Physics of Auroral Phenomena
Abstract. Calibration of image intensity is a common problem that hampers the use of TV data in quantitative auroral studies. The availability of simultaneous photometry observations allowed us to carry out relative calibration. An example of such calibration is described in this report. The data of...
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| Format: | Text |
| Language: | English |
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2004
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| Online Access: | http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.1050.7647 http://pgia.ru:81/seminar/archive/2004/2_fields/Kozelov1.pdf |
| Summary: | Abstract. Calibration of image intensity is a common problem that hampers the use of TV data in quantitative auroral studies. The availability of simultaneous photometry observations allowed us to carry out relative calibration. An example of such calibration is described in this report. The data of two instruments located at Barentsburg, Svalbard (78.1 o N, 14.24 o E, 75.17MLAT, 112.1MLON) are used: a TV all-sky camera and a meridian scanning photometer. The scan trajectory in the TV field of view was traced by stars crossings. The calibration procedure was based on comparison of the surrogate keogram constructed from TV data and the keograms really observed by the scanning photometer in 557.7 and 427.8. nm emission spectral bands. The calibration curve (intensity of the auroral emission as a function of TV gray level) was approximated in each 5-degrees interval of zenith angle to obtain the angle dependence. In both cases of aurora emission used, it was found that the calibrated surrogate keogram constructed from TV data reproduced reasonably well the fine small-scale structure of bright aurora observed by the scanning photometer. |
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