CCD $UBV(RI)_{C}$ Photometry of Twenty Open Clusters

TL;DR

This study presents CCD photometry for 20 open clusters, deriving their fundamental parameters and comparing them with literature, revealing systematic differences due to various assumptions and calibrations, and exploring their Galactic distribution and origins.

Contribution

First comprehensive CCD $UBV(RI)_C$ photometry analysis of 20 open clusters, providing updated parameters and insights into their Galactic context and formation history.

Findings

No metallicity gradient detected within 6.82-15.37 kpc range.

Good agreement between morphological and isochrone ages for 12 clusters.

Young, metal-poor clusters may be linked to stellar over-densities or accretion events.

Abstract

Fundamental astrophysical parameters have been derived for 20 open clusters (O\!Cs) using CCD~$U\!BV\!(RI)_C$ photometric data observed with the 84~cm telescope at the San Pedro M\'artir National Astronomical Observatory, M\'exico. The interstellar reddenings, metallicities, distances, and ages have been compared to the literature values. Significant differences are usually due to the usage of diverse empirical calibrations and differing assumptions, such as concerning cluster metallicity, as well as distinct isochrones which correspond to differing element-abundance ratios, internal stellar physics, and photometric systems. Different interstellar reddenings, as well as varying reduction and cluster-membership techniques, are also responsible for these kinds of systematic differences and errors. The morphological ages, which are derived from the morphological indices ($\delta V$ and $\delta 1$) in the CM diagrams, are in good agreement with the isochrone ages of 12 O\!Cs, those with good red clump (RC) and red giant (RG) star candidates. No metal abundance gradient is detected for the range $6.82 \leq R_{GC} \leq 15.37$ kpc, nor any correlation between the cluster ages and metal abundances for these 20 O\!Cs. Young, metal-poor O\!Cs, observed here in the third Galactic quadrant, may be associated with stellar over-densities, such as that in Canis Major (Martin et al.) and the Monoceros Ring (Newberg et al.), or signatures of past accretion events, as discussed by Yong et al. and Carraro et al.