is the third most distant known radio galaxy at a redshift of
. It has an
FR II edge brightened double radio morphology (Fanaroff-Riley 1974).
At low frequency
(see Figure 2a) the spectral index between 38 MHz (Rees 1990) and
178 MHz (Gower et.
al)
= -O.9X is greater than -1. Thus it would not
be selected as a USS in the meter
wavelength range.
The western lobe A in 4C60.07 is the brighter and flatter spectrum of the two lobes (see Figure 3). Polarization is detected in this lobe at both 20 cm and 6 cm with a depolarization measure DP = X. At higher resolution (Figure 3g and 3j) lobe A is resolved into a primary and secondary hot spot (A1 and A2), each with separate polarization angles. Of the two, A2 is less polarized.
The eastern lobe B is completely depolarized. There is extended emission in both 20 cm and 6 cm back towards the center. In the high resolution image lobe B is resolved into two main components (B1 and B2) co-linear with the overall axis. Both of these components are still completely depolarized at high resolution. The series of marginally detected spots along the radio axis suggests that the extended emission seen in the low resolution images is due to a jet. The western most spot is near the center of the two lobes and could be the core, but only deeper high frequency observations will decide the issue. If the core does lie near the center of the two lobes, then the depolarization features are contrary to what one would expect from the Laing-Garrington effect (Laing 1988, Garrington et al 1988, LG hereafter). On the other hand, if B1 is the core, then the polarization properties become consistent with the LG effect, but the source is then highly asymmetric.
The optical and infrared emission are faint, and the morphology is
uncertain. In each
band, however, the emission is extended along the radio axis
demonstrating the alignment
effect (Chambers et al. 1987, McCarthy et al. 1987, Chambers &Miley
1989). The aligned
optical and K band light are spatially coincident with the extended
radio emission between
the lobes, i.e. the "jet" as discussed above. The data is limited
by the faintness of the
object, but it does suggest that there are strong color gradients
within the object. Both the
R and I band show a curved feature to the south, the K band image
shows a component or
red companion to the north
.
All images contain very faint diffuse emission.
The comparatively simple radio morphology of 4C60.07 (i.e. compared to 4C41.17 at the same redshift) makes it an ideal candidate for follow up studies.