UVIS Performance Status

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Presentation transcript:

UVIS Performance Status Bill McClintock UVIS Team Meeting 7-10-2006

EUV Sensitivity Comparison EUV sensitivity appears to be stable since the star burn UVIS Team Meeting 7-10-2006

EUV Flat Field Comparison EUV flat field performance appears to be stable since the star burn UVIS Team Meeting 7-10-2006

FUV Sensitivity Comparison FUV sensitivity appears to continuously decline at short wavelengths and increase at long wavelengths UVIS Team Meeting 7-10-2006

FUV Flat Field Comparison Star burned rows have significant degradation UVIS Team Meeting 7-10-2006

FUV Sensitivity Comparison FUV flat field shows evidence for Lyman Alpha ‘burn in’ UVIS Team Meeting 7-10-2006

Calibration Red Patch 1999-016 Center Occultation lens in place 2001-299 Mosaic 2002-155 Center (Star burn) 2002-198 Slit Drift-Spica Flat Field 2003-140 Slit Drift-Spica Flat Field 2005-029 Slit Step (12 rows) 2005-115 Slit Step (12 rows) 2005-217 Slit Step (12 rows) 2005-295 Slit Step (64 rows) 2006-037 Slit Drift (64 rows) 2006-079 Slit Step (12 rows) 2006-115 Slit Drift (14 rows) UVIS Team Meeting 7-10-2006

Calibration Red Patch Based on 1999-016 observation, which included the occultation lens Lens transmission removed using the ratio of 2001-093 lens/no lens observations. Red patch corrector derived using the 2005-295 long-slit scan (all 64 rows) Corrects the row to row variations in the flat field but not the column to column variations Use FUV_red_patch_1 if there is no additional row to row flatfield corrector Use FUV_red_patch_1_w_as_ff if you also apply Andrew Steffl’s flat field corrector UVIS Team Meeting 7-10-2006

Calibration Red Patch Except for the star burned rows, the shape of row to row FUV sensitivity is constant to ~ 20%. Star burn UVIS Team Meeting 7-10-2006