Page History
TESS provides several data levels , from raw pixels to highly detrended light curve. Users should chose for those investigating time series phenomena. Users should choose which they desire depending on their scientific needs.
| Gliffy Diagram | ||||||
|---|---|---|---|---|---|---|
|
Short Cadence Data
...
The highest level, most processed light curves are ready to search for exoplanets. However, this can remove some of the astrophysical signals. Scientists wanting to study stellar variability may choose to use the conditioned light curve, the Simple Aperture Photometry light curve, or perform their own detrending. The conditioned light curves (PDCSAP_FLUX column) attempt to remove systematic instrumental variations by fitting and removing those signals that are common to all stars on the same CCD. However, this fitting method is sometimes known to remove true astrophysical signals, forcing the user to revert to an earlier data level. For instance, the user can start with the pixel-level data or choose a different method to remove the instrumental systematics from the flux time series.
| Gliffy Diagram | ||||||
|---|---|---|---|---|---|---|
|
...