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Institut für Astronomie und Astrophysik

Abteilung Astronomie

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dynpsrch Source code in dynpsrch.pro

dynpsrch

Name
       dynpsrch
Purpose
       produce a dynamical period search of a timeseries
       and display PSD or \chi^2 of Epoch Fold
Category
       time series analysis
Calling Sequence
       dynpsrch,tt,rr,file,ghost=ghost,dt=dt,tlen=tlen,
          pmin=pmin,pmax=pmax,numf=numf, /log, /epoch, /nolabel
Input Parameters
       tt:     time
       rr:     count rate
       file:   file name of encapsulated PS-File to be produced
Optional Input Parameters
       dt:     time distance between individual PSDs (default: 4)
       tlen:   length of the individual time series that are used
                 to generate the PSD
       pmin:   minimum period to consider (2.*dt default)
       pmax:   maximum period to consider (tlen/2)
       numf:   number of frequency points (500)
       sig :   significance levels (99, and 99.9 %)
       raterr: error bars for rate. Plot symbols instead of lines.
       sunangdist: angular distance between the sun and the ASM
               object. Make an angular distance versus time plot.
       multiple: number of simulations to obtain the significance
               levels, if not set or <=0, then the significance is
               computed from the standard formula, and not using
               simulations (faster, but not recommended...)
       ylaxisv: The data values for each tick mark for the y left
               axis.
Keyword Parameters
       ghost:  invoke ghostscript after plot is done
       gray:   gray scale plot instead of color
       color:  It's color instead of count rate
       tbin:   Do psym=10 plots, with errors, in a way that will make
                even Joern happy (i.e., gaps are explicit)
       nolabel: Don't put a label on the ASM significance levels!
       log:    Make logarithmic period axes on the plot
       epoch:  Epoch fold instead of Lomb-Scargle (default)
       window: Apply a Welch Window to the data
Output Parameters
       an encapsulated postscript file is produced
Optional Output
       px: PSD values for lomb-Scargle periodogram or \chi^2 values
           for Epoch Fold
       period: period corresponding to each PSD value for
           lomb-Scargle periodogram or trial periods for Epoch Fold
       maxchi2per: period of maximum chi^2 for Epoch Fold
       psdpeaksort : array with the maximum peak from the lom-Scargle
           periodogram pro each simulation
       simsigni : power threshold corresponding to the given
           false alarm probabilities fap according to white
           noise simulations for the PSD;
Restrictions
       it is not checked whether the desired period range is
       meaningful
Procedure
       pieces of length tlen of the time series are transformed
       with the lomb scargle periodogram or epoch folded and then
       are normalized to the maximum value. The result is plotted.
Example

Procedures Used
       Requires: scargle.pro, epfold.pro (=> pfold.pro), jwoploterr,
                 jwmjdaxis, jwdateaxis, open_print, close_print
Revision History
       Version 0.5: 1999/08/07 (dynscarg): Joern Wilms
           (wilms@astro.uni-tuebingen.de)
       Version 0.6: 1999/08/25: Joern Wilms
           I hope the normalization is now finally all right...
       Version 0.7: 1999/08/26: Michael Nowak
           (mnowak@rocinante.colorado.edu)
           Added raterr as an optional input, color as a keyword,
           tbin as a keyword
       Version 0.8 (dynpsrch): 1999/10/21: Michael Nowak
           Added log as a keyword, to produce logarithmic plots
           Added epoch as a keyword, to do an epoch fold instead
           tvscal now centers pixels on mid-point of PSD/Fold, &
             width of plot is now more carefully calculated
           pmin is defaulted to 2.*dt
       Version 0.9: 1999/11/02: Michael Nowak
           Following Padi Boyd's suggestion, added padding of lightcurves
             to allow dynamical PSD to be done over whole lightcurve range.
           Added keyword to window function the lightcurve with a
             Welch window.
       Version 1.0: 1999/11/30: Sara Benlloch
           Added sunangdist as a optional input, to plot the angular
           distance between the sun and the ASM object versus the
           time, in order to check the sun influence.
       Version 1.1: 2000/08/31: Sara Benlloch / J. Wilms
           adopted to new (fast) scargle routine

Last modified by pro2html on 2005 January 04 at 16:45 UTC

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