  Our current knowledge of carbon stars in the Local Group and beyond, is
discussed. Although many carbon stars and late M-stars have been identified in
external galaxies a coherent understanding in terms of the chemical evolution-
and star formation rate-history of a galaxy is still largely lacking. Issues
that need to be addressed are: 1) for some of the larger galaxies only a small
fraction in area has been surveyed so far, 2) surveys have been conducted using
different techniques, and may be incomplete in bolometric magnitude, 3) only
for some galaxies is there information about the late M-star population, 4) not
all galaxies in the Local Group have been surveyed, 5) only for a sub-set of
stars are bolometric magnitudes available.
  From the existing observations one can derive the following: the formation of
carbon stars is both a function of metallicity and star-formation. In galaxies
with a similar star-formation rate history, there will be relatively more
carbon stars formed in the system with the lower metallicity. On the other
hand, the scarcity of AGB type carbon stars in some systems with the lowest
metallicity indicates that these galaxies have had a low, if any,
star-formation rate history over the last few Gyrs.
