Abstract
We present polarization maps with 6''.4 x 10''.7 resolution. The total intensity distributiin is dominated by the compact heads. The flux of the central source is 0.8 +- 0.15 Jy. The polarization distribution of the two lobes are quite similar. For both, the tails show smooth, large-scale structure and reach at least 30% linear polarization in places.Comparison with a 5 GHz map shows that the spectral index varies from -1 on the heads to less than -1.7 inward along the tails. This gradient is interpreted in terms of synchrotron losses occurring in the relativistic plasma as it flows out from the heads.For the NW component, comparison of the position angles of the polarized emission at 5 GHz with our maps shows changes in the amount of rotation of +- 45/sup 0/ with angular scales of approx.1'', but little depolarization at 5 GHz. The latter suggests that the thermal electron density within this lobe is at most 10/sup -3/ cm/sup -3/. The SE tail is highly depolarized at 5 GHz. We suggest that the polarization behavior of both components is perhaps caused by a lumpy Faraday rotating screen in the vicinity of the galaxy but outside the radio lobes.
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