An Astrometric and Photometric Study of the Intermediate-Age Open Cluster NGC 2158 and Its Eclipsing Binary [Nbn2015]78

Abdelaziz, A.E.; Hendy, Y. H. M.; Shokry, Ahmed; Saad, S. M.; Kamal, F. Y.; Edris, K. A.

doi:10.22201/ia.01851101p.2020.56.02.07

Cited by 4 publications

(3 citation statements)

References 38 publications

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“…In total, 71/31 member stars of 12/10 OCs 9 are found for the APO-/LM-LRGB samples through crossmatching with the catalog of C18, with further clipping of a few outliers by using line-of-sight velocity and metallicity estimated from APOGEE and LAMOST. Comparisons of our distances of OCs with those published in the literature (e.g., Piatti et al 2003;Bragaglia et al 2006;Carraro et al 2010;Lim et al 2014;Çakmak et al 2020;Abdelaziz et al 2020;Dias et al 2021) are shown in Figure 9 and Table 3. Our distances of OCs agree very well with those distances determined previously, with a negligible median offset of the relative differences in distance ΔD/D of −0.8%/−0.6% and a standard deviation value of 5.6%/3.4% for the APO/LM-LRGB samples.…”

Section: Validation Of Distance Estimatesmentioning

confidence: 74%

The Circular Velocity Curve of the Milky Way from 5–25 kpc Using Luminous Red Giant Branch Stars

Zhou

Huang

et al. 2023

ApJ

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We present a sample of 254,882 luminous red giant branch (LRGB) stars selected from the APOGEE and LAMOST surveys. By combining photometric and astrometric information from the Two Micron All Sky Survey and Gaia survey, the precise distances of the sample stars are determined by a supervised machine-learning algorithm: the gradient-boosted decision trees. To test the accuracy of the derived distances, member stars of globular clusters (GCs) and open clusters are used. The tests by cluster member stars show a precision of about 10% with negligible zero-point offsets, for the derived distances of our sample stars. The final sample covers a large volume of the Galactic disk(s) and halo of 0 < R < 30 kpc and ∣Z∣ ≤ 15 kpc. The rotation curve (RC) of the Milky Way across the radius of 5 ≲ R ≲ 25 kpc has been accurately measured with ∼54,000 stars of the thin disk population selected from the LRGB sample. The derived RC shows a weak decline along R with a gradient of −1.83 ± 0.02 (stat.) ± 0.07 (sys.) km s−1 kpc−1, in excellent agreement with the results measured by previous studies. The circular velocity at the solar position, yielded by our RC is 234.04 ± 0.08 (stat.) ± 1.36 (sys.) km s−1, again in great consistency with other independent determinations. From the newly constructed RC, as well as constraints from other data, we have constructed a mass model for our Galaxy, yielding a mass of the dark matter halo of M 200 = (8.05 ± 1.15) × 1011 M ⊙ with a corresponding radius of R 200 = 192.37 ± 9.24 kpc and a local dark matter density of 0.39 ± 0.03 GeV cm−3.

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Section: Validation Of Distance Estimatesmentioning

confidence: 74%

The Circular Velocity Curve of the Milky Way from 5–25 kpc Using Luminous Red Giant Branch Stars

Zhou

Huang

et al. 2023

ApJ

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“…Our estimated value of color-excess in Gaia bands (E(BP − RP )) is 0.43 mag from the isochrones fitting to the CMD's. We have calculated the interstellar reddening (E(B − V )) as 0.34 mag using the transformation equations (E(B − V )= 0.785 E(BP − RP )) as taken from Abdelaziz et al (2020). Distance modulus (m − M G =12.51 mag) of IC 1434 provides the heliocentric distance as 3.2±0.1 kpc.…”

Section: Age and Distance Estimation Using Cmdmentioning

confidence: 99%

Study of an intermediate age open cluster IC 1434 using ground-based imaging and Gaia DR2 astrometry

Hendy,

Bisht

2021

Preprint

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We present a detailed photometric and kinematical analysis of poorly studied open cluster IC 1434 using CCD VRI, APASS, and Gaia DR2 database for the first time. By determining the membership probability of stars, we identified the 238 most probable members with a probability higher than 60% by using proper motion and parallax data as taken from the Gaia DR2 catalog. The mean proper motion of the cluster is obtained as µ x = −3.89 ± 0.19 and µ y = −3.34 ± 0.19 mas yr −1 in both the directions of right ascension and declination. The radial distribution of member stars provides cluster extent as 7.6 arcmin. We have estimated the interstellar reddening (E(B-V)) as 0.34 mag using the transformation equations from literature. We obtained the values of cluster age and distance are 631 ± 73 Myr and 3.2 ± 0.1 Kpc.

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“…Stellar photometry is a basic tool to study the physical properties of young stellar systems Lim et al 2015a;Abdelaziz et al 2020. However, since most young open clusters are distributed in the Galactic plane, it is essential to discriminate cluster members from field interlopers to determine the reliable results.…”

Section: Introductionmentioning

confidence: 99%

The Sejong Open Cluster Survey (SOS). VII. A Photometric Study of the Young Open Cluster IC 1590

Kim

Lim

Bessell

et al. 2021

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Young open clusters are ideal laboratories to understand star formation process. We present deep U BV I and Hα photometry for the young open cluster IC 1590 in the center of the H II region NGC 281. Early-type members are selected from U BV photometric diagrams, and low-mass pre-main sequence (PMS) members are identified by using Hα photometry. In addition, the published X-ray source list and Gaia astrometric data are also used to isolate probable members. A total of 408 stars are selected as members. The mean reddening obtained from early-type members is E(B − V ) = 0.40 ± 0.06 (s.d.).We confirm the abnormal extinction law for the intracluster medium. The distance

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An Astrometric and Photometric Study of the Intermediate-Age Open Cluster NGC 2158 and Its Eclipsing Binary [Nbn2015]78

Cited by 4 publications

References 38 publications

The Circular Velocity Curve of the Milky Way from 5–25 kpc Using Luminous Red Giant Branch Stars

The Circular Velocity Curve of the Milky Way from 5–25 kpc Using Luminous Red Giant Branch Stars

Study of an intermediate age open cluster IC 1434 using ground-based imaging and Gaia DR2 astrometry

The Sejong Open Cluster Survey (SOS). VII. A Photometric Study of the Young Open Cluster IC 1590

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