Hello friends.
The fact is that following some of the threads that have opened my friend Oscar in "The Edge of the Cosmos" and where masterfully shows us the wonders of the visual that are open clusters, have resumed a project that had something left and that started long ago in the hands of Dr. Hugo Levato, an astrophysicist in Argentina. The work is aimed at conducting a study on the population of binary star clusters.
Well, today when I was taking a look at the double open cluster Berkeley 58, located about 7.2 ' Cassiopeiae CG (Delta Cephei type variable), I noticed STI 1249 (258 ยบ rho theta 20 ") that surprisingly and as Cassiopeiae CG is also located about 7.2 'northeast of the center of the cluster.
turns out that the component "A" of this dual discovered by Stein in 1913 and so far only three times, seems to have a partner "C" with a proper motion similar and is not shared by "B".
Here is a picture of the 1249 ITS Berkeley about 58 ...
And this one showing the RGB composite showing the movements of the components "A" and "C?".
The data for each of the components:
ID:
"A" ... ... 2MASS 00004277 +6103260
"B" ... ... 2MASS 00004007 +6103219
"C" ... ...
2MASS 00004089 +6103105
Magnitude V:
"A" ... ... 10.1
"B" ... ... 12.5
"C" ... ... 14.3 pM
UCAC3:
"A" (+90.1 +22.5)
"B" (-7.5-2.9)
"C" (?? ??)
And finally an animation so you can appreciate that the movement itself (which seems common ...) of the components "A" and "C" means that, over the years drift away from the component "B".
Although as usual would be needed to confirm, which distances and proper motions of "A" and "C" are compatible, I would almost say that the component connected physically with the 1249 STI primary is that I actually presented as "C".
you soon.
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