Hyperspectral imaging of aurora and airglow at KHO Fred Sigernes 1,*, Yuriy Ivanov 2, Sergey Chernouss 3, Trond Trondsen 4, Alexey Roldugin 3, Yury Fedorenko 3, Boris Kozelov 3, Andrey Kirillov 3, Ilia Kornilov 3, Vladimir Safargaleev 3, Silje Holmen 1, Margit Dyrland 1, Dag Lorentzen 1 and Lisa Baddeley 1 1 The University Centre in Svalbard (UNIS), N-9171 Longyearbyen, Norway 2 Main Astronomical Observatory, National Academy of Sciences, Ukraine 3 Polar Geophysical Institute, Murmansk Region, Apatity, Russia 4 Keo Scientific Ltd., Calgary, Alberta, Canada MLTI Waves and Dynamics at Polar Latitudes Workshop, Utah State University, 9-11 October 2012

THE KJELL HENRIKSEN OBSERVATORY – KHO Prof. Dr 2 K. Henriksen KHO 1) Instrumental module (30x) 2) Service Section 3) Platform Summer view Location More info at:

KHO TELESCOPE IN ADDITION a)Magnetometers b)Scintillation receivers (GPS) c)Riometer d)Weather station e)Web cameras

KHO 1.University Centre in Svalbard 2.University of Oslo 3.University of Tromsø 4.University of Alaska, Fairbanks 5.University College London 6.University of Wales Aberystwyth 7.University of Southampton 8.University of New Hampshire 9.Augsburg College 10.Tohoku University 11.National Institute of Polar Research Japan 12. Finnish Meteorological Institute 13.Embry Riddle Aeronautical University 14.Danish Meteorological Institute * 15.Air Force Research Laboratory * 16.Laboratoire de Planétologie de Grenoble 17.Institute of Radio Astronomy 18.AVINOR 19.The Polar Institute of China 20.The University of Electro-Communications Tokyo The 10 KHO … & excellent students!

LYR INTERNET KHO - UNIS – ARS - MINE 7

HYPERSPECTRAL IMAGING AT KHO Picture of the assembled Spextube Imagers. M is rotary table, T front surface mirror, L1 front lens, A 35mm camera lens adapter, O laser pointer, B barrel contains spectroscope, L3 camera lens, CCD camera head, I lift table, and E two steel bars. Inspired by SP3 (1993). Fiskeriforskning (1997) The FishTube spectrograph

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(a)Airspex 1 Imager (b)(b) video camera (c)(c) tripod (d)(d) dome Airspex 2 Imager – Swedish version! AGF331 Remote Sensing and Advanced Spectroscopy ( ) The Oriel FICS spectral imager Experimental setup Dornier Dronespex I-IV

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Electronic Machine Shops ~14 days Purchase optics and mounts FS-IKEA ? AURORAL LOW LIGHT HYPERSPECTRAL IMAGING?

The NORUSCA All-sky cameras Two NORUSCA II 1st Generation all-sky cameras (A) and (B). (1) Front element of all-sky lens, (2) 24 x 4 inch2 mount plate, (3) collimator lens tube, (4) lens mount, (5) ring holders, (6) filter box, (7) camera lens, and (8) EMCCD detector. Instrumental volume is ~ 65 x 18 x 16 cm3. Total mass is 8.9 kg. NORUSCA II-E fish-eye lens specifications Spectral range 430 – 750 nm Paraxial focal length3.5 mm F-numberf/1.1 Number of lens elements12 Field of view 180 º (circular) Filter diameter35 mm Angle of incident on filter   7 º Dimensions Ø 110 × 320 mm Camera lens mountC-mount EMCCD detector: - PI ProEM 512B x 8.2 mm deg. air cooled - Back-illuminated; 90% QE

Optical layout and design of the NORUSCA II Camera Lens mechanics and optical diagram of the NORUSCA II all-sky lens: (1)focusing mechanism and collimator lenses, (2) filter box - chamber, (2)(3) camera lens, and (4) camera head.

The NORUSCA II Point Spread function Resolution: ~ 60 lp/mm

Filter: Liquid Crystal Tunable Filter (LCTF) (Cambridge Research & Instrumentation, Inc.). *P. J. Miller, “Use of Tunable Liquid Crystal Filters to Link Radiometric and Photometric Standards”, Metrologia 28, 145 – 149 (1991). Spectral tuning is obtained by using electronically controlled liquid crystal wave plates to a Lyot filter design*. The wave plates behave as optical birefringent elements with an electrically variable retardance. Retardance is termed the optical path difference between the ordinary and extraordinary rays passing through a birefringent element. The latter is controllable due the effect that the liquid crystal molecules are orientation sensitive to electric fields applied between the plates. Since the retardance is directly linked to wavelength, the filters are tunable. Our filter: 400–720nm 550nm

System performance 1. Focus tests Crossed scatter plots work best Source: 1 mm diameter 1m

System performance 2. Mapping function Mapping function coefficients NORUSCAII all-sky lens R in units of[PIXELS][mm] A0A A1A A2A Source: -1 mm diameter pinhole -Schott NG9 -Distance = 1m -Rotation in steps of 10 deg. 2nd order polynomial fit: R is for  > 30º in-between the mapping functions of an equal area and an orthographic fisheye lens, and its maximum R max = 4.08 mm at  = 90 º matches the size of the EMCCD. Note:

System performance 3. Spectral characteristics - center pixel! [mW m -2 nm -1 ] [R s CTS -1 ]

System performance 3. Spectral characteristics – auroral emissions Channel # Wavelength [nm] Emission species FWHM [nm] Calibration factor [R s CTS -1 ] N2+N [OI] [OI] N2+N Background HH NII NII NaI [OI] HH N 2 1P(6-3) N 2 1P(5-2) N2N Background The minimum detection threshold signal is assumed to be 3 times the dark noise level, or 3  = 150 CTS/s. For the green [OI] nm emission, the minimum detection limit then becomes 550 R.

First Samples Screen dump of raw data from the camera at 630 nm. View from authors office desk at UNIS. Exposure time 10 ms at gain 40. Composite RGB color image. Red (R) nm, green (G) nm and blue (B) nm. Or …

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Raw data January :15:03 UT

Nightside aurora Media 1 Panel (A): Color composite image from the NORUSCA II camera 24th of January 2012 at 15:15 UT. Location is the Kjell Henriksen Observatory (KHO). The Red color component of the image is at center wavelength 630 nm, Green at nm and Blue at nm

Dayside aurora Panel (A): Color composite image from the NORUSCA II camera 29 th of December 2011 at 08:55:00UT. Location is the Kjell Henriksen Observatory (KHO). The Red color component of the image is at center wavelength 630 nm, Green at nm and Blue at nm. Media 2

Concluding remarks (preliminary) NORUSCA II: New hyperspectral all-sky camera (430 – 720 nm). Wavelength element (filter): LCTF with FWHM = nm. Novel C-mount NORUSCA II–E All-sky lens f/value=1.1. Detects ~1/2 kR of auroral emissions in just 1 sec. No moving mechanical parts to swap center wavelength. It uses 50 ms to swap between 41 available center wavelengths. Opens for new processing methods such as classification The major disadvantage of the system is the low transmission of the LCTF, especially in the blue part of the spectrum.

Acknowledgement We wish to thank The Research Council of Norway through the project named: Norwegian and Russian Upper Atmosphere Co-operation On Svalbard part 2 # /S30 (NORUSCA2).