All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1904f1.ps} \end{figure}$ Figure 1: Near-IR CMD of SMC stars from 2MASS within the observed MACHO fields (dots). The C-stars region is marked by two perpendicular dashed lines: C-stars with $J-K_{\rm s} \leq 2$ mag are indicated with blue circles; red triangles refer to obscured AGB stars ( $J-K_{\rm s}>2$ mag). The position of the RGB-tip is also indicated. In the upper right corner we show the number of sources with $K_{\rm s}\leq 12$ vs. $J-K_{\rm s}$ colour; note that the branch of C-stars is well separated. See the electronic edition of the Journal for a colour version of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm]{1904f2.ps} \end{figure}$ Figure 2: J-H vs. $H-K_{\rm s}$ diagram of SMC stars within the MACHO fields with $K_{\rm s} < 14$ mag. The dashed line corresponds to $J-K_{\rm s}=1.33$ mag. Symbols are as in Fig. 1. See the electronic edition of the Journal for a colour version of the figure.
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In the text

$\begin{figure} \par\includegraphics[height=5.2cm,width=5.1cm,clip]{1904f3a.ps}\h... ...*{6mm} \includegraphics[height=5.2cm,width=5.1cm,clip]{1904f3c.ps} \end{figure}$ Figure 3: Panel a): absolute distance between 2MASS and RAW93 stars in the ${\rm MC}^2$ catalogue. Panel b): $K_{\rm s}$ vs. $J-K_{\rm s}$ CMD of all SMC stars in the MACHO field (small black dots). C-stars included in the RAW93 catalogue and within the MACHO fields are plotted as red squares. Blue crosses represent the sample of photometrically selected C-stars. Near-IR photometry comes from the 2MASS survey. Panel c): histogram of C-stars in our photometrically selected sample (empty) and in the RAW93 catalogue (dashed). See the electronic edition of the Journal for a colour version of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1904f4.ps} \end{figure}$ Figure 4: Locations of C-stars in the observed SMC MACHO fields (6 large squares each indicated by its MACHO field number). Small black dots are all photometrically selected C-stars in the SMC; blue crosses refer to C-stars with $\vert d_{{\rm MACHO}} - d_{{\rm 2MASS}} \vert \leq 3$ $^{\prime \prime }$ . Small red squares are C-stars from the RAW93 catalogue cross-correlated with the ${\rm MC}^2$ catalogue. See the electronic edition of the Journal for a colour version of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1904f5.ps} \end{figure}$ Figure 5: Histogram of the absolute distance between 2MASS sources and their MACHO counterparts. The dashed line is drawn at 3 $^{\prime \prime }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1904f6.ps} \end{figure}$ Figure 6: Comparison between the period and amplitude derived in this work and those from Cioni et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{1904f7.ps} \end{figure}$ Figure 7: Comparison between the period and amplitude derived in this work and those from Ita et al. (2004b) and G04.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1904f8.ps} \end{figure}$ Figure 8: $\langle K_{\rm s} \rangle _0$ vs. $\log P$ relation for all C-stars in the sample (small black dots). Large dots are first periods (P₁) for stars with $flag(2)\le 2$ and flag(3)=1; blue open squares P₁ for stars with $flag(2)\le 2$ and flag(3)=2 and 3; red crosses correspond to the second period (P₂) of stars indicated by squares. The $\langle K_{\rm s} \rangle _0$ magnitude is the average of DENIS and 2MASS measurements, dereddened as explained in the text. Letters identify the parallel sequences as defined by Wood et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1904f9.ps} \end{figure}$ Figure 9: Histogram of all the periods found for $B_{\rm M}$ light-curves, though for $R_{\rm M}$ light-curves results are very similar. The empty histogram shows the distribution of P₁ and the shaded histogram of P₂. Letters indicate sequences as in Wood et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1904f10.ps} \end{figure}$ Figure 10: The ratio between the longer to the shorter period versus the longer period. Black-filled circles represent stars with P₁>P₂, while red open squares sources with P₁<P₂. In the upper left corner we show an enlargement of the lowest ratios.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{1904f11.ps} \end{figure}$ Figure 11: Period distribution as a function of amplitude in the two MACHO photometric bands.
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In the text

$\begin{figure} \center \includegraphics[width=8.2cm,clip]{1904f12.ps} \end{figure}$ Figure 12: Period distribution ( $\log(P_1)$ ) of stars with $0.05\leq A_{{\rm phot}}(B_{\rm M})\leq 0.2$ (empty) and $A_{{\rm phot}}(B_{\rm M})> 0.2$ (shaded).
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{1904f13.ps} \end{figure}$ Figure 13: $(J-K_{\rm s})_0$ vs. the $B_{\rm M}$ -band amplitude a) and vs. $\log~(P_1)$ b) for all C-stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1904f14.ps} \end{figure}$ Figure 14: Distribution of the number of sources populating each $\it BCD$ sequence versus $K_{\rm s}$ magnitude and versus $J-K_{\rm s}$ colour. The empty histogram indicates the first period (P₁) and the shaded histogram the second period (P₂).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1904f15.ps} \end{figure}$ Figure 15: $M_{{\rm bol}}$ vs. $\log P$ relation for all stars in the sample and overplotted theoretical tracks by Vassiliadis & Wood (1993). Green triangles indicate stars with $(J-K_{\rm s})_0 > 2.1$ and $flag(2)\leq 2$ , while other symbols are as in Fig. 8. Masses are indicated on the right hand side of each track. See the electronic edition of the Journal for a colour version of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1904fA1.ps} \end{figure}$ Figure A.1: Examples of light-curves with different values of the data-quality flag(1). Data with photometric errors $0.05 \leq \sigma _{\rm X} < 0.1$ are plotted as black dots; data with $0.01 \leq \sigma _{\rm X} < 0.05$ are plotted as red squares; and data with $\sigma _{\rm X} < 0.01$ as green crosses. Left ( right) panels illustrate $B_{\rm M}$ ( $R_{\rm M}$ ) photometry. See the electronic edition of the Journal for a colour version of the figure.

