Results of the summarizing process for the arXiv paper: 2304.04294v1

This paper presents a comprehensive analysis of three open clusters, NGC 189, NGC 1758 and NGC 7762. The authors used CCD UBV photometric and Gaia Data Release 3 (DR3) data to identify the most probable member stars in each cluster based on membership analyses. They determined their color excesses $E(B-V)$ and photometric metallicities [Fe/H] separately using UBV two-color diagrams. The results showed that $E(B-V)$ is $0.590 \pm 0.023$ mag for NGC 189, $0.310 \pm 0.022$ mag for NGC 1758 and $0.640 \pm 0.017$ mag for NGC 7762; while the photometric metallicity [Fe/H] is $-0.08 \pm 0.03$ dex for both NGC 189 and NGC 1758, and $-0.12 \pm 0.02$ dex for NGC 7762 respectively. The authors also obtained distance moduli and ages of the clusters by comparing PARSEC isochrones with the color-magnitude diagrams constructed from UBV and Gaia photometric data while keeping constant color excesses and metallicities for each cluster during this process. They found that the estimated isochrone distance is $1201 \pm 53$ pc for NGC 189, $902 \pm33$ pc for NGC 1758, and $911\pm31$ pc for NGC7762 which are compatible with values obtained from trigonometric parallax measurements; furthermore they determined that the ages of the clusters are 500 Myr $\pm50$, 650 Myr $\pm50$,and 2000 Myr $\pm200$, respectively for NGC189 ,NGC1758 ,andNGC7762 . Additionally, they conducted galactic orbit integration of the clusters to find that while both NGC189 andNGC7762 enter the solar circle during their orbits; NGC1758 completely orbits outside it . Overall, this study provides valuable insights into the properties and characteristics of these open clusters as well as contributes to our understanding of stellar system formation and evolution processes .

• The paper analyzes three open clusters: NGC 189, NGC 1758, and NGC 7762.
• CCD UBV photometric and Gaia Data Release 3 (DR3) data were used to identify member stars in each cluster based on membership analyses.
• Color excesses $E(B-V)$ and photometric metallicities [Fe/H] were determined separately using UBV two-color diagrams.
• Distance moduli and ages of the clusters were obtained by comparing PARSEC isochrones with color-magnitude diagrams constructed from UBV and Gaia photometric data while keeping constant color excesses and metallicities for each cluster during this process.
• The estimated isochrone distance is $1201 \pm 53$ pc for NGC 189, $902 \pm33$ pc for NGC 1758, and $911\pm31$ pc for NGC7762 which are compatible with values obtained from trigonometric parallax measurements.
• The ages of the clusters are 500 Myr $\pm50$, 650 Myr $\pm50$,and 2000 Myr $\pm200$, respectively for
• NGC189 ,NGC1758 ,andNGC7762.
• Galactic orbit integration of the clusters was conducted to find that while both
• NGC189 andNGC7762 enter the solar circle during their orbits;
• NGC1758 completely orbits outside it.

Exploring the Open Clusters NGC 189, NGC 1758 and NGC 7762

Open clusters are important objects for studying stellar evolution processes and understanding star formation in our galaxy. In a recent study, researchers have conducted a comprehensive analysis of three open clusters: NGC 189, NGC 1758 and NGC 7762. The authors used CCD UBV photometric and Gaia Data Release 3 (DR3) data to identify the most probable member stars in each cluster based on membership analyses. They then determined their color excesses $E(B-V)$ and photometric metallicities [Fe/H] separately using UBV two-color diagrams.

Color Excesses ($E(B-V)$)

The results showed that $E(B-V)$ is $0.590 \pm 0.023$ mag for NGC 189, $0.310 \pm 0.022$ mag for NGC 1758 and $0.640 \pm 0.017$ mag for NGC 7762; while the photometric metallicity [Fe/H] is $-0.08 \pm 0.03$ dex for both NGC 189 and NGC 1758, and $-0.12 \pm 0