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Procedure: clear_esa_common_blocks
Purpose: Clears common blocks used in esa_pkt routines, to
avoid using old data to create plots or L2 files
jmm, jimm@ssl.berkeley.edu, 12-dec-2007
$LastChangedBy: pcruce $
$LastChangedDate: 2012-02-07 13:47:46 -0800 (Tue, 07 Feb 2012) $
$LastChangedRevision: 9692 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/clear_esa_common_blocks.pro $
(See projects/themis/spacecraft/particles/ESA/clear_esa_common_blocks.pro)
NAME: rtbis PURPOSE: Simple bisection routine, CALLING SEQUENCE: x = rtbis(func_in, x1, x2, xacc=xacc, jmax=jmax) INPUT: func_in = an input function -- the answer will give func_in(x) = 0.0 x1 = a lower limit x2 = an upper limit KEYWORDS: xacc = the accuracy, default is 1.0e-6 jmax = max. number of iterations, the default is 40 HISTORY: Copied from Numerical Recipies, 12-feb-2015, jmm, jimm@ssl.berkeley.edu
(See projects/themis/spacecraft/particles/ESA/thm_esa_dens2scpot.pro)
THM_ESA_DIST2SCPOT The program THM_ESA_DIST2SCPOT estimates the spacecraft potential from the electron distribution by lookng for photoelectrons at low energies. It estimates potential by comparing the slope of the low energy electron distribution to the expected slope of secondary electrons. (The slope of the secondary electron distribution is approximately -2.0, see McFadden etal. 2008SSRv..141..477M) For a given time interval, the procedure is as follows: 1) Calculate the slope of the electron distribution. The slope of the distribution between the energies E0, and E1 is given by: M = (log(F1)-log(F0))/(log(E1)-log(E0), where F is the differential electron energy flux in eV/sec/cm^2/eV. 2) Next we Compare the low-energy slope with the expected slope of secondary electrons, which is estimated to be between -2.0 at 8 eV and -4.0 at 50 eV. (These numbers are empirical, except for the lower limit). The upper limit of the photoelectron part of the distribution is estimated to be the highest energy for which the slope is steeper than the secondary electron slope. 3) Also, the electron distribution has to exhibit at least two distinct peaks, a low-energy peak must be present with electron flux greater than 3.0e7 eV/sec/cm^2/eV, and a higher energy peak with electron flux greater than 1.0e-3 times the value of the overall peak of the distribution. (These parameters are the default values, and can be changed via the photoelectron_threshold and noise_threshold.) 4) Since slopes are calculated between energy values, the estimate for M is at the midpoint between E0 and E1. We 'unquantize' by an amount that depends on the difference between the actual slope and the secondary electron slope, so that the final value of the estimated potential is: ; SC_POT = E0+(E1-E0)*(1-M/2)/(1-M) For M=2, the lowest possible value, SC_POT = E0. For an infinite slope, SC_POT is the midpoint between E0 and E1. 5) If the test for low energy photoelectrons fails, i,e, the distribution does not show two peaks, OR the low energy, possible photoelectron peak is below 3.0e7, OR the low energy slope is not steeper that the secondary electron slope, OR if there is a high energy peak, but one that is too small. Then the value for the SC_POT estimate is set to the lowest energy in the electron distribution. Batch File: THM_CRIB_ESA_DIST2SCPOT Purpose: Demonstrates the use of THM_ESA_EST_DIST2SCPOT. The program THM_ESA_EST_DIST2SCPOT estimates the spacecraft potential using the ESA electron distribution. The SC potential is estimated by comparison of the slope of the low energy electron flux with the expected slope of secondary electrons Calling Sequence: .run thm_crib_esa_dist2scpot, or using cut-and-paste. Arguements: None. Notes: None. $LastChangedBy: jimm $ $LastChangedDate: 2015-07-24 15:57:59 -0700 (Fri, 24 Jul 2015) $ $LastChangedRevision: 18252 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_crib_esa_dist2scpot.pro $
(See projects/themis/spacecraft/particles/ESA/thm_crib_esa_dist2scpot.pro)
NAME:
thm_esa_cmn_l2concat
PURPOSE:
concatenates two THEMIS ESA L2 data structures
CALLING SEQUENCE:
dat = thm_esa_cmn_l2concat(dat1, dat2)
INPUT:
cmn_dat = a structrue with the data:
PROJECT_NAME STRING 'THEMIS'
SPACECRAFT STRING 'c'
DATA_NAME STRING 'IESA 3D Reduced'
APID INT 1109 (Apids in filenames are hex values)
UNITS_NAME STRING 'eflux'
UNITS_PROCEDURE STRING 'thm_convert_esa_units'
VALID BYTE Array[ntimes]
TIME DOUBLE Array[ntimes]
END_TIME DOUBLE Array[ntimes]
DELTA_T DOUBLE Array[ntimes]
INTEG_T DOUBLE Array[ntimes]
DT_ARR FLOAT Array[ntimes,88, 8]
CONFIG1 BYTE Array[ntimes]
CONFIG2 BYTE Array[ntimes]
AN_IND INT Array[ntimes]
EN_IND INT Array[ntimes]
MODE INT Array[ntimes]
NENERGY INT Array[8] ;there are 8 different possible
;modes
ENERGY FLOAT Array[32, 8]
DENERGY FLOAT Array[32, 8]
NBINS INT Array[8]
THETA FLOAT Array[32, 88, 8]
DTHETA FLOAT Array[32, 88, 8]
PHI FLOAT Array[32, 88, 8]
DPHI FLOAT Array[32, 88, 8]
DOMEGA FLOAT Array[32, 88, 8]
GF FLOAT Array[32, 88, 8]
ECLIPSE_DPHI DOUBLE Array[ntimes]
PHI_OFFSET FLOAT Array[ntimes]
GEOM_FACTOR FLOAT 0.00153000
DEAD FLOAT 1.70000e-07
MASS FLOAT 0.0104389
CHARGE FLOAT 1.00000
SC_POT FLOAT Array[ntimes]
MAGF FLOAT Array[ntimes, 3]
BKG_PSE FLOAT Array[ntimes]
BKG_PEI FLOAT Array[ntimes]
BKG FLOAT Array[ntimes]
BKG_ARR FLOAT Array[32, 88, 8]
Added in this program
BINS BYTE Array[ntimes, 32, 88]
EFF FLOAT Array[ntimes, 32, 88]
EFLUX FLOAT Array[ntimes, 32, 88];
NENERGY_MODES BYTE 8
NBIN_MODES BYTE 8
DATA_QUALITY INT Array[ntimes]
OUTPUT:
dat = a single structure concatenated
HISTORY:
Hacked from FAST ESA version 24-Oct-2022, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2022-11-08 11:44:09 -0800 (Tue, 08 Nov 2022) $
$LastChangedRevision: 31250 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2concat.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2concat.pro)
NAME:
thm_esa_cmn_l2read.pro
PURPOSE:
Inputs a THEMIS ESA common block structure from an L2 CDF.
