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StrongGravity
KYNreverb
Commits
13857d6e
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13857d6e
authored
Aug 04, 2016
by
Michal Dovčiak
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13857d6e
**To use the KYNrefrev model in XSPEC you need:**
Table of contents
=================
*
[
source files
](
https://projects.asu.cas.cz/files/note/345/KYNrefrevv1.3.4.tar.gz
)
,
*
[
Model description
](
#modeldescription
)
*
[
Installation
](
#installation
)
*
[
Required files
](
#requiredfiles
)
*
[
Usage in XSPEC
](
#usageinxspec
)
*
[
Usage outside of XSPEC
](
#usageoutsideofxspec
)
*
[
Parameters of the model
](
#parametersofthemodel
)
*
[
Definition in XSPEC
](
#definitioninxspec
)
*
[
Definition outside XSPEC
](
#definitionoutsidexspec
)
*
[
Output files created
](
#outputfilescreated
)
*
KY tables:
[
KBHlamp_qt.fits
](
http://www.astro.cas.cz/dovciak/pub/KY/KBHlamp_qt.fits
)
and [KBHtables80.fits]
(http://www.astro.cas.cz/dovciak/pub/KY/KBHtables80.fits),
Model description
=================
*
[
REFLION(X)
](
https://heasarc.gsfc.nasa.gov/xanadu/xspec/models/reflion.html
)
tables:
The KYNrefrev model computes the time dependent reflection spectra of the disc
as a response to a flash of primary powerlaw radiation from a point source
located on the axis of the blackhole accretion disc.
_Assumptions of the model:_
*
central Kerr black hole,
*
Keplerian, geometrically thin, optically thick, ionised disc with different
radial density profiles,
*
stationary hot pointlike patch of plasma located on the system rotation axis
and emitting isotropic powerlaw radiation,
*
full relativistic raytracing code in vacuum is used for photon paths from the
corona to the disc and to the observer and from the disc to the observer,
*
reprocessing in the ionised accretion disc is computed for each radius from
REFLIONX tables for constant density slab illuminated by powerlaw radiation,
*
the ionisation of the disc is set for each radius according to the amount of
the incident primary flux and the density of the accretion disc,
*
several limb brightening/darkening prescriptions for directionality of the
reprocessed emission are used.
_Output of the code:_
*
time dependent spectra (only when used outside of XSPEC) of the disc response
and observed primary flash,
*
integrated spectrum,
*
light curve for a given energy band,
*
lag as a function of frequency between given energy bands,
*
lag as a function of energy for different frequencies.
Installation
============
Required files

*
Source files in the main repository directory.
*
KY tables:
[
KBHlamp_qt.fits
](
https://owncloud.asu.cas.cz/index.php/s/xg64GRMSRGiWOPR
)
(also
[
here
](
http://www.astro.cas.cz/dovciak/pub/KY/KBHlamp_qt.fits
)
)
and
[
KBHtables80.fits
](
https://owncloud.asu.cas.cz/index.php/s/WP8aLN168MJgcB9
)
(also
[
here
](
http://www.astro.cas.cz/dovciak/pub/KY/KBHtables80.fits
)
).
*
[
REFLION(X)
](
https://heasarc.gsfc.nasa.gov/xanadu/xspec/models/reflion.html
)
tables (unpack gzipped files):

[
reflion.mod
](
https://heasarc.gsfc.nasa.gov/xanadu/xspec/models/reflion.mod.gz
)
(
old
)
,

[
reflionx.mod
](
https://heasarc.gsfc.nasa.gov/xanadu/xspec/models/reflionx.mod.gz
)
,
or in case the links are not available
or in case the links are not available or if the tables there are updated and
their format/structure has changed:

[
reflion.mod
](
https://owncloud.asu.cas.cz/index.php/s/6CWcb0o5Ssjehju
)
(or
[
here
](
http://www.astro.cas.cz/dovciak/pub/KYexternal/reflion.mod
)
)
(old),

[
reflionx.mod
](
https://owncloud.asu.cas.cz/index.php/s/Q6biiTPM1QBMtiT
)
(or
[
here
](
http://www.astro.cas.cz/dovciak/pub/KYexternal/reflionx.mod
)
).

