SYGMA Module

GCE SYGMA (Stellar Yields for Galaxy Modelling Applications) module

Functionality

This tool allows the modeling of simple stellar populations. Creating a SYGMA instance runs the simulation while extensive analysis can be done with the plot_* functions found in the chem_evol_plot module. See the DOC directory for a detailed documentation.

Made by

v0.1 NOV2013: C. Fryer, C. Ritter

v0.2 JAN2014: C. Ritter

v0.3 APR2014: C. Ritter, J. F. Navarro, F. Herwig, C. Fryer, E. Starkenburg,

M. Pignatari, S. Jones, K. Venn1, P. A. Denissenkov & the NuGrid collaboration

v0.4 FEB2015: C. Ritter, B. Cote v0.5 MAY2016: C. Ritter; Note: See from now the official releases via github.

Usage

Simple run example:

>>> import sygma as s

Get help with

>>> help s

Now start a calculation by providing the initial metal fraction iniZ, the final evolution time tend, and the total mass of the SSP:

>>> s1=s.sygma(iniZ=0.0001, tend=5e9, mgal=1e5)

For more information regarding the input parameter see below or try

>>> s.sygma?

For plotting utilize the plotting functions (plot_*) as described further below, for example:

>>> s1.plot_totmasses()

You can write out the information about the composition of the total ejecta of a SSP via

>>> s.write_evol_table(elements=['H','C','O'])

Yield tables are available in the NUPYCEE subdirectory yield/textunderscore tables. Add your yield tables to this directory and SYGMA will be able to read the table if you have specified the $table$ variable. Only for tables with Z=0 is the variable $pop3/textunderscore table$ used. Both tables need yields specified in the SYGMA (and OMEGA) yield input format. See the default table for the structure. It is important to provide an initial abundance file which must match the number of species provided in the yield tables. Provide the file in the iniAbu directory inside the directory yield/extunderscore tables. The input variable with which the table file can be specified is $iniabu/textunderscore table$. For the necessary structure see again the default choice of that variable.

For example with artificial yields of only H-1, you can try

>>> s2 = s.sygma(iniZ=0.0001,dt=1e8,tend=1.5e10, mgal=1e11,table='yield_tables/isotope_yield_table_h1.txt',
    sn1a_table='yield_tables/sn1a_h1.txt',iniabu_table='yield_tables/iniab1.0E-04GN93_alpha_h1.ppn.txt')

class sygma.sygma(sfr='input', imf_type='kroupa', alphaimf=2.35, imf_bdys=[0.1, 100], sn1a_rate='power_law', iniZ=0.0, dt=1000000.0, special_timesteps=30, nsmerger_bdys=[8, 100], tend=13000000000.0, mgal=10000.0, transitionmass=8, iolevel=0, ini_alpha=True, table='yield_tables/isotope_yield_