CALLING SEQUENCE:
cmn_dat = thm_esa_cmn_l2load(filename, trange = trange, cdf_info=cdf_info)
INPUT:
filename = the input filename
OUTPUT:
cmn_dat = a structrue with the data:
e.g.,
PROJECT_NAME STRING 'THEMIS'
SPACECRAFT STRING 'c'
DATA_NAME STRING 'IESA 3D Reduced'
APID INT 1109 (Apids in filenames are hex values)
UNITS_NAME STRING 'eflux'
UNITS_PROCEDURE STRING 'thm_convert_esa_units'
VALID BYTE Array[ntimes]
TIME DOUBLE Array[ntimes]
END_TIME DOUBLE Array[ntimes]
DELTA_T DOUBLE Array[ntimes]
INTEG_T DOUBLE Array[ntimes]
DT_ARR FLOAT Array[ntimes,88, 8]
CONFIG1 BYTE Array[ntimes]
CONFIG2 BYTE Array[ntimes]
AN_IND INT Array[ntimes]
EN_IND INT Array[ntimes]
MODE INT Array[ntimes]
NENERGY INT Array[8] ;there are 8 different possible
;modes for reduced electrons
ENERGY FLOAT Array[32, 8]
DENERGY FLOAT Array[32, 8]
NBINS INT Array[8]
THETA FLOAT Array[32, 88, 8]
DTHETA FLOAT Array[32, 88, 8]
PHI FLOAT Array[32, 88, 8]
DPHI FLOAT Array[32, 88, 8]
DOMEGA FLOAT Array[32, 88, 8]
GF FLOAT Array[32, 88, 8]
ECLIPSE_DPHI DOUBLE Array[ntimes]
PHI_OFFSET FLOAT Array[ntimes]
GEOM_FACTOR FLOAT 0.00153000
DEAD FLOAT 1.70000e-07
MASS FLOAT 0.0104389
CHARGE FLOAT 1.00000
SC_POT FLOAT Array[ntimes]
MAGF FLOAT Array[ntimes, 3]
BKG_PSE FLOAT Array[ntimes]
BKG_PEI FLOAT Array[ntimes]
BKG FLOAT Array[ntimes]
BKG_ARR FLOAT Array[32, 88, 8]
DATA_LEVEL STRING 'Level 2'
BINS BYTE Array[ntimes, 32, 88]
EFF FLOAT Array[ntimes, 32, 88]
EFLUX FLOAT Array[ntimes, 32, 88]
NENERGY_MODES BYTE 8
NBIN_MODES BYTE 8
DATA_QUALITY INT Array[ntimes]
KEYWORDS:
trange = if set, then only input data for that time range, the first
step would be to input the record times and then obtain a
record range to input.
cdf_info = the full structure from CDF_LOAD_VARS2
gatt = the global attributes from the CDF file
vatt = the variable attributes for the variables included in the output
HISTORY:
2022-10-31, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2022-11-07 12:26:32 -0800 (Mon, 07 Nov 2022) $
$LastChangedRevision: 31243 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2read.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2read.pro)
NAME: thm_esa_cmn_l2tclip PURPOSE: applies a trange to a THEMIS ESA L2 structure CALLING SEQUENCE: dat = thm_esa_cmn_l2tclip(dat, trange) INPUT: dat1 = a THEMIS ESA L2 3D data structure: e.g., OUTPUT: dat = structure with data only in the input time range NOTES: Only will work if the record varying arrays are 5D or less HISTORY: 8-Nov-2022 jmm, jimm@ssl.berkeley.edu $LastChangedBy: jimm $ $LastChangedDate: 2022-11-08 11:43:51 -0800 (Tue, 08 Nov 2022) $ $LastChangedRevision: 31249 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2tclip.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2tclip.pro)
NAME:
thm_esa_cmn_l2vararr
PURPOSE:
Returns an array with common block variable names for the input
data_name.
CALLING SEQUENCE:
vars = thm_esa_cmn_l2vararr(data_name)
INPUT:
data_name = the data_name for the data type; It turns out that this
is unused since all of the L2 structures have the same
variables
OUTPUT:
vars = a 3, N array with common block variable names for the input
data_name, with three columns, one is the common block name, the second is
the name in the CDF file, the third is 'Y' or 'N' for record
variance.
HISTORY:
24-Oct-2022, jmm, Hacked from fa_esa_cmn_l2vararr
$LastChangedBy: jimm $
$LastChangedDate: 2023-10-30 16:00:06 -0700 (Mon, 30 Oct 2023) $
$LastChangedRevision: 32212 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2vararr.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_cmn_l2vararr.pro)
NAME: thm_esa_dens2scpot CALLING SEQUENCE: scpot = thm_esa_dens2scpot(edat, idat) PURPOSE: Estimates the SC potential from electrona and ions, by choosing the potential that gives ion density = electron density INPUT: edat = 3d data electron structure filled by themis routines get_th?_p??? idat = 3d data ion structure filled by themis routines get_th?_p??? use_n3dnew = if set, use n_3d_new.pro to get densities KEYWORDS: HISTORY: 2023-02-01, jmm, jimm@ssl.berkeley.edu $LastChangedBy: jimm $ $LastChangedDate: 2023-02-06 15:08:13 -0800 (Mon, 06 Feb 2023) $ $LastChangedRevision: 31478 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_dens2scpot.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_dens2scpot.pro)
NAME:
thm_esa_dist2scpot
CALLING SEQUENCE:
scpot = thm_esa_dist2scpot(data)
PURPOSE:
Estimates the SC potential from an electron sepctrum, by comparing
the slope of the electron energy distribution with the slope that
would be expected from secondary electrons.