[
reflion.mod
](
http://www.astro.cas.cz/dovciak/pub/KYexternal/reflion.mod
)
(
old
)
,

[
reflionx.mod
](
http://www.astro.cas.cz/dovciak/pub/KYexternal/reflionx.mod
)
.
Usage in XSPEC


The code is compiled inside XSPEC with the following command (assuming all the
source files and FITS tables are in the directory /path/to/KYNrefrev):
The code is compiled inside XSPEC with the following command (assuming all the source files and FITS tables are in the directory /path/to/KYNrefrev):
*
`initpackage kynrefrev lmodel.dat /path/to/KYNrefrev`
.
To use the KYNrefrev model inside XSPEC, first the package needs to be loaded and directory with KYNrefrev set:
To use the KYNrefrev model inside XSPEC, first the package needs to be loaded
and directory with KYNrefrev set:
*
`lmod kynrefrev /path/to/KYNrefrev`
,
*
`xset KYDIR /path/to/KYNrefrev`
.
Then the model may be used:
*
`mo kynrefrev`
.
_Note_
:
In case of segmentation fault, one may need to increase the stack size, e.g. with the command
`ulimit s unlimited`
or
`ulimit s 65532`
.
In case of segmentation fault, one may need to increase the stack size, e.g.
with the command
`ulimit s unlimited`
or
`ulimit s 65532`
.

**For use outside of XSPEC:**
Usage outside of XSPEC

*
One also needs the Makefile and libxspec library available
[
here
](
https://projects.asu.cas.cz/files/note/344/outside.tar.gz
)
.
*
One also needs the Makefile and libxspec library included in the directory
'other'.
*
The library to work with FITS files (libcfitsio.so) is needed, thus one needs
to
define the name of the library and path to it in the provided Makefile.
*
The library to work with FITS files (libcfitsio.so) is needed, thus one needs
to
define the name of the library and path to it in the provided Makefile.
*
The model parameters have to be changed inside the source file.
*
Compile with the make command:
*
`make kynrefrev`
for everything, i.e. light curves, spectra and Fourier transforms (real,
imaginary parts, amplitudes and phases).
* `make kynrefrev`
*
Run the code:
* `./kynrefrev`.
*
The model creates various files described below.
_Note_
:
In case of segmentation fault, one may need to increase the stack size, e.g. with the command
`ulimit s unlimited`
or
`ulimit s 65532`
.
_Note_
:
In case of segmentation fault, one may need to increase the stack size, e.g.
with the command
`ulimit s unlimited`
or
`ulimit s 65532`
.

Parameters of the model
=======================
#### **1. Parameters of the model**
Definition in XSPEC