In the text

$\begin{figure} \par\includegraphics[width=17.25cm,clip]{1904fA2.ps} \par\end{figure}$ Figure A.2: Examples of light-curves with different values of flag(2). Left ( right) panels illustrate $B_{\rm M}$ ( $R_{\rm M}$ ) photometry. For each band we show the periodogram and the light-curve in the phase and time domain. See the electronic edition of the Journal for a colour version of the figure.

In the text

$\begin{figure} \par\includegraphics[width=17.25cm,clip]{1904fA3.ps} \end{figure}$ Figure A.3: As in Fig. A.2, but for flag(3).

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1904fA4.ps} \end{figure}$ Figure A.4: Histogram of the power of the first period ( $B_{\rm M}$ -light curves) as a function of the defined fit-quality flag. The relative number of stars is indicated in each panel.

In the text

$\begin{figure} \center \includegraphics[width=8cm,clip]{1904fA5.ps} \end{figure}$ Figure A.5: Distributions of the first period ( $B_{\rm M}$ -light-curves) as a function of the power value ( left panels) and flag(2) ( right panels).

In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1904fA6.ps} \end{figure}$ Figure A.6: Relation between the first periods derived from $B_{\rm M}$ and $R_{\rm M}$ light-curves.

In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1904fA7.ps} \end{figure}$ Figure A.7: Panel a, b): The residual $(A_{{\rm phot}}-A_{{\rm fit}})$ is plotted against $A_{{\rm phot}}$ . Panel c, d): Histogram of the amplitude is reported for $B_{\rm M}$ c) and $R_{\rm M}$ d) magnitudes. Panel e): Difference between amplitude from $R_{\rm M}$ - and $B_{\rm M}$ -light curves. Only stars with flag(2)<3 are shown.

In the text

$\begin{figure} \par\includegraphics[width=8.25cm]{1904f2.ps} \end{figure}$	Figure 2: J-H vs. $H-K_{\rm s}$ diagram of SMC stars within the MACHO fields with $K_{\rm s} < 14$ mag. The dashed line corresponds to $J-K_{\rm s}=1.33$ mag. Symbols are as in Fig. 1. See the electronic edition of the Journal for a colour version of the figure.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1904f5.ps} \end{figure}$	Figure 5: Histogram of the absolute distance between 2MASS sources and their MACHO counterparts. The dashed line is drawn at 3 $^{\prime \prime }$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1904f6.ps} \end{figure}$	Figure 6: Comparison between the period and amplitude derived in this work and those from Cioni et al. (2003).
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{1904f7.ps} \end{figure}$	Figure 7: Comparison between the period and amplitude derived in this work and those from Ita et al. (2004b) and G04.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1904f9.ps} \end{figure}$	Figure 9: Histogram of all the periods found for $B_{\rm M}$ light-curves, though for $R_{\rm M}$ light-curves results are very similar. The empty histogram shows the distribution of P₁ and the shaded histogram of P₂. Letters indicate sequences as in Wood et al. (1999).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1904f10.ps} \end{figure}$	Figure 10: The ratio between the longer to the shorter period versus the longer period. Black-filled circles represent stars with P₁>P₂, while red open squares sources with P₁<P₂. In the upper left corner we show an enlargement of the lowest ratios.
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{1904f11.ps} \end{figure}$	Figure 11: Period distribution as a function of amplitude in the two MACHO photometric bands.
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$\begin{figure} \center \includegraphics[width=8.2cm,clip]{1904f12.ps} \end{figure}$	Figure 12: Period distribution ( $\log(P_1)$ ) of stars with $0.05\leq A_{{\rm phot}}(B_{\rm M})\leq 0.2$ (empty) and $A_{{\rm phot}}(B_{\rm M})> 0.2$ (shaded).
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{1904f13.ps} \end{figure}$	Figure 13: $(J-K_{\rm s})_0$ vs. the $B_{\rm M}$ -band amplitude a) and vs. $\log~(P_1)$ b) for all C-stars.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1904f14.ps} \end{figure}$	Figure 14: Distribution of the number of sources populating each $\it BCD$ sequence versus $K_{\rm s}$ magnitude and versus $J-K_{\rm s}$ colour. The empty histogram indicates the first period (P₁) and the shaded histogram the second period (P₂).
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