Prior to determining flux:

• Ran mode and Sigma filters on simulated blue and visual Double Cluster, with flat background (mean=900, sigma=10)
• Ran star finder, used threshold = pixel Mode + 1*maximum sigma.
• For each cluster of pixels found by algorithm, found approximate centre coordinates of star using:

Aperture Photometry:

• Subract mode filter from image to remove background.
• Set radius around central coordinates of star.
• Sum ADU of each pixel within set radius, gain 'raw flux' value (not true total flux).

• Flux of the brightest star in double cluster as a function of radius:
  
• Radius will be set to 12 from the graph as the flux levels out above 12.

• For simulations, frames are aligned
• For both simulated frames, minimum seperation between stars (in pixels) ~3.
• Match stars with minimum seperation.
• For real data, calculate transformation based on position of brightest star.

• Used following equation to calculate magnitudes of simulated data (simplified from proper magnitude calculation):

• c is a scaling factor - calculated based on difference of original and calculated magnitude of brightest star.
• HR diagram (with c=0):
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• Total stars matched and plotted: 86
• Comparing with input magnitude - set scale factors in reconstructed data to match minimum magnitude point in true data:
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• Also attempted for real data - not properly scaled, and needed to set threshold to mode+5*sigma:
• 
• Total stars matched and plotted: 96