*
The meaning of the input parameters are explained at the beginning of the kynrefrev.c file.
The parameters when the code runs under XSPEC are defined in the usual way as for other XSPEC
models. The parameter definitions when run outside of XSPEC must be changed directly inside the source
code. Summary of the parameters:
*
The meaning of the input parameters are also explained at the beginning of
the kynrefrev.c file. The parameters when the code runs under XSPEC are
defined in the usual way as for other XSPEC models. The parameter
definitions when run outside of XSPEC must be changed directly inside the
source code. Summary of the parameters:
* **par1 ... a/M**
 black hole angular momentum (1 ≤ a/M ≤ 1)
...
...
@@ 71,25 +153,28 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
* **par4 ... ms**
 switch for inner edge
 0: we integrate from inner edge = par3
 1: if the inner edge of the disc is below marginally stable orbit (MSO)
then we integrate emission
above MSO only
 2: we integrate from inner edge given in units of MSO, i.e. inner
edge = par3 × r~mso~ (the same
applies for outer edge)
 1: if the inner edge of the disc is below marginally stable orbit (MSO)
then we integrate emission
above MSO only
 2: we integrate from inner edge given in units of MSO, i.e. inner
edge = par3 × r~mso~ (the same
applies for outer edge)
* **par5 ... rout**
 outer edge of nonzero disc emissivity (in GM/c^2 or in r~mso~)
* **par6 ... phi**
 lower azimuth of nonzero disc emissivity (degrees)
* **par7 ... dphi**
 (phi + dphi) is upper azimuth of nonzero disc emissivity 0° ≤ dphi ≤ 360°
 (phi + dphi) is upper azimuth of nonzero disc emissivity 0° ≤
dphi ≤ 360°
* **par8 ... M/M8**
 black hole mass in units of 10^8 solar masses
* **par9 ... height**
 height on the axis (measured from the center) at which the primary source is located (GM/c^(2))
 height on the axis (measured from the center) at which the primary
source is located (GM/c^(2))
* **par10 ... PhoIndex**
 powerlaw energy index of the primary flux
* **par11 ... Np**
 dN/dt/dΩ, the intrinsic local (if negative) or the observed (if positive)
primary isotropic flux in the Xray energy range 210keV in units of L~Edd~
 dN/dt/dΩ, the intrinsic local (if negative) or the observed
(if positive) primary isotropic flux in the Xray energy range 210keV
in units of L~Edd~
* **par12 ... NpNr**
 ratio of the primary to the reflected normalization
 1: selfconsistent model for isotropic primary source
...
...
@@ 103,15 +188,17 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
* **par15 ... abun**
 Fe abundance (in solar abundance)
* **par16 ... alpha**
 position of the cloud centre in GM/c^2 in alpha coordinate (alpha being the impact
parameter in φdirection, positive for approaching side of the disc)
 position of the cloud centre in GM/c^2 in alpha coordinate (alpha being
the impact parameter in φdirection, positive for approaching side
of the disc)
* **par17 ... beta**
 position of the cloud centre in GM/c^2 in beta coordinate (beta being the impact
parameter in θdirection, positive in up direction, i.e. away from the disc)
 position of the cloud centre in GM/c^2 in beta coordinate (beta being
the impact parameter in θdirection, positive in up direction,
i.e. away from the disc)
* **par18 ... rcloud**
 radius of the obscuring cloud
 the meaning of cloud is inverted for negative values of rcloud, i.e.
only the radiation behind
the cloud is computed
 the meaning of cloud is inverted for negative values of rcloud, i.e.
only the radiation behind
the cloud is computed
* **par19 ... zshift**
 overall Doppler shift
* **par20 ... limb**
...
...
@@ 120,29 +207,34 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
 2: for Haardt's limb brightening (flux ~ ln (1+1/μ))
* **par21 ... tab**
 which reflion table to use
 1: reflion (the old one, lower cutoff energy at 1eV, not good for PhoIndex > 2)
 1: reflion (the old one, lower cutoff energy at 1eV, not good for
PhoIndex > 2)
 2: reflionx (the newer one, lower cutoff energy at 100eV)
* **par22 ... sw**
 switch for the way how to compute the refl. spectra
 1: use the computed ionisation parameter, ξ, for the interpolation in reflion, i.e. use proper
total incident intensity with the shifted cutoffs
 2: use the ionisation parameter, ξ, correspondent to the computed normalization of the incident flux, i.e. do not shift
the cutoffs when computing the total incident intensity
 1: use the computed ionisation parameter, ξ, for the interpolation
in reflion, i.e. use proper total incident intensity with the
shifted cutoffs
 2: use the ionisation parameter, ξ, correspondent to the computed
normalization of the incident flux, i.e. do not shift the cutoffs
when computing the total incident intensity
* **par23 ... ntable**
 defines fits file with tables (0 ≤ ntable ≤ 99), currently the
tables with ntable=80 are correct
for this model
 defines fits file with tables (0 ≤ ntable ≤ 99), currently the
tables with ntable=80 are correct
for this model
* **par24 ... nradius**
 number of grid points in radius
 if negative than the number of radial grid points is dependent on height as
nradius / height^( 0.66)
 if negative than the number of radial grid points is dependent on
height as
nradius / height^( 0.66)
* **par25 ... division**
 type of division in radial integration
 0: equidistant radial grid (constant linear step)
 1: exponential radial grid (constant logarithmic step)
 >1: mixed radial grid with a constant logarithmic step in the inner region and with a constant
linear step in the outer region; the total nradius (par24) number of points is divided in
the 3:2 ratio in these regions; the value of par25 gives the transition radius between these
regions (in GM/c^(2))
 >1: mixed radial grid with a constant logarithmic step in the inner
region and with a constant linear step in the outer region; the
total nradius (par24) number of points is divided in the 3:2 ratio
in these regions; the value of par25 gives the transition radius
between these regions (in GM/c^(2))
 1: mixed radial grid with the transition radius at 2×height
* **par26 ... nphi**
 number of grid points in azimuth
...
...
@@ 151,77 +243,97 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
* **par28 ... nt**
 number of time subbins per one time bin
* **par29 ... t1/f1/E1**
 the time to be used in XSPEC for the spectrum (0 means average spectrum, i.e. divided by the flare
duration)
 the frequency to be used in XSPEC for the energy dependent Fourier transform (0 means average values
in the range of 0 to the first wrapping frequency)