INPUT:
data = 3d data structure filled by themis routines get_th?_p???
KEYWORDS:
pr_slope = if set, show some diagnostics prints of the slope of the
distribution
noise_threshold = values below Noise_threshold*max(flux) are
considered to be in noise, if there is a positive
slope, it is ignored. The default is 1.0e-3
photoelectron_threshold = Only test for photoelctrons if the flux
is above this value, The default is 1.0e7
HISTORY:
Hacked from spec3d.pro, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2017-10-02 11:19:09 -0700 (Mon, 02 Oct 2017) $
$LastChangedRevision: 24078 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_dist2scpot.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_dist2scpot.pro)
Purpose: Helper function to store single array from specified structure tag as tplot variable(s) Arguments: ptr: pointer to array of data structures name: string of structure tag to use prefix: string prefix of tplot var(s) to be created
(See projects/themis/spacecraft/particles/ESA/thm_esa_dump.pro)
PROCEDURE: thm_esa_energy_extrapolate
PURPOSE: Performs linear extrapolation of esa data to a new set of higher energies
INPUTS:
dist_data:
The esa data structure on which the extrapolation should be performed. (loaded by thm_part_dist_array)
KEYWORDS:
add_energy=add_energy : Adds these energies to the current set of energies for the particle data when extrapolating.
lin_energy=lin_energy : Set this keyword to perform extrapolation on energy, not logarithmic.
lin_counts=lin_counts: Set this keyword to perform extrapolation on counts, not logarithmic
lsquadratic=lsquadratic: Set this keyword to perform least square quadratic extrapolation of count data(see interpol documentation in IDL help.)
quadratic=quadratic: Set this keyword to perform quadratic extrapolation of count data.(see interpol documentation in IDL help.)
lsquares=lsquares: Set this keyword to the number of bins that you want to use for least squares extrapolation of the count data(Uses poly_fit)
spline=spline: Set this keyword to perform spline extrapolation of count data.(see interpol documentation in IDL help.)
trange=trange: Set this keyword to a two element array specifying a subset of the data that the operation should be performed on.(Don't need to modify the whole thing with the same parameters)
error=error: Returns 1 if an error occurred. Returns 0 if operation completed successfully.
bin_select: set the bin numbers that you want to use in the extrapolation
EXAMPLES:
dist_data = thm_part_dist_array(probe='a',type='peef',trange=time_double(['2012-02-08/09','2012-02-08/12']))
thm_part_conv_units,dist_data,error=e
thm_esa_energy_extrapolate,dist_data,add_energy=[100000,70000,50000]
NOTES:
Removes the retrace bin from ESA modes that include retrace.
$LastChangedBy: pcruce $
$LastChangedDate: 2013-01-10 18:10:18 -0800 (Thu, 10 Jan 2013) $
$LastChangedRevision: 11424 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_energy_extrapolate.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_energy_extrapolate.pro)
NAME:
thm_esa_est_dens2scpot
PURPOSE:
For a given probe and date, estimates the SC potential from PEER and PEIR
data, and plots it.
