CCD UBV photometry and kinematics of the open cluster NGC 225

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BİLİR S., Bostanci Z. F., YONTAN T., GÜVER T., BAKIŞ V., AK T., ...Daha Fazla

ADVANCES IN SPACE RESEARCH, cilt.58, sa.9, ss.1900-1914, 2016 (SCI-Expanded) identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 58 Sayı: 9
  • Basım Tarihi: 2016
  • Doi Numarası: 10.1016/j.asr.2016.06.039
  • Dergi Adı: ADVANCES IN SPACE RESEARCH
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Sayfa Sayıları: ss.1900-1914
  • Anahtar Kelimeler: Galaxy, Open cluster and associations, Individual, NGC 225, Stars, Hertzsprung Russell (HR) diagram, LOCAL STELLAR KINEMATICS, METALLICITY CALIBRATION, RAVE DATA, SPACE VELOCITIES, PROPER MOTIONS, MODELS, STARS, MASS, SEXTRACTOR, MEMBERSHIP
  • Akdeniz Üniversitesi Adresli: Evet

Özet

We present the results of CCD UBV photometric and spectroscopic observations of the open cluster NGC 225. In order to determine the structural parameters of NGC 225, we calculated the stellar density profile in the cluster's field. We estimated the probabilities of the stars being physical members of the cluster using the existing astrometric data. The most likely members of the cluster were used in the determination of the astrophysical parameters of the cluster. We calculated the mean radial velocity of the cluster as V-r = 8.3 +/- 5.0 km s(-1) from the optical spectra of eight stars in the cluster's field. Using the mml : mrow > U - B vs B - V two-colour diagram and UV excesses of the F-G type main-sequence stars, the reddening and metallicity of NGC 225 were inferred as E(B - V) = 0.151 +/- 0.047 mag and [Fe/H] = -0.11 +/- 0.01 dex, respectively. We fitted the colour-magnitude diagrams of NGC 225 with the PARSEC isochrones and derived the distance modulus, distance and age of the cluster as mu(V) = 9.3 +/- 0.07 mag, d = 585 +/- 20 pc and t = 900 +/- 100 Myr, respectively. We also estimated the galactic orbital parameters and space velocity components of the cluster and found that the cluster has a slightly eccentric orbit of e = 0.07 +/- 0.01 and an orbital period of P-orb = 255 +/- 5 Myr. (C) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved.