Stellar populations of NGC 5053 were investigated with AstroSat

Globular cluster NGC 5053. Credit: Sloan Digital Sky Survey.

Using the AstroSat spacecraft, Indian astronomers have inspected a galactic globular cluster known as NGC 5053. Results of the study, presented in a paper published May 27 on the arXiv pre-print repository, provide important insights into the stellar population of this cluster. Globular clusters (GCs) are collections of tightly bound stars orbiting galaxies. Astronomers perceive them as natural laboratories enabling studies on the evolution of stars and galaxies. In particular, globular clusters could help researchers to better understand the formation history and evolution of early-type galaxies as the origin of GCs seems to be closely linked to periods of intense star formation.

At a distance of about 57,000 light-years away from the Earth, NGC 5053 is one of the most metal-poor Galactic GCs. Although NGC 5053 was discovered in 1784, almost 150 years later it was confirmed as a globular cluster. This was mainly due to the cluster's high latitude, richness in faint stars, and presence of variable stars. Now, to shed more light on the stellar content of NGC 5053, a group of astronomers led by Kolencheri Jithendran Nikitha of the Indian Institute of Space science and Technology in Kerala, India, decided to observe this cluster with the Ultra Violet Imaging Telescope (UVIT) onboard AstroSat. The study was complemented by data from ESA's Gaia satellite.

The researchers wrote, in this paper, that we present the photometric analysis of the globular cluster NGC 5053 using the FUV [far-ultraviolet] and NUV [near-ultraviolet] filters of UVIT, in combination with Gaia observations.

The team managed to construct a catalog of 1884 ultraviolet stars of NGC 5053 and carried out their photometry. By analyzing the proper motion of these stars from Gaia data, they were able to identify members of this cluster. According to the study, NGC 5053 has a significant population of blue horizontal branch (HB) stars, which is typical for metal-poor GCs. Furthermore, the astronomers located candidates of stellar populations that were not identified by previous observations, including 14 blue straggler star (BSS) candidates and one extreme horizontal branch (EHB) star. The observations also allowed the researchers to identify the known populations of BSSs, and blue horizontal branch (BHB) stars, RR-Lyrae stars, and SX Phoenicis (SX-Phe) stars.

The researchers noted that radial distribution and spectral energy distribution (SED) of the BSS population of NGC 5053 seem to suggest that they have a collisional origin. This scenario is consistent with the previous speculations indicating a possibility of collisional origin for BSSs in low-density clusters similar to NGC 5053. In addition, the study found that NGC 5053 has a metallicity at a level of -1.9 and its age was estimated to be about 12.5 billion years.

Journal Information:  K. J. Nikitha et al, Stellar populations of the globular cluster NGC 5053 investigated using AstroSat-Ultra Violet Imaging Telescope. arXiv:2205.13839v1 [astro-ph.GA], arxiv.org/abs/2205.13839