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Figure 1: The light squares indicate the approximate positions of our observed fields with respect to MACHO's fields #6 and #13. The elongated rectangle identifies the position of the OGLE II field LMC_SC21. North is up and East is left. |
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Figure 2: Comparison between instrumental CMDs (all based on two frames) of the 1999 and 2001 datasets. Left panel: DoPhot reductions of the 1999 data; central panel: DAOPHOT+ALLSTAR reductions of the 2001 data; right panel: DAOPHOT+ALLSTAR+ALLFRAME reductions of the 2001 data. |
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Figure 12: Differences between magnitude-averaged and intensity-averaged mean magnitudes for the variable stars in field A ( upper panels) and B ( lower panels), separately. |
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Figure 13:
Position of the variable stars on the
V vs. B-V colour-magnitude diagram of field A.
Different symbols are used for the various type of variables
(RR Lyrae stars: filled circles; candidate Anomalous Cepheids: open squares;
blended variables: asterisks; Cepheids:
filled squares; binaries: filled triangles; crosses: ![]() |
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Figure 14: Same as Fig. 13 for the variable stars in Field B. |
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Figure 15: Schematic light curves of a resolved ab-type RR Lyrae star in field A (filled circles) and of its blend with a clump star in the same field (open circles). |
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Figure 16: Light curves of the variable stars #5106 ( left panels) and #10320 ( right panels), open circles and crosses correspond to the 2001 and 1999 data, respectively. |
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Figure 17: Comparison between our and MACHO mean V magnitudes for the variable stars in common. Residuals are: this paper - MACHO. Filled and open symbols are used for variable stars in field A and B, respectively. Triangles are the double mode RR Lyrae stars. |
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Figure 18: Comparison between our and Kovács ( top panel) and Alves ( bottom panel) mean V magnitudes for the variable stars in common. Residuals are: this paper - others. Filled and open symbols are used for variable stars in field A and B, respectively. |
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Figure 19: Point-to-point comparison of the light curves for ab-type RR Lyrae stars in common with Kovács subsample. Filled dots: our photometry, three arms crosses: MACHO photometry. These represent the best ( left) and worst ( right) cases. |
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Figure 20: Comparison with MACHO photometry (Alves subsample) for non-variable stars brighter than 18.25 mag. Residuals are this paper minus MACHO. Lines indicate the linear fits of the average residuals of all bins. |
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Figure 21: Same as Fig. 20 for non-variable with 18.25 <V< 21 mag. |
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Figure 22: Point-to-point comparison of the V light curves for 3 ab-type RR Lyrae stars and a Classical Cepheid ( lower right panel) in common with OGLE II. Filled dots: our photometry, three arms crosses: OGLE II photometry. As in Fig. 19, these represent the best ( left) and worst ( right) cases. |
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Figure 23: Comparison between our and Ogle II mean V and B magnitudes for the variable stars in common. Residuals are: this paper - OGLE II. Open symbols are used for the most deviating stars (see text). |
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Figure 24: Comparison between our and OGLE II photometry for the about 14 000 stars in common. Residuals are this paper minus OGLE II. |
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Figure 25:
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Figure 26: Number vs. Period histogram of the single-mode RR Lyrae variables in our sample (125 objects). |
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Figure 27:
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Figure 28:
Left panel: run of the ![]() ![]() ![]() |
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Figure 29:
Star-to-star comparison between MV values ( left panel) and
(B-V)0 colours ( right panel)
derived from the Fourier parameters of the light curves and the
corresponding observed quantities. For ease of comparison
we show the 1:1 lines.
Filled and open symbols mark variables with
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Figure A.1: B,V,I light curves of the ab-type RR Lyrae stars in field A, variables are ordered by increasing period. Open and filled symbols are used for the 1999 and 2001 data, respectively. |
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Figure A.1: continued. |
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Figure A.1: continued. |
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Figure A.1: continued. |
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Figure A.1: continued. |
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Figure A.1: continued. |
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Figure A.2: B,V,I light curves of the c-type RR Lyrae stars in field A, variables are ordered by increasing period. Open and filled symbols are used for the 1999 and 2001 data, respectively. |
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Figure A.2: continued. |
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Figure A.4: B,V,I light curves of Classical Cepheids in field A, variables are ordered by increasing period. Open and filled symbols are used for the 1999 and 2001 data, respectively. |
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Figure A.6: B,V,I light curves of the ab-type RR Lyrae stars in field B, variables are ordered by increasing period. Open and filled symbols are used for the 1999 and 2001 data, respectively. |
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Figure A.6: continued. |
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Figure A.6: continued. |
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Figure A.6: continued. |
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Figure A.7: B,V,I light curves of the c-type RR Lyrae stars in field B, variables are ordered by increasing period. Open and filled symbols are used for the 1999 and 2001 data, respectively. |
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Figure A.7: continued. |
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Figure A.9: B,V,I light curves of binaries in field B, variables are ordered by increasing period. Open and filled symbols are used for the 1999 and 2001 data, respectively. |
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Figure 3:
LMC sub-field A1 (
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Figure 4:
FORS1 LMC sub-field A4 (
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Figure 5:
FORS1 LMC sub-field A2 (
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Figure 6:
FORS1 LMC sub-field A3 (
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Figure 7:
FORS1 LMC sub-field B1 (
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Figure 8:
FORS1 LMC sub-field B4 (
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Figure 9:
FORS1 LMC sub-field B2 (
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Figure 10:
FORS1 LMC sub-field B3 (
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Figure 11:
Left panel: finding chart of the ab-type RR Lyrae star #3805, which is
located slightly outside
sub-field A4 in the East direction.
Right panel: finding chart of the c-type RR Lyrae star #1387, which is located slightly
outside sub-field B4 in the South/East direction.
Both maps show a
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