Table 4: Line-of-sight properties for the observed post-AGB stars.
Name E(B-V) d Ref. E(B-V)IS $d_{\rm max}$ E(B-V)IS E(B-V)-CS DCS / HV
  observed kpc     kpc scaling no scaling min  
01005+7910 0.2 $\pm$ 0.1 3   0.11 1.7 0.11      
02229+6208 1.67 $\pm$ 0.09 >2.2   0.60 5 0.99   0.68 CS2
04296+3429 1.3 $\pm$ 0.1 3.5   0.23 3.3 0.23   1.07 CS1
    5.4, 5 2, 9 0.23          
05113+1347 1.1 $\pm$ 0.2 5 9 0.14 2.1 0.14   0.96 CS1
05251-1244 0.23 $\pm$ 0.09       1 0.18      
05341+0852 1.65 $\pm$ 0.09 10 9 0.16 2.4 0.16   1.49 CS1
06530-0213 1.7 $\pm$ 0.2 3 9 0.36 5 0.41   1.29 CS2
07134+1005 0.4 $\pm$ 0.1       2.8 0.024 0.14 0.38 / 0.26 HV / CS2
08005-2356 0.7 $\pm$ 0.3       4 0.18 0.27 0.52 / 0.43 CS2
08143-4406 0.8 $\pm$ 0.1 4 9 0.55 5.8 0.66      
08544-4431 1.45 $\pm$ 0.09       6 0.99   0.46 CS2?
12175-5338 0.25 $\pm$ 0.09       3 0.24      
16594-4656 2.2 $\pm$ 0.3 2.6 10, 11   7 2.1     CS (*)
17086-2403 0.86 $\pm$ 0.09 6 9 0.56 2 0.56   0.3 HV (CS2?)
17097-3210 0.06 $\pm$ 0.05 (0.2)   (0.08) 5 0.95      
17150-3224 0.68 $\pm$ 0.09 <18 (2) 9 (0.9) 5 1.8      
17245-3951 1.0 $\pm$ 0.1       5 1.0 1.5   HV
17395-0841 1.1 $\pm$ 0.2       2 0.87   0.23 HV
17423-1755 1.13 $\pm$ 0.09 3.2-3.7   0.6 4 0.60   0.53 CS1 / HV
17436+5003 0.24 $\pm$ 0.09 1.2   0.03 0.9 0.026 0.064 0.18 CS1
18025-3906 1.15 $\pm$ 0.09       2 0.23 0.34 0.92 / 0.81 CS1 / HV
18062+2410 0.6 $\pm$ 0.2 4.5-5.3   0.14 1.4 0.14   0.46 CS1 / HV
HD 172324 0.03 $\pm$ 0.02       1.5 0.056 0.11    
19114+0002 0.60 $\pm$ 0.05 1.5 4 0.32 5 0.54 0.62   HV
19200+3457 0.3 $\pm$ 0.1       2.9 0.15 0.22    
19386+0155 1.05 $\pm$ 0.09       2.9 0.35   0.80 CS1
19500-1709 0.37 $\pm$ 0.09 >4 12   1.0 0.20      
20000+3239 1.6 $\pm$ 0.1 (5, 8)   (1.0, 1.7) >10 >1.7   ?  
20462+3416 0.38 $\pm$ 0.09       4 0.25 0.38   HV
22023+5249 0.52 $\pm$ 0.09 3.3-3.9   0.47, 0.50 5 0.52 0.55   HV
22223+4327 0.2 $\pm$ 0.1       2.6 0.21      
22272+5435 0.9 $\pm$ 0.2 1.6, 2.7 8 0.26, 0.39 4.5 0.47   0.43 CS2
23304+6147 1.4 $\pm$ 0.2 4.7, 5 5, 9 0.64 4.5 0.64   0.76 CS2

DCS = dominated by circumstellar reddening; HV = high radial velocity; CS1 designated DCS based on lat/long vs. reddening, excluding those that are discarded based on interstellar (IS) reddening estimate. CS2 indicates DCS found by estimating the upper limit to the IS reddening.
[1] Reddy et al. (1999); [2] Klochkova et al. (1999); [3] García-Lario et al. (1999); [4] Zacs et al. (1999a,b); [5] Klochkova et al. (2000); [6] Bakker et al. (1997); [7] Hrivnak & Kwok 1991; [8] Woodsworth et al. (1990); [9] Reddy & Parthasarathy (1996); [10] Hrivnak et al. (2000); [11] van de Steene & van Hoof (2003); [12] Clube & Gledhill (2004), A(V)=1.2. (*) IRAS 16594-4656 is a well known bi-polar PPN which is thought to have a high internal extinction (see also Sect. 4.3).

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