Astronomy & astrophysics supplement series vol:87 issue:2 pages:361-382
In this paper the properties of a group of stars is examined, that are selected on the basis of the properties of two known post-AGB stars, HR 4049 and HD 213985. It is shown that the stars from this sample that probably are post-AGB stars all show IR excess. This excess can be due to hot (T almost-equal-to 1000 K), cool (T almost-equal-to 300 K) or hot and cool dust. The stars showing the hot dust all have mass loss rates that are substantially larger than the mass loss rates of the stars showing only cool dust. This indicates that mass loss continues after the AGB at a substantial rate (about 10(-7) M./yr). Selection criteria are given on the basis of which post-AGB stars can be selected from the literature.