This page was created by the IDL library routine
mk_html_help2.
Last modified: Wed Jul 1 14:02:38 2009.
thm_crib_asi.pro usage: .run thm_crib_asi Written by Harald Frey $LastChangedBy: kenb-win2000 $ $LastChangedDate: 2007-02-11 21:26:08 -0500 (Sun, 11 Feb 2007) $ $LastChangedRevision: 379 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/trunk/idl/themis/examples/thm_crib_asi.pro $
(See themis/examples/thm_crib_asi.pro)
procedure: thm_crib_calc.pro purpose: demonstrate how to use the mini-language program 'calc' usage: .run thm_crib_fgm $LastChangedBy: pcruce $ $LastChangedDate: 2008-09-15 17:05:42 -0700 (Mon, 15 Sep 2008) $ $LastChangedRevision: 3501 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_calc.pro $
(See themis/examples/thm_crib_calc.pro)
Batch File: THM_CRIB_EFI Purpose: Demonstrate the loading, calibration, and plotting of THEMIS EFI data. Calling Sequence: .run thm_crib_fbk, or using cut-and-paste. Arguements: None. Notes: None. $LastChangedBy: jwl $ $LastChangedDate: 2009-06-11 14:54:28 -0700 (Thu, 11 Jun 2009) $ $LastChangedRevision: 6149 $ $URL $
(See themis/examples/thm_crib_efi.pro)
NAME: thm_crib_esa_read_gmoms PURPOSE: This crib shows how to extract the ground-based moments from level 2 ESA data files Note on variable/routine names: Particle variables/routines follow the naming convention th[a/b/c/d/e]_p[e/s][i/e][f/r/b] where th=themis, [a/b/c/d/e]=spacecraft, p=particle, [e/s]=ESA or SST instrument, [i/e]=ion/electron, [f/r/b]=full/reduced/burst distribution 3-dec-2007, jmm, jimm@ssl.berkeley.edu $LastChangedBy: jimm $ $LastChangedDate: 2007-12-03 17:40:09 -0800 (Mon, 03 Dec 2007) $ $LastChangedRevision: 2139 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_esa_read_gmoms.pro $
(See themis/examples/thm_crib_esa_read_gmoms.pro)
Procedure: thm_crib_esa_slice2d
Propose: Example to call the pro file of thm_esa_slice2d. PNG or PS files of ESA (ion or
electron) Distribution Functions for the spacecraft (sc) and the type of data (full, reduced
or burst) would be automatically printed, and the output file would be a 2-D slice of the
3-D distribution function. The detailed slice properties (such as the definition of x and y
axis, the two limits of the slice, etc) can be found in thm_esa_slice2d.
Remarks: You can select a start time and an end time to produce a set of distribution function plots
with the time increments (specified by INCREMENT) no less than 3 seconds. For each plot, it
is allowed to have a longer interval than 3 seconds (specified by TIMEINTERVAL) with the
distribution function being averaged during the whole time interval. Also you need to designate
the folder (specified by OUTPUTFOLDER) that you wish to put the output files.
