YONTAN, T., S. BILIR, Z.F. BOSTANCI, T. AK, S. KARAALI, T. GUVER, S. AK, S. DURAN and Ernst PAUNZEN. CCD UBVRI photometry of NGC 6811. Astrophysics and Space Science. DORDRECHT: Springer, 2015, vol. 355, No 2, p. 267-281. ISSN 0004-640X. Available from: https://dx.doi.org/10.1007/s10509-014-2175-5.
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Basic information
Original name CCD UBVRI photometry of NGC 6811
Authors YONTAN, T. (792 Turkey), S. BILIR (792 Turkey), Z.F. BOSTANCI (792 Turkey), T. AK (792 Turkey), S. KARAALI (792 Turkey), T. GUVER (792 Turkey), S. AK (792 Turkey), S. DURAN (792 Turkey) and Ernst PAUNZEN (40 Austria, belonging to the institution).
Edition Astrophysics and Space Science, DORDRECHT, Springer, 2015, 0004-640X.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher Netherlands
Confidentiality degree is not subject to a state or trade secret
Impact factor Impact factor: 1.678
RIV identification code RIV/00216224:14310/15:00080725
Organization unit Faculty of Science
Doi http://dx.doi.org/10.1007/s10509-014-2175-5
UT WoS 000350206600008
Keywords in English Galaxy: open cluster and associations: individual: NGC 6811; Stars: Hertzsprung Russell (HR) diagram
Tags AKR, rivok
Changed by Changed by: Ing. Andrea Mikešková, učo 137293. Changed: 29/3/2016 15:12.
Abstract
We present the results of CCD UBVRI observations of the open cluster NGC 6811 obtained on 18th July 2012 with the 1 m telescope at the TUBITAK National Observatory (TUG). Using these photometric results, we determine the structural and astrophysical parameters of the cluster. The mean photometric uncertainties are better than 0.02 mag in the V magnitude and B - V, V - R, and V - I colour indices to about 0.03 mag for U - B among stars brighter than magnitude V = 18. Cluster member stars were separated from the field stars using the Galaxia model of Sharma et al. (2011) together with other techniques. The core radius of the cluster is found to be r(c) = 3.60 arcmin. The astrophysical parameters were determined simultaneously via Bayesian statistics using the colour-magnitude diagrams V versus B - V, V versus V - I, V versus V - R, and V versus R - I of the cluster. The resulting most likely parameters were further confirmed using independent methods, removing any possible degeneracies. The colour excess, distance modulus, metallicity and the age of the cluster are determined simultaneously as E(B-V) = 0.05 +/- 0.01 mag, mu = 10.06 +/- 0.08 mag, [M/H] = -0.10 +/- 0.01 dex and t = 1.00 +/- 0.05 Gyr, respectively. Distances of five red clump stars which were found to be members of the cluster further confirm our distance estimation.
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GP14-26115P, research and development projectName: Vstříc k jednotné škále metalicity pro otevřené hvězdokupy
Investor: Czech Science Foundation
3SGA5916, interní kód MUName: Hvězdy a hvězdokupy v Magellanových mračnech (Acronym: Webda MaC)
Investor: South-Moravian Region, Incoming grants
7AMB14AT015, research and development projectName: Nový pohled na magnetické hvězdy (Acronym: MAGSTARS)
Investor: Ministry of Education, Youth and Sports of the CR
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