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Complete samples of 2MASS stars in 3 fields of differing metallicities (andpossibly differing age distributions) have been extracted and cross-correlatedwith MACHO and ISO data to determine their variability and mass-lossproperties. In each M_K histogram a fall-off in numbers is seen above the tipof the RGB. The luminosity of the tip increases with metallicity as does theaverage J-K at given M_K. The proportion of stars with high H-K increases atlower metallicities. This results from the increasing proportion of C stars.All 3 fields contain similar types of variables, mainly short-period, Mira-likeand double-period (having long and short periods). The proportion of variablestars decreases at lower metallicities and the minimum period associated with agiven amplitude gets longer. Various trends are seen in the K, log P diagramsof each field. The Magellanic Cloud fields largely resemble each other but theBulge field is noticeably different. The stars that follow the 'A' K,log Prelation in the Bulge hardly extend beyond the M giant tip and the other groupsalso appear truncated in M_K relative to their Magellanic Cloud counterparts.In the Clouds there are many stars with periods around 200-300d that follow the'C' or Mira relation but have relatively small amplitudes. The mid-IR sampledetected by ISOCAM during the Magellanic Cloud Mini-Survey appears to bereliable and complete for sources with M_K more luminous than -7 mag, i.e., forthose close to the top of the AGB. The various colour-colour andcolour-magnitude diagrams reflect the increasing dominance of C stars at lowmetallicity. Mira magnitude vs log P relations exist up to at least 7 microns.Mass-loss from longer-period and double-period SRVs occurs at similar rates ineach field, despite differences in metallicity.Comment: 14 pages, 16 figures, A&A accepted, better resolution available from  ftp://ftp.saao.ac.za/pub/is

Late-type giant variables in NGC 6522, LMC and SMC. How do they differ?