1. You will find here simulated light curves containing short duration flares and eclipses, created with SIXTE and SRCTOOL.
Some basic infos:
* The SIXTE event files were created for a source flux of 1e-11 erg/s, with a power-law spectrum (nH=0.5, Gamma=2).
* The input light curves for SIXTE are defined by (H=heaviside function, t=time):
a) FLARE: P1+P2*H(t-P3)*exp(-(t-P3)/P4) with P1=base level, P2=amplitude, P3=start of flare, P4=decay constant
b) ECLIPSE: P1-P2*H(t-P3)*(1-H(t-P4)) with P1=base level, P2=amplitude, P3=eclipse ingress, P4=eclipse egress
with total duration of ~40s (single scan) and time sampling of 0.1 s
* From the event files created by SIXTE, light curves are generated using the eSASS SRCTOOL, with 2 s time sampling.
Example of light curves (3 with flares and 3 with eclipses, 7 telescopes merged):
flare_am05.2_du07.6_040_LightCurve_source_1.fits
flare_am11.0_du04.5_040_LightCurve_source_1.fits
flare_am15.0_du03.9_040_LightCurve_source_1.fits
eclip_am02.0_du16.3_040_LightCurve_source_1.fits
eclip_am04.0_du21.1_040_LightCurve_source_1.fits
eclip_am05.8_du25.9_040_LightCurve_source_1.fits
The value of the simulated amplitude (P2) and flare/eclipse duration (P4, in s), is indicated in the file name.
2. The code to perform flare, eclipse and linear model fits is available here (*):
The algorithm was developed within the EXTraS project (aperiodic variability working group).
The returned parameters are: non-reduced chi-square, d.o.f., p-value, parameters values and errors.
The script to read the input light curve, perform the linear/eclipse/flare fit and calculate the signal-to-noise ratio of the flare/eclipse is (*):
An example of how to call the above routines and print output values, is given here (*):
(*) python file to retrieve under "Attachment/get" tabs.