 the time to be used in XSPEC for the spectrum (0 means average
spectrum, i.e. divided by the flare duration)
 the frequency to be used in XSPEC for the energy dependent Fourier
transform (0 means average values in the range of 0 to the first
wrapping frequency)
 positive values are in sec or Hz
 negative values are in GM/c^3 or (GM/c^(3))^(1)
 if different than par30, the value gives the lower end of the time/frequency interval of interest
 if same as par30, then the functions are computed for this value of the time/frequency of interest
 in case of frequency dependent lags it defines the lower value of the energy band of interest in keV
 if different than par30, the value gives the lower end of the
time/frequency interval of interest
 if same as par30, then the functions are computed for this value of
the time/frequency of interest
 in case of frequency dependent lags it defines the lower value of the
energy band of interest in keV
* **par30 ... t2/f2/E2**
 used only if different than par29 and if par29 is nonzero
 its value gives the upper end of the time/frequency interval of interest
 its value gives the upper end of the time/frequency interval of
interest
 positive values are in sec or Hz
 negative values are in GM/c^3 or (GM/c^(3))^(1)
 in case of frequency dependent lags it defines the upper value of the energy band of interest in keV
 in case of frequency dependent lags it defines the upper value of the
energy band of interest in keV
* **par31 ... E3**
 it defines the lower value of the reference energy band for lag or amplitude energy dependence as well
as in case of frequency dependent lags and amplitudes
 it defines the lower value of the reference energy band for lag or
amplitude energy dependence as well as in case of frequency dependent
lags and amplitudes
 if zero no reference band is used
 if negative, the whole energy band is used as a reference band for lagenergy spectra, always excluding
the current energy bin; it must be nonnegative in case of lagfrequency dependence
 if negative, the whole energy band is used as a reference band for
lagenergy spectra, always excluding the current energy bin; it must be
nonnegative in case of lagfrequency dependence
* **par32 ... E4**
 it defines the upper value of the reference energy band for lagenergy
dependence as well as in case
of frequency dependent lags
 it defines the upper value of the reference energy band for lagenergy
dependence as well as in case
of frequency dependent lags
* **par33 ... tshift/Af**
 lag shift for lagenergy dependence in case of par35=+6
 multiplicative factor in case of adding empirical hard lags Af×f^(qf), used for par35=+16
 multiplicative factor in case of adding empirical hard lags
Af×f^(qf), used for par35=+16
* **par34 ... Amp/qf**
 multiplicative factor for the amplitudeenergy dependence in case of par35=+5
 powerlaw index in case of adding empirical hard lags Af×f^(qf), used for par35=+16
 multiplicative factor for the amplitudeenergy dependence in case of
par35=+5
 powerlaw index in case of adding empirical hard lags Af×f^(qf),
used for par35=+16
* **par35 ... photar_sw**
 defines output in the XSPEC (photar array)
 0: spectrum for time interval defined by par29 and par30
 _the following values correspond to energy dependent Fourier transform
at the frequency band defined
by par29 and par30:_
 _the following values correspond to energy dependent Fourier transform
at the frequency band defined
by par29 and par30:_
 1: real part of FT of the relative reflection
 2: imaginary part of FT of the relative reflection
 3: amplitude of FT of the relative reflection
 4: phase of FT of the relative reflection
 5: amplitude for the relative reflection divided by amplitude in the reference energy band defined
by par31 and par32
 6: lag for the relative reflection with respect to reference energy band defined by par31 and par32
 5: amplitude for the relative reflection divided by amplitude in the
reference energy band defined by par31 and par32
 6: lag for the relative reflection with respect to reference energy
band defined by par31 and par32
 1: real part of FT including primary radiation
 2: imaginary part of FT including primary radiation
 3: amplitude of FT including primary radiation
 4: phase of FT including primary radiation
 5: amplitude including the primary radiation divided by amplitude in the reference energy band
defined by par31 and par32
 6: lag diluted by primary radiation with respect to reference energy band defined by par31 and par32
 _the following values correspond to frequency dependent Fourier transform for the energy band of
interest defined by par29 and par30:_
 5: amplitude including the primary radiation divided by amplitude in
the reference energy band defined by par31 and par32
 6: lag diluted by primary radiation with respect to reference energy
band defined by par31 and par32
 _the following values correspond to frequency dependent Fourier
transform for the energy band of interest defined by par29 and par30:_
 11: real part of FT of the relative reflection
 12: imaginary part of FT of the relative reflection
 13: amplitude of FT of the relative reflection
 14: phase of FT of the relative reflection
 15: amplitude for the relative reflection divided by amplitude in the reference energy band
defined by par31 and par32
 16: lag for the relative reflection with respect to reference energy band defined by par31 and par32
 15: amplitude for the relative reflection divided by amplitude in
the reference energy band defined by par31 and par32
 16: lag for the relative reflection with respect to reference energy
band defined by par31 and par32
 11: real part of FT including primary radiation
 12: imaginary part of FT including primary radiation
 13: amplitude of FT including primary radiation
 14: phase of FT including primary radiation
 15: amplitude including the primary radiation divided by amplitude in the reference energy band
defined by par31 and par32
 16: lag diluted by primary radiation with respect to reference energy band defined by par31 and par32
 15: amplitude including the primary radiation divided by amplitude in
the reference energy band defined by par31 and par32
 16: lag diluted by primary radiation with respect to reference energy
band defined by par31 and par32
* **par36 ... nthreads**
 how many threads should be used for computations
* **par37 ... norm**
 **has to be set to unity!**
*
Parameters that need to be defined inside the
**kynrefrev.c**
code when run outside of XSPEC:
Definition outside XSPEC

