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Commit 9e7cecd1 authored by Yan Zhaojun's avatar Yan Zhaojun
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csst_mci_sim/csst_mci_sim.py
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......@@ -55,79 +55,36 @@ Contact Information: zhaojunyan@shao.ac.cn
"""
import galsim
import pandas as pd
from scipy.integrate import simps
#from scipy.integrate import simps
from datetime import datetime, timedelta
from astropy.time import Time
from astropy.coordinates import get_sun
# import scipy.io as sio
# import cmath
import numpy as np
from tqdm import tqdm
from astropy.table import Table
# from astropy.wcs import WCS as WCS
from astropy.io import fits
from astropy import units as u
import os, sys, math
import configparser as ConfigParser
# from optparse import OptionParser
# from matplotlib import pyplot as plt
from matplotlib import pyplot as plt
from scipy import ndimage
sys.path.append('./csst_mci_sim')
##sys.path.append('..')
from CTI import CTI
from support import logger as lg
from support import cosmicrays
from support import shao
from support import sed
#from shao import onOrbitObsPosition
from support import MCIinstrumentModel
from joblib import Parallel, delayed
#import multiprocessing
from astropy.coordinates import SkyCoord
from scipy import interpolate
from scipy.signal import fftconvolve
import pandas
# sys.path.append('../MCI_inputData/TianCe')
# sys.path.append('../MCI_inputData/SED_Code')
# set the folder
FOLDER ='../'
#####################################################################################
###############################################################################
import ctypes
import astropy.coordinates as coord
from scipy.interpolate import interp1d
########################### functions #########################
def transRaDec2D(ra, dec):
# radec转为竞天程序里的ob, 赤道坐标系下的笛卡尔三维坐标xyz.
x1 = np.cos(dec / 57.2957795) * np.cos(ra / 57.2957795)
......@@ -191,41 +148,6 @@ def earth_angle(time_jd, x_sat, y_sat, z_sat, ra_obj, dec_obj):
angle = 180 - angle_a - angle_b.degree
return angle
#################################################3
# def MCIinformation():
# """
# Returns a dictionary describing MCI CCD. The following information is provided (id: value - reference)::
# dob: 0 - CDM03 (Short et al. 2010)
# fwc: 90000 - CCD spec EUCL-EST-RS-6-002 (for CDM03)
# rdose: 30000000000.0 - derived (above the PLM requirement)
# sfwc: 730000.0 - CDM03 (Short et al. 2010), see also the CCD spec EUCL-EST-RS-6-002
# st: 5e-06 - CDM03 (Short et al. 2010)
# svg: 1e-10 - CDM03 (Short et al. 2010)
# t: 0.01024 - CDM03 (Short et al. 2010)
# trapfile: cdm_euclid.dat - CDM03 (derived, refitted to CCD204 data)
# vg: 6e-11 - CDM03 (Short et al. 2010)
# vth: 11680000.0 - CDM03 (Short et al. 2010)
# :return: instrument model parameters
# :rtype: dict
# """
# #########################################################################################################
# out=dict()
# out.update({'dob' : 0, 'rdose' : 8.0e9,
# 'parallelTrapfile' : 'cdm_euclid_parallel.dat', 'serialTrapfile' : 'cdm_euclid_serial.dat',
# 'beta_s' : 0.6, 'beta_p': 0.6, 'fwc' : 90000, 'vth' : 1.168e7, 't' : 20.48e-3, 'vg' : 6.e-11,
# 'st' : 5.0e-6, 'sfwc' : 730000., 'svg' : 1.0e-10})
# return out
#######################################
def CCDnonLinearityModel(data, beta=6e-7):
......@@ -346,13 +268,7 @@ def make_c_coor(fov, step):
##############################################################################
###############################################################################
# def str2time(strTime):
# if len(strTime)>20:#
# msec=int(float('0.'+strTime[20:])*1000000) # microsecond
# str2=strTime[0:19]+' '+str(msec)
# return datetime.strptime(str2,'%Y %m %d %H %M %S %f')
##############################################################################
#datetime to mjd
def time2mjd(dateT):
......@@ -444,18 +360,10 @@ def deg2HMS(ra0, dec0):
hhmmss=ss[0:2]+ss[3:5]+ra_ss
return hhmmss+dms_d+dms_m+dms_s
################################################################################
# def cut_radius(rcutstar, mstar, mag):
# return rcutstar * 10**(0.4*2*(mstar-mag)/3.125)
# def core_radius(rcorestar, mstar, mag):
# return rcorestar * 10**(0.4*(mstar-mag)/2)
# def v_disp(sigstar, mstar, mag):
# return sigstar * 10**(0.4*(mstar-mag)/3.57)
###############################################################################
###############################################################################
#####################################################################################
#############################################################################
#### distortion function
def distortField(ra, dec, ch):
......@@ -586,18 +494,6 @@ def cal_pos(center_ra, center_dec, rotTel, rotSky, sRa, sDec):
# return a.reshape(sh).sum(-1).sum(1)
#####################################################################
# def float2char(a, z):
# ### a is input float value
# ### transfer float a to chars and save z bis
# b=str(a)
# n=len(b)
# if z>=n:
# return b
# else:
# return b[:z]
#########################################################
def centroid(data):
......@@ -621,327 +517,8 @@ def centroid(data):
