0001+058 The optical identification is a fuzzy object close to the detection 
0001+058  limit situated between the two radio lobes. An object of R=22.7+/-0.3 
0001+058  is located about 4" to the SW of the western lobe. Another close-by, 
0001+058  much fainter object (R=23.2+/-0.4) is seen about 5" North of the 
0001+058  eastern lobe. 
0018+052 It cannot be entirely excluded that the optical identification of this 
0018+052  radio source is not located on a bad CCD column. For this reason, 
0018+052  the source remains undetected down to R=23.
0030+061 This is a clear empty field since no optical object is visible within 
0030+061  a radius of 6" from the radio source.
0048+072 The optical field without radio contours is shown in the inset of the 
0048+072  overlay in Fig. 1. A faint object with R=21.9+/-0.1 seen at the centre
0048+072  of the inset, which coincides with the mid-point of the two radio 
0048+072  lobes, is a likely identification. Another candidate is the brighter 
0048+072  object with R=20.8+/-0.1 situated ~4" NW of the radio centre.
0127-195 This radio source is located in a clear empty field.
0321-042 The R-band overlay image shown in Fig. 1 has been taken with EFOSC 2 at
0321-042  the NTT which has a higher resolution than the B-band image used for 
0321-042  the photometry (see Table 1). The optical identification, more clearly
0321-042  seen in the inset of the overlay, is a QSO with redshift z=2.53, based
0321-042  on prominent broad Ly{alpha} and C IV lines.
0348+013 The hint of a wide-angle-tail radio morphology signifies the presence 
0348+013  of a cluster. Interestingly, the optical counterpart is a QSO with 
0348+013  redshift z=1.12, based  on several emission lines visible in our 
0348+013  spectra. About 9" to the SW of the quasar, a foreground elliptical 
0348+013  galaxy is seen for which we find a redshift z=0.27. The R-band image 
0348+013  shown in Fig. 1 has been taken with EFOSC 2 at the NTT which has a 
0348+013  higher resolution than the R-band image used for the photometry.
0355-037 The R-band overlay image shown in Fig. 1 resulted from a 30min exposure
0355-037  taken with EFOSC 2 at the NTT which has a higher resolution than the 
0355-037  R-band image used for the photometry (see Table 1). The optical ID 
0355-037  lies closer to the eastern lobe of the radio source. It has a fuzzy 
0355-037  appearance, roughly extended along the radio axis. It has a northward 
0355-037  extension of 5", which is also seen on the EFOSC 1 image used for the
0355-037  photometry. It could possibly be a chain of fainter galaxies, or even 
0355-037  a tidal tail resulting from a merger event.
0410-198 Our results for this source are published in Giraud et al. 
0410-198  (1996A&A...309..733G). It is identified with the dominant galaxy of a 
0410-198  z=0.79 cluster. A remarkable optical extended emission-line region 
0410-198  (EELR) of low excitation and size, ~100kpc, was found associated with 
0410-198  the radio galaxy. The EELR bears a close morphological relationship 
0410-198  to the radio lobes which exhibit Z-shaped symmetry. The EELR appears 
0410-198  to consists of three cones associated with the radio galaxy and a 
0410-198  neighbouring galaxy also located at the same redshift and connected to
0410-198  the former by a long stellar filament.
0423-199 The optical counterpart is clearly extended along the two radio lobes 
0423-199  (see inset in Fig. 1). Our low-dispersion spectra yielded a redshift 
0423-199  z=1.12 based on three (narrow?) emission lines (C III]{lambda}1909, 
0423-199  Mg II{lambda}2800, [O II]{lambda}3727).
0424-197 An almost point-like object lies at the position of this barely 
0424-197  resolved radio source.
0430-197 Only a pointing optical image (3min exposure) is available for this 
0430-197  small diameter radio source which remains unidentified down to R=22.7.
0430-197  A deeper image is needed.
0441+049 The optical counterpart is a diffuse object with two peaks separated by
0441+049  2" along the radio axis.
0449-195 The optical counterpart of this marginally resolved radio source is not
0449-195  visible in our 3min pointing image. A deeper image is needed for this
0449-195  source.
0551-196 A galaxy of R=22.3+/-0.2 which is seen at the centre of the overlay is 
0551-196  situated roughly midway between the two widely separated radio 
0551-196  "lobes". This is a possible identification. However, since the 
0551-196  southern lobe is itself resolved into two components, it is possible 
0551-196  that the two lobes are in fact independent radio sources. In that 
0551-196  event, their optical counterparts are undetected down to R=23.7.
