This very high redshift object was discovered and its properties first described by Chambers et al. 1990. Since then several groups have obtained new results in the radio, submillimeter, infrared, and optical: Carilli &Owen 1994, Carilli, Owen &Harris 1995, Dunlop et al. 1994, Chini &Kruegel 1994. Graham et al. 1994, Djorgovski et al 1995, Miley et al 1992, and Hippelein &Meisenheimer 1993.
In Figure 4 we show a large scale 20 cm map of the field of 4C41.17. (See also the multifrequency maps in Chambers et al 1990 and Carilli &Owen 1995). There are (at least) two other radio sources in the field of 4C41.17 (D and E in Table 2). The source D (also noted by Carilli &Owen) has no optical identification on our plate material. There is a very faint blue diffuse object at the position of source E; it has no strong emission lines.
Carilli &Owen identified the core (N) with deep 3.5 cm observations.
Their high
frequency observations are deeper than those of Chambers et al. 1990,
and their positions
are slightly offset. In Table 2 and in the discussion below we adopt
the Carilli &Owen
radio positions, although the difference is not significant. A more
crucial issue is the
optical astrometry of the field. Hippelein &Meisenheimer 1993 present
astrometric plate
measurements for the their Ly map which places the peak of the
Lyman alpha emission
at a significantly different location relative to the radio lobes than
that of Chambers et
al. 1990. If we were to adopt the position of the peak of the HM map
then the Ly
and
continuum would be entirely displaced from radio lobes. This seems
unlikely. Thus for the
registration and optical comparison of the HST data with the radio
data we use the optical
astrometry of Chambers et al 1990. Note that the present results differ
in position, scale, and orientation from Miley et al 1992.