Color Correction

So far all our work has produced magnitudes that are unique to the equipment used to produce them. Many times data may be combined with data taken with outer equipment.

The calibrate the data to a standard will allow it to be useful. To do this, the magnitudes must be corrected with color transformation coefficients. Determining Color Coefficients To determine the color transformation cefficients the first thing that must be done is to image some stadard stars whose BVRI magnitudes are known. In the Winter and early spring, the open cluster M67 proides a good grouping for this purpose.

Figure 1 M67 Open Cluster Figure 2 Finder Chart RA 08h 51m 21s, Dec +11d 46.3’ (2000) Figure 3 BVRI Magnitudes Details Coming Created 1 February 2007 Modified 13 February 2007 Return

Further reading

• Color correction — Wikipedia