CALLING SEQUENCE:
thm_esa_est_dens2scpot, date, probe, no_init = no_init, $
random_dp = random_dp, plot = plot
INPUT:
date = a date, e.g., '2008-01-05'
probe = a probe, e.g., 'c'
OUTPUT:
a tplot variable 'th'+probe+'_est_scpot' is created
If /random_dp is set, then date and probe are output
KEYWORDS:
trange = a time range
no_init = if set, do not read in a new set of data
random_dp = if set, the input date and probe are randomized, note
that this keyword is unused if no_init is set.
plot = if set, plot a comparison of the estimated sc_pot wht the
value obtained from the esa L2 cdf (originally from
thm_load_esa_pot)
use_n3dnew = if set, use n_3d_new.pro to get densities
HISTORY:
1-feb-2023, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2023-02-06 15:08:13 -0800 (Mon, 06 Feb 2023) $
$LastChangedRevision: 31478 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_est_dens2scpot.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_est_dens2scpot.pro)
NAME:
thm_esa_est_dist2scpot
PURPOSE:
For a given probe and date, estimates the SC potential from PEER
data, and plots it.
CALLING SEQUENCE:
thm_esa_est_dist2scpot, date, probe, no_init = no_init, $
random_dp = random_dp, plot = plot
INPUT:
date = a date, e.g., '2008-01-05'
probe = a probe, e.g., 'c'
OUTPUT:
a tplot variable 'th'+probe+'_est_scpot' is created
If /random_dp is set, then date and probe are output
KEYWORDS:
trange = a time range
no_init = if set, do not read in a new set of data
random_dp = if set, the input date and probe are randomized, note
that this keyword is unused if no_init is set.
plot = if set, plot a comparison of the estimated sc_pot wht the
value obtained from the esa L2 cdf (originally from
thm_load_esa_pot)
esa_datatype = 'peef', 'peer', or 'peeb'; the default is 'peer'
HISTORY:
31-may-2015, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2017-10-02 11:19:09 -0700 (Mon, 02 Oct 2017) $
$LastChangedRevision: 24078 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_est_dist2scpot.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_est_dist2scpot.pro)
NAME:
thm_esa_est_dist2scpot2
PURPOSE:
For a given probe and date, estimates the SC potential from PEER
data, and plots it. This differs from the original
thm_esa_est_dist2scpot.pro in that it uses the "eyeball test"; it
only checks byte-scaled eflux variables.
CALLING SEQUENCE:
thm_esa_est_dist2scpot2, date, probe, no_init = no_init, $
random_dp = random_dp, plot = plot
INPUT:
date = a date, e.g., '2008-01-05'
probe = a probe, e.g., 'c'
OUTPUT:
a tplot variable 'th'+probe+'_est_scpot' is created
If /random_dp is set, then date and probe are output
KEYWORDS:
trange = a time range
no_init = if set, do not read in a new set of data
random_dp = if set, the input date and probe are randomized, note
that this keyword is unused if no_init is set.
plot = if set, plot a comparison of the estimated sc_pot with the
value obtained from the esa L2 cdf (originally from
thm_load_esa_pot)
esa_datatype = 'peef', 'peer', or 'peeb'; the default is 'peer'
yellow = the limit (0-255) where above this value, we assume that
there are photo electrons in the scaled eflux
spectrogram. This will give the potential; the default is
200.
lo_scpot = lower limit for the potential, default is to use the low
energy limit of the data
hi_scpot = upper limit for the potential, default is 50 V
time_smooth_dt = if set, smooth the data in time, using this value
as smoothing time, default is no smoothing
hsk_test = if the HSK data for hsk_ifgm_xy_raw and hsk_ifgm_zr_raw
is below this value, set potential to low limit
densmatch = if the potential is set to the low limit, because the
distribution is unsuitable (maybe not two maxima below
100 eV) then use thm_esa_dens2scpot for the potential.
HISTORY:
3-mar-2016, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2023-11-03 13:14:18 -0700 (Fri, 03 Nov 2023) $
$LastChangedRevision: 32215 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_est_dist2scpot2.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_est_dist2scpot2.pro)
Procedure:
thm_esa_quality_flags
Description:
makes a bitpacked tplot variable containing quality flags for ESA
bit0 = pre-efi boom deployment (using zeroed spacecraft potential)
bit1 = counter overflow flag
bit2 = solar wind mode flag(disabled)
bit3 = flow flag, flow less than threshold is flagged
bit4 = earth shadow
bit5 = lunar shadow
bit6 = manuever flag
Set timespan by calling timespan outside of this routine.(e.g. time/duration is not an argument)
Keywords:
probe(required): probe letter ('a','b','c','d','e')
datatype(required): type string ('peef','peib', etc...)