*
The model parameters need to be defined inside the
**kynrefrev.c**
code
when run outside of XSPEC (the code needs to be recompiled after changing
them):
 _energy_ in the following lines:
...
...
@@ 248,8 +360,9 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
ener_low[4] = E_MIN;
ener_high[4] = E_MAX;
 _all basic parameters_ of the model (physical ones as well as those defining resolution grid for
computations) are defined in the following lines:
 _all basic parameters_ of the model (physical ones as well as those
defining resolution grid for computations) are defined in the following
lines:
param[ 0] = 1.; // a/M
param[ 1] = 30.; // thetaO
...
...
@@ 289,8 +402,8 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
param[35] = 4.; // nthreads
param[36] = 1.; // norm
 some parameters are later changed in the loops for convenience (to
create files for grid of
parameters), see lines as:
 some parameters are later changed in the loops for convenience (to
create files for grid of
parameters), see lines as:
for (ia=0;ia<=1;ia++){
param[0] = (double) ia;
...
...
@@ 300,105 +413,144 @@ In case of segmentation fault, one may need to increase the stack size, e.g. wit
param[8] = 1.5 * (100./1.5)**((ih1.)/19.);
#### **2. Output files created**
Output files created
====================
*
The output files are created only when the code is run outside XSPEC.
*
The following naming scheme is used for the output files:

