PAC DATA
Raw data: Only process applied here is the wavelength calibration.
Field of view (~ 70º)centered on the magnetic zenith.
Magnetic zenith
Fig. 1: PAC seeing emissions from an hydrogen lamp [Ha (656.3 nm) and Hb (486.1 nm)]
Magnetic zenith
Fig.2: PAC seeing a clear sky (dominated by the green (557.7 nm) and the red (630.0 nm) lines) with unresolved stars (horizontal lines).
Magnetic zenith
Fig.3: PAC seeing a cloudy sky in the north part (e.g., strong Hg lines around the green line) and a clear sky in the south part.
Magnetic zenith
Fig.4: PAC seeing a sky filled with thick clouds. Around 589.0 nm, presence of an absorption feature from high pressure sodium lights in a near-by town.
Magnetic zenith
Fig.5: Intense electron aurora arcs present at the center of field of view. Intensification of the green (557.7 nm) and the red (630.0 nm) lines, presence of N2 1P bands.
Magnetic zenith
Fig.6: Proton aurora identified with the presence of Ha. Note unresolved stars in the north.
Fig.7: PAC spectra for the center of the field of view, as a function of time, for January 20th, 2002. The sun influence is noticeable before 15:30 UT. The proton aurora starts around 18:30 UT. Several intense electron arcs occur between 19:30 and 22 UT.
Fig.7: PAC spectra for the center of the field of view, as a function of time, for February 1st, 2002.