###############################################################################
# def fftrange(n, dtype=float):
# """FFT-aligned coordinate grid for n samples."""
# return np.arange(-n//2, -n//2+n, dtype=dtype)
###############################################################################
# def dft2(ary, Q, samples, shift=None):
# """Compute the two dimensional Discrete Fourier Transform of a matrix.
# Parameters
# ----------
# ary : `numpy.ndarray`
# an array, 2D, real or complex. Not fftshifted.
# Q : `float`
# oversampling / padding factor to mimic an FFT. If Q=2, Nyquist sampled
# samples : `int` or `Iterable`
# number of samples in the output plane.
# If an int, used for both dimensions. If an iterable, used for each dim
# shift : `float`, optional
# shift of the output domain, as a frequency. Same broadcast
# rules apply as with samples.
# Returns
# -------
# `numpy.ndarray`
# 2D array containing the shifted transform.
# Equivalent to ifftshift(fft2(fftshift(ary))) modulo output
# sampling/grid differences
# """
# # this is for dtype stabilization
# Q = float(Q) ## Q=lambda*f/D/pixelsize
# n, m = ary.shape ###ary maybe is the pupil function
# N, M = samples,samples
# X, Y, U, V = (fftrange(n) for n in (m, n, M, N))
# a = 1 / Q
# ###################################################################
# Eout_fwd = np.exp(-1j * 2 * np.pi * a / n * np.outer(Y, V).T)
# Ein_fwd = np.exp(-1j * 2 * np.pi * a / m * np.outer(X, U))
# #############################################################################
# out = Eout_fwd @ ary @ Ein_fwd #### ary is the input pupil function
# return out
##############################################################################
# def idft2(ary, Q, samples, shift=None):
# """Compute the two dimensional inverse Discrete Fourier Transform of a matrix.
# Parameters
# ----------
# ary : `numpy.ndarray`
# an array, 2D, real or complex. Not fftshifted.
# Q : `float`
# oversampling / padding factor to mimic an FFT. If Q=2, Nyquist sampled
# samples : `int` or `Iterable`
# number of samples in the output plane.
# If an int, used for both dimensions. If an iterable, used for each dim
# shift : `float`, optional
# shift of the output domain, as a frequency. Same broadcast
# rules apply as with samples.
# Returns
# -------
# `numpy.ndarray`
# 2D array containing the shifted transform.
# Equivalent to ifftshift(ifft2(fftshift(ary))) modulo output
# sampling/grid differences
# """
# # this is for dtype stabilization
# Q = float(Q) ## Q=lambda*f/D/pixelsize
# n, m = ary.shape ###ary maybe is the pupil function
# N, M = samples
# X, Y, U, V = (fftrange(n) for n in (m, n, M, N))
# ###############################################################################
# nm = n*m
# NM = N*M
# r = NM/nm
# a = 1 / Q
# ###################################################################
# # Eout_fwd = np.exp(-1j * 2 * np.pi * a / n * np.outer(Y, V).T)
# # Ein_fwd = np.exp(-1j * 2 * np.pi * a / m * np.outer(X, U))
# Eout_rev = np.exp(1j * 2 * np.pi * a / n * np.outer(Y, V).T) * (1/r)
# Ein_rev = np.exp(1j * 2 * np.pi * a / m * np.outer(X, U)) * (1/nm)
# ###########################################################################
# out = Eout_rev @ ary @ Ein_rev
# return out
###############################################################################