**AAA**
is 100
×
the horizon value (thus 100 means a=1 and 200 means a=0),

**AAA**
is 100
×
the horizon value (thus 100 means a=1 and 200 means
a=0),

**BB**
is the inclination in degrees,

**CCCC**
is 10
×
the height (e.g. 0030 means h=3),

**u1**
is used for phase unwrapped in frequency dependence,

**u2**
is used for phase unwrapped in energy dependence.
*
All spectra and light curves are always computed in photon numbers and per
keV and per second, time is in
seconds and frequency in Hz.
*
All spectra and light curves are always computed in photon numbers and per
keV and per second, time is in
seconds and frequency in Hz.
*
The output files created by
**kynrefrev.c**
code:

below by relative reflection it is meant the disc response divided by the total primary flux in the
flash.

**kynrefrev_photar.dat**
→
the values as would be given inside XSPEC,

below by relative reflection it is meant the disc response divided by the
total primary flux in the flash.

**kynrefrev_photar.dat**
→
the values as would be given inside
XSPEC,

**kynrefrev_AAA_BB_CCCC.txt**
→
the summary of parameter values,

**kynrefrev_AAA_BB_CCCC_far.dat**
→
the time evolving observed reflection spectrum where the
energy changes with rows and the time changes with columns,

**kynrefrev_AAA_BB_CCCC_flux_prim.dat**
→
the total observed primary flux (i.e. integrated in
energy) per second, it is constant during the duration of the flare,

**kynrefrev_AAA_BB_CCCC_lc.dat**
→
the light curve of the observed reflection (2^nd column)
where we integrated over the whole energy range, the 1^st column contains the time,

**kynrefrev_AAA_BB_CCCC_spectrum.dat**
→
the time integrated spectrum of the observed
reflection (2^nd column) and the observed primary (3^rd column), both are divided by the flare
duration, the 1^st column contains the central value of the energy bins in keV.

**kynrefrev_AAA_BB_CCCC_bands_lc.dat**
→
the light curves for the observed reflection (2^nd
and higher columns) where in each column the light curve is integrated over different energy band
(defined in the code), the 1^st column contains the time,

**kynrefrev_AAA_BB_CCCC_bands_prim.dat**
→
the observed primary flux per second, it is
constant during the duration of the flare where in each column the flux is
integrated over different energy band (defined in the code).

**kynrefrev_AAA_BB_CCCC_far.dat**
→
the time evolving observed
reflection spectrum where the energy changes with rows and the time
changes with columns,

**kynrefrev_AAA_BB_CCCC_flux_prim.dat**
→
the total observed primary
flux (i.e. integrated in energy) per second, it is constant during the
duration of the flare,

**kynrefrev_AAA_BB_CCCC_lc.dat**
→
the light curve of the observed
reflection (2^nd column) where we integrated over the whole energy range,
the 1^st column contains the time,

**kynrefrev_AAA_BB_CCCC_spectrum.dat**
→
the time integrated
spectrum of the observed reflection (2^nd column) and the observed
primary (3^rd column), both are divided by the flare duration, the 1^st
column contains the central value of the energy bins in keV.

**kynrefrev_AAA_BB_CCCC_bands_lc.dat**
→
the light curves for the
observed reflection (2^nd and higher columns) where in each column the
light curve is integrated over different energy band (defined in the
code), the 1^st column contains the time,

**kynrefrev_AAA_BB_CCCC_bands_prim.dat**
→
the observed primary flux
per second, it is constant during the duration of the flare where in each
column the flux is integrated over different energy band (defined in the
code).

