1. BASIC HYPER SPECTRAL IMAGING
Fred Sigernes 1,2,3,4
1 The University Centre in Svalbard (UNIS), N-9171 Longyearbyen, Norway
2 The Birkeland Centre for Space Science (BCSS)
3 The Kjell Henriksen Observatory (KHO)
4 Centre for Autonomous Marine Operations and Systems (AMOS) NTNU
Lectures: TTK20 Hyperspectral remote sensing, Module 1, AMOS – NTNU, September, 2018.

2. Lecture plan: TTK20 Hyperspectral remote sensing Module 1
Instructor: Adjunct Professor Fred Sigernes
Day 1
09:15 – 11:00
Basic Spectroscopy
13:15 – 15:00
Spectral Designs
Day 2
09:15 – 11:000
System Optics
13:15 – 15:00
Throughput and Etendue
Day 3
09:15 – 11:000
Calibration
13:15 – 15:00
Imaging spectroscopy
Lectures: TTK20 Hyperspectral remote sensing, Module 1, AMOS – NTNU, September, 2018.

3. J. Moen 3, 1, S. Chernouss 4, and C. S. Deehr 5
Sensitivity Calibration of Narrow Field of View
Optical Instruments
F. Sigernes 1, T. Svenøe 2, J. Holmes 1, M. Dyrland 1, D.A. Lorentzen 1,
J. Moen 3, 1, S. Chernouss 4, and C. S. Deehr 5
1 The University Center in Svalbard (UNIS), N-9171 Longyearbyen, Norway.
2 The Norwegian Polar Institute, Ny-Ålesund, Norway
3 Institute of Physics, University of Oslo, Norway
4 Polar Geophysical Institute, Apatity, Russia
5 Geophysical Institute, University of Alaska, Fairbanks, USA

4. BACKGROUND
The increasing number of low light level optical instruments operated in Svalbard (Longyearbyen, Barentsburg and Ny-Ålesund) for monitoring auroras and airglow phenomena emphasizes the need for establishing accurate calibration routines of international standard.
CONTENT
EXPERIMENTAL SETUP AT UNIS
THEORETICAL BASIS
TRANSFER OF LAMP CERTIFICATE
SCREEN BRIGHTNESS CONTROL

5. 2. THE UNIS LABORATORY
(1) 18 x 18 inch2 Lambertian surface, (2) rails, (3) adjustable mobile table, (4) spectrograph, (5) door with baffle, (6) room lights, (7) tungsten lamp, (8) power cable to lamp filament.

6. 1. THEORETICAL BASIS a) Lambertian surface b) Calibration setup
Irradiance certificate
Entering emission rate
Reemitted radiation
Then
Lambert’s Cosine law for intensity
Radiance towards instrument becomes
Total hemispherical emission flux rate
Since inverse square law is
Exitance of screen
The generalized Rayleigh

7. 2. THE UNIS LABORATORY (B) WAVELENGTH CALIBRATION
(A) THE FICS SPECTROGRAPH
Low pressure mercury pen lamp
Mercury vapour tube
Fluorescent tube
Fixed Imaging Compact Spectrograph (FICS SN 7743): (A) concave holographic grating, (B) flat mirror, (C) detector (CCD), (D) fiber bundle, (E) entrance slit
Coefficients
Constants
a 0
x 10 +3
a 1
x 10 0
a 2
x 10 -4
Range 2560 – Å; FWHM ~ 80Å

8. 3. RESULTS TRANSFER OF LAMP CERTIFICATE CERTIFIED 1000W TUNGSTEN
ORIEL SN NIST TRACABLE
SECONDARY STANDARD
200W TUNGSTEN (FRED01)
KEY PARAMETERS:
Exposure time 160 msec
z = 8.56 m
Filter: BK-7
FUNCTIONAL FIT (DOTTED LINE):
a = 73.9 and b =

9. 3. RESULTS SCREEN BRIGHTNESS CONTROL KEY PARAMETERS: Secondary FEL
200W Tungsten
Exposure 160 msec
z = 8.56 m
Filter: BK-7
Distance step = 0.5 m

10. CONCLUDING REMARKS So far:
The optical laboratory at UNIS is constructed according to basic Lambertian theory to calibrate narrow field of view low light level optical instruments.
Secondary certification of a 200W Tungsten lamp has been conducted in the visible part of the spectrum (4000 – 8000 Å).
A procedure to control screen brightness without change in spectral shape by varying the screen-lamp distance from 8 down to 3.5m has been demonstrated in the kR/Å range of the visible spectrum.
Future:
A low power 45W tungsten lamp is needed to calibrate below 1kR.
Secondary certification above 8000 Å requires appropriate cut-off filters.
A new monochromatic need to be installed and ready for use as source to calibrate filters instruments. …