###############################################################################
# def opd2psf(opd,cwave,oversampling):
# '''
# calculate psf from opd data with defined wavelength
# Parameters
# ----------
# opd : TYPE
# the input opd data.
# cwave : TYPE
# the defined wavelength.
# '''
# D=2;
# focLength=41.253 # % MCI focal length in meters
# pixel=10/oversampling # % pixel size in microns
# opd=opd*1e9; ## convert opd unit of meter to nm
# zoomopd=ndimage.zoom(opd, 2, order=1)
# m,n=np.shape(zoomopd);
# clambda=cwave;
# wfe=zoomopd/clambda; #%% the main telescope aberration ,in wavelength;
# Q=clambda*1e-3*focLength/D/pixel
# pupil=np.zeros((m,m));
# pupil[abs(zoomopd)>0]=1;
# #idx=pupil>0;
# Nt=512
# phase=2*np.pi*wfe; #% wavefront phase in radians
# #%generalized pupil function of channel1;
# pk=pupil*np.exp(cmath.sqrt(-1)*(phase))
# pf=dft2(pk, Q, Nt)
# pf2 = abs(pf)**2
# psfout=pf2/pf2.sum()
# cx,cy=centroid(psfout)
# psf=ndimage.shift(psfout,[Nt/2-1-cy, Nt/2-1-cx],order=1, mode='nearest' )
# return psf
########################################################################
# def cal_PSF_new(channel,wfetimes,oversampling):
# # filed postion: Ra=ys1, Dec=ys2
# ############ use opd cal PSF on the defined field;
# #% psf interpolation test 20210207
# # xfmin=-0.07 # % the filed minmum value in the x direction in degrees
# # xfmax= 0.07 #% the filed maxmum value in the x direction in degrees
# # yfmin=-0.35 #% the filed minmum value in the y direction in degrees
# # yfmax=-0.49 # % the filed maxmum value in the y direction in degrees
# cfx= 0.2*3600; # % field center in x derection in arcsec;
# cfy= -0.45*3600; # % field center in y derection in arcsec;
# #wavelength=[255,337,419,501,583,665,747,829,911,1000]
# cwave=dict()
# if channel == 'g':
# cwave[channel]=475
# waven=4
# if channel == 'r':
# cwave[channel]=625
# waven=6
# if channel == 'i':
# cwave[channel]=776
# waven=7
# n=np.arange(1,101,1)
# ffx= 0.1+ 0.02222222*((n-1)%10)
# ffy=-0.35-0.02222222*np.floor((n-0.1)/10)
# psf=dict()
# fx=dict()
# fy=dict()
# fx[channel]=ffx*3600-cfx
# fy[channel]=ffy*3600-cfy
# Nt=512
# psf[channel]=np.zeros((len(n),Nt,Nt))
# for i in range(len(n)):
# #waven
# # waven=4
# # fieldn=10
# file=self.information['dir_path']+'MCI_inputData/MCI_wavefront/wave_'+str(waven+1)+'/wavefront/opd_'+str(i+1)+'.mat'
# data=sio.loadmat(file)
# opd=data['opd'] ## opd data;
# psf[channel][i,:,:]=opd2psf(wfetimes*opd, cwave[channel],oversampling)
# hdu1=fits.PrimaryHDU(psf[channel])
# hdu1.header.append(('channel', channel, 'MCI PSF channel'))
# hdu1.header['pixsize']=(0.05/oversampling, 'PSF pixel size in arcsec')
# hdu1.header['wfetimes']=(wfetimes, 'wavefront