http://noneq.strw.leidenuniv.nl/

tables HM01

wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Hydrogen.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Helium.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Carbon.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Nitrogen.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Oxygen.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Neon.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Magnesium.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Silicon.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Sulphur.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Caclium.HM01.hdf5 wget http://noneq.strw.leidenuniv.nl/hdf5tables/IonRates_Iron.HM01.hdf5

some scripts

plot_cooling_fct.py

./plot_collisional_ionisation_rate.py # beta(T) ionisation par collision ./plot_photo_ionisation_rate.py # gamma(Z) ionisation par UV background ./plot_heating_rate.py # epsilon(Z) photo heating rate ./plot_heating_rate_Zsol.py # compare the photo heating rates of neutral atoms, assuming a solar metallicity ./plot_recombination_rate.py # alpha(T) recombinaison

./plot_densities.py # plot densities as a function of time

./plot_heating.py # Photo Heating Efficiency as a function of redshift (needs to be muliplied by n_ix for real units)

read the tables

import h5py

table = h5py.File("HM01/IonRates_Hydrogen.HM01.hdf5") table = h5py.File("HM01/IonRates_Oxygen.HM01.hdf5")

table.keys()

2. header ####

table['Header'].keys()

[u'AtomicWeight', u'ElementName', u'Ion_Names', u'Ions', u'N_Ions', u'N_Redshifts', u'N_Temperatures', 176 u'Redshifts', u'SolarMassFraction', u'SolarNumberRatio', u'Temperatures']

table['Header']['Ions'].value

2. Rates ####

table['Rates'].keys()

[u'AlphaDi', # alpha dielectronic u'AlphaRad', # alpha radiative alpha = AlphaDi+AlphaRad (N_Ion , N_Temperatures) u'BetaColl', # beta collision (N_Ion , N_Temperatures) u'CTHeionof', #??? (N_Ion , N_Temperatures) u'CTHerecof', #??? (N_Ion , N_Temperatures) u'CTHionof', #??? (N_Ion , N_Temperatures) u'CTHrecof', # ??? (N_Ion , N_Temperatures) u'Cool', # Lambda_prime () (N_Ion , N_Temperatures) u'GammaPhot', # ??? Gamma photoionisation (N_Ion,N_Redshifts, 10?) u'Heat'] # ??? photo heating efficiency (N_Ion,N_Redshifts)

table['Rates']['AlphaDi'].value # 2x176 (2 ion x 176 temperature 176)

solar abundances

yves          SolarMassFraction

H 0.70649785 He 0.28055534

O 0.0108169 0.00549262 ???

Si 0.000996529 0.00068259

Mg 0.000924316 0.00059071 Fe 0.00176604 0.00110322

In Wiersma

Default Cloudy solar abundances

ni/nH               MassFraction
                    = ni/nH*Ai *MassFraction_H

H 1 0.7065 He 0.1 0.2806 C 2.46e-4 2.07e-3 O 4.90e-4 5.49e-3 Si 3.47e-5 6.83e-4 Mg 3.47e-5 5.91e-4 Fe 2.82e-5 1.10e-3

from Grevesse

                    dans chimie.yr.dat
                    = ni/nH*Ai
ni/nH

H 1 He 0.0851138038 C 3.311311e-04 O 6.760830e-04 Si 3.548134e-05 Mg 3.801894e-05 0.000924316 Fe 3.162278e-05 0.00176604