Spectral Classification in Nine Open Clusters.

Svolopoulos, S. N.

doi:10.1086/147436

Cited by 8 publications

(11 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…From the estimated distance modulus and the colour excess, we find the distance of NGC 225 as d = 585 ± 20 pc, which is in agreement with that found by Lattanzi et al (1991) within errors. A comparison of the reddening values with those estimated in previous studies shows that the colour excess obtained in this study is smaller than E(B − V ) = 0.29 mag given by Johnson et al (1961) and Svolopoulos (1962), while it is in agreement roughly with E(B − V ) = 0.25 ± 0.08 mag found by Lattanzi et al (1991) within errors. The distance modulus obtained in this study (m − M) = 9.30 ± 0.07 mag is in agreement with the previous estimates of (m − M) = 9.0 and (m − M) = 9.1 mag (Svolopoulos, 1962;Hoag & Applequist, 1965) within errors, as well.…”

Section: Discussionsupporting

confidence: 86%

“…Johnson et al (1961) measured the reddening for the cluster as E(B − V ) = 0.29 mag using the data presented by Hoag et al (1961). Svolopoulos (1962) determined the spectral classes for a number of stars in the field of the cluster, for which the photoelectric magnitudes were already given by Hoag et al (1961), and measured the reddening, the distance modulus and the distance of the cluster as E(B − V ) = 0.29 mag, (m − M) = 9.0 mag and d = 630 pc, respectively. Hoag & Applequist (1965) measured H γ equivalent widths of the brighter stars in the field of the cluster photoelectrically and determined their spectral classes.…”

mentioning

confidence: 99%

See 1 more Smart Citation

CCD UBV Photometry and Kinematics of the Open Cluster NGC 225

Bilir,

Bostanci,

Yontan

et al. 2016

Preprint

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionsupporting

confidence: 86%

mentioning

confidence: 99%

CCD UBV Photometry and Kinematics of the Open Cluster NGC 225

Bilir,

Bostanci,

Yontan

et al. 2016

Preprint

View full text Add to dashboard Cite

show abstract

“…This distance was later modified by Johnson et al (1961) who determined a reddening of E(B − V ) = 0.08 and a distance of 630 pc. UBV measurements of 28 stars were reported by Hoag et al (1961) and Svoupoulus (1962) found the same reddening and distance, but from spectroscopy he determined the following values for distance and reddening: 660 pc and E(B − V ) = 0.05. In 1965 Hoag et al (1965) gave new spectral classification for five stars.…”

Section: Introductionsupporting

confidence: 59%

uvby--beta photoelectric photometry of NGC 7063

Pena,

Machado,

Garrido

2007

Preprint

View full text Add to dashboard Cite

show abstract

“…On the contrary, Bilir et al (2016) reported a larger estimation of age, 𝜏 = 900 ± 100 Myr, with the same distance 𝐷 = 585 ± 20 pc. Svolopoulos (1962) found a distance 𝐷 = 630 pc. Evaluation of color excess 𝐸 (𝐵 − 𝑉) varies from 0.151 ± 0.047 (Bilir et al 2016) to 0.25 ± 0.08 mag (Lattanzi et al 1991) and 0.29 mag (Svolopoulos 1962;Subramaniam et al 2006).…”

Section: Introductionmentioning

confidence: 98%

The young Galactic cluster NGC 225: binary stars content and total mass estimate

Yalyalieva,

Carraro,

Glushkova

et al. 2022

Preprint

View full text Add to dashboard Cite

Galactic star clusters are known to harbour a significant amount of binary stars, yet their role in the dynamical evolution of the cluster as a whole is not comprehensively understood. We investigated the influence of binary stars on the total mass estimate for the case of the moderately populated Galactic star cluster NGC 225. The analysis of multi-epoch radial velocities of the 29 brightest cluster members, obtained over two observational campaigns, in 1990-1991 and in 2019-2020, yields a value of binary fraction of 𝛼 = 0.52 (15 stars out of 29). Using theoretical isochrones and Monte Carlo simulations we found that the cluster mass increases at least 1.23 times when binaries are properly taken into account. By combining Gaia EDR3 photometric data with our spectroscopic observations, we derived estimates of NGC 225 fundamental parameters foras follows: mean radial velocity < 𝑉 𝑟 >= −9.8 ± 0.7 km s −1 , log(𝜏)=8.0-8.2 dex, distance 𝐷 = 676 ± 22 pc, and colour excess 𝐸 (𝐵 − 𝑉) = 0.29 ± 0.01 mag.

show abstract

Spectral Classification in Nine Open Clusters.

Cited by 8 publications

References 0 publications

CCD UBV Photometry and Kinematics of the Open Cluster NGC 225

CCD UBV Photometry and Kinematics of the Open Cluster NGC 225

uvby--beta photoelectric photometry of NGC 7063

The young Galactic cluster NGC 225: binary stars content and total mass estimate

Contact Info

Product

Resources

About