CCD UBV $\mathit{UBV}$ photometry of the open cluster NGC 6819

Ak, T.; Bostancı, Z. F.; Yontan, Talar; Bilir, S.; Güver, T.; Ak, S.; Urgup, H.; Paunzen, E.

doi:10.1007/s10509-016-2707-2

Cited by 24 publications

(28 citation statements)

References 72 publications

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“…This section is a summary of the methods utilized to determine the fundamental parameters of Frolov 1 and NGC 7510 (for background details on methodology, see Ak et al 2016; Banks et al 2020; Bilir et al 2016; Bostancı et al 2018; Yontan et al 2019). We obtained reddening and metallicity estimates by fitting observational models on the TCDs, while distance moduli and ages were determined simultaneously by fitting theoretical isochrones on CMDs.…”

Section: Cluster Parametersmentioning

confidence: 99%

A study of open clusters Frolov 1 andNGC7510 usingCCD UBVphotometry and GaiaDR2astrometry

Yontan

Bilir

et al. 2021

Astron Nachr

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We present reddening, photometric metallicity, age, and distance estimates for the Frolov 1 and NGC 7510 open clusters based on charge-coupled device (CCD) UBV photometric and Gaia data. Photometric observations were collected using the 1-m telescope of the TÜBİTAK National Observatory. Gaia data release 2 (DR2) proper motion data in the direction of two groupings were used to identify cluster membership. We determined mean proper motion values of ( α cos δ, δ ) = (− 3.02 ± 0.10, − 1.75 ± 0.08) and (−3.66 ± 0.07, −2.17 ± 0.06) mas year −1 for Frolov 1 and NGC 7510, respectively. We used two-color diagrams to obtain E(B − V) color excesses for Frolov 1 and NGC 7510 of 0.65 ± 0.06 and 1.05 ± 0.05 mag, respectively. We derived the photometric metallicity of Frolov 1 as [Fe/H] = 0.03 ± 0.03 dex and adopted a solar metallicity for NGC 7510. Based on these reddening and metallicities, we determined the distance moduli and ages of the clusters by fitting stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (PARSEC) isochrones to the cluster color-magnitude diagrams. Isochrone-fitting distances for Frolov 1 and NGC 7510 are 2, 864 ± 254 and 2, 818 ± 247 pc, respectively, which correspond to the ages 35 ± 10 Myr and 18 ± 6 Myr. We also calculated mean Gaia distances and compared them with those given in the literature and in this study, concluding that our results are in good agreement with previous work. Finally, we calculated the mass function slopes and found them to be X = −1.21 ± 0.18 for Frolov 1 and X = −1.42 ± 0.27 for NGC 7510.

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Section: Cluster Parametersmentioning

confidence: 99%

A study of open clusters Frolov 1 andNGC7510 usingCCD UBVphotometry and GaiaDR2astrometry

Yontan

Bilir

et al. 2021

Astron Nachr

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“…In this section we summarised the techniques applied during the cluster analyses (for detailed analyses on methods used see Bilir et al (2006Bilir et al ( , 2010Bilir et al ( , 2016; Yontan et al (2015Yontan et al ( , 2019Yontan et al ( , 2021; Bostancı et al (2015Bostancı et al ( , 2018; Ak et al (2016); Banks et al (2020)). We estimated reddening and photometric metallicities from TCDs on an individual basis, then keeping these parameters as a constants we fitted theoretical isochrones on CMDs to determine distance moduli and age simultaneously.…”

Section: Astrophysical Parameters Of the Clustersmentioning

confidence: 99%

A study of the Czernik 2 and NGC 7654 open clusters using CCD UBV photometric and Gaia EDR3 data

Akbulut,

Ak,

Yontan

et al. 2021

Preprint

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“…The aperture photometry packages of IRAF were utilized to measure the instrumental magnitudes of the standard stars. From the observations of the standard stars (Landolt, 2009), atmospheric extinction and transformation coefficients for the observing system were determined through the equations given in Janes & Hoq (2013) and Ak et al (2016). The coefficients for that particular night are listed in Table 2 of Yontan et al (2015).…”

Section: Photometrymentioning

confidence: 99%

“…We find the reddening and metallicity of the cluster following two independent methods. Its distance modulus and age were inferred by fitting stellar isochrones to the observed CMDs, while keeping the reddening and metallicity constant (Bilir et al, 2010;Yontan et al, 2015;Bostancı et al, 2015;Ak et al, 2016).…”

mentioning

confidence: 99%

CCD UBV Photometry and Kinematics of the Open Cluster NGC 225

Bilir,

Bostanci,

Yontan

et al. 2016

Preprint

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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 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 [F e/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 µ 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.

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CCD UBV $\mathit{UBV}$ photometry of the open cluster NGC 6819

Cited by 24 publications

References 72 publications

A study of open clusters Frolov 1 andNGC7510 usingCCD UBVphotometry and GaiaDR2astrometry

A study of open clusters Frolov 1 andNGC7510 usingCCD UBVphotometry and GaiaDR2astrometry

A study of the Czernik 2 and NGC 7654 open clusters using CCD UBV photometric and Gaia EDR3 data

CCD UBV Photometry and Kinematics of the Open Cluster NGC 225

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