0634-196 This barely resolved radio source is a clear empty field located 
0634-196  towards the Galactic anticentre (b=-12.4{deg}).
0852+124 Our results for this source are published in Gopal-Krishna et al. 
0852+124  (1995A&A...303..705G). A giant cloud of Ly{alpha} emission at z=2.468 
0852+124  extended over ~100kpc is associated with the southern radio lobe. The
0852+124  equivalent width of Ly{alpha} is exceptionally large (~1000{AA} in the
0852+124  rest-frame) and the line profile indicates expansion at a velocity of 
0852+124  ~550km/s, probably driven by the radio lobe from within. The Ly{alpha}
0852+124  emission shows a sharp cut-off near the radio galaxy indicative of a 
0852+124  dusty disc around the galaxy, oriented roughly perpendicular to the 
0852+124  radio axis.
0918-194 The only optical object detected between the two radio lobes is a 
0918-194  galaxy at {alpha}=09:21:15.7, {delta}=-19:37:43 (J2000).
0946+077 The optical counterpart of this small diameter (3") radio source is 
0946+077  below the detection limit in our image, R>23.3. There is a 
0946+077  bright object about 7" West of the radio position.
1005-046 Since our VLA map shows the size of this source to be 100", its flux 
1005-046  density given in the Molonglo Reference Catalogue at 408MHz (MRC does
1005-046  not give integrated flux) might be significantly underestimated. Hence
1005-046  we have computed the spectral index using the flux densities estimated
1005-046  from the NVSS map (353mJy at 1.4GHz) and the Parkes survey (87mJy at
1005-046  4.85GHz; Griffith et al., 1995, Cat. <VIII/38>). We further note that 
1005-046  our VLA map shows a prominent radio core in this triple source, which 
1005-046  contributes ~9mJy at 4.85GHz.
1005-046  The optical identification is a bright, narrow emission-line radio 
1005-046  galaxy (NELG) at a redshift z=0.618. A close inspection of the image 
1005-046  shows that the optical counterpart could be a tight chain of three 
1005-046  objects. The southern radio hot spot coincides with a point-like 
1005-046  optical object with R=19.7+/-0.1.
1048+002 The optical identification lies closer to the northern radio lobe and 
1048+002  is seen more clearly near the centre of the inset. After 4h of 
1048+002  integration, the optical spectrum shows two narrow faint emission 
1048+002  lines that we tentatively identify with Mg II{lambda}2800 and 
1048+002  [O II]{lambda}3727 at z=0.71. Note also that a faint optical object is
1048+002  coincident with the outer edge of the southern radio lobe.
1059+107 The optical ID is a galaxy that coincides with the central radio 
1059+107  component and is elongated along the radio axis. A relatively bright 
1059+107  star is located 6" to the SE of the galaxy.
1132+112 The optical ID of this radio source is a point-like object 
1132+112  with R=22.0+/-0.1.
1146+052 The best candidate for optical identification is a R=22.6+/-0.1 galaxy 
1146+052  situated at {alpha}=11:48:47.9, {delta}=+04:55:25 (J2000). It could 
1146+052  be the dominant member of a distant cluster. Our 2h spectrum of this 
1146+052  galaxy shows a strong [O II]{lambda}3727 emission line and a rich 
1146+052  Balmer absorption spectrum, reminiscent of other cluster sources 
1146+052  (Melnick et al., 1997A&A...318..337M). Unfortunately, our B 300 
1146+052  spectra cuts off just where we would expect to see the [O III] 
1146+052  emission lines at z=0.42, so we cannot be certain of the LINER nature 
1146+052  of this source.
1224-085 The identified optical structure consists of a R=23.5+/-0.3 point-like 
1224-085  object and a faint, 6" long wisp to SW coincident with the southern 
1224-085  radio lobe and elongated along the radio axis. The entire structure 
1224-085  has R~22.
1238-074 The radio structure is poorly resolved in our low-resolution VLA map. 
1238-074  The only object within 5" of the radio peak is a R~23 fuzzy object 
1238-074  situated at {alpha}=12:40:48.0, {delta}=-07:43:18 (J2000).
1245+115 The likely optical counterpart is a point-like object located 6" NW 
1245+115  of a bright star.  
1246-081 The optical counterpart of this slightly resolved (~1") radio source is
1245+115  a R=22.8+/-0.4 object. A fainter object is also seen 2" NE of it.
