Loading csst_mci_sim/support/sed.pydeleted 100755 → 0 +0 −242 Original line number Diff line number Diff line #!/usr/bin/env python # -*- coding:utf-8 -*- # @Author: Shuai Feng (hebtu.edu.cn) # @Time: 2022-09-25 import numpy as np from scipy.interpolate import interp1d from astropy.io import fits from astropy.io import ascii from astropy import units as u # ---------------- # Magnitude Module from scipy.interpolate import interp1d def Calzetti_Law(wave, Rv = 4.05): """Dust Extinction Curve by Calzetti et al. (2000) Args: wave (float): Wavelength Rv (float, optional): Extinction curve. Defaults to 4.05. Returns: float: Extinction value E(B-V) """ wave_number = 1./(wave * 1e-4) reddening_curve = np.zeros(len(wave)) idx = np.logical_and(wave >= 1200, wave <= 6300) reddening_curve[idx] = 2.659 * ( -2.156 + 1.509 * wave_number[idx] - 0.198 * \ (wave_number[idx] ** 2)) + 0.011 * (wave_number[idx] **3 ) + Rv idx = np.logical_and(wave >= 6300, wave <= 22000) reddening_curve[idx] = 2.659 * ( -1.857 + 1.040 * wave_number[idx]) + Rv return reddening_curve def reddening(wave, flux, ebv = 0.0, law = 'calzetti', Rv = 4.05): """ Reddening an input spectra through a given reddening curve. Args: wave (float): Wavelength of input spectra flux (float): Flux of input spectra ebv (float, optional): Extinction value. Defaults to 0. law (str, optional): Extinction curve. Defaults to 'calzetti'. Rv (float, optional): _description_. Defaults to 4.05. Returns: float: Flux of spectra after reddening. """ if law == 'calzetti': curve = Calzetti_Law(wave, Rv = Rv) fluxNew = flux / (10. ** (0.4 * ebv * curve)) return fluxNew def flux_to_mag(wave, flux, path, band='GAIA_bp'): """Convert flux of given spectra to magnitude Args: wave (float): Wavelength flux (float): Flux of spectra band (str, optional): Filter band name. Defaults to 'GAIA_bp'. Returns: float: value of magnitude """ # /home/yan/MCI_sim/MCI_input/SED_Code/data ##import os ###parent = os.path.dirname(os.path.realpath(__file__)) band = ascii.read(path+'MCI_inputData/SED_Code/seddata/' + band + '.dat') wave0= band['col1'] curv0= band['col2'] # Setting the response func = interp1d(wave0, curv0) response = np.copy(wave) ind_extra = (wave > max(wave0)) | (wave < min(wave0)) response[ind_extra] = 0 ind_inside = (wave < max(wave0)) & (wave > min(wave0)) response[ind_inside] = func(wave[ind_inside]) # Total Flux Tflux = np.trapz(flux * response, wave) / np.trapz(response, wave) return -2.5 * np.log10(Tflux) def calibrate(wave, flux, mag, path,band='GAIA_bp'): """ Calibrate the spectra according to the magnitude. Args: wave (float): Wavelength flux (float): Flux of spectra mag (float): Input magnitude. band (str, optional): Filter band name. Defaults to 'GAIA_bp'. Returns: float: Flux of calibrated spectra. Units: 1e-17 erg/s/A/cm^2 """ inst_mag = flux_to_mag(wave, flux, path,band = band) instflux = 10 ** (-0.4 * inst_mag) realflux = (mag * u.STmag).to(u.erg/u.s/u.cm**2/u.AA).value # Normalization flux_ratio = realflux / instflux flux_calibrate = flux * flux_ratio * 1e17 # Units: 10^-17 erg/s/A/cm^2 return flux_calibrate # ------------ # SED Template class Gal_Temp(): """ Template of Galaxy SED """ def __init__(self,path): ###import os ###parent = os.path.dirname(os.path.realpath(__file__)) self.path=path hdulist = fits.open(self.path+'MCI_inputData/SED_Code/seddata/galaxy_temp.fits') self.wave = hdulist[1].data['wave'] self.flux = hdulist[2].data self.age_grid = hdulist[3].data['logAge'] self.feh_grid = hdulist[3].data['FeH'] def toMag(self, redshift = 0): """Calculating magnitude Args: redshift (float, optional): redshift of spectra. Defaults to 0. """ wave = self.wave * (1 + redshift) self.umag = flux_to_mag(wave, self.flux, self.path,band='SDSS_u') self.gmag = flux_to_mag(wave, self.flux, self.path,band='SDSS_g') self.rmag = flux_to_mag(wave, self.flux, self.path,band='SDSS_r') self.imag = flux_to_mag(wave, self.flux, self.path,band='SDSS_i') self.zmag = flux_to_mag(wave, self.flux, self.path,band='SDSS_z') class Star_Temp(): """ Template of Stellar SED """ def __init__(self,path): ##import os self.path=path ####parent = os.path.dirname(os.path.realpath(__file__)) ###print("获取其父目录——" + parent) # 从当前文件路径中获取目录 hdulist = fits.open(path+'MCI_inputData/SED_Code/seddata/stellar_temp.fits') self.wave = hdulist[1].data['wave'] self.flux = hdulist[2].data self.Teff_grid = hdulist[3].data['Teff'] self.FeH_grid = hdulist[3].data['FeH'] self.bpmag = flux_to_mag(self.wave, self.flux, path,band='GAIA_bp') self.rpmag = flux_to_mag(self.wave, self.flux, path,band='GAIA_rp') def toMag(self): wave = self.wave self.bpmag = flux_to_mag(wave, self.flux, self.path,band='GAIA_bp') self.rpmag = flux_to_mag(wave, self.flux, self.path,band='GAIA_rp') # ------------- # SED Modelling def Model_Stellar_SED(wave, bp, rp, temp): """Modelling stellar SED based on bp, rp magnitude Args: wave (float): Wavelength bp (float): Magnitude of GAIA BP band rp (float): Magnitude of GAIA RP band temp (class): Class of stellar template Returns: float array: Spectral energy distribution of stellar SED, which have the same length to the input wave """ color0 = bp - rp colors = temp.bpmag - temp.rpmag idx = np.argmin(np.abs(colors - color0)) flux0 = temp.flux[idx] flux1 = np.interp(wave, temp.wave, flux0) flux = calibrate(wave, flux1, rp, band = 'GAIA_rp') return flux def Model_Galaxy_SED(wave, ugriz, z, temp, path): """Modelling galaxy SED based on u,g,r,i,z magnitude Args: wave (float): Wavelength ugriz (float, array): The array of magnitude of SDSS ugriz band z (float): Redshift temp (class): Class of gaalxy template Returns: float array: Spectral energy distribution of stellar SED, which have the same length to the input wave """ sed = 10. ** (-0.4 * ugriz) sed = sed / sed[2] ntemp = len(temp.rmag) dmag = np.zeros(ntemp) for j in range(ntemp): ugriz0 = np.array([temp.umag[j], temp.gmag[j], temp.rmag[j], temp.imag[j], temp.zmag[j]]) sed0 = 10. ** (-0.4 * ugriz0) sed0 = sed0 / sed0[2] dmag[j] = np.sum(np.abs(sed - sed0)) idx = np.argmin(dmag) flux0 = temp.flux[idx] # Effect of E(B-V) ri0 = ugriz[2] - ugriz[3] ri = temp.rmag - temp.imag dri = ri0 - ri[idx] Alambda = Calzetti_Law(np.array([6213 / (1 + z), 7625 / (1 + z)])) eri0 = (Alambda[0] - Alambda[1]) ebv = dri/eri0 if ebv<0: ebv=0 if ebv>0.5: ebv=0.5 flux1 = reddening(temp.wave, flux0, ebv = ebv) flux2 = np.interp(wave, temp.wave * (1 + z), flux1) flux = calibrate(wave, flux2, ugriz[2], path, band = 'SDSS_r') return flux No newline at end of file Loading
