Preliminary Results from the SOHO Offpoint

August 20, 2002

 

EUV 195 Flat-fields

 

The two following images compare the EUV flat-field derived from calibration lamps, and the flat-field derived from the offpoint data using the Kuh algorithm. The CalLamp-derived flat-field is a bit more noisy, but this should improve soon.

CalLamp-derived Flat-field
Offpoint-derived Flat-field

 

Before and After

Here, "before and after" comparisons in the four wavelengths. The left column shows the raw data, the middle column shows the data corrected with a CalLamp-derived flat-field, and the right column shows the data corrected with the offpoint-derived flat-field. Obviously, our current model of the degradation is not that bad ! The scaling is the same in all the images so you can see that not only does the flat-field correct for spatial variations, but also for the overall flux. The remaining dark (and noisy) patches are regions where the combination of a low photon flux with a very poor response of the CCD produced a very weak or inexistent signal. You simply can't recover any information where there was no signal in the first place !

Preliminary analysis confirms the relationship between the CCD response in the visible and in the EUV, and the weak wavelength dependance in the EUV between the short (171/195) and long (284/304) wavelength channels of EIT.

Raw data
CalLamp-derived Correction
Offpoint-derived Correction

1
7
1

1
9
5

2
8
4

3
0
4

 

Web curator: Frédéric Auchère
Responsible NASA official: Joseph B. Gurman, Facility Scientist, Solar Data Analysis Center
joseph.b.gurman@gsfc.nasa.gov
+1 301 286-4767
NASA Goddard Space Flight Center
Solar Physics Branch / Code 682

Last revised: Tuesday, August 20, 2002 4:31 PM - F. Auchère