NGC 3293 is a young cluster in the southern celestial hemisphere in the Carina constellation.

It was found by Nicolas-Louis de Lacaille in 1751 and is around 8000 to 8400 lightyears distant from us. This cluster has about 100 stars that are brighter than the 14th magnitude. The majority of these stars are blue supergiants, but there are a few red giants, including V361 Carinae, a notable 7th magnitude red giant. This cluster is also known as the Gem Cluster because its blue and red stars glitter beautifully in the sky when viewed through any telescope, resembling a jewel box.

In a recent research in 2022, a group of astronomers led by Thierry Morel of the University of Liège in Belgium performed a spectroscopic investigation of NGC 3293 to evaluate the features of the star B-type population. They discovered that the cluster may be older than previously assumed. Despite being dominated by blue giants, the existence of red giants suggests that it might be up to 20 million years old rather than 12 million.

In order to study NGC 3293 further and investigate the relationships between the colours, brightnesses, and the age and chemical composition of the cluster as a whole, I collected  images in B, V, and R filters. I made these observations via Skynet using the Prompt 6 telescope in the Cerro Tololo Inter-American Observatory. Additionally, using Afterglow and Cluster Astromancer I discovered some of the properties of this cluster.

Using afterglow I was able to rendder a good quality color image of NGC_3293.

The goal was to obtain more exact numbers in order to conduct further study on this cluster. Through this experience, I was able to learn some of the strategies that astronomers and others in the field use to collect more precise data in order to improve on previous results made with less modern equipment and get a greater knowledge of what happens in our universe. This cluster, in particular, is particularly brilliant, thus exposure durations are considerably shorter to avoid overexposure.

Most of the numbers I tested were consistent with SIMBAD’s database. Kharchenko et al. (2013) also researched this cluster. However, using Cluster Astromancer, I generated HR Diagrams to compare our numbers and determine which parameters suited the dataset better and were more accurate.

Kharchenko et al	Mine
Distance (in kpc) 2.441 log(Age) 6.75 (10log(Age)) = Age in years 5620000 Metalicity 0 E(B – V) 0.333	Distance (in kpc) 2.4 (kpc) log(Age) 7.15 (10log(Age)) = Age in years 14.13 (Myrs) Metalicity -0.1 E(B – V) 0.35

With my mesured calculation and renddering I got RP vs (BP – RP), R vs (B – R), V vs (B – V), H vs (J – H), i have uploaded these image  to this drive : Isochrone_iamge

I also added my tri-color image to this drive( due to the server not able to upload my image : NGC_3293 image

After completing my research of this cluster, I gained a deeper grasp of the field, the data gathering procedure, and the rationale underlying the analysis.