1248-108 The central radio component lies within 1.5" of a pair of optical 
1248-108  objects which are themselves separated by 2" and have an integrated 
1248-108  R=22.7+/-0.3. One of these objects is the likely optical ID.
1317-194 An object of R=24.4+/-0.2 is seen 1.5" NE of the central component of 
1317-194  this extended radio source. The astrometry has been independently 
1317-194  checked using a 10min exposure taken with EFOSC 1 at the ESO 3.6m 
1317-194  telescope. This image is less deep but includes five reference stars 
1317-194  and confirms the astrometry as shown in the overlay.
1324-104 The likely optical ID is close to the north-eastern radio lobe and 
1324-104  appears to be extended.
1329-195 An optical object is seen about 2.5" offset from the radio peak towards
1329-195  NE. Within the astrometric uncertainties for this case, this object is
1329-195  the likely identification. Faint and narrow emission lines of 
1329-195  [C II]{lambda}2326 and Mg II{lambda}2800 are visible in our 2h 
1329-195  spectrum of this object indicating that the radio source is probably a
1329-195  NELG at a redshift z=0.98.
1411-192 Our results for this source are published in Gopal-Krishna et al. 
1411-192  (1992A&A...254...42G). An EELR of size ~100kpc and z=0.477 is 
1411-192  associated with this double radio source. Its [O II]{lambda}3727 
1411-192  emission line has a very large rest-frame equivalent width (350{AA}), 
1411-192  consistent with the high radio luminosity. Intriguingly, we found that
1411-192  its optical spectrum is ultra-soft, with 
1411-192  [O II]{lambda}3727/[O III]{lambda}5007=10, nearly 30 times the typical
1411-192  value for distant 3CR radio galaxies (van Breugel & McCarthy, 1990,
1411-192  ASP Conf. Ser., 10, 359). Together with Hydra A, this source thus 
1411-192  provides an outstanding example of extremely low-ionization optical 
1411-192  emission-line spectra being associated with powerful radio galaxies 
1411-192  (Melnick et al., 1997A&A...318..337M). Unfortunately, the object is 
1411-192  seen very close to a bright star, so it is difficult to say whether it
1411-192  is a cluster source like Hydra A.
1443-198 Deep multi-color optical observations of this source have been reported
1443-198  by us (Giraud et al., 1996A&A...311..446G). The source was identified 
1443-198  with a z=0.753 elliptical galaxy in the process of formation by 
1443-198  accreting material from neighbouring galaxies, all members of a group.
1443-198  The radio source has a central core and two relatively relaxed lobes 
1443-198  consistent with its being in a cluster.
1509-158 The peak of this unresolved radio source lies just ~15" from a pair of 
1509-158  bright stars. No optical identification is visible above a detection 
1509-158  limit of R~24. The radio flux measurement at 2.7 GHz (Effelsberg) 
1509-158  contains a significant contribution from a  10" double radio source 
1509-158  located 2.8' to the NW of 1509-158. Due to this, the true spectral 
1509-158  index of this source is probably even steeper than the -1.24 value 
1509-158  given in Table 1. The parameters of the confusing source, estimated 
1509-158  from our VLA observations, are {alpha}=15:12:22.7, {delta}=-15:58:05 
1509-158  (J2000), with a flux density equal to 36mJy at 5GHz 
1509-158  (Kulkarni et al. 2005, in prep.).
1523-017 The radio map of this triple source is taken from the VLA 5GHz 
1523-017  observations by Bennett et al. (1986, Cat. <VIII/52>). The redshift of
1523-017  the optical counterpart, z=0.93, was derived from a 3h low-dispersion 
1523-017  (B 1000) spectrum taken with EFOSC 1. The spectrum shows prominent, 
1523-017  probably narrow, Mg II and [O II] emission lines. The presence of H+K
1523-017  in absorption and the lack of strong [O III] emission lines indicate 
1523-017  that this object may be a LINER.
1612-208 The optical counterpart of this unresolved radio source is quite bright
1612-208  and point-like. The blue spectrum of this object obtained from 2h 
1612-208  integration with EFOSC 1 is typical of an elliptical galaxy at z=0.31.
1612-208  The lack of emission lines and the compactness of the object, however,
1612-208  are rather puzzling.
