Table 1: Hot post-AGB stars.
Star No. IRAS Name Optical l b IRAS fluxes (Jy.)
      Sp. type     12 $\mu $ 25 $\mu $ 60 $\mu $ 100 $\mu $
1. 12584-4837 Hen3-847 Be1 304.60 +13.95 36.07 48.75 13.04 3.31
2. 13266-5551 -55 5588 B1Ibe 308.30 +6.36 0.76 35.90 35.43 11.66
3. 14331-6435 Hen3-1013 B3Ie 313.89 -4.20 4.04 108.70 70.71 20.61
4. 16206-5956 SAO 243756 A0Ia2 326.77 -7.49 0.36L 11.04 12.30 4.83
5. 17203-1534   B1IIIpe 8.55 +11.49 0.32 10.70 6.88 3.37
6. 17311-4924 Hen3-1428 B1IIe 341.41 -9.04 18.34 150.70 58.74 17.78
7. 17423-1755 Hen3-1475 Be 9.36 +5.78 7.05 28.31 63.68 33.43
8. 17460-3114 SAO 209306 O8III 358.42 -1.88 6.26 20.82 12.20 220.40L
9. 18023-3409 LSS 4634 B2IIIe 357.61 -6.31 0.26L 2.94 1.82 25.64L
10. 18062+2410 SAO 85766 B1I3 50.67 +19.79 3.98 19.62 2.90 1.00L
11. 18371-3159 LSE 63 B1Iabe 2.92 -11.82 0.25L 6.31 5.16 1.95
12. 18379-1707 LSS 5112 B1IIIpe 16.50 -5.42 1.67 23.76 7.12 3.66L
13. 19590-1249 LSIV-12 111 B1Ibe 29.18 -21.26 0.29: 10.26 6.45 1.77:
14. 22023+5249 LSIII +5224 B4 99.30 -1.96 1.02 24.69 14.52 3.93L
15. 22495+5134 LSIII +5142 PN5 104.84 -6.77 0.54 12.37 7.18 3.12
A colon : indicates moderate quality IRAS flux, L is for an upper limit.
The spectral types are from Parthasarathy et al. (2000a) except 1 Kazarovets et al. (2000); 2 Schild et al. (1983); 3 Parthasarathy et al. (2000b); 4 Simbad database; 5 Acker et al. (1992).


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