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Table 1:

PN mimics removed from our PN sample. Columns R1 and R2 are the emission line ratios [OIII] $\lambda $4363/H$\gamma $ and [OIII] $\lambda $5007/H$\beta $, respectively (Gutiérrez-Moreno et al. 1995). NIR magnitudes are from 2MASS (Skrutskie et al. 2006).
PN G Name RA (J2000) Dec (J2000) R1 R2 J-H $H-K_{\rm s}$ $K_{\rm s}$ Remarks Ref.
006.1+04.1 - 17 44 10.6 -21 29 21 - - 1.24 1.91 11.10 Sy?,H,P (f)
356.1-02.1 PHR 1744-3319 17 44 51.8 -33 19 30 - - - - - Sy? (a)
355.5-02.8 MPA 1746-3412 17 46 18.5 -34 12 37 - - - - - Sy,A,OVI (b)
355.0-03.3 PPA 1746-3454 17 46 51.4 -34 54 05 0.76 0.94 1.96 2.04 11.45 Sy,A,H,OII (a)
359.5-01.3 JaSt 68 17 49 50.9 -30 03 10 - - - - - U,A (c)
000.0-01.1 JaSt 2-6 17 50 01.0 -29 33 25 - - 2.76 1.97 6.16 Sy?,N,OII,P (c), (d)
356.4-03.5 PHR 1751-3349 17 51 15.0 -33 49 11 - - 2.30 1.72 9.99 Sy?,A,N (b)
358.0-02.7 Al 2-O 17 51 45.4 -32 03 04 - 9.3 0.98 0.89 10.84 Sy?,P (i)
000.2-01.4 JaSt 79 17 51 53.5 -29 30 53 1.4 11.2 1.65 1.14 7.11 Sy,A,F,M (c)
354.8-04.6 PPA 1752-3542 17 52 05.9 -35 42 06 1.8 2.7 - - - Sy,P (a)
000.6-02.3 H 2-32 17 56 24.2 -29 38 07 - 0.1 0.38 0.86 12.57 Sy?,A,H,P (j)
356.2-05.1 K 5-37 17 57 15.7 -34 47 34 - - 0.09 1.82 11.86 Sy? (l)
001.0-02.6 Sa 3-104 17 58 25.9 -29 20 48 0.5 1.6 0.72 0.80 11.81 Sy,A,OII (h)
003.4-01.9 MPA 1801-2655 18 01 06.3 -26 55 59 0.7 1.2 1.19 0.62 8.02 Sy,A,H,M (b)
356.9-05.8 M 2-24 18 02 02.9 -34 27 47 1.4 3.7 1.78 1.83 9.31 Sy,N (e)
002.9-02.7 PHR 1803-2746 18 03 05.1 -27 46 44 3.0 8.1 - - - Sy,A (a)
003.0-02.8 PHR 1803-2748 18 03 31.2 -27 48 27 0.2 0.5 1.05 2.16 10.56 Sy,A,H,N,OVI (b)
001.2-03.9 ShWi 5 18 03 53.8 -29 51 22 1.5 9.4 0.60 0.60 11.90 Sy,A,F (g)
001.7-03.6 MPA 1804-2918 18 04 04.9 -29 18 46 0.1 0.2 0.88 0.34 7.78 Sy,A,H,M,OII (b)
001.7-03.8 ShWi 7 18 05 05.5 -29 20 15 0.2 4.2 0.67 -0.01 13.02 Sy?,A,N,OII (g)
003.9-02.8 PHR 1805-2659 18 05 43.5 -26 59 46 - - 0.50 0.42 10.96 F*,A,M (a)
004.0-03.0 M 2-29 18 06 40.8 -26 54 56 1.0 4.0 0.41 1.17 12.32 Sy?,H,N,OII,V (k)
004.1-03.0 PHR 1806-2652 18 06 56.0 -26 52 54 0.1 4.1 0.95 0.64 12.90 Sy,F,M,N,OII,OVI?,V (a)
359.7-05.5 PPA 1807-3158 18 07 19.7 -31 58 09 - - 0.41 1.69 12.31 Sy?,P (a)
004.1-03.3 PPA 1808-2700 18 08 01.4 -27 00 16 0.5 3.8 1.03 0.30 9.18 Sy,M,N,OII,V (a)
003.6-04.0 PHR 1809-2745 18 09 51.8 -27 45 54 - - 1.15 1.75 9.32 Sy?,OVI,P (a)
Remarks: Sy(?): Symbiotic star (suspected); F*: Flare star; U: Unlikely PN; A: AAOmega observations; F: [FeVII] $\lambda\lambda$5721, 6087 present; H: Broad H$\alpha $; M: Late-type features; N: Resolved Nebula; OII: OGLE-II coverage; OVI: OVI $\lambda $6830 present; P: Other MASH observations; V: FLAMES observations.
References: (a) Parker et al. (2006); (b) this work; (c) Jacoby & Van de Steene (2004); (d) Matsunaga et al. (2005); (e) Zhang & Liu (2003); (f) Górny (2006); (g) Shaw & Wirth (1985); (h) Sanduleak (1976); (i) Allen (1979); (j) Haro (1952); (k) Hajduk et al. (2008); (l) Kohoutek (2002).


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