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CCD \({U\!B\!V\!(R\!I)}_{KC}\) photometry of NGC 2323 and NGC 2539 open clusters

  • İnci Akkaya OralhanEmail author
  • Raúl Michel
  • William J. Schuster
  • Yüksel Karataş
  • Yonca Karsli
  • Carlos Chavarría
Article
  • 16 Downloads

Abstract

The open clusters NGC 2323 and NGC 2539 have been analysed using CCD \(U\!B\!V\!(R\!I)_{KC}\) photometric data, observed at the San Pedro Mártir Observatory. Cluster memberships have been determined with the proper motion and parallax measures from the GaiaDR2 astrometric data release. Photometric metal and heavy element abundances have been obtained as \(([M/H],\;Z) = (-0.10,~0.012)\) (NGC 2323) and \((-0.31,\;0.007)\) (NGC 2539) from the \(\delta (U\)B) technique in the two-colour diagrams, which are used to select the appropriate PARSEC isochrones. The estimated reddening of NGC 2323 is \(E(B-V)=0.23\pm 0.04\) using 11 early type stars. For NGC 2539, we find \(E(B-V)= 0.02\pm 0.06\). For \((B-V)\) colour, distance moduli and distances for NGC 2323 and NGC 2539 are derived as \((V_{0}-M_V, d\ \mathrm{(pc)}) = (10.00\pm 0.10, 1000\pm 50)\) and \((V_{0}-M_V, d \mathrm{(pc)}) = (10.00\pm 0.04, 1000\pm 20)\), respectively. The median GaiaDR2 distance \(d=1000\pm 140\) pc (\(\varpi =0.998\pm 0.136\) mas) for the likely members of NGC 2323 is in concordance with its four-colour photometric distances 910–1000 pc. For NGC 2539, its GaiaDR2 distance \(d=1330\pm 250\) pc (\(\varpi =0.751\pm 0.139\) mas) is close to its four-colour photometric distances, 1000 pc. Fitting the PARSEC isochrones to the colour magnitude diagrams (CMDs) gives an old age, \(890\pm 110\) Myr, for NGC 2539. Whereas NGC 2323 has an intermediate age, \(200\pm 50\) Myr. One red clump/red giant candidate (BD-12 2380) in the CMDs of NGC 2539 has been confirmed as a member in terms of the distances \(d_{I} =950\pm 50\) pc and \(d_{V}=910\pm 90\) pc of VI filters within the uncertainties, as compared to the distance \(1000\pm 20\) pc of NGC 2539. This giant’s GaiaDR2 distance (\(d=1200\pm 70\) pc) is not close to these photometric distances.

Keywords

Galaxy evolution open clusters and associations—individual Hertzsprung–Russell and colour magnitude diagrams 

Notes

Acknowledgements

The observations of this publication were made at the National Astronomical Observatory, San Pedro Mártir, Baja California, México, and the authors wish to thank the staff of the Observatory for their assistance during these observations. They thank H. Cakmak for useful help on the manuscript. This research made use of the WEBDA open-cluster database of J.-C. Mermilliod and also the SIMBAD database. This work has been supported by the CONACyT (México) projects 33940, 45014 and 49434, and PAPIIT-UNAM (México) projects IN111500 and IN103014. This paper has made use of the results from the European Space Agency (ESA) space mission Gaia, the data from which were processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by the national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is http://www.cosmos.esa.int/gaia.

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Copyright information

© Indian Academy of Sciences 2019

Authors and Affiliations

  • İnci Akkaya Oralhan
    • 1
    Email author
  • Raúl Michel
    • 2
  • William J. Schuster
    • 2
  • Yüksel Karataş
    • 3
  • Yonca Karsli
    • 1
  • Carlos Chavarría
    • 2
  1. 1.Department of Astronomy and Space Science, Science FacultyErciyes UniversityKayseriTurkey
  2. 2.Observatorio Astronomico NacionalUniversidad Nacional Autonoma de MéxicoEnsenadaMexico
  3. 3.Department of Astronomy and Space Sciences, Science FacultyIstanbul UniversityIstanbulTurkey

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