The plots are updated as and when the data becomes available, usually the delay is of the order of one day.
Sometimes, the very recent data shows dips down to very low fluxes or longer gaps than the actual gaps in observations.
This is an artifact due to inaccuracies in
predicted spacecraft orbit, resulting in consideration that the XSM is viewing the Sun while it is occulted by the Moon. Typically, these get updated in 5-7 days when revised spacecraft ephemeris becomes available after orbit determination.
The fluxes shown are obtained by integrating the observed spectrum with XSM over the specified energy range. Complete spectral
data is available for download from Chandrayaan-2 Data Archive at ISSDC.
Durations marked by shaded background and red color for the flux correspond to the periods when the beryllium window
is present in front of the detector attenuating the flux at lower energies, below 2 keV. Thus, during these periods, the fluxes shown
are scaled to the 1-8 Angstrom / 1-15 keV range from the measured flux above 2 keV, and would be slightly under estimated.
There are periods when the Sun is not visible for multiple days with XSM and if the selected date range
contains only such periods then the plot window will show "No solar observations available".
See Observing seasons and Visibility for more details.
For observations in during Noon-Midnight seasons where the observations are sparse, the uncertainties in fluxes may be
up to 10-15%.
Any periodic variations seen in the flux over orbital periods of ~120 minutes should be ignored
as such variations could be due to the uncertainties in the effective area correction.
