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Institut für Astronomie und Astrophysik

Abteilung Astronomie

Sand 1, D-72076 Tübingen, Germany
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Table of Contents


Several subroutines used in Tübingen for time series analysis.

Index of Subroutines

acf Compute the autocorrelation function of an evenly sample lightcurve
cygx1_rmsflux calculate the rms variability sigma and the mean flux of 1s-lightcurve segments, bin sigma as a function of segment flux and fit a linear function (according to Uttley, Ph. and McHardy, I.M., MNRAS 2001, 323, L26-L30)
dcf compute the Edelson & Krolik discrete correlation function
deadtime_simul modify evenly binned lightcurve (given by a time array and a count rate array) to take into account counting statistics; reproduce the effects of paralyzable (default) or nonparalyzable deadtime of a given length on the count rate; return modified count rate array
dynpsrch produce a dynamical period search of a timeseries and display PSD or \chi^2 of Epoch Fold
dynscarg produce a dynamical scargle periodogram of a timeseries and display PSD OBSOLETE, DO NOT USE!!!!!!!!!!!!!
epferror estimate epoche folding error with monte-carlo simulation approach.
getphase.pro NO EXPLANATION
gtimerge combine and purify two gti lists
lc_done Simulate a light-curve with a power-law distributed periodogram
lssm_process return a one dimensional LSSM model evenly time series state equation : x(t) = 'AR[p]_process' observation equation : y(t) = C*x(t)+noise , noise = N(0,lssmsig)
pfold folds a lightcurve with a given period or frequency and returns the resulting profile
PLOT_PERIOD Plots a periodic data set stacked each period above the other. Gaps are ommited. Period is aligned acording first element of time array modulo period (i.e. first shown plot always contains first time tag).
pp_correlate correlates a pulse profile with a template profile and returns the index of the shifted profile that matches the template at best
qpo_lc Simulate lightcurves for computation of period significance
qpo_progress display a progress counter and related statistics
rebinlc rebin a time series to a new, evenly spaced, time binning
rmsflux To test the rms-flux correlation (according to Uttley, Ph. and McHardy, I.M., MNRAS 2001, 323, L26-L30), rmsflux.pro calculates the mean PSD and its error of a number of given equally spaced lightcurve segments, that all contain a mean flux within a given range (flux bins). The Miyamoto normalization is used and the PSD is Poisson noise and deadtime corrected.
rndpwrlc Simulate a light-curve with a power-law distributed periodogram
scargle Compute the lomb-scargle periodogram of an unevenly sampled lightcurve
sf Compute the structure function of a lightcurve, according to the definitions given by Nandikotkur et al., 1997, AIP Conf. Proc 410, 1361P for the evenly case and Paltani et al., 1997 A&A 327, 539P for the unevenly case.
shotnoise_process return a Standard Shot Noise model evenly time series s(t) = SUM_{i} h(t-t(i)) where h(t) = exp(-t/tau)*U(t) with U(t) = {0 for t let than 0,h0 for t great equal 0}
timegap find gaps in a time array, determine gap and segment lengths
timmerlc Simulate a light-curve with a general periodogram shape
zhangfunction calculate and return the value of the defined ancillary functions to obtain the autocovariance function in the nonparalyzable dead time case, for the article of Zhang et al., "Dead-time modifications to fast Fourier transform power spectra", The Astrophysical Journal, 449:930-935, 1995

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Jörn Wilms (wilms@astro.uni-tuebingen.de)
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