Cluster | Filter | Observation | Number of | Min, max exposure | Seeing |
(Galaxy) | night | observations | time (s) | (arcsec) | |
KMHK264
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B | N4 | 2 | 60, 300 | 1.3-1.4 |
(LMC) | V | N4 | 2 | 30, 200 | 1.2-1.3 |
NGC 1777 | B | N1 | 5 | 120, 300 | 1.6-1.8 |
(LMC) | V | N1 | 5 | 60, 200 | 1.6-2.0 |
NGC 1902 | B | N1, N4, N5 | 4 | 40, 300 | 1.2-1.8 |
(LMC) | V | N1, N4, N5 | 4 | 20, 200 | 1.1-1.6 |
NGC 2155 | B | N3 | 3 | 60, 600 | 1.2 |
(LMC) | V | N3 | 4 | 30, 300 | 1.1-1.2 |
IC 2146 | B | N4 | 3 | 60, 1200 | 1.2-1.3 |
(LMC) | V | N4 | 4 | 30, 600 | 1.2 |
L9 | B | N5 | 3 | 60, 600 | 1.3-1.4 |
(SMC) | V | N5 | 4 | 30, 300 | 1.1-1.4 |
L13 | B | N5 | 2 | 120, 600 | 1.3-1.4 |
(SMC) | V | N5 | 3 | 60, 300 | 1.2-1.4 |
L45
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B | N5 | 3 | 60, 600 | 1.3-1.4 |
(SMC) | V | N5 | 3 | 30, 300 | 1.3-1.4 |
NGC 152 | B | N4 | 4 | 60, 1200 | 1.2-1.4 |
(SMC) | V | N4 | 5 | 30, 600 | 1.1-1.2 |
NGC 220
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B | N1, N2, N4, N5 | 8 | 40, 300 | 1.3-1.9 |
(SMC) | V | N1, N2, N4, N5 | 10 | 20, 200 | 1.3-1.8 |
NGC 458 | B | N1, N3, N4, N5 | 5 | 60, 300 | 1.2-1.9 |
(SMC) | V | N1, N3, N4, N5 | 5 | 30, 300 | 1.1-1.8 |
NGC 643 | B | N2, N3 | 5 | 120, 1200 | 1.2-2.2 |
(SMC) | V | N2, N3 | 12 | 30, 600 | 1.1-2.3 |
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The Magellanic Clouds (MC) are well-known targets for the investigation of simple stellar populations, since they present a great number of populous young and intermediate age clusters, which allow to test evolutionary theories for a combination of masses and metallicities not present in our Galaxy. In a previous paper (Brocato et al. 2001) we have recently presented B,V CMDs for 21 globular clusters in the LMC and 1 in the SMC, as obtained on the basis of HST snapshots. In this paper we extend this investigation by using observational data from the ESO 1.54-m Danish Telescope.
With respect to the previous survey, the present study
obviously relies on a worse seeing,
but presents also the relevant advantage of providing
data in a larger field of view
(
), covering the whole cluster
and a large portion of the surrounding stellar field.
As we shall discuss later on, the quality of the CM diagrams
presented in this paper appears largely comparable with
the ones in the previous investigation.
In this way we shall add 4 clusters to the previous sample of the LMC clusters
(2 of our 6 LMC clusters were already investigated in the previous paper),
extending the investigation to 10 clusters in the SMC in order
to allow the investigation of
stellar populations in both Clouds.
Section 2 gives information on the observations and on the adopted data reduction procedures. The CM diagrams of clusters and surrounding fields are presented in Sect. 3 where the major features of the diagrams are briefly discussed. In Sect. 4 we discuss the stellar populations of the fields, whereas a study of the red clumps in both LMC and SMC fields is presented in Sect. 5. In Sect. 6 we finally present some brief concluding remarks.
Copyright ESO 2002