LAST EDITED BY XUZHI ZHOU 4-24-2008
(See themis/examples/thm_crib_esa_slice2d.pro)
Batch File: THM_CRIB_EXPORT Purpose: Demonstrate tplot export functions Calling Sequence: .run thm_crib_export, or using cut-and-paste. Arguements: None. Notes: None. $LastChangedBy: pcruce $ $LastChangedDate: 2008-09-18 15:48:50 -0700 (Thu, 18 Sep 2008) $ $LastChangedRevision: 3517 $ $URL $
(See themis/examples/thm_crib_export.pro)
Procedure: thm_crib_fac Purpose: A crib on showing how to transform into field aligned coordinates DSL coordinates Notes: $LastChangedBy: jimmpc $ $LastChangedDate: 2009-05-29 15:10:52 -0700 (Fri, 29 May 2009) $ $LastChangedRevision: 6004 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_fac.pro $
(See themis/examples/thm_crib_fac.pro)
Batch File: THM_CRIB_FBK Purpose: Demonstrate the loading, calibration, and plotting of THEMIS FBK (Filter Bank) spectral data. Calling Sequence: .run thm_crib_fbk, or using cut-and-paste. Arguements: None. Notes: None. $LastChangedBy: kenb-mac $ $LastChangedDate: 2007-08-01 22:11:55 -0700 (Wed, 01 Aug 2007) $ $LastChangedRevision: 1319 $ $URL $
(See themis/examples/thm_crib_fbk.pro)
Batch File: THM_CRIB_FFT Purpose: Demonstrate the loading, calibration, and plotting of THEMIS FFT spectra (ParticleBurst and WaveBurst) data Calling Sequence: .run thm_crib_fft, or using cut-and-paste. Arguements: None. Notes: None. Written by Patrick Cruce(with liberal copying from thm_crib_fit.pro)
(See themis/examples/thm_crib_fft.pro)
thm_crib_fgm.pro usage: .run thm_crib_fgm Written by Hannes Schwarzl and Ken Bromund $LastChangedBy: jwl $ $LastChangedDate: 2008-08-04 16:03:31 -0700 (Mon, 04 Aug 2008) $ $LastChangedRevision: 3342 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_fgm.pro $
(See themis/examples/thm_crib_fgm.pro)
Batch File: THM_CRIB_FIT Purpose: Demonstrate the loading, calibration, and plotting of THEMIS FIT (On-Board E- and B-Field SpinFit) data. Calling Sequence: .run thm_crib_fit, or using cut-and-paste. Arguements: None. Notes: None. Written by John Bonnell $LastChangedBy: jimmpc $ $LastChangedDate: 2009-05-29 15:10:52 -0700 (Fri, 29 May 2009) $ $LastChangedRevision: 6004 $ $URL $
(See themis/examples/thm_crib_fit.pro)
pro thm_crib_gmag This is an example crib sheet that will load ground mag data. Open this file in a text editor and then use copy and paste to copy selected lines into an idl window. Or alternatively compile and run using the command: .RUN THM_CRIB_GMAG
(See themis/examples/thm_crib_gmag.pro)
pro thm_crib_make_AE
This is an example crib sheet that will calculate and plot "pseudo" geomagnetic
indices (thmAE, thmAU, thmAL) as derived from THEMIS ground magnetometer data.
In future, it is planned to include ground magnetometer data from other magnetometer
networks. Note that currently the calculation of these "pseudo" indices does not
subtract quiet day variation but simply the median.
Open this file in a text editor and then use copy and paste to copy
selected lines into an idl window.
Written by Andreas Keiling, 15 May 2008
Modifications:
Changed name from thm_crib_AE to thm_crib_make_AE, added print info/stops,
remove DEL_DATA,'*' command, W.M.Feuerstein, 6/2/2008.
$LastChangedBy: jimm $
$LastChangedDate: 2009-02-06 13:01:05 -0800 (Fri, 06 Feb 2009) $
$LastChangedRevision: 4910 $
$URL $
(See themis/examples/thm_crib_make_ae.pro)
pro thm_crib_mom This is an example crib sheet that will load onboard MOMent data. It also shows how to compute moments from the full distributions. Data is corrected for spacecraft potential. Open this file in a text editor and then use copy and paste to copy selected lines into an idl window. Or alternatively compile and run using the command: .RUN THM_CRIB_MOM
(See themis/examples/thm_crib_mom.pro)
Procedure: thm_crib_mva Purpose: A crib on showing how to transform into minimum variance analysis coordinates Notes: $LastChangedBy: jimmpc $ $LastChangedDate: 2009-05-29 15:10:52 -0700 (Fri, 29 May 2009) $ $LastChangedRevision: 6004 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_mva.pro $
(See themis/examples/thm_crib_mva.pro)
NAME: thm_crib_overplot
PURPOSE: this crib describes how to generate overview plots
if there are any arguments or features for these
procedures you would like to request, please feel
free to ask.