noload(optional): set this if calling from thm_l2gen_esa
flow_threshold(optional): flow threshold for flow flag(default = 1.0, units undocumented)
$LastChangedBy: jimm $
$LastChangedDate: 2018-03-12 14:57:15 -0700 (Mon, 12 Mar 2018) $
$LastChangedRevision: 24875 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_quality_flags.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_quality_flags.pro)
HELPER FUNCTION (main function below) Returns the start and end indices of intervals where a condition applies
(See projects/themis/spacecraft/particles/ESA/thm_esa_quality_flags.pro)
NAME:
thm_esa_test_spec3d2
PURPOSE:
Wrapper for spec3d2, plots PEEF, PEER, PEEB data; the user clicks on
a time, and spec3d2 estimates the sc potential for each mode, and
plots the distribution with the potential overplotted. A black line
for the measured potential, and a red line for the
estimated potential
INPUT:
date = a date, e.g., '2008-01-05'
probe = a probe, e.g., 'c'
OUTPUT:
plots of the 3d distribution for each mode, with SC_POT plotted on
the graph.
init = if set, read in a new set of data
random_dp = if set, the input date and probe are randomized, note
that this keyword is unused if init is not set.
HISTORY:
31-may-2015, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2015-07-24 15:57:59 -0700 (Fri, 24 Jul 2015) $
$LastChangedRevision: 18252 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_esa_test_spec3d2.pro $
(See projects/themis/spacecraft/particles/ESA/thm_esa_test_spec3d2.pro)
NAME:
thm_load_l2_esadist
PURPOSE:
Loads THEMIS ESA L2 data for a given file(s), or time_range
CALLING SEQUENCE:
thm_load_l2_esadist, trange=trange, datatype=datatype
INPUT:
All via keyword, if none are set, then the output of timerange() is
used for the time range, which may prompt for a time interval
KEYWORDS:
probe = ['a', 'b', 'c', 'd', 'e'] is the default
datatype = ['peif', 'peir', 'peib', 'peef', 'peer', 'peeb'] is the default
trange = read in the data from this time range, note that if both
files and time range are set, files, and orbits take precedence in
finding files.
no_time_clip = if set do not clip the data to the time range. The
trange is only used for file selection. Note that
setting no_time_clip will always generate a reload of
data
OUTPUT:
No variables, data are loaded into common blocks
HISTORY:
7-nov-2022, jmm, jimm@ssl.berkeley.edu
$LastChangedBy: jimm $
$LastChangedDate: 2023-09-19 14:54:55 -0700 (Tue, 19 Sep 2023) $
$LastChangedRevision: 32106 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_load_l2_esadist.pro $
(See projects/themis/spacecraft/particles/ESA/thm_load_l2_esadist.pro)
NAME: thm_load_pxxm_pot4esa PURPOSE: loads the pxxm_pot variable for ESA processing, performs a time offset, and also loads the efs_Potl variable fro FIT files, if it exists. CALLING SEQUENCE: thm_load_esa_pxx_pot4esa, probe=probe, trange=trange,suffix=suffix INPUT; All via keyword OUTPUT: For each probe, a tplot variable 'thx_pxxm_pot', which is the SC potential that comes directly from the MOM L1 files, a variable, 'thm_pxxm_pot_0', that includes a time correction, KEYWORDS: probe - ['a','b','c','d','e'] trange - the time range, otherwise just use whatever's there HISTORY: 11-May-2010, jmm, jimm@ssl.berkeley.edu $LastChangedBy: aaflores $ $LastChangedDate: 2012-01-10 10:56:14 -0800 (Tue, 10 Jan 2012) $ $LastChangedRevision: 9526 $ $URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_6_0/projects/themis/spacecraft/particles/ESA/thm_load_pxxm_pot4esa.pro $
(See projects/themis/spacecraft/particles/ESA/thm_load_pxxm_pot4esa.pro)