**kynrefrev_AAA_BB_CCCC_real.dat**
→
the real part of the FFT of the relative reflection with frequency
changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_imag.dat**
→
the imaginary part of the FFT of the relative reflection with
frequency
changing with rows and energy with columns,
→
the imaginary part of the FFT of the relative reflection with
frequency
changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_ampl.dat**
→
the amplitude of the FFT of the relative reflection with frequency
changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_phase.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_u1.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_u2.dat**
→
the phase of the FFT of the relative reflection with

**kynrefrev_AAA_BB_CCCC_phase.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_u1.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_u2.dat**
→
the phase of the FFT of the
relative reflection with frequency changing with rows and energy with
columns,

**kynrefrev_AAA_BB_CCCC_real_tot.dat**
→
the real part of the FFT of
the total signal (reflection response plus primary flash) with frequency
changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_imag_tot.dat**
→
the imaginary part of the
FFT of the total signal (reflection response plus primary flash) with
frequency changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_real_tot.dat**
→
the real part of the FFT of the total signal
(reflection response plus primary flash) with frequency changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_imag_tot.dat**
→
the imaginary part of the FFT of the total signal
(reflection response plus primary flash) with frequency changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_ampl_tot.dat**
→
the amplitude of the FFT of the total signal
(reflection response plus primary flash) with frequency changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_phase_tot.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_tot_u1.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_tot_u2.dat**
→
the phase of the FFT of the total signal (reflection
response plus primary flash) with frequency changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_bands_real.dat**
→
the real part, as a function of frequency, of the
FFT of the relative reflection integrated in different energy bands as defined in the code (2^nd and
higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_imag.dat**
→
the imaginary part, as a function of frequency, of
the FFT of the relative reflection integrated in different energy bands as defined in the code (2^nd
and higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_ampl.dat**
→
the amplitude, as a function of frequency, of the
FFT of the relative reflection integrated in different energy bands as defined in the code (2^nd and
higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_phase.dat**
,
**kynrefrev_AAA_BB_CCCC_bands_phase_u1.dat**
→
the phase,
as a function of frequency, of the FFT
of the relative reflection integrated in different energy bands as defined in the code (2^nd and higher

**kynrefrev_AAA_BB_CCCC_ampl_tot.dat**
→
the amplitude of the FFT of
the total signal (reflection response plus primary flash) with frequency
changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_phase_tot.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_tot_u1.dat**
,
**kynrefrev_AAA_BB_CCCC_phase_tot_u2.dat**
→
the phase of the FFT of
the total signal (reflection response plus primary flash) with frequency
changing with rows and energy with columns,

**kynrefrev_AAA_BB_CCCC_bands_real.dat**
→
the real part, as a
function of frequency, of the FFT of the relative reflection integrated
in different energy bands as defined in the code (2^nd and higher
columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_imag.dat**
→
the imaginary part, as a
function of frequency, of the FFT of the relative reflection integrated
in different energy bands as defined in the code (2^nd and higher
columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_ampl.dat**
→
the amplitude, as a
function of frequency, of the FFT of the relative reflection integrated
in different energy bands as defined in the code (2^nd and higher
columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_phase.dat**
,
**kynrefrev_AAA_BB_CCCC_bands_phase_u1.dat**
→
the phase, as a
function of frequency, of the FFT of the relative reflection integrated
in different energy bands as defined in the code (2^nd and higher
columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_real_tot.dat**
→
the real part, as a function of frequency,
of the FFT of the total signal (reflection response plus primary flash) integrated in different energy
bands as defined in the code (2^nd and higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_imag_tot.dat**
→
the imaginary part, as a function of frequency,
of the FFT of the total signal (reflection response plus primary flash) integrated in different energy
bands as defined in the code (2^nd and higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_ampl_tot.dat**
→
the amplitude, as a function of frequency,
of the FFT of the total signal (reflection response plus primary flash) integrated in different energy
bands as defined in the code (2^nd and higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_bands_phase_tot.dat**
,
**kynrefrev_AAA_BB_CCCC_bands_phase_tot_u1.dat**
→
the phase, as a function of frequency, of the
FFT of the total signal (reflection response plus primary flash) integrated in different energy bands as
defined in the code (2^nd and higher columns), the 1^st column contains the frequency,

**kynrefrev_AAA_BB_CCCC_freq_wrap.dat**
→
the first wrapping frequency for the phase computed
for the relative reflection (the lowest one from all energy bins)