error magnification to CSST primary wavefront ')
# dtime=datetime.datetime.utcnow().strftime('%Y -%m -%d %H: %M: %S')
# hdu1.header.add_history('PSF is generated on :'+dtime)
# hdu2=fits.ImageHDU(fx[channel])
# hdu2.header.append(('field_X', 'arcsec'))
# hdu3=fits.ImageHDU(fy[channel])
# hdu3.header.append(('field_Y', 'arcsec'))
# newd=fits.HDUList([hdu1,hdu2,hdu3])
# PSFfilename=self.information['dir_path']+'MCI_inputData/PSF/PSF_'+channel+'.fits'
# newd.writeto(PSFfilename,overwrite=True)
# return
#############################################################################
# def cal_Filter_PSF(wfetimes):
# # filed postion: Ra=ys1, Dec=ys2
# ############ use opd cal PSF on the defined field;
# #% psf interpolation test 20210207
# # xfmin=-0.07 # % the filed minmum value in the x direction in degrees
# # xfmax= 0.07 #% the filed maxmum value in the x direction in degrees
# # yfmin=-0.35 #% the filed minmum value in the y direction in degrees
# # yfmax=-0.49 # % the filed maxmum value in the y direction in degrees
# oversampling=2
# cfx= 0.2*3600; # % field center in x derection in arcsec;
# cfy= -0.45*3600; # % field center in y derection in arcsec;
# wavelist =np.array([255, 337,419,501,583,665,747,829,911,1000])
# filterP=np.load(self.information['dir_path']+'MCI_inputData/MCI_filters/mci_filterPWTC.npy',allow_pickle=True).item()
# fn=np.arange(1,101,1) ### PSF field point
# ffx= 0.1+ 0.02222222*((fn-1)%10)
# ffy=-0.35-0.02222222*np.floor((fn-0.1)/10)
# psf=dict()
# fx=dict()
# fy=dict()
# fx=ffx*3600-cfx
# fy=ffy*3600-cfy
# Nt=512
# for filterk in filterP.keys():
# filtername=filterk
# ## print(filtername)
# filterwaveC=filterP[filterk]['Clambda']
# filterFwhm=filterP[filterk]['FWHM']
# fdis=abs(filterwaveC-wavelist)
# findex=np.argsort(fdis)
# waven=findex[0]
# psf[filtername]=dict()
# psf[filtername]['psf_field_X'] =fx
# psf[filtername]['psf_field_Y'] =fy
# psf[filtername]['psf_scale'] =0.05/oversampling
# psf[filtername]['wfetimes'] =wfetimes
# psf[filtername]['psf_mat'] =np.zeros( (Nt,Nt,7,len(fn)) )
# psf[filtername]['filter_name'] =filtername
# psf[filtername]['filter_channel']=filterP[filterk]['channel']
# psf[filtername]['psf_iwave'] =np.zeros(7)
# for ii in range(len(fn)):
# #waven
# # waven=4
# # fieldn=10
# file=self.information['dir_path']+'MCI_input/MCI_wavefront/wave_'+str(waven+1)+'/wavefront/opd_'+str(ii+1)+'.mat'
# data=sio.loadmat(file)
# opd=data['opd'] ## opd data;
# for kk in range(7):
# ###
# wavek=filterwaveC+filterFwhm*(kk-3)*0.25
# psfd=opd2psf(wfetimes*opd, wavek, oversampling)
# psf[filtername]['psf_mat'][:,:,kk,ii]=psfd[:,:]
# if ii==0:
# psf[filtername]['psf_iwave'][kk]=wavek
# np.save(self.information['dir_path']+'mci_sim_result/'+filtername+'_PSF.npy', psf[filtername])
# return
#########################################################################
'''
PSF interpolation for MCI_sim
......@@ -1145,8 +722,6 @@ class MCIsimulator():
#ghost ratio can be in engineering format, so getfloat does not capture it...