$LastChangedBy: pcruce $
$LastChangedDate: 2008-01-30 12:39:05 -0800 (Wed, 30 Jan 2008) $
$LastChangedRevision: 2328 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_overplot.pro $
(See themis/examples/thm_crib_overplot.pro)
PROCEDURE: thm_crib_part_getspec
***** A copy and paste crib *****
PURPOSE:
A crib showing how to create energy and angular spectrograms using
THM_PART_GETSPEC.
DETAILS
THM_PART_GETSPEC is a wrapper that takes user input and creates tplot
variables containing energy and/or angular spectra of ESA and SST data. The
tplot variables created end in 'en_eflux' for energy spectra and 'an_eflux'
plus a suffix corresponding to the type of angular spectrum specified by
the ANGLE keyword for angular spectra by default. The user can select a
range of probe(s), PROBE, and time range, TRANGE, of interest. The energy
range of interest, ERANGE, is specified in eV. The user can also choose to
create tplot variable for one or more data types, DATA_TYPE. The phi, PHI,
and theta, THETA, ranges of interest, specified in DSL coordinates, can also
be input, by the user. SUFFIX specifies a string that will be added to the
*an_eflux*' tplot variables.
If the phi range is greater than 360 degrees, then the phi bins at the
beginning of the phi range are added and wrapped around the end of phi
range. For example, if phi=[0,420], the phi bins corresponding to 0-60
degrees are appended to the top of the plot.
The START_ANGLE keyword specifies the start of the y-axis (phi). This is
useful to center the spectra plot on the y-axis at a particular phi angle.
If this keyword is not set, the y-axis starts at the first angle input to
the PHI keyword.
Use the ENERGY and ANGLE keywords to specify whether to create tplot
variables for energy and/or angular spectra. The ANGLE keyword is also used
to specify the type of angular spectrum created (e.g. phi, theta, pa, gyro).
If neither of ENERGY and ANGLE keywords are specified, then both are turned
on and the angular spectrum type defaults to phi.
When set, the AUTOPLOT keyword enables to the tplot variables to be
automatically plotted using some simple code located at the end of
THM_PART_GETSPEC. The tplot variables created are properly formatted by
THM_PART_MOMENTS2 and THM_PART_GETSPEC whether or not AUTOPLOT is set.
Setting AUTOPLOT will also create a default tplot title containing the
theta, phi, and energy ranges used to create the plot.
After reading in the user's input, THM_PART_GETSPEC then calls THM_LOAD_SST
and/or THM_LOAD_ESA_PKT to load the particle data. THM_PART_MOMENTS2 is
then called to format the spectra data based on the user's input and create
the tplot variables. THM_PART_MOMENTS2 calls THM_PART_GETANBINS in order to
determine which energy/angle bins should be turned on/off. If there's a mode
change, THM_PART_MOMENTS2 will re-call THM_PART_GETANBINS to account for any
changes in the mode's anglemap.
Pitch angle (ANGLE='pa') and gyrovelocity (ANGLE='gyro') spectra are generated
by gridding a globe in a field-aligned coordinate (FAC) system at regular
intervals along pitch (latitude) and gyrovelocity (longitude) as specified by
the REGRID keyword. These FAC angle bins are then rotated back into the
native DSL coordinates of the particle distribution data. The flux assigned
to a given FAC angle bin is determined by native angle bin to which the center
of FAC angle bin has been rotated. So if a FAC angle bin center is rotated
into the 88th angle bin of the probe's particle distribution data, the flux
for that FAC angle bin is the same as the flux in angle bin 88 of the
particle distribution data. This rotation occurs for each time sample of the
probe's particle data.
