Download presentation

Presentation is loading. Please wait.

Published byMax Sparling Modified over 2 years ago

1
1 st post launch SCIAMACHY calibration & Verification Meeting L1b Astrium Friedrichshafen – Germany 24 July 2002 First Level 1b Spectral Calibration analysis

2
2 Level 1b Spectral Calibration analysis: content The Spectral Calibration philosophy The Iecf Spectral Calibration Algorithm Related Verification Tasks: orbit behaviour Analysis specifics First results Other Spectral Calibration Verification Tasks Recommendations

3
3 The Spectral Calibration Philosophy Objective : to assign a wavelength to each individual SCIA detector pixel during the flight. Method : the relation between pixel index and wavelength is described by a 4 th order polynomial: To derive a set of calibration coefficients two calibration sources, the SLS and the sun, are analysed. Stability : due to ageing of the instrument, the wavelength parameters needs to be updated on a regular basis. Iecf, Instrument Engineering and Calibration Facility, guarantees long term stability of scientific measurements.

4
4 The Iecf Spectral Calibration Algorithm Task : to determine coefficients of the 4 th order polynomial for each channel as function of the orbital regions. Input: Level 1b Newly Calculated Spectral ADS Method : for each polynomial coefficient, given by the Spectral ADS as a function of orbital phase, a harmonic fit has to be performed in order to parameterise the orbital dependence. The coefficients values are then computed for a set of 12 fixed orbital phases:

5
5 Related verification Task: orbit behaviour L1.01.02: Number of orbital regions for spectral calibration L1.09.03: Orbit region dependency Due to the instrument’s thermal environment along the orbit, the spectral calibration can be expected to show orbital dependency. Therefore SLS measurements shall be executed along the entire orbit to investigate whether the number of measurements and the number of orbital regions are sufficient and the orbit phase boundaries are chosen properly.

6
6 Analysis specifics and overview Level 1b product: SCI_NL__0PNPDK20020621_182502_000062172007_00056_01613_0129.N1 Orbits: 1613 States: 10 SLS States (predefined State_ID 59 ), on 87 total States Channel 1 : variation long the orbit is close or less to 1/100 of a pixel Channel 2 : not analysed due to erroneous key-data set used by the Level 0 to 1b processor Channels 3, 4, 5 and 6 : variation long the orbit is close or less to 1/100 of a pixel Channel 7 and 8 : not analysed for no in-flight dark current correction of the the raw lamp spectrum

7
First Results: Orbit dependency for Channel 1 The algorithm performs correctly the harmonic fit of the coefficients. … but is this the best approach to the Spectral Calibration?

8
First Results: Orbit dependency for Channel 3 The algorithm performs correctly the harmonic fit of the coefficients. … but is this the best approach to the Spectral Calibration?

9
First Results: Orbit dependency for Channel 4 The algorithm performs correctly the harmonic fit of the coefficients. … but is this the best approach to the Spectral Calibration?

10
First Results: Orbit dependency for Channel 5 The algorithm performs correctly the harmonic fit of the coefficients. … but is this the best approach to the Spectral Calibration?

11
First Results: Orbit dependency for Channel 6 The algorithm performs correctly the harmonic fit of the coefficients. … but is this the best approach to the Spectral Calibration?

12
First Analysis: the harmonic fit approach for Channel 1 Orbit 1613 Maximum variation long the orbit: 1.1509E-03 nm or 0.01 of a pixel

13
First Analysis: the harmonic fit approach for Channel 3 Orbit 1613 Maximum variation long the orbit: 2.1606E-02 nm or 0.090 of a pixel

14
First Analysis: the harmonic fit approach for Channel 4 Orbit 1613 Maximum variation long the orbit: 1.5229E-03 nm or 0.007 of a pixel

15
First Analysis: the harmonic fit approach for Channel 5 Orbit 1613 Maximum variation long the orbit: 2.0408E-02 nm or 0.07 of a pixel

16
First Analysis: the harmonic fit approach for Channel 6 Orbit 1613 Maximum variation long the orbit: 3.2390E-02nm or 0.041 of a pixel

17
First analysis: variation on the input for Channel 1 Coefficient average long the orbit as reference Maximum variation long the orbit from average: 1.5786E-03 nm or 0.013 of a pixel Maximum variation long the orbit from fit: 1.1509E-03 nm or 0.01 of a pixel

18
First analysis: variation on the input for Channel 3 Coefficient average long the orbit as reference Maximum variation long the orbit from average: 2.2911E-03 nm or 0.010 of a pixel Maximum variation long the orbit from fit: 2.1606E-02 nm or 0.090 of a pixel

19
First analysis: variation on the input for Channel 4 Coefficient average long the orbit as reference Maximum variation long the orbit from average: 1.8100E-03 nm or 0.008 of a pixel Maximum variation long the orbit from fit: 1.5229E-03 nm or 0.007 of a pixel

20
First analysis: variation on the input for Channel 5 Coefficient average long the orbit as reference Maximum variation long the orbit from average: 3.2879E-03 nm or 0.012 of a pixel Maximum variation long the orbit: 2.0408E-02 nm or 0.07 of a pixel

21
First analysis: variation on the input for Channel 6 Coefficient average long the orbit as reference Maximum variation long the orbit from average: 4.2989E-03 nm or 0.006 of a pixel Maximum variation long the orbit: 3.2390E-02nm or 0.041 of a pixel

22
22 First Analysis: Summary

23
23 All Spectral Cal Related Verification Tasks L1.01.02 Number of orbital regions for spectral calibration L1.02.03 Wavelength calibration - selected line list not changes L1.02.04 Slit function parameters unchanged L1.09.01 Verification of precise basis for spectral calibration L1.09.02 Verification of selected lines for calibration L1.09.03 Verify orbit region dependency L1.09.04 Verify whether SLS or Fraunhofer calibration shall be the baseline L1.14.01: Wavelength calibration differences monitoring

24
24 Level 1b Spectral Calibration analysis: Recommendations The approach averaging the coefficients from the Level 1b seems to give better results Fit based on a lower order polynomial shall be investigated …

Similar presentations

OK

SPACE TELESCOPE SCIENCE INSTITUTE Operated for NASA by AURA COS Science Calibration & Instrument Status TIPS 20 Nov 2003 Last COS TIPS Aug 2003.

SPACE TELESCOPE SCIENCE INSTITUTE Operated for NASA by AURA COS Science Calibration & Instrument Status TIPS 20 Nov 2003 Last COS TIPS Aug 2003.

© 2017 SlidePlayer.com Inc.

All rights reserved.

Ads by Google

Ppt on forest society and colonialism free download Ppt on life study of mathematical quotes Ppt on saving natural resources Ppt on swami vivekananda thoughts Ppt on id ego superego definition Download maths ppt on number system for class 9 Ppt on pre ignition Ppt on autonomous car project Ppt on instrument landing system theory Ppt on conservation of endangered species