self.information['ghostratio'] = float(self.config.get(self.section, 'ghostRatio'))
###################################################################################################
##################################################################################################
......@@ -1201,27 +776,12 @@ class MCIsimulator():
save_cosmicrays =self.save_cosmicrays )
#####################################################################
# self.log.info('Using the following input values:')
# for key, value in self.information.items():
# self.log.info('%s = %s' % (key, value))
# self.log.info('Using the following booleans:')
# for key, value in self.booleans.items():
# self.log.info('%s = %s' % (key, value))
return
#########################################################################################
# def make_c_coor(self, bs, nc):
# '''
# Draw the mesh grids for a bs*bs box with nc*nc pixels
# '''
# ds=bs/nc
# xx01 = np.linspace(-bs/2.0,bs/2.0-ds,nc)+0.5*ds
# xx02 = np.linspace(-bs/2.0,bs/2.0-ds,nc)+0.5*ds
# xg2,xg1 = np.meshgrid(xx01,xx02)
# return xg1,xg2
##########################################################################################
##############################################################################
###############################################################################
def _createEmpty(self):
"""
......@@ -1236,32 +796,8 @@ class MCIsimulator():
self.image_i=np.zeros((self.information['ysize'], self.information['xsize']), dtype=float)
return
#########################################################################################################################
#########################################################################################################
# def smoothingWithChargeDiffusion(self, image, sigma=(0.32, 0.32)):
# """
# Smooths a given image with a gaussian kernel with widths given as sigmas.
# This smoothing can be used to mimic charge diffusion within the CCD.
# The default values are from Table 8-2 of CCD_273_Euclid_secification_1.0.130812.pdf converted
# to sigmas (FWHM / (2sqrt(2ln2)) and rounded up to the second decimal.
# .. Note:: This method should not be called for the full image if the charge spreading
# has already been taken into account in the system PSF to avoid float counting.
# :param image: image array which is smoothed with the kernel
# :type image: ndarray
# :param sigma: widths of the gaussian kernel that approximates the charge diffusion [0.32, 0.32].
# :param sigma: tuple
# :return: smoothed image array
# :rtype: ndarray
# """
# return ndimage.filters.gaussian_filter(image, sigma)
###############################################################################
##############################################################################
def _loadGhostModel(self):
"""
Reads in a ghost model from a FITS file and stores the data to self.ghostModel.
......@@ -1316,16 +852,12 @@ class MCIsimulator():
##print('print information:', self.information)
###########################################################################
now=datetime.utcnow()
#data_time=now.strftime("%Y-%m-%d-%H-%M-%S")
result_day=now.strftime("%Y-%m-%d")
if self.information['dir_path'] =='/nfsdata/share/simulation-unittest/mci_sim/':
self.result_path = self.information['dir_path'] +'mci_sim_result/'+result_day
else:
......@@ -1339,7 +871,6 @@ class MCIsimulator():
self.result_path = '/data/mcisimdata/'+result_day
if os.path.isdir(self.result_path)==False:
os.mkdir(self.result_path)
os.mkdir(self.result_path+'/cali_Data')
......@@ -1359,7 +890,6 @@ class MCIsimulator():
self.log = lg.setUpLogger(self.result_path+'/log_Data/MCIsim_'+self.source+'_'+data_time+'_Num_'+str(simnumber)+'.log')
self.log.info('-------STARTING A NEW SIMULATION------------')
for key, value in self.information.items():
......@@ -1376,16 +906,11 @@ class MCIsimulator():
