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Figure 1:
Continuum subtracted spectra taken 1![]() ![]() ![]() ![]() ![]() |
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Figure 2: Continuum flux along the Sun-comet line, measured at 5540 Å to 5575 Å. The different colors give the profiles at different nights. Isolated peaks in the profiles are caused by stars within the slit. Positive distance is counted towards the projected solar direction, negative in the antisolar direction. |
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Figure 3:
Continuum flux perpendicular to the Sun-comet
line, measured at 5540 Å to 5575 Å. The different colors give the profiles at different nights. Isolated peaks in the profiles are caused by stars within the slit. Positive distance is counted towards the 270![]() ![]() |
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Figure 4: CN emission flux along the Sun-comet line for different nights. Positive distance values are counted in the projected solar direction, negative values in the antisolar direction. |
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Figure 5:
CN emission flux perpendicular to the Sun-comet line for different nights. Positive distance values are counted in the 270![]() ![]() |
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Figure 6:
CN line flux in the inner coma (![]() ![]() ![]() ![]() ![]() |
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Figure 7:
CN line flux over rotational phase. The values displayed are taken at the 0![]() ![]() |
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