**kynrefrev_AAA_BB_CCCC_fft_tot_int.dat**
→
energy dependent average values of the FFT of the total
signal (real part, imaginary part, amplitude, phase, unwrapped phase, delay, ratio of the amplitudes for
the energy band of interest and reference energy band, delay between the energy band of interest and
reference energy band computed from wrapped and unwrapped phases and directly averaged delay between the
two energy bands as well as the ratio of the amplitudes and delay difference between the energy band of
interest and reference energy band where reference energy band always excludes the current energy bin),
the average is computed in the range of 0 to the first wrapping frequency, the 1^st column contains
the central value of energy bins in keV; the FFT here is averaged over frequencies for real and imaginary
parts first and then, from the result, all the rest quantities are computed except for the
directly averaged delay, where the delay is computed first from real and imaginary parts of the FFT for
each frequency and only then it is averaged (just for comparison).

**kynrefrev_AAA_BB_CCCC_fft_tot_fband.dat**
→
energy dependent average values of the FFT of the total
signal (real part, imaginary part, amplitude, phase, unwrapped phase, delay, ratio of the amplitudes for
the energy band of interest and reference energy band, delay between the energy band of interest and
reference energy band computed from wrapped and unwrapped phases and directly averaged delay between the
two energy bands as well as the ratio of the amplitudes and delay difference between the energy band of
interest and reference energy band where reference energy band always excludes the current energy bin),
the average is computed in the frequency range given by param[28] and param[29], the 1^st column
contains the central value of energy bins in keV; the FFT here is averaged over frequencies for real and
imaginary parts first and then, from the result, all the rest quantities are computed except for the
directly averaged delay, where the delay is computed first from real and imaginary parts of the FFT for
each frequency and only then it is averaged (just for comparison).

**kynrefrev_AAA_BB_CCCC_bands_real_tot.dat**
→
the real part, as a
function of frequency, of the FFT of the total signal (reflection
response plus primary flash) integrated in different energy bands as
defined in the code (2^nd and higher columns), the 1^st column contains
the frequency,

**kynrefrev_AAA_BB_CCCC_bands_imag_tot.dat**
→
the imaginary part,
as a function of frequency, of the FFT of the total signal (reflection
response plus primary flash) integrated in different energy bands as
defined in the code (2^nd and higher columns), the 1^st column contains
the frequency,

**kynrefrev_AAA_BB_CCCC_bands_ampl_tot.dat**
→
the amplitude, as a
function of frequency, of the FFT of the total signal (reflection
response plus primary flash) integrated in different energy bands as
defined in the code (2^nd and higher columns), the 1^st column contains
the frequency,

**kynrefrev_AAA_BB_CCCC_bands_phase_tot.dat**
,
**kynrefrev_AAA_BB_CCCC_bands_phase_tot_u1.dat**
→
the phase, as a
function of frequency, of the FFT of the total signal (reflection
response plus primary flash) integrated in different energy bands as
defined in the code (2^nd and higher columns), the 1^st column contains
the frequency,

**kynrefrev_AAA_BB_CCCC_freq_wrap.dat**
→
the first wrapping
frequency for the phase computed for the relative reflection (the lowest
one from all energy bins)

**kynrefrev_AAA_BB_CCCC_fft_tot_int.dat**
→
energy dependent average
values of the FFT of the total signal (real part, imaginary part,
amplitude, phase, unwrapped phase, delay, ratio of the amplitudes for the
energy band of interest and reference energy band, delay between the
energy band of interest and reference energy band computed from wrapped
and unwrapped phases and directly averaged delay between the two energy
bands as well as the ratio of the amplitudes and delay difference between
the energy band of interest and reference energy band where reference
energy band always excludes the current energy bin), the average is
computed in the range of 0 to the first wrapping frequency, the 1^st
column contains the central value of energy bins in keV; the FFT here is
averaged over frequencies for real and imaginary parts first and then,
from the result, all the rest quantities are computed except for the
directly averaged delay, where the delay is computed first from real and
imaginary parts of the FFT for each frequency and only then it is
averaged (just for comparison).

**kynrefrev_AAA_BB_CCCC_fft_tot_fband.dat**
→
energy dependent