The size of the FAC system grid is specified with the REGRID = [m,n], a two-
element array in which the first element of the array specifies the number
of grid elements in the gyrovelocity (longitudinal) direction while the second
element sets he number of grid elements in the pitch (latitudinal)
direction. Increasing the number of elements in the FAC system grid will
increase the accuracy of the pitch angle and gyrovelocity angle spectra as it
decreases the degree to which the FAC bins overlap into one or more native
distribution angle bin. Suitable numbers for m and n are numbers like 2^k.
So far, k=2-6 has been tested and work. Other numbers will work provided
180/n and 360/m are rational.
The PITCH and GYRO keywords set the angle range of interest for pitch angle
and gyrovelocity spectra plots similarly to the THETA and PHI keywords.
Setting PHI and THETA will affect pitch angle and gyrovelocity plot, but the
PITCH and GYRO keywords will be ignored when the ANGLE keyword is set to
'PHI' or 'THETA'. Energy spectra, generated by using the /ENERGY keyword, will
also be affected by PITCH and GYRO settings.
The OTHER_DIM keyword specifies the second axis for the field aligned
coordinate system, necessary when plotting pitch angle or gyrovelocity spectra.
See THM_FAC_MATRIX_MAKE for more info. If the keyword is not set in
THM_PART_GETSPEC, OTHER_DIM defaults to 'mphigeo'.
Also, when calculating pitch angle and/or gyrovelocity spectra
THM_FAC_MATRIX_MAKE might require the data be de-gapped in order to
calculate the rotation matrix. If so, the /degap keyword and tdegap keywords
can passed in the call to THM_PART_GETSPEC. See TDEGAP and
THM_FAC_MATRIX_MAKE for more info.
The /NORMALIZE keyword will normalize the flux for each time sample in a
spectra plot to values between 0 and 1.
BADBINS2MASK is a 0-1 array that will be mask SST bins with a NaN to
eliminate artifacts such as sun contamination. The array should have the same
number of elements as the number of angle bins for a given data type. A 0
indicates that will be masked with a NaN. This is basically the output from
the bins argument of EDIT3DBINS.
The DATAGAP is very useful when you want to overlay burst mode spectra plots
over full mode spectra. Set the DATAGAP keyword to a number of seconds that
is less than the time gap of the burst data, but greater than the sample
interval of the underlying full mode data. This way the time gaps between
the burst mode data won't be interpolated by SPECPLOT and cover up the full
mode data between the burst mode data.
NOTES:
- All angles are in DSL coordinates
- All datatypes are now valid
- Theta input must satisfy: -90 < theta[0] < theta[1] < 90
- Phi input must be specified in ascending order in degrees
(e.g. [270, 450] or [-90, 90] to specify the 'daylight' hemisphere in DSL
coordinates)
- Incorporates improvements contained in v1.2
CREATED BY: Bryan Kerr
VERSION: 1.2
$LastChangedBy: bckerr $
$LastChangedDate: 2009-01-14 10:15:19 -0800 (Wed, 14 Jan 2009) $
$LastChangedRevision: 4464 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_part_getspec.pro $
(See themis/examples/thm_crib_part_getspec.pro)
Name: thm_crib_plotxy
Purpose:crib to demonstrate capabilities of plotxy
Notes: run it by compiling in idl and then typing ".go"
or copy and paste.
$LastChangedBy: pcruce $
$LastChangedDate: 2008-02-06 13:43:58 -0800 (Wed, 06 Feb 2008) $
$LastChangedRevision: 2352 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/ssl_general/trunk/tplot/tplotxy.pro $
(See themis/examples/thm_crib_plotxy.pro)
Name: thm_crib_plotxyvec
Purpose:crib to demonstrate capabilities of plotxyvec
Notes: run it by compiling in idl and then typing ".go"
or copy and paste.
The options: hsize,color,hthick,solid, & thick from the arrow
routine are usable in this routine.
