SIMBAD references

The observed scatter of the lithium abundance around a "plateau" is revisited for three samples of stars for which the temperature has been determined from either the excitation temperature, or the dereddened color (b-y)_o or the profile of the H_αwings. Systematic differences are noted between the three methods of temperature determination. From sample to sample the rms observed scatter of the lithium abundance varies from 0.06dex to 0.08dex (to be compared to the value 0.13 previously found by Thorburn (1994), for another sample of stars). We show that in all cases but one, this scatter is fully explained by the temperature and equivalent width errors. The intrinsic scatter, if real, is small.