csst_mci_sim/support/sed.pydeleted 100755 → 0 +0 −242 Original line number Diff line number Diff line #!/usr/bin/env python # -*- coding:utf-8 -*- # @Author: Shuai Feng (hebtu.edu.cn) # @Time: 2022-09-25 import numpy as np from scipy.interpolate import interp1d from astropy.io import fits from astropy.io import ascii from astropy import units as u # ---------------- # Magnitude Module from scipy.interpolate import interp1d def Calzetti_Law(wave, Rv = 4.05): """Dust Extinction Curve by Calzetti et al. (2000) Args: wave (float): Wavelength Rv (float, optional): Extinction curve. Defaults to 4.05. Returns: float: Extinction value E(B-V) """ wave_number = 1./(wave * 1e-4) reddening_curve = np.zeros(len(wave)) idx = np.logical_and(wave >= 1200, wave <= 6300) reddening_curve[idx] = 2.659 * ( -2.156 + 1.509 * wave_number[idx] - 0.198 * \ (wave_number[idx] ** 2)) + 0.011 * (wave_number[idx] **3 ) + Rv idx = np.logical_and(wave >= 6300, wave <= 22000) reddening_curve[idx] = 2.659 * ( -1.857 + 1.040 * wave_number[idx]) + Rv return reddening_curve def reddening(wave, flux, ebv = 0.0, law = 'calzetti', Rv = 4.05): """ Reddening an input spectra through a given reddening curve. Args: wave (float): Wavelength of input spectra flux (float): Flux of input spectra ebv (float, optional): Extinction value. Defaults to 0. law (str, optional): Extinction curve. Defaults to 'calzetti'. Rv (float, optional): _description_. Defaults to 4.05. Returns: float: Flux of spectra after reddening. """ if law == 'calzetti': curve = Calzetti_Law(wave, Rv = Rv) fluxNew = flux / (10. ** (0.4 * ebv * curve)) return fluxNew def flux_to_mag(wave, flux, path, band='GAIA_bp'): """Convert flux of given spectra to magnitude Args: wave (float): Wavelength flux (float): Flux of spectra band (str, optional): Filter band name. Defaults to 'GAIA_bp'. Returns: float: value of magnitude """ # /home/yan/MCI_sim/MCI_input/SED_Code/data ##import os ###parent = os.path.dirname(os.path.realpath(__file__)) band = ascii.read(path+'MCI_inputData/SED_Code/seddata/' + band + '.dat') wave0= band['col1'] curv0= band['col2'] # Setting the response func = interp1d(wave0, curv0) response = np.copy(wave) ind_extra = (wave > max(wave0)) | (wave < min(wave0)) response[ind_extra] = 0 ind_inside = (wave < max(wave0)) & (wave > min(wave0)) response[ind_inside] = func(wave[ind_inside]) # Total Flux Tflux = np.trapz(flux * response, wave) / np.trapz(response, wave) return -2.5 * np.log10(Tflux) def calibrate(wave, flux, mag, path,band='GAIA_bp'): """ Calibrate the spectra according to the magnitude. Args: wave (float): Wavelength flux (float): Flux of spectra mag (float): Input magnitude. band (str, optional): Filter band name. Defaults to 'GAIA_bp'. Returns: float: Flux of calibrated spectra. Units: 1e-17 erg/s/A/cm^2 """ inst_mag = flux_to_mag(wave, flux, path,band = band) instflux = 10 ** (-0.4 * inst_mag) realflux = (mag * u.STmag).to(u.erg/u.s/u.cm**2/u.AA).value # Normalization flux_ratio = realflux / instflux flux_calibrate = flux * flux_ratio * 1e17 # Units: 10^-17 erg/s/A/cm^2 return flux_calibrate # ------------ # SED Template class Gal_Temp(): """ Template of Galaxy SED """ def __init__(self,path): ###import os ###parent = os.path.dirname(os.path.realpath(__file__)) self.path=path hdulist = fits.open(self.path+'MCI_inputData/SED_Code/seddata/galaxy_temp.fits') self.wave = hdulist[1].data['wave'] self.flux = hdulist[2].data self.age_grid = hdulist[3].data['logAge'] self.feh_grid = hdulist[3].data['FeH'] def toMag(self, redshift = 0): """Calculating magnitude Args: redshift (float, optional): redshift of spectra. Defaults to 0. """ wave = self.wave * (1 + redshift) self.umag = flux_to_mag(wave, self.flux, self.path,band='SDSS_u') self.gmag = flux_to_mag(wave, self.flux, self.path,band='SDSS_g') self.rmag = flux_to_mag(wave, self.flux, self.path,band='SDSS_r') self.imag = flux_to_mag(wave, self.flux, self.path,band='SDSS_i') self.zmag = flux_to_mag(wave, self.flux, self.path,band='SDSS_z') class Star_Temp(): """ Template of Stellar SED """ def __init__(self,path): ##import os self.path=path ####parent = os.path.dirname(os.path.realpath(__file__)) ###print("获取其父目录——" + parent) # 从当前文件路径中获取目录 hdulist = fits.open(path+'MCI_inputData/SED_Code/seddata/stellar_temp.fits') self.wave = hdulist[1].data['wave'] self.flux = hdulist[2].data self.Teff_grid = hdulist[3].data['Teff'] self.FeH_grid = hdulist[3].data['FeH'] self.bpmag = flux_to_mag(self.wave, self.flux, path,band='GAIA_bp') self.rpmag = flux_to_mag(self.wave, self.flux, path,band='GAIA_rp') def toMag(self): wave = self.wave self.bpmag = flux_to_mag(wave, self.flux, self.path,band='GAIA_bp') self.rpmag = flux_to_mag(wave, self.flux, self.path,band='GAIA_rp') # ------------- # SED Modelling def Model_Stellar_SED(wave, bp, rp, temp): """Modelling stellar SED based on bp, rp magnitude Args: wave (float): Wavelength bp (float): Magnitude of GAIA BP band rp (float): Magnitude of GAIA RP band temp (class): Class of stellar template Returns: float array: Spectral energy distribution of stellar SED, which have the same length to the input wave """ color0 = bp - rp colors = temp.bpmag - temp.rpmag idx = np.argmin(np.abs(colors - color0)) flux0 = temp.flux[idx] flux1 = np.interp(wave, temp.wave, flux0) flux = calibrate(wave, flux1, rp, band = 'GAIA_rp') return flux def Model_Galaxy_SED(wave, ugriz, z, temp, path): """Modelling galaxy SED based on u,g,r,i,z magnitude Args: wave (float): Wavelength ugriz (float, array): The array of magnitude of SDSS ugriz band z (float): Redshift temp (class): Class of gaalxy template Returns: float array: Spectral energy distribution of stellar SED, which have the same length to the input wave """ sed = 10. ** (-0.4 * ugriz) sed = sed / sed[2] ntemp = len(temp.rmag) dmag = np.zeros(ntemp) for j in range(ntemp): ugriz0 = np.array([temp.umag[j], temp.gmag[j], temp.rmag[j], temp.imag[j], temp.zmag[j]]) sed0 = 10. ** (-0.4 * ugriz0) sed0 = sed0 / sed0[2] dmag[j] = np.sum(np.abs(sed - sed0)) idx = np.argmin(dmag) flux0 = temp.flux[idx] # Effect of E(B-V) ri0 = ugriz[2] - ugriz[3] ri = temp.rmag - temp.imag dri = ri0 - ri[idx] Alambda = Calzetti_Law(np.array([6213 / (1 + z), 7625 / (1 + z)])) eri0 = (Alambda[0] - Alambda[1]) ebv = dri/eri0 if ebv<0: ebv=0 if ebv>0.5: ebv=0.5 flux1 = reddening(temp.wave, flux0, ebv = ebv) flux2 = np.interp(wave, temp.wave * (1 + z), flux1) flux = calibrate(wave, flux2, ugriz[2], path, band = 'SDSS_r') return flux No newline at end of file
