# Finding Flares¶

First you’ll need a de-trended light curve (Find out how here.). If you have a raw FlareLightCurve we can call rawflc, for Kepler and TESS light curves use:

>>> flc = rawflc.detrend("savgol")


K2 is more difficult, and computationally intense, but doable with:

>>> flc = rawflc.detrend("k2sc")


Now you have a de-trended light curve flc, and you can search it for flares:

>>> flc = flc.find_flares()


This will return the initial light curve with a new attribute - flares, which is a DataFrame with the following columns:

• ampl_rec - recovered amplitude measured relative to the quiescent stellar flux
• ed_rec - recovered equivalent duration of the flare, that is, the are under the light curve with quiescent flux subtracted.
• ed_rec_err - the minimum uncertainty on equivalent duration derived from the uncertainty on the flare flux values (see Davenport (2016) for details, Eq. (2)).
• cstart, cstop, istart, istop, tstart, tstop - start and end of flare candidates in units of cadence, array index and actual time in days.