#### load telescope efficiency data
self.tel_eff=np.load(self.information['dir_path']+'MCI_inputData/tel_eff/tel_eff.npy',allow_pickle=True).item()
#### load MCI filter data
self.filterP=np.load(self.information['dir_path']+'MCI_inputData/MCI_filters/mci_filterPWTC.npy',allow_pickle=True).item()
return
################################################################################
......@@ -1521,14 +1046,6 @@ class MCIsimulator():
wave = np.linspace(2500,11000, 8501) # set the wavelenth for MCI from 250nm to 1100nm
# wavearr =self.earthshine_wave # A
# fluxarr =self.earthshine_flux # erg/s/cm^2/A/arcsec^2
# earthshinefluxarr=np.interp(wave, wavearr, fluxarr) # erg/s/cm^2/A/arcsec^2
# wavearr =self.zodiacal_wave # A
# fluxarr =self.zodiacal_flux # erg/s/cm^2/A/arcsec^2
# zodiacalfluxarr=np.interp(wave, wavearr, fluxarr) # erg/s/cm^2/A/arcsec^2
skynoise_flux=self.earthshine_flux+self.zodiacal_flux # erg/s/cm^2/A/arcsec^2
......@@ -1607,13 +1124,6 @@ class MCIsimulator():
self.log.info('Stat catlog file name is %s' % (starcat))
######################################################################
# da=fits.open(self.information['dir_path']+'MCI_inputData/star_input/'+starcat)
# df2=da[1].data
# del da
##########################################
df2=pandas.read_csv(self.information['dir_path']+'MCI_inputData/star_input/'+starcat)
......@@ -1753,8 +1263,6 @@ class MCIsimulator():
########## finish save PSF fits ##########################################
############################################################################
###### add binary stars to the star catlog #######
nsrcs=len(self.star['ra_gaia'])
......@@ -1790,8 +1298,6 @@ class MCIsimulator():
#######################################################################
nlayccd = 0
############################################
ra = self.information['ra_pnt0']
......@@ -1803,9 +1309,6 @@ class MCIsimulator():
y_sat=float(self.orbit_pars[self.orbit_exp_num,2])
z_sat=float(self.orbit_pars[self.orbit_exp_num,3])
wave0, zodi0 = self.zodiacal(ra, dec, self.TianCe_day) # erg/s/cm^2/A/arcsec^2
self.log.info('dir_path:')
......@@ -1899,9 +1402,6 @@ class MCIsimulator():
#################### generate star image ##########
for j in tqdm(range(nsrcs)): ### nsrcs length
if j==0:
......@@ -1913,9 +1413,7 @@ class MCIsimulator():
starRa = 3600.0*( newRa[j] ) # ra of star, arcsecond
starDec = 3600.0*( newDec[j] ) # dec of star, arcsecond
###################################################################
###################################################################
fsx,fsy=cal_pos(center_ra,center_dec, rotTelPos, rotSkyPos, starRa, starDec)
row= fsy/pixelscale+self.information['ysize']/2-0.5 ### row number on CCD image
......@@ -1928,7 +1426,6 @@ class MCIsimulator():
nlayccd=nlayccd+1
if self.debug:
if nlayccd>1:
break
......@@ -1976,8 +1473,6 @@ class MCIsimulator():
####### use SED_code to generate star SED #######
# SED of j-th star
umag = self.star['umag'][j]
gmag = self.star['gmag'][j]
rmag = self.star['rmag'][j]
......@@ -1987,7 +1482,6 @@ class MCIsimulator():
# Input redshift
redshift = 0
# Loading galaxy SED template
t=sed.Gal_Temp(self.information['dir_path'])
# Calculating the magnitude (u, g, r, i, z) of each template
......@@ -1996,8 +1490,6 @@ class MCIsimulator():
ugriz = np.array([umag, gmag, rmag, imag, zmag])
star_flux = sed.Model_Galaxy_SED(wave, ugriz, redshift, t, self.information['dir_path'])
##cal_SED_photons(self, flux_arr):
intscales,PSF_eff_weight=self.cal_SED_photons(star_flux)
......@@ -2020,8 +1512,6 @@ class MCIsimulator():
if nlayccd %10 == 0:
self.log.info('Star number on CCD is = %i' % (nlayccd))
######
st_phot_C1.append(intscales['g'])
st_phot_C2.append(intscales['r'])
......@@ -2115,8 +1605,6 @@ class MCIsimulator():
cx0,cy0=centroid(image.array)
#self.log.info('finish appfat ........')
