Multicolour CCD photometry of old open clusters:. King 5 and Be 20

Details Multicolour CCD photometry of old open clusters:. King 5 and Be 20 Multicolour CCD photometry of old open clusters:. King 5 and Be 20

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...372...71d&link_type=abstract

Astronomy and Astrophysics, v.372, p.71-84 (2001)

Astronomy and Astrophysics

Astrophysics

8

Hertzsprung-Russel (Hr) Diagram, Open Clusters, Individual: King 5, Be 20

Scientific paper

We present multicolour CCD photometry for two poorly studied open clusters (King 5 and Be 20). Photometry for a field near King 5 was also carried out to estimate the contamination by field stars. The colour magnitude diagrams (CMD) of the clusters show a well defined main sequence extending to the limit of the photometry, V ~20 mag. The reddening for King 5, estimated from the colour-colour diagram, is ~ 0.82, whereas that for Be 20 as estimated by comparing theoretical main-sequence (MS) with the observed MS is 0.10. The morphology of the CMDs indicates that these clusters are old. The CMD of Be 20 shows a globular cluster-like horizontal branch. In case of King 5 the comparison of observational CMDs with the standard isochrones of VandenBerg (\cite{VandenBerg85}) indicates an apparent discrepancy between the shape of the turnoff and isochrones. The CMDs of King 5 seem to be better understood in terms of stellar models with convective overshoot. The comparison of the CMDs with the stellar models by Bertelli et al. (\cite{Bertelli94}) with convective overshoot produces a good fit for a metallicity Z = 0.008 and an age = 1 Gyr for King 5 and 5 Gyr for Be 20. An apparent distance modulus (m-M) = 14.0 and 15.1 has been estimated for King 5 and Be 20 respectively. They correspond to a distance of 1900 +/-100 pc and 9026 +/- 480 pc, respectively. The radial density distribution in King 5 indicates that there is an excess of low mass stars in the outer region of the cluster, whereas the density distribution in Be 20 shows a good fit with the empirical King (\cite{King62}) model. For both clusters, observations have also been carried out to search for variable stars. Tables 2 to 4 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/372/71

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