A2746_2a/b  (P=0.03)  The radio morphology suggests a possible
A2746_2a/b  wide-angle tailed (WAT) radio galaxy with the host G near the
A2746_2a/b  radio centroid.
A2746_8     (P=0.0005)  The St object near the radio centroid is
A2746_8     accepted as the identification, but the fainter G~4" to the east,
A2746_8     with P=0.008, may be an alternative identification.
A2837_1     (P=0.0002)  Fig. 3 shows an unambiguous identification
A2837_1     with a G near the source centroid.
A2837_6     (P=0.0008)  The most likely identification is the G
A2837_6     near the source centroid, but a fainter G (P=0.03) near the radio
A2837_6     axis 10" to the NE may be the host of an unresolved narrow-angle
A2837_6     tailed (NAT) radio galaxy.
A2837_8     Although no identification is listed, Fig. 3 shows
A2837_8     a G 13" to the south of the radio centroid (P=0.08) that may be
A2837_8     the host of an unresolved WAT.
A2837_9     (P=0.002)  A faint G near the radio centroid is not
A2837_9     clear in the R-band image of Fig. 3, but is verified by the B
A2837_9     and IR images.  The two brighter G's to the NE and NW of the
A2837_9     centroid could be hosts to either an unresolved NAT (P=0.002)
A2837_9     or WAT (P=0.002) respectively; they are probably cluster galaxies.
A2837_10    (P=0.0005)  The faint G in Fig. 3, 1" to the NNW of
A2837_10    the radio centroid, is confirmed on UKST-B and ESO-R images.
A2837_11    (P=0.006)  The bright G, 8" to the ENE, could be a
A2837_11    cluster member. and is accepted as the identification.  The faint
A2837_11    object near the radio centroid appears only on the 2nd-epoch Sky
A2837_11    Survey B-image, but not on the 1st-epoch one, and is therefore
A2837_11    probably a plate defect.
A2837_14    (P=0.005)  Figure 3 shows a  G, 4" to the NE of the
A2837_14    radio centroid which we accept as the identification.  The object
A2837_14    is not bright enough for cluster membership. The faint object ~15"
A2837_14    to the west has a high probability of projection.
A3126_2     The St  7" to the south of the radio centroid has
A3126_2     P=0.02, but its position relative to the radio centroid and major
A3126_2     axis does not support its status as an identification.
A3126_9     The bright G is a secure identification for this
A3126_9     extended source. It is a cluster member by its brightness.
A3126_10a/b The well-defined double source is probably a distant
A3126_10a/b FR II radio galaxy.
A3126_13/16 Here we see two separate sources, one extended
A3126_13/16 (#13, NW) and the other (#16, SE) much more compact; both are
A3126_13/16 identified with bright elliptical galaxies, in fact the two
A3126_13/16 brightest are spectroscopically confirmed cluster members, which
A3126_13/16 are projected onto the cluster at angular distances of 1.0' and
A3126_13/16 0.2' from the X-ray centroid respectively. The compact SE source
A3126_13/16 (#16) coincides with the brightest cluster galaxy and is
A3126_13/16 closer in projection to the cluster's X-ray centroid.  Given the
A3126_13/16 positional uncertainty of ~1' of the REFLEX position for an
A3126_13/16 extended source like this (Edge 2006, priv. comm.), A3216_16 and its
A3126_13/16 associated galaxy could well be at the dynamical centre of the 
A3126_13/16 cluster. There is good evidence from the digitized image of 
A3126_13/16 the 2-nd epoch UKST Red Survey for a halo surrounding them. Another 
A3126_13/16 unusual feature of this pair of radio sources is the marked 
A3126_13/16 difference in their radio spectra. The compact SE source has a 
A3126_13/16 fairly flat spectrum (alpha=-0.27+/-0.54), while the extended NW 
A3126_13/16 source has a more normal spectral index of -0.90+/-0.16. The flat 
A3126_13/16 spectrum and compact nature of the SE source suggest that this 
A3126_13/16 elliptical is dominated by an AGN, while the NW source is possibly a
A3126_13/16 partially resolved NAT whose projected tails extend almost to the 
A3126_13/16 cluster's X-ray centroid.
A3126_25    (P=0.0013)  The comparatively bright St object, 6" to
A3126_25    the NNW of the radio centroid, is accepted as the identification
A3126_25    for this extended source.
A3126_27    (P=0.0003)  The faint G near the centroid of
A3126_27    this extended radio source is accepted as the most likely
A3126_27    identification. The St object 22" to the NNW of the centroid has
A3126_27    P=0.23 and is not associated with the radio source.
A3126_28    (P=0.005)  The comparatively bright G, 5" to the SSW
A3126_28    of the radio centroid, is accepted as the identification.
A3216_2     (P=0.00003)  The bright elliptical G near the radio
A3216_2     centroid is accepted as the identification, and considered a
A3216_2     cluster member.
A3216_6a/b  (P=0.00009)  The comparatively bright G near the
A3216_6a/b  radio centroid is accepted as the identification, and considered
A3216_6a/b  a cluster member. The fainter St object, 7" to the NNE, may be
A3216_6a/b  a projected object with P=0.023.
A3216_7     The extended source is probably an unresolved NAT;
A3216_7     the host G is 16" to the NE of the radio centroid along the major
A3216_7     axis. Its probability of projection is P=0.06 with respect to
A3216_7     the radio centroid, but its proximity to the major axis makes
A3216_7     the identification more secure.
