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Douglas Tucker, 11/12/2012 06:08 PM
MJD56241-i¶
Form of the Photometric Equation¶
i_std = -2.5log10(counts[ADU]/sec) - a_i - k_i*X - b_i*( (i-z)_std - 0.09) ) where: i_std is the standard, or calibrated, magnitude of the star (i-z)_std is the standard, or calibrated, i-z color of the star a_i is the photometric zeropoint in i k_i is the first-order extinction in i b_i is the instrumental color term coefficient in i X is the airmass 0.09 is a "fiducial" reference color for stars in i-z (based on SDSS experience) Note that there is a separate photometric zeropoint (a_i) and instrumental color term coefficient (b_i) for each CCD.
NCSA Processing Results¶
- psmFitDESDM-20121109i.csv : CSV file of Fit to the Photometric Equation
- PSM_QA_res_vs_ccd_20121109i.jpg : Residuals vs. Airmass
- PSM_QA_res_vs_color_20121109i.jpg : Residuals vs. Color
- PSM_QA_res_vs_mag_20121109i.jpg : Residuals vs. Magnitude
- PSM_QA_res_vs_mjd_20121109i.jpg : Residuals vs. MJD
- PSM_QA_res_vs_imageid_20121109i.jpg : Residuals vs. Image ID
- PSM_QA_res_vs_focalplaneXY_20121109i.jpg : Residuals vs. x,y Position on Focal Plane
- PSM_QA_res_20121109i.txt : Residuals in Tabular Format