1621-196 Although this object has a large radio size, its optical identification
1621-196  remains uncertain. The nearest object to the radio centre is a 
1621-196  R=21.6+/-0.2 point-like object, which we suggest as the possible 
1621-196  identification. However, it is offset by 4" to the South of the faint
1621-196  radio peak seen between the two radio lobes. In addition to the R-band
1621-196  photometry, we also took a 15 min V-band exposure using EFOSC 1 from 
1621-196  which we get V=21.2+/-0.1 and V-R=-0.4 assuming that the object did 
1621-196  not vary over the 11 months time interval between the two 
1621-196  observations. If a higher resolution radio map confirms the faint, 
1621-196  central peak to be the radio nucleus then its separation from the 
1621-196  suggested optical ID would be four times the rms astrometric error. 
1621-196  Any other optical ID would have to be below the detection limit of the
1621-196  image (R~25 for a point source).
1623-194 The optical counterpart of this radio source is a point-like object.
1631-222 The source lies in a crowded field close to the Galactic plane 
1631-222  (latitude +16{deg}). The only detected object within 2" is a 
1631-222  R=25.5+/-0.4 object located about 2" North of the radio peak. This is
1631-222  the likely optical ID for this unresolved radio source.
1632-199 This compact steep spectrum radio source lies in a clear empty field.
1859-187 This extended radio source lies in a crowded field close to the 
1859-187  Galactic plane (latitude -10.7{deg}). The inset shows five bright 
1859-187  objects near the mid-point between the two radio lobes. Of these, the 
1859-187  western-most object, which is slightly extended, is the most likely 
1859-187  optical identification.
2011-169 The optical counterpart of this compact steep spectrum radio source is 
2011-169  undetected down to a very deep level (R=25.6).
2023-156 There is a hint of a central radio component. The NS extended optical 
2023-156  object is offset from this component by 1.5" to the North, which is 
2023-156  within the astrometric error, and is therefore the likely optical 
2023-156  counterpart.
2057-179 The suggested optical ID partially overlaps with the image of a 1.6mag 
2057-179  brighter elliptical galaxy located about 3" to the South. A 2h 
2057-179  spectrum obtained with EFOSC 2 at the ESO/MPI 2.2 m telescope shows a 
2057-179  rich emission-line spectrum at z=0.92. The adjacent elliptical galaxy 
2057-179  is at z=0.6.
2105-119 The best candidate appears to be the slightly extended object located 
2105-119  about 1.3" West of the radio position. A very faint fuzz is coincident
2105-119  with the radio peak.
2222-057 The spectral index of this radio source has a large uncertainty of 
2222-057  +/-0.2 (see Sect. 2.1). No object is seen within the radio contours 
2222-057  above the detection limit of the image (R~23).
2232-062 A tight clustering of bright stars is seen within 20" West of this 
2232-062  radio source. This considerably degrades the quality of detection of 
2232-062  the faint (R~23.5) optical counterpart observed between the two radio
2232-062  lobes.
2236-039 This compact steep-spectrum radio source coincides with a barely 
2236-039  detected fuzz with R~23 situated in a crowded field.
2236-047 The results of our detailed optical observations of this source have 
2236-047  been reported by Melnick et al. (1993A&A...271L...5M). The distorted 
2236-047  double radio source is identified with a z=0.552 cD galaxy which is 
2236-047  member of a cluster (Kulkarni et al. 2005, in prep.). Between this 
2236-047  galaxy and another similarly bright galaxy to the NE, which is a 
2236-047  member of the same cluster, an unusually bright and straight arc-like 
2236-047  feature was found by Melnick et al. (1993A&A...271L...5M). We 
2236-047  interpreted it as the image of a pair of merging galaxies at z=1.116, 
2236-047  highly magnified due to gravitational lensing by the foreground 
2236-047  cluster (see also Kneib et al., 1994A&A...290L..25K).
2245-037 On the assumption that the two radio components of this source are 
2245-037  physically associated, the most likely optical identification is the 
2245-037  bright (R=20.8+/-0.1) object roughly located midway between them. On 
2245-037  the other hand, it is quite possible that the two radio components are
2245-037  independent radio sources (particularly since the western component is
2245-037  itself a 6" double). In that case, the optical features detected 
2245-037  towards each of them would be their likely optical IDs. The magnitudes
2245-037  of these objects are R=22.7+/-0.2 for the western lobe and 
2245-037  R=20.8+/-0.1 for the source close the eastern lobe.
2347+015 More sensitive radio imaging is needed to confirm if this source is a 
2347+015  wide-angle tail. The likely optical identification is coincident with 
2347+015  the radio peak.