Background flux back

How dark is your sky? Compare it with other locations!

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CCD images can be used to determine sky-glow intensity. Simple measurements of background (the “empty space” between stars) counts (ADU) are sufficient to compare skies that have been imaged with the same scope, camera, setup, filter, and exposure time. Because CCD is a linear detector, ADU measurements reveal the relative brightness of different skies (for example an image with background 1000 ADU accumulated twice as many sky-glow photons as an image with 500 ADU background).

Thanks to Stan Moore who developed the basics and calculation for the background flux.

NOTE: He is currently working on a more robust and generalized model that will compute background photon flux and mag/arcsec2 for any camera and common filters.

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