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Figure 1: Difference in photometry, after the following offsets have been applied: I(denis-ogle) = -0.018, J(denis-2mass) = -0.090, K(denis-2mass) = -0.14. Stars with an I-band amplitude < 0.05 mag are used in the analysis. Plotted are about 12 000, 8700, and 5700 stars, top to bottom. |
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Figure 2: First entries of electronically available figure with all lightcurves. The fit is indicated by the (red) solid line. Crosses indicate data points not included in the fit. |
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Figure 3:
K-band PL-relation, for the SMC ( left) and LMC ( right). Panels
indicate selection on I-band amplitude. Carbon stars are indicated
by filled circles, M- and S-stars by open circels. All periods from
Table 2 that fulfil
|
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Figure 3: continued. |
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Figure 4:
Histograms of the LMC K-band 2MASS magnitude distribution for different "boxes'' and I-band amplitude cuts. The histograms for the M-stars (vertical lines), C-stars (hatched), and total are shown. The luminosity function for sequence "D'' is likely to be incomplete for
|
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Figure 5: As Fig. 4 for the SMC. |
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Figure 6: Amplitudes versus periods for the LMC ( left) and SMC ( right) variables. Symbols as in Fig. 3. |
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Figure 7: Colour-Period diagram for the LMC ( top left and top right) and SMC ( bottom left and bottom right) objects. The period with the largest amplitude is plotted. Symbols as in Fig. 3. |
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Figure 8: K-band PL-relation for the (LMC) stars that have undergone a period change over the past two decades of at least 0.1 dex. Historical and current period are connected by a line, with the current period marked by a solid circle. |
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Figure 9: Representative lightcurves of stars that have changed pulsation mode over the last 2 decades. The fit is indicated by the (red) solid line. Crosses indicate data points not included in the fit. Complete figure is available in the electronic form at EDP Sciences. |
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Figure 10:
Distribution function of the ratio of the historical to the current
period near a value of unity. The mean of all values is 1.00179. The
solid line is a Gaussian fit with a |
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Figure 11:
Distribution function of the ratio of the fundamental ( top panels) and
first overtone ( bottom panels) pulsation period over a 17 year
timespan, on a linear (left-hand side), and logarithmic
(right-hand side) scale for a 2 |
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Figure 12: LMC ( top 2 rows) and SMC ( bottom 2 rows) colour-colour diagrams using 2MASS and DENIS photometry for the spectroscopically selected sample ( left 2 columns) and the infrared selected sample ( right 2 columns). Note the difference in scale! Symbols as in Fig. 3, with dots indicating objects without spectroscopic classification. |
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Figure 13: Lightcurves of the reddest stars in (J-K). Note the faintness in I. Nine of the 15 stars have been detected in the MSX survey. Complete figure is available in electronic form at EDP Sciences. |
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Figure 14: K-band PL-relation for the large amplitude variables in the IR selected sample, for the SMC ( left) and LMC ( right). |
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Figure 15:
SED of one of the stars in the IR selected sample, MSX 83 annex
OGLE050854.21-690046.4. Plotted are the OGLE I, 2MASS JHK, MSX Aband and IRAS 12 and 25 |
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Figure 16: Period distribution of the LMC ( left panel) and SMC ( right panel) variables in box "C'' with I-band amplitudes larger than 0.15 mag. Shown are the histograms for the M-stars (vertical lines), C-stars (hatched), and total. |
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Figure 2: First entries of electronically available figure with all lightcurves. The fit is indicated by the (red) solid line. Crosses indicate data points not included in the fit. |
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Figure 2: continued. |
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Figure 2: continued. |
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Figure 9: Representative lightcurves of stars that have changed pulsation mode over the last 2 decades. The fit is indicated by the (red) solid line. Crosses indicate data points not included in the fit. Complete figure is available in the electronic form at EDP. |
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Figure 9: continued. |
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Figure 13: Lightcurves of the reddest stars in (J-K). Note the faintness in I. Nine of the 15 stars have been detected in the MSX survey. Complete figure is available in electronic form at EDP. |
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Figure 13: continued. |
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Figure 13: continued. |
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