A3216_9     (P=0.00006)  The bright G near the radio centroid is
A3216_9     the favoured identification, but the other three G's within the
A3216_9     central two contours are bright enough to be cluster members;
A3216_9     they have values of P between 0.01 and 0.00007.
A3216_10    (P=0.004)  Although the G is displaced 9" from
A3216_10    the radio centroid along the major axis, it is accepted as the
A3216_10    identification for this radio source. It is bright enough for
A3216_10    cluster membership.
A3216_14    A bright St object (m_R=13.7) is 4.4" from the
A3216_14    radio centroid of this unresolved source, but its accurate radio
A3216_14    coordinates suggest that the objects are not associated. There
A3216_14    is no overlay in Fig. 3.
A3230_1     Figure 3 shows four optical objects within the
A3230_1     radio contours: three G's and one St (the fainter of the two
A3230_1     images to the SW). All four objects within the contours have a
A3230_1     low probability of projection with respect to the radio centroid
A3230_1     (P<0.01) but only the bright E/S0 galaxy ~20" to the south east of
A3230_1     the radio peak, and the brighter of the two fainter galaxies (7"
A3230_1     south of the radio peak) are bright enough to be cluster members.
A3230_1     The bright E/S0 SE of the radio centroid is accepted as the most
A3230_1     likely identification, as it is positioned along the major axis
A3230_1     of this extended source.
A3230_4     (P=0.0002)  The bright elliptical G near the
A3230_4     radio centroid is accepted as the identification for this
A3230_4     extended source; it is possibly the host galaxy of an unresolved
A3230_4     WAT. Despite the clear elongation of the radio contours, a gaussian
A3230_4     fit was unable to yield a deconvolved size.
A3230_9     (P=0.02)  The faint St identification for this extended
A3230_9     source is displaced 6" along the major axis to the NNW of the radio
A3230_9     centroid. It is tabulated in the UK-R and UK-B SuperCOSMOS data.
A3230_11    (P=0.00004)  There are two bright G's at 1" and 4"
A3230_11    to the south of the radio centroid, but the brighter one nearer
A3230_11    the radio centroid is accepted as the identification. The other
A3230_11    galaxy is also bright enough for cluster membership.  There is
A3230_11    no overlay in Fig. 3.
A3827_2     Fig. 3 shows no clear identification for this slightly
A3827_2     extended source.  It is possibly a distant FR II.
A3827_3     (P=0.0024)  The St object, close to the radio centroid,
A3827_3     is accepted as the identification. The faint G, 24" along the major
A3827_3     axis to the SSW of the radio centroid, is probably a projected
A3827_3     object with P=0.2; this G is too faint to be a cluster member.
A3827_4     The bright elliptical G near the radio centroid is
A3827_4     clearly the identification. The distorted nature of the outer
A3827_4     contour to the SSE may be due to the close negative contour. The
A3827_4     source is clearly extended in PA~60{deg}, but a deconvolved size
A3827_4     was not yielded in a gaussian fit.
A3827_8     (P=0.002)  The bright elliptical G to the NNW of
A3827_8     the radio centroid of this extended source is accepted as the
A3827_8     identification. The relatively bright St near the SSW outer
A3827_8     contour may be a projected object with P=0.10.
A3827_11a/b The two St objects within the contours of the double
A3827_11a/b radio source are likely to be projections with P=0.21 and P=0.24
A3827_11a/b respectively. This is probably a distant FR II radio galaxy.
A3827_14    Within the radio contours are an St (24"@78{deg}) and
A3827_14    a G (12"@203{deg}). Their projection probabilities are  P=0.26
A3827_14    and P=0.08 respectively. The G is not bright enough for cluster
A3827_14    membership and neither object is an acceptable identification.
A3827_21    (P=0.009)  The faint G displaced 5" along the
A3827_21    major axis to the NNE of the radio centroid is the accepted
A3827_21    identification.  We discard the bright galaxy 16" to the SSE of
A3827_21    the radio centroid (2MASX J22015849-5943068) as the identification
A3827_21    for its separation from the radio centroid and for its significant
A3827_21    displacement from the major axis of the radio source.
A3827_24a/b The Sp is unlikely to be a projected object whether
A3827_24a/b identified with component b (P=0.002) or associated with the
A3827_24a/b centroid of the double (P=0.035). The identification in Table 3
A3827_24a/b is with component b, and is bright enough to be a cluster spiral.
A3827_26    The faint objects near the outer contour of this
A3827_26    extended radio source to the east and north of the radio centroid
A3827_26    are likely to be projections with P=0.54 and 0.50 respectively.
A3836_9a/b  Neither of the components of this apparent double are
A3836_9a/b  resolved at 2.38 GHz and no identification  can be detected. If
A3836_9a/b  it is a real double, it is probably a distant FR II radio galaxy.
A3836_17    The faint St object to the north of the radio centroid
A3836_17    is unlikely to be a projection (P=0.02), but its 7"  separation
A3836_17    from the centroid of the radio source and its offset from the
A3836_17    major axis are not consistent with an identification.
A3836_19a/b (P=0.11)  There is a possibility that the faint G
A3836_19a/b between the components is a projected object, but its proximity
A3836_19a/b to the major axis of the double improves the security of the
A3836_19a/b identification. It is not bright enough for a cluster elliptical.