NGC 2414: A Young Star Cluster with Potential Planetary Formation
Located 1.3 degrees southwest of the well-known open cluster luminaries M46 and M47, NGC 2414 is a young star cluster with a lot of potential for planetary formation research. When observing this object through a telescope, the first thing you’ll notice is a central bright star with a magnitude of 8.2 (SAO 153056).
In order to study NGC 2414 and investigate the relationships between the colours, brightnesses, and the age and chemical composition of the cluster as a whole, I collected 15 total images, 5 in each of the filters B, V, and R with telescopes PROMPT-MO-1, Prompt5, with total exposure durations of 60, 30 and 20 seconds in B, V, and R filters respectively, with other imaging parameters, using Skynet. I used Afterglow and Cluster Pro Plus for their purposes and I found these basic results:
Distance : 4.95 kpc +- 30%
Proper Motion in RA: -1.407 +- 0.15
DEC: 1.441 +- 0.169 mas/yr
Log(age): 6.9 log(yr)
Metallicity: -2.02 solar
E(B-V): 0.65 mag
Number of cluster stars = 96.
More parameters:
WEBDA page data for open cluster NGC 2414
| Right Ascension (2000) | 07 33 12 | |
|---|---|---|
| Declination (2000) | -15 27 12 | |
| Galactic longitude | 231.412 | |
| Galactic latitude | 1.946 | |
| Distance [pc] | 3455 | |
| Reddening [mag] | 0.508 | |
| Distance modulus [mag] | 14.27 | |
| Log Age | 6.976 |
Using afterglow I layered the images taken in their filters to process a coloured image of the clusterÂ
Below is the archived image from AladinLite
NGC 2414 is a great example of a star cluster with a lot of potential for scientific research. By studying the young stars within this cluster, astronomers can learn more about the formation and evolution of planets in our universe.
I found it very fascinating collecting images of this cluster and processing them to see the images come to life in colour. The differences between the original image and the image adjusted for the reddening was such an interesting way to see images come together and give life to the star cluster .
In comparison to the parameters listed in Gaia everything was very similar and lined up nicely however they did not have a listed metallicity and with the isochrone model I managed to fit it better with my added metallicity , When I plotted their data, the turn off point does not quite fit the top of the main sequence. I think my model has a good fit and I feel confident about my results.
REFERENCES:
https://webda.physics.muni.cz/cgi-bin/ocl_page.cgi?dirname=ngc2414
https://aladin.u-strasbg.fr/AladinLite/