############################################
############################################
photons.x=photons.x-cx0*0.025
......@@ -2176,8 +1664,6 @@ class MCIsimulator():
tab['st_magi']=np.asarray(st_magi)
tab['st_magz']=np.asarray(st_magz)
###################################33
......@@ -2196,63 +1682,6 @@ class MCIsimulator():
################################################################################
################################################################################
#################################################################################
########################################################################
# def earthshine(self, theta):
# """
# For given theta angle, return the earth-shine spectrum.
# :param theta: angle (in degree) from the target to earth limb.
# :return: the scaled solar spectrum
# template_wave: unit in A
# template_flux: unit in erg/s/cm^2/A/arcsec^2
# """
# # read solar template
# solar_template = pd.read_csv(self.information['dir_path']+'MCI_inputData/refs/solar_spec.dat', sep='\s+',
# header=None, comment='#')
# template_wave = solar_template[0].values
# template_flux = solar_template[1].values
# # read earth shine surface brightness
# earthshine_curve = pd.read_csv(self.information['dir_path']+'MCI_inputData/refs/earthshine.dat',
# header=None, comment='#')
# angle = earthshine_curve[0].values
# surface_brightness = earthshine_curve[1].values
# # read V-band throughtput
# cat_filter_V = pd.read_csv(self.information['dir_path']+'MCI_inputData/refs/filter_Bessell_V.dat', sep='\s+',
# header=None, comment='#')
# filter_wave = cat_filter_V[0].values
# filter_response = cat_filter_V[1].values
# # interplate to the target wavelength in V-band
# ind_filter = (template_wave >= np.min(filter_wave)) & (template_wave <= np.max(filter_wave))
# filter_wave_interp = template_wave[ind_filter]
# filter_response_interp = np.interp(filter_wave_interp, filter_wave, filter_response)
# filter_constant = simps(filter_response_interp * filter_wave_interp, filter_wave_interp)
# template_constant = simps(filter_response_interp * template_wave[ind_filter] * template_flux[ind_filter],
# template_wave[ind_filter])
# dwave = filter_wave_interp[1:] - filter_wave_interp[:-1]
# wave_eff = np.nansum(dwave * filter_wave_interp[1:] * filter_response_interp[1:]) / \
# np.nansum(dwave * filter_response_interp[1:])
# # get the normalized value at theta.
# u0 = np.interp(theta, angle, surface_brightness) # mag/arcsec^2
# u0 = 10**((u0 + 48.6)/(-2.5)) # target flux in erg/s/cm^2/Hz unit
# u0 = u0 * 3e18 / wave_eff**2 # erg/s/cm^2/A/arcsec^2
# factor = u0 * filter_constant / template_constant
# norm_flux = template_flux * factor # erg/s/cm^2/A/arcsec^2
# self.earthshine_wave=template_wave # A
# self.earthshine_flux=norm_flux
# return
# ########################################################################################################################################################################################################################################################
def zodiacal(self, ra, dec, time):
"""
......@@ -2821,8 +2250,6 @@ class MCIsimulator():
###############################################################################
###############################################################################
###############################################################################
def generatePRNU(self, ave=1.0, sigma=0.01):
......@@ -2924,9 +2351,6 @@ class MCIsimulator():
cosmics_r = cosmicrays.cosmicrays(self.log, crImage, self.information['exptime'], crInfo=self.cr)
cosmics_i = cosmicrays.cosmicrays(self.log, crImage, self.information['exptime'], crInfo=self.cr)
#add cosmic rays up to the covering fraction
#CCD_cr = cosmics.addUpToFraction(self.information['coveringFraction'], limit=None)
CCD_cr_g = cosmics_g.addUpToFraction(self.information['coveringfraction']*self.information['exptime']/300.0, limit=None)
CCD_cr_r = cosmics_r.addUpToFraction(self.information['coveringfraction']*self.information['exptime']/300.0, limit=None)
