Nearby open clusters with tidal features: Golden sample selection and 3D structure

¹ School of Physics and Optoelectronic Engineering, Anhui University, Hefei 230601, China
² Purple Mountain Observatory, Chinese Academy of Sciences, Yuanhua Road 10, Nanjing 210023, China
³ Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
⁴ Instituto de Astrofísica, Dep. de Ciencias Físicas, Facultad de Ciencias Exactas, Universidad Andres Bello, Av. Fernández Concha 700, Santiago, Chile
⁵ Purple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Yuanhua Road 10, Nanjing 210033, China
⁶ School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China

^★ Corresponding author: cy@ahu.edu.cn

Received: 21 February 2025
Accepted: 23 April 2025

Abstract

Open clusters offer unique opportunities to study stellar dynamics and evolution under the influence of their internal gravity, the Milky Way’s gravitational field, and the interactions with encounters. Using the Gaia DR3 data for a catalog of open clusters within 500 parsecs that exhibit tidal features reported by the literature, we applied a novel method based on 3D principal component analysis to select a “golden sample” of nearby open clusters with minimal line-of-sight distortions. This approach ensures a systematic comparison of 3D and 2D structural parameters for tidally perturbed clusters. The selected golden sample includes Blanco 1, Melotte 20, Melotte 22, NGC 2632, NGC 7092, NGC 1662, Roslund 6, and Melotte 111. We analyzed these clusters by fitting both 2D and 3D King Profiles to their stellar density distributions. Our results reveal systematic discrepancies, with most of the golden sample clusters exhibiting larger 3D tidal radii compared to their 2D counterparts, demonstrating that the 2D projection effects bias the measured cluster size. Furthermore, the 3D density profiles show stronger deviations from the King profiles at the tidal radii (Δρ_3D > Δρ_2D), highlighting enhanced sensitivity to tidal disturbances. Additionally, we investigated the spatial distribution of cluster members relative to their bulk motion in the Galactic plane. We find that some clusters exhibit tidal features oriented perpendicular to their direction of motion, which can be attributed to the fact that the current surveys only detect the curved inner regions of the tidal features. In conclusion, this work offers a golden sample of nearby open clusters that are most reliable for 3D structure analysis and underscores the necessity of 3D analysis when characterizing OC morphological asymmetries, determining cluster size, and identifying tidal features.