$LastChangedBy: pcruce $
$LastChangedDate: 2008-08-04 12:16:47 -0700 (Mon, 04 Aug 2008) $
$LastChangedRevision: 3337 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_plotxyvec.pro $
(See themis/examples/thm_crib_plotxyvec.pro)
Name: thm_crib_plotxyz
Purpose:crib to demonstrate capabilities of plotxyz
Notes: run it by compiling in idl and then typing ".go"
or copy and paste.
SEE ALSO: bin1d.pro,bin2d.pro,plotxyz.pro
$LastChangedBy: pcruce $
$LastChangedDate: 2008-02-06 13:43:58 -0800 (Wed, 06 Feb 2008) $
$LastChangedRevision: 2352 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/ssl_general/trunk/tplot/tplotxy.pro $
(See themis/examples/thm_crib_plotxyz.pro)
********************************************************************** thm_crib_scm.pro : IDL batch file to get, clean and calibrate SCM data with thm_cal_scm K. Bromund O. Le Contel & P. Robert, CETP ********************************************************************** $LastChangedBy: kenb-mac $ $LastChangedDate: 2007-10-02 09:25:57 -0700 (Tue, 02 Oct 2007) $ $LastChangedRevision: 1646 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_scm.pro $
(See themis/examples/thm_crib_scm.pro)
Batch File: THM_SPINFIT
Purpose: Demonstration of finding spin fit parameters for spinning data.
The FIT module calculates the E-Field and B-Field vectors by taking 32 points at equal angles
and fitting a sine wave least squares fit to the data. The best fit of the data is defined by the
formula: A + B*cos() + C*sin(). The module calculates the standard deviation of the fit
called Sigma, and the number of points remaining in the curve called N.
Calling Sequence:
Cut-and-paste the code to the command line.
Arguments:
required parameters:
var_name_in = tplot variable name containing data to fit
keywords:
sigma = If set, will cause program to output tplot variable with sigma for each period.
npoints = If set, will cause program to output tplot variable with number of points in fit.
spinaxis = If set, program will output a tplot variable storing the average over the spin axis dimension
for each time period.
median = If spinaxis set, program will output a median of each period instead of the average.
plane_dim = Tells program which dimension to treat as the plane. 0=x, 1=y, 2=z. Default 0.
axis_dim = Tells program which dimension contains axis to average over. Default 0. Will not
create a tplot variable unless used with /spinaxis.
min_points = Minimum number of points to fit. Default = 5.
alpha = A parameter for finding fits. Points outside of sigma*(alpha + beta*i)
will be thrown out. Default 1.4.
beta = A parameter for finding fits. See above. Default = 0.4
phase_mask_starts = Time to start masking data. Default = 0
phase_mask_ends = Time to stop masking data. Default = -1
sun2sensor = Tells how much to rotate data to align with sun sensor.
Notes:
The module determines which data is more than xN * �N (sN = standard deviation) away from fit,
and removes those points and repeats the fit. The second time the standard deviation is
smaller so the tolerance is increased a bit. The tolerance xN varies with try as:
Alpha*NBeta, where A=1.4 and Beta=0.4 provide good results. The operation continues
until no points are outside the bounds and the process is considered convergent.
Written by Katherine Ramer
$LastChangedBy: Katherine Ramer$
$LastChangedDate: 2009-05-06 10:57:09 -0700 (Wed, 06 May 2009) $
$LastChangedRevision: 5789 $
$URL $
(See themis/examples/thm_crib_spinfit.pro)
pro thm_sst_crib This is an example crib sheet that will load Solid State Telescope data. Open this file in a text editor and then use copy and paste to copy selected lines into an idl window. Or alternatively compile and run using the command: .RUN THM_SST_CRIB Author: Davin Larson Modified: 2007-07-19 by Matt Davis. This a simplified version of Davin's original crib and is intended to demonstrate the very basics of loading in the SST energy spectrograms. The more comprehensive crib can be found with the SST routines in: idl/themis/spacecraft/particles/SST/thm_sst_crib.pro $Id: thm_crib_sst.pro 1586 2007-09-18 12:42:50Z davin-win $
(See themis/examples/thm_crib_sst.pro)
PROCEDURE: thm_crib_sst_contamination
Purpose: 1. Demonstrate the basic procedure for removal of sun contamination,
electronic noise, and masking.
