Dynamical analysis of NGC 110: cluster of fainter stars or data fluctuation?

TL;DR

This study investigates whether NGC 110 is a genuine cluster of faint stars or an artifact of data fluctuations, using optical and IR data, but data quality issues limit definitive conclusions.

Contribution

The paper analyzes the stellar enhancement of NGC 110 across multiple bands and introduces a magnitude scatter factor to understand star characteristics, highlighting data limitations.

Findings

No stellar enhancement detected below 16.5 mag in I band.

Proper motion differences suggest field contamination.

Mass function and segregation could not be reliably studied.

Abstract

The stellar enhancement of the cluster NGC 110 is investigated in various optical and infrared (IR) bands. The radial density profile of the IR region does not show a stellar enhancement in the central region of the cluster. This stellar deficiency may be occurring by undetected fainter stars due to the contamination effect of massive stars. Since, our analysis is not indicating the stellar enhancement below 16.5 mag of I band, therefore the cluster is assumed to be a group of fainter stars. The proposed magnitude scatter factor would be an excellent tool to understand the characteristic of colour-scattering of stars. The most probable members do not coincide with the model isochronic fitting in the optical bands due to poor data quality of P P MXL catalogue. The different values of the mean proper motions are found for the fainter stars of the cluster and field regions, whereas similar values are obtained for radial zones of the cluster. The symmetrical distribution of fainter stars of the core are found around the best solution of isochrone. The mass function and mass segregation studies are not possible due to higher uncertainty of the photometric data. The number of the massive stars of the cluster region is low in comparison with the field region due to completed evolution life of the massive stars.