CCD_cr_i = cosmics_i.addUpToFraction(self.information['coveringfraction']*self.information['exptime']/300.0, limit=None)
......@@ -2937,8 +2361,6 @@ class MCIsimulator():
self.image_r += CCD_cr_r
self.image_i += CCD_cr_i
#save cosmic ray image map
#self.cosmicMap = CCD_cr
if self.save_cosmicrays and self.cosmicRays:
......@@ -3120,8 +2542,6 @@ class MCIsimulator():
y = np.round(cosmetics[:, 1]).astype(int) ## col number
value = np.round(cosmetics[:, 2]).astype(int)
#cosmetics_r=np.zeros((4636,235526))
self.log.info('Adding cosmetic defects to C2 channel:' )
for xc, yc, val in zip(x, y, value):
if 0 < xc < 4616 and 27 < (yc % 1499) <1179:
......@@ -3817,10 +3237,6 @@ class MCIsimulator():
ofd_g.header['EPOCH'] =(np.float32(time2jd(t3.utcnow())), 'equinox of pointing RA and Dec')
ofd_g.header['EXPTIME']=(np.float32(self.information['exptime']), 'exposure time (s)')
# ss1='HDU checksum'
# ss2='data unit checksum'
# ofd_g.header['CHECKSUM']=( data_time[:19] , ss1)
# ofd_g.header['DATASUM'] =( data_time[:19] , ss2)
ofd_g.header['CHECKSUM'] =(0, '0')
################################################
########## finish header for 0 layer ####################
......@@ -4039,10 +3455,7 @@ class MCIsimulator():
hdu_g.header['EPOCH'] =(np.float32(time2jd(t3.utcnow())), 'equinox of pointing RA and Dec')
hdu_g.header['CHECKSUM'] =(0, '0')
##############################################################
#####
# hdu_g.header['CHECKSUM'] =('','HDU checksum updated yyyy-mm-ddTHH:MM:SS')
# hdu_g.header['DATASUM'] =('','data unit checksum updated yyyy-mm-ddTHH:MM:SS')
################ finish MCI header for image layer in G channel
##############################################################################################333
......@@ -4199,10 +3612,6 @@ class MCIsimulator():
ofd_r.header['EPOCH'] =(np.float32(time2jd(t3.utcnow())), 'equinox of pointing RA and Dec')
ofd_r.header['EXPTIME']=(np.float32(self.information['exptime']), 'exposure time (s)')
# ss1='HDU checksum'
# ss2='data unit checksum'
# ofd_r.header['CHECKSUM']=( data_time[:19] , ss1)
# ofd_r.header['DATASUM'] =( data_time[:19] , ss2)
ofd_r.header['CHECKSUM'] =(0, '0')
################################################
########## finish header for 0 layer ####################
......@@ -4419,10 +3828,6 @@ class MCIsimulator():
hdu_r.header['EPOCH'] =(np.float32(time2jd(t3.utcnow())), 'equinox of pointing RA and Dec')
hdu_r.header['CHECKSUM'] =(0, '0')
##############################################################
#####
# hdu_r.header['CHECKSUM'] =('','HDU checksum updated yyyy-mm-ddTHH:MM:SS')
# hdu_r.header['DATASUM'] =('','data unit checksum updated yyyy-mm-ddTHH:MM:SS')
################ finish MCI header for image layer in G channel
##############################################################################################333
......@@ -4580,10 +3985,6 @@ class MCIsimulator():
ofd_i.header['EPOCH'] =(np.float32(time2jd(t3.utcnow())), 'equinox of pointing RA and Dec')
ofd_i.header['EXPTIME']=(np.float32(self.information['exptime']), 'exposure time (s)')
# ss1='HDU checksum'
# ss2='data unit checksum'
# ofd_i.header['CHECKSUM']=( data_time[:19] , ss1)
# ofd_i.header['DATASUM'] =( data_time[:19] , ss2)
ofd_i.header['CHECKSUM'] =(0, '0')
################################################
########## finish header for 0 layer ####################
......@@ -4805,8 +4206,6 @@ class MCIsimulator():
hdu_i.header['CHECKSUM'] =(0, '0')
##############################################################
#####
################ finish MCI header for image layer in G channel
##############################################################################################333
......@@ -5336,7 +4735,7 @@ class MCIsimulator():
def runMCIsim(sourcein,configfile,dir_path, debug, iLoop):
print('路径Test：dir_path', dir_path)
print('Path Test：dir_path', dir_path)
sim= dict()
sim[iLoop] = MCIsimulator(configfile)
......
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