1 Detailed descriptions of individual identifications for PNe with comment 
 1  key 1 were given in Luo et al., 2005, Cat. J/ApJS/159/282
 2 G000.0-01.3 (PPA1751-2933; Fig. A2): faint, oval nebula, designated as 
 2  'likely' PN. The optical angular diameter is ~12" while the faint 
 2  radio source appears to be more extended.
 3 G004.8-01.1 (PHR1801-2522; Fig. A2): confirmed, compact PN, very bright 
 3  at 1.4GHz (~67mJy). Faint wings are very likely image artefacts and not 
 3  associated with the nebula.
 4 G010.0-01.5 (PHR1813-2057; Fig. A2): confirmed, bright, oval and compact PN 
 4  with possible ansae and MSX detection in all four bands. The faint radio 
 4  extension to the south (~4mJy) is very likely not associated with the nebula
 5 G025.9+03.4 (PHR1826-0435; Fig. A2): faint, slightly oval, true PN with 
 5  enhanced opposing lobes and bipolar core. Optical angular diameter 
 5  (~20") is a factor of 2 smaller than FWHM of the NVSS restoring beam. 
 5  Thus, the radio 'wing' is probably a background source.
 6 G026.4+02.7 (PHR1829-0431; Fig. A2): small (~20"), faint, semi-circular
 6  nebula with bipolar core designated as a true PN. The radio 'wing', 
 6  extending to the south of the nebulosity, is not visible in available 
 6  optical bands and it is very likely a faint background source.
 7 G034.1-01.6 (MPA1859+0017; Fig. A2): faint and compact (~10") confirmed
 7  PN. Radio source, located ~90" from the radio detection, appears 
 7  slightly extended but not correlated to this PN.
 8 G322.4-00.1a (MPA1523-5710; Fig. A2): confirmed bipolar PN from the MASH-II 
 8  supplement super-imposed over the shell of the nearby supernova remnant 
 8  (SNR) G322.5-00.1 discovered in the MOST survey of the southern Galactic 
 8  plane (Whiteoak, 1992MNRAS.256..121W). The southern radio extension is 
 8  a part of the SNR shell and it is not correlated to this PN. However, the 
 8  fitted flux could be overestimated as a result of the underlying large-scale
 8  structure.
 9 G332.3-00.9 (PHR1619-5131; Fig. A2): while the coincidence of the optical 
 9  position from the MASH with the radio excess in the SUMSS/MGPS-2 radio image
 9  looks quite convincing we did not find a radio counterpart in the MGPS-2 
 9  catalogue. Thus, this PN is designated with suspect radio identification. 
 9  The measured flux density of 13.7mJy is well above the usual rms noise 
 9  of 1.0mJy/beam. However, the local rms noise (or the large-scale 
 9  structures) in the vicinity of this PN is significantly above the average 
 9  (~4mJy/beam).
10 G352.6+02.2 (PPA1717-3349; Fig. A3): a compact optical nebula 
10  ({theta}opt<10"), designated as a 'likely' PN. The nearby extended 
10  radio source has a positional association with the IRAS source 17146-3344. 
10  The ratio between IRAS fluxes at 12 and 25um is 1.3, which implies 
10  association with an OH/IR star. The extended source is relatively faint 
10  (S1.4GHz<15mJy) so the confusion of this PN is probably only a mild one.
11 G354.6-01.4 (PPA1737-3414; Fig. A3): the radio flux (~7mJy) from the compact 
11  ({theta}opt~~ 6") true PN is probably highly confused from the much 
11  brighter, and very likely unrelated, nearby object (S1.4GHz=177mJy).
12 G355.8+01.7 (MPA1728-3132; Fig. A3): confirmed planetary nebula from the 
12  MASH-II supplement. Optical size of the nebula is 4". The position of 
12  the correlated NVSS radio peak is ~6" away from the estimated optical 
12  position. Also, the radio source appears to be relatively extended. This 
12  implies that the angular size of this PN could be much larger than seen 
12  in H{alpha}.
13 G356.5-01.8 (PPA1744-3252; Fig. A3): possible PN. The radio-continuum flux 
13  (~6mJy) from the compact ({theta}opt~~6") nebula is probably only 
13  mildly confused from the nearby, stronger, radio source 
13  (174423-325116; S1.4GHz=31mJy).
14 G000.3-01.6 (PHR1752-2930; Fig. A3): compact ({theta}opt~~8"), true PN close 
14  to star. Radio detected by Van de Steene & Jacoby (2001, Cat. J/A+A/373/536)
14  with measured flux densities at 6  and 3cm of 8.5  and 2.5mJy, 
14  respectively. Also cross-correlated with NVSS source 175252-293000 with flux
14  density of 4.1mJy. The confusion with a nearby, radio brighter 
14  (~40mJy at 1.4GHz) NVSS radio source 175256-293044 is possible.
15 G302.3-00.5 (PHR1246-6324; Fig. A3): small bipolar PN, clearly visible in the
15  radio. The radio source is centred on the PN and shows possible extended 
15  structure in a direction opposite to possible bipolar outflows. It is not 
15  clear if this structure is related to the PN or is it a faint background 
15  source.
16 G291.6-00.2 (PHR1115-6059; Fig. A4): bright, large (~100"), circular nebula 
16  designated as 'likely' PN. Radio detection at 0.843GHz appears to be 
16  associated with the H{alpha} bright NW edge. Estimated flux density is 
16  flagged as the low limit due to the marginal detection.
