\begin{table}%T1
      \caption{\label{tab:mimic}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 (Guti\'errez-Moreno et~al. 1995). NIR magnitudes are from 2MASS (Skrutskie et~al. \cite{Skrutskie2006}).    }
      \small%\centerline
{
   \begin{tabular}{llllrrrrrll}
      \hline\hline
      PN G& Name & RA (J2000) & Dec (J2000) & $R1$ & $R2$ & $J-H$ & $H-K_{\rm s}$ & $K_{\rm s}$ & Remarks & Ref.\\ 
      \hline
  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 & $-$27 45 54     & --&-- & 1.15 & 1.75 & 9.32            & Sy?,OVI,P     & (a)     \\            
   \hline
   \end{tabular}}
   \smallskip
      \emph{Remarks}:    Sy(?): Symbiotic star (suspected); F$*$: 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.\\
      \emph{References}: 
      (a)~Parker et~al. (\cite{Parker2006}); (b)~this work; (c)~Jacoby \& Van de Steene (\cite{Jacoby2004}); (d)~Matsunaga et~al. (\cite{Matsunaga2005});
      (e)~Zhang \& Liu (\cite{Zhang2003}); (f)~G\'orny (2006); (g)~Shaw \& Wirth (\cite{Shaw1985}); (h)~Sanduleak (\cite{Sanduleak1976}); (i)~Allen (\cite{Allen1979});
      (j)~Haro (\cite{Haro1952}); (k)~Hajduk et~al. (\cite{Hajduk2008}); (l)~Kohoutek (\cite{Kohoutek2002}).
\par
   \end{table}