Quote:
Originally Posted by SkyViking
Incidentally Lars was my supervisor on an astronomy project back when I studied at Copenhagen Uni in the 90's. We used a Meade LX200 to take images of the double cluster in Perseus from the rooftop of the old Copenhagen Observatory and calculate the age of the clusters. .
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Hi Rolf,
did you end up with a Color-Magnitude diagram of the cluster(s)?
And if so, was it accurate enough to superpose some isochrones and then replicate the cluster age that has been determined through very precise photometry?
How did your cluster main-sequence look? (well-defined, or noisy?)
I don't see too many amateurs making Color-Magnitude (e.g. B-V or U-B vs. apparent magnitude) diagrams of clusters.
I thought it was interesting that a fairly simple technique using the C-M diagram of the Carina dwarf galaxy's field was able to quite reliably distinguish the stars belonging to this galaxy from the foreground stars belonging to the MW and the LMC. All that would be needed for amateurs to do this kind of work would be the ability to measure accurate magnitudes, though it would not be easy to do at >20 apparent magnitude.
Cheers, Robert