2024/06/12 by Neelam Panwar, Panwar, Neelam, C. Rishi +11 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.2406.08261
openalex publication_date 2024/06/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a multi-wavelength analysis of the young star cluster Berkeley 59 (Be 59) based on the Gaia data and deep infrared (IR) observations with the 3.58-m Telescopio Nazionale Galileo and Spitzer space telescope. The mean proper motion of the cluster is found to be μαcosδ ∼ -0.63 mas yr-1 and μδ ∼ -1.83 mas yr-1 and the kinematic distance of the cluster, ∼ 1 kpc, is in agreement with previous photometric studies. Present data is the deepest available near-IR observations for the cluster so far and reached below 0.03 M_\odot. The mass function of the cluster region is calculated using the statistically cleaned color-magnitude diagram and is similar to the Salpeter value for the member stars above 0.4 M_\odot. In contrast, the slope becomes shallower (Γ ∼ 0.01 ± 0.18) in the mass range 0.04 - 0.4 M_\odot, comparable to other nearby clusters. The spatial distribution of young brown dwarfs (BDs) and stellar candidates shows a non-homogeneous distribution. This suggests that the radiation feedback from massive stars may be a prominent factor contributing to the BD population in the cluster Be 59. We also estimated the star-to-BD ratio for the cluster, which is found to be ∼ 3.6. The Kolomogorov-Smirnov test shows that stellar and BD populations significantly differ, and stellar candidates are near the cluster center compared to the BDs, suggesting mass segregation in the cluster toward the substellar mass regime.