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csst-sims
csst_ifs_sim
Commits
dd1608ee
Commit
dd1608ee
authored
May 11, 2024
by
Yan Zhaojun
Browse files
debug
parent
a5489f19
Pipeline
#4473
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in 0 seconds
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1
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2
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csst_ifs_sim/csst_ifs_sim.py
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dd1608ee
...
...
@@ -22,23 +22,11 @@ from scipy.signal import fftconvolve
from
scipy
import
ndimage
import
cmath
import
configparser
as
ConfigParser
# from support import IFSinstrumentModel
# from support import cosmicrays
# from support import logger as lg
# from CTI import CTI
import
os
from
scipy.interpolate
import
interp1d
import
astropy.coordinates
as
coord
import
ctypes
import
sys
# from csst_ifs_sim.support import IFSinstrumentModel
# from csst_ifs_sim.support import cosmicrays
# from csst_ifs_sim.support import logger as lg
# from csst_ifs_sim.CTI import CTI
sys
.
path
.
append
(
'./csst_ifs_sim'
)
conf
.
auto_max_age
=
None
...
...
@@ -91,23 +79,21 @@ Note:: This class is Python 3 compatible.
"""
######################## functions definition ################################
"""
Charge Transfer Inefficiency
============================
This file contains a simple class to run a CDM03 CTI model developed by Alex Short (ESA).
This now contains both the official CDM03 and a new version that allows different trap
parameters in parallel and serial direction.
class
CDM03bidir
():
"""
Charge Transfer Inefficiency
============================
This file contains a simple class to run a CDM03 CTI model developed by Alex Short (ESA).
:requires: NumPy
:requires: CDM03 (FORTRAN code, f2py -c -m cdm03bidir cdm03bidir.f90)
This now contains both the official CDM03 and a new version that allows different trap
parameters in parallel and serial direction.
"""
:requires: NumPy
:requires: CDM03 (FORTRAN code, f2py -c -m cdm03bidir cdm03bidir.f90)
#CDM03bidir
class
CDM03bidir
():
"""
Class to run CDM03 CTI model, class Fortran routine to perform the actual CDM03 calculations.
:param settings: input parameters
...
...
@@ -181,8 +167,6 @@ class CDM03bidir():
Set up the logger.
"""
self
.
logger
=
True
# if self.log is None:
# self.logger = False
def
applyRadiationDamage
(
self
,
data
,
iquadrant
=
0
):
...
...
@@ -309,20 +293,17 @@ def lg(log_filename, loggername='logger'):
##############################################################################
"""
IFS Instrument Model
====================
The file provides a function that returns IFS related information such as pixel
size, dark current, gain...
"""
def
IFSinformation
():
"""
Returns a dictionary describing VIS. The following information is provided (id: value - reference)::
IFS Instrument Model
====================
The file provides a function that returns IFS related information such as pixel
size, dark current, gain...
Returns a dictionary describing VIS. The following information is provided
(id: value - reference)::
:return: instrument model parameters
:rtype: dict
...
...
@@ -353,30 +334,24 @@ def CCDnonLinearityModel(data, beta=6e-7):
return
out
#############################################################################
"""
Cosmic Rays
===========
This simple class can be used to include cosmic ray events to an image.
By default the cosmic ray events are drawn from distributions describing
the length and energy of the events. Such distributions can be generated
for example using Stardust code (http://ieeexplore.ieee.org/stamp/stamp.jsp?arnumber=04636917).
The energy of the cosmic ray events can also be set to constant for
testing purposes. The class can be used to draw a single cosmic ray
event or up to a covering fraction.
:requires: NumPy
:requires: SciPy
:version: 0.2
"""
from
scipy.interpolate
import
InterpolatedUnivariateSpline
class
cosmicrays
():
"""
Cosmic Rays
===========
This simple class can be used to include cosmic ray events to an image.
By default the cosmic ray events are drawn from distributions describing
the length and energy of the events. Such distributions can be generated
for example using Stardust code (http://ieeexplore.ieee.org/stamp/stamp.jsp?arnumber=04636917).
The energy of the cosmic ray events can also be set to constant for
testing purposes. The class can be used to draw a single cosmic ray
event or up to a covering fraction.
Cosmic ray generation class. Can either draw events from distributions or
set the energy of the events to a constant.
...
...
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