17 G337.4+02.6 (PHR1625-4522; Fig. A4): very large, diffuse nebula designated as
17  a 'likely' PN in MASH. The radio counterpart (not catalogued in the MGPS-2) 
17  is a faint 'patch' of extended emission placed over the brighter nebular 
17  region. Estimated flux density is flagged as the low limit.
18 G356.6-01.9 (PHR1745-3246; Fig. A4): confirmed, slightly extended PN with 
18  central concentration with a radio counterpart catalogued in the MGPS-2. 
18  From Fig. A4 can be seen that radio peak is slightly offset from the 
18  brightest part of nebulosity. Apparent extension in the SN direction is an 
18  effect of the beam elongation due to the low declination.
19 G013.3+01.1 (PHR1810-1647; Fig. A4): slightly oval, confirmed PN, with 
19  prominent internal structure. The NVSS detection peaks over the brightest 
19  part of the possible shell. Estimated flux density is flagged as the low 
19  limit due to the marginal detection.
20 G222.5+07.6 (BMP0736-0500; Fig. A5): relatively large (~80"), extremely faint
20  elliptical PN. The suspect radio detection from the NVSS is placed on the 
20  brighter part of the nebula.
21 G247.5-04.7 (PHR0742-3247; Fig. A5): large, elliptical, diffuse PN. The NVSS 
21  detection is suspected (barely above 1{sigma} rms local noise level) and 
21  coincides with the brightest parts of the shell.
22 G254.5-02.7 (PHR0808-3745; Fig. A5): large, diffuse nebula designated as 
22  'likely' PN. The NVSS suspect radio detection is placed on the brighter 
22  part of the nebula.
23 G297.0-04.9 (PHR1150-6704; Fig. A5): S-bar shaped, confirmed PN, with 
23  internal knots. Radio detection (MGPS-2) is suspect due to the relatively 
23  large offset from the H{alpha} bright region. However, it is important to 
23  emphasize the similarity with position and extent of radio-peak offset seen 
23  in PHR1739-3829.
24 G309.5+00.8 (PHR1346-6116; Fig. A5): partial arcuate nebula with sharp 
24  western edge, designated as 'likely' PN. A faint radio source found in 
24  MGPS-2 (not catalogued) is placed over the fainter region and it is 
24  considered as suspect.
25 G324.3+01.1 (PHR1529-5458; Fig. A5): possible PN, with strongly elongated, 
25  irregular emission and with possible superposed arcuate nebula. The 
25  associated radio source from MGPS-2 is extended and approximately follows 
25  the brightness distribution of H{alpha} emission. However, as can be seen 
25  from the presented histogram equalized quotient image, the radio peak is 
25  placed over the low H{alpha} emission region. The nebula is approximately 
25  twice the size of the MOST synthesized beam FWHM.
26 G332.3+07.0 (PHR1547-4533; Fig. A5): very faint, circular nebula designated 
26  as a 'likely' PN in MASH. The radio detection at 0.843GHz appears extended 
26  but covers only the inner (fainter) part of the nebula.
27 G351.1-03.9 (PHR1739-3829; Fig. A5): bright, bipolar, confirmed PN. As in the
27  case of PHR1748-3538, the radio emission at 1.4GHz appears to be generally 
27  correlated with the H{alpha} but with a radio peak ~20" from the brightest 
27  parts of the nebula. In contrast to of the PHR1748-3538, the radio 'wings' 
27  are, in this case, in the direction of possible bipolar outflows. It is 
27  flagged as a suspect radio detection.
28 G354.5-03.9 (PHR1748-3538; Fig. A5): oval ring PN with faint outer 
28  extensions, designated as a true PN with optical dimensions 56x39". As 
28  stated in Luo et al., 2005, Cat. J/ApJS/159/282, the bright radio peak is 
28  about 60" away from the optical centroid. A bright offset radio source is 
28  catalogued in NVSS as a possible complex object 174818-35375 with a flux 
28  density estimate of S1.4GHz=44.4+/-1.8mJy. The flux density of the nebula 
28  itself is estimated to be S1.4GHz=3.2+/-0.6mJy. Fig. A5 (left-hand panel in 
28  the bottom row) shows the histogram equalized quotient image overlaid with 
28  contours from the 1.4GHz NVSS image. A bright, ring-like structure is 
28  visible, with possible bipolar outflows. While the radio emission is 
28  extended in the direction of the bright region of nebulosity, the radio peak
28  does not appear to be correlated with H{alpha} emission. We also found a 
28  nearby bright radio source in cross-correlation with the MGPS-2 catalogue. 
28  It peaks at a similar position to the NVSS bright source with a flux density
28  at 0.843GHz of 70.8+/-2.6mJy. The spectral index ({alpha}~~-0.8) of this 
28  object clearly points out to the non-thermal origin. Thus, we can definitely
28  conclude non-association with the PN. Unfortunately, the mosaic containing 
28  this region (J1742M36) was not available, and we have not been able to 
28  examine if similar extended emission, seen at 1.4GHz, exists at 0.843GHz. A 
28  faint radio source, to the left of the nebulosity, also does not appear to 
28  be associated with this PN.
29 G015.5+02.8 (BMP1808-1406; Fig. A5): very large (~470"), confirmed elliptical
29  PN with enhanced opposing edges. The detection of the NVSS source placed 
29  over the bright SW H{alpha} emission region is flagged as a suspect and, 
29  regarding very low surface brightness of this PN, it is very likely that it 
29  is due to chance coincidence.