CCD UBV photometric study of five open clusters-Dolidze 36, NGC 6728, NGC 6800, NGC 7209, and Platais 1

Bostanci Z. F., Yontan T., Bilir S., Ak T., Guver T., Ak S., ...More

ASTROPHYSICS AND SPACE SCIENCE, vol.363, no.7, 2018 (SCI-Expanded) identifier identifier

  • Publication Type: Article / Article
  • Volume: 363 Issue: 7
  • Publication Date: 2018
  • Doi Number: 10.1007/s10509-018-3364-4
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Keywords: Galaxy: open cluster and associations: individual: Dolidze 36, NGC 6728, NGC 6800, NGC 7209, Platais 1, Stars: Hertzsprung Russell (HR) diagram, OPEN STAR-CLUSTERS, GALACTIC OPEN CLUSTERS, DIGITAL SKY SURVEY, STELLAR EVOLUTION, PROPER MOTIONS, SURVEY 2MASS, PARAMETERS, TRANSFORMATIONS, CALIBRATION, MEMBERSHIP
  • Istanbul University Affiliated: Yes


In this study, we present CCD UBV photometry of poorly studied open star clusters, Dolidze 36, NGC 6728, NGC 6800, NGC 7209, and Platais 1, located in the first and second Galactic quadrants. Observations were obtained with T100, the 1-m telescope of the TBA degrees TAK National Observatory. Using photometric data, we determined several astrophysical parameters such as reddening, distance, metallicity and ages and from them, initial mass functions, integrated magnitudes and colours. We took into account the proper motions of the observed stars to calculate the membership probabilities. The colour excesses and metallicities were determined independently using two-colour diagrams. After obtaining the colour excesses of the clusters Dolidze 36, NGC 6728, NGC 6800, NGC 7209, and Platais 1 as , , , , and mag, respectively, the metallicities are found to be , , , , and dex, respectively. Furthermore, using these parameters, distance moduli and age of the clusters were also calculated from colour-magnitude diagrams simultaneously using PARSEC theoretical models. The distances to the clusters Dolidze 36, NGC 6728, NGC 6800, NGC 7209, and Platais 1 are , , , , and pc, respectively, while corresponding ages are , , , , and Myr, respectively. Our results are compatible with those found in previous studies. The mass function of each cluster is derived. The slopes of the mass functions of the open clusters range from 1.31 to 1.58, which are in agreement with Salpeter's initial mass function. We also found integrated absolute magnitudes varying from -4.08 to -3.40 for the clusters.