2.. Demonstrate removal of suncontamination via various methods.
3. Demonstrate the correction of inadvertant masking in SST data
4. Demonstrate scaling data for loss of solid angle in SST measurements.
5. Demonstrate substraction of electronic noise by selecting bins in a specific region
6. Show how to use these techniques for both angular spectrograms,energy spectrgrams, and moments.
SEE ALSO:
thm_remove_sunpulse.pro(this routine has the majority of the documentation)
thm_part_moments.pro, thm_part_moments2.pro, thm_part_getspec.pro
thm_part_dist.pro, thm_sst_psif.pro, thm_sst_psef.pro,thm_sst_erange_bin_val.pro
thm_crib_part_getspec.pro
$LastChangedBy: jimmpc $
$LastChangedDate: 2009-05-29 15:10:52 -0700 (Fri, 29 May 2009) $
$LastChangedRevision: 6004 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_sst_contamination.pro $
(See themis/examples/thm_crib_sst_contamination.pro)
Batch File: THM_CRIB_STATE Purpose: Demonstrate the loading, coordinate transformation, plotting and labeling with state data Calling Sequence: .run thm_crib_state, or using cut-and-paste. Arguements: None. Notes: None. $LastChangedBy: jimm $ $LastChangedDate: 2008-05-13 18:02:53 -0700 (Tue, 13 May 2008) $ $LastChangedRevision: 3080 $ $URL $
(See themis/examples/thm_crib_state.pro)
Name: thm_crib_tplotxy
Purpose:crib to demonstrate capabilities of tplotxy
Notes: run it by compiling in idl and then typing ".go"
or copy and paste.
$LastChangedBy: pcruce $
$LastChangedDate: 2008-02-06 13:43:58 -0800 (Wed, 06 Feb 2008) $
$LastChangedRevision: 2352 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/ssl_general/trunk/tplot/tplotxy.pro $
(See themis/examples/thm_crib_tplotxy.pro)
PROCEDURE: thm_crib_tplot_overlay ***** A copy and paste crib ***** PURPOSE: A crib showing how to overlay spectra on top of spectra. DETAILS This crib shows how to combine full and burst mode spectra into one plot by overlaying the burst mode data on top of the full mode data. The DATAGAP keyword is very useful when you want to overlay burst mode spectra plots over full mode spectra. Set the DATAGAP keyword to a number of seconds that is less than the time gap of the burst data, but greater than the sample interval of the underlying full mode data. This way the time gaps between the burst mode data won't be interpolated by SPECPLOT and cover up the full mode data between the burst mode data. CREATED BY: Bryan Kerr
(See themis/examples/thm_crib_tplot_overlay.pro)
Name: thm_crib_trace
Purpose:crib to demonstrate use of Tsyaganenko trace routines, and means for generating plots of trace routines.
Notes: run it by compiling in idl and then typing ".go"
or copy and paste. If you want, you can just edit the parameters for the
routine and run it as is.
SEE ALSO: idl/external/IDL_GEOPACK/trace/ttrace_crib.pro
idl/ssl_general/cotrans/aacgm/aacgm_example.pro
idl/themis/examples/thm_crib_tplotxy.pro
$LastChangedBy: pcruce $
$LastChangedDate: 2008-09-18 15:48:50 -0700 (Thu, 18 Sep 2008) $
$LastChangedRevision: 3517 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/thmsoc/tags/tdas_5_11/idl/themis/examples/thm_crib_trace.pro $
(See themis/examples/thm_crib_trace.pro)
**********************************************************************
thm_crib_twavpol.pro : with twavpol.pro
**********************************************************************
This version stores these outputs as tplot variables with the
specified prefix
These are follows:
Wave power: On a linear scale, at this stage no units
Degree of Polarisation:
This is similar to a measure of coherency between the input
signals, however unlike coherency it is invariant under
coordinate transformation and can detect pure state waves
which may exist in one channel only.100% indicates a pure
state wave. Less than 70% indicates noise. For more
information see J. C. Samson and J. V. Olson 'Some comments
on the description of the polarization states
of waves' Geophys. J. R. Astr. Soc. (1980) v61 115-130
Wavenormal Angle:
the angle between the direction of minimum
variance calculated from the complex off diagonal
elements of the spectral matrix and the Z direction
of the input
ac field data. For magnetic field data in
field aligned coordinates this is the
wavenormal angle assuming a plane wave.
Ellipticity:The ratio (minor axis)/(major axis) of the
ellipse transcribed by the field variations of the
components transverse to the Z direction. The sign
indicates the direction of rotation of the field vector in
the plane. Negative signs refer to left-handed
rotation about the Z direction. In the field
aligned coordinate system these signs refer to
plasma waves of left and right handed
polarisation.
Helicity:Similar to Ellipticity except defined in terms of the
direction of minimum variance instead of Z. Stricltly the Helicity
is defined in terms of the wavenormal direction or k.
However since from single point observations the
sense of k cannot be determined, helicity here is
simply the ratio of the minor to major axis transverse to the
minimum variance direction without sign.
Written by : Kaori(I'll remember to get her last name soon)
$LastChangedBy: pcruce $
$LastChangedDate: 2007-12-06 14:56:54 -0800 (Thu, 06 Dec 2007) $
$LastChangedRevision: 2161 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/ssl_general/trunk/misc/tplotxy.pro $
(See themis/examples/thm_crib_twavpol.pro)
NAME:
thm_fgm_fit_correlate_tplot.pro
Purpose:
Uses ssl_correlation_shift.pro to do a correlation shift
analysis on the vector lengths(math not cs vectors) of a
selected fgm mnemonic and fit data
CATEGORY:
THEMIS-SOC
CALLING SEQUENCE:
pro thm_fgm_fit_correlate_tplot,fit_name, fgm_name, store_name, correlation_floor = correlation_floor, point_number = point_number, lag_step_number = lag_step_number, time_step_size = time_step_size, bin_size = bin_size
INPUTS:
fit_name: the tplot name of the fit data to be compared. RAW
LEVEL 1 FIT DATA IS REQUIRED, E.G., 'tha_fit'
fgm_name: the tplot name of the fgm_data to be
compared
store_name: the name of a tplot variable in which to store the result
correlation_floor: optional, if set filters all results where
the correlation between functions is too poor(default:0.0)
point_number: optional, the minimum number of points of
overlap necessary to try correlating a bin(default:10)
lag_step_number: optional, checks plus or minus lag_steps * time steps
to correlate the vectors (default:5)
time_step_size: optional, the size of the time step to use when
interpolating and correlating the vectors, in
seconds(default:1/8 seconds)
bin_size: optional, the size of each bin in seconds
(default:60 seconds)
OUTPUTS:
stores the time and the shift values in the selected tplot_var
KEYWORDS:
COMMENTS: This function will probably die horribly if time
values are not monotonic.
PROCEDURE:
EXAMPLE:
MODIFICATION HISTORY:
Written by: Patrick Cruce(pcruce@gmail.com)
2007-06-06 V1.0
KNOWN BUGS: tcs_vector_length doesn't filter NANs so it may output
arithmetic warnings
(See themis/examples/thm_fgm_fit_correlate_tplot.pro)