All Figures

	Figure 1: Location of the fields observed by ISO (continuous line) and MACHO (dashed line) in the SMC. The ISO fields lie in the bar of the galaxy and are each in size. Both right ascension (RA) and declination (DEC) are in degrees.
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In the text

	Figure 2: Histogram of the absolute distance between the 2MASS counterpart of an ISO-MCMS source and the corresponding MACHO source.
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In the text

Figure 3: Diagrams for the sources in the sample with a MACHO-RED light-curve and f=1 or f=6. a) KS versus relation. Letters ABCD identify the parallel sequences as defined in Wood et al. (1999). Filled symbols indicate probable C-rich objects. b) PLRs and overplotted theoretical tracks by Vassiliadis & Wood (1993). The numbers indicate the initial mass of the stars in each track. c) Amplitude distribution as a function of bolometric magnitude. d) PLRs for sources with an amplitude above the dashed line indicated in c), q>100 and f=1. The continuous line is the Mira PLR fitted through the crosses corresponding to P<420 days obtained by Feast et al. (1989); a distance modulus of m-M=18.99 (Cioni et al. 2000) has been applied. Symbols identify O-rich stars (open circles), C-rich stars (filled circles) and Feast et al. (1989) variables (crosses).

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In the text

	Figure 4: Variable O- and C-rich AGB stars a). The histogram of the amplitude of variation b) and that of the period distribution c) are shown for sources of both types. The amplitude as a function of period is shown in d).
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In the text

Figure 5: Colour-magnitude diagrams (J-KS, KS) for variable stars classified as Mira a), SRa b) and SRb c) according to their periodicity and amplitude of variation. d) is the same diagram for variable sources which could not be classified in one of the three categories because of low S/N or an extremely irregular light-curve. The vertical dotted line indicates the separation between O-rich and C-rich stars as in Fig. 3.

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In the text

	Figure 6: Colour-magnitude diagrams (KS-LW10, LW10) for the same groups of sources as in Fig. 5.
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In the text

	Figure 7: Colour-colour diagrams (KS-LW2, LW2-LW10) for the same groups of sources as in Fig. 5.
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In the text

	Figure 8: Histogram of the differences between the 2MASS and DCMC magnitudes of all the sources in the sample.
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In the text

Figure B.1: The bolometric correction BCI as a function of the I-J colour for the O-rich (open circles) and C-rich (filled circles) variable stars in the sample. The continuous line is the relation derived by Alvarez et al. (2000) for cool O-rich stars.


In the text

Figure B.2: The bolometric correction BCK as a function of the J-KS colour for the O-rich (empty circles) and C-rich (filled circles) variable stars in the sample. The lines are the relations derived by Montegriffo et al. (1998) for Population II giants of low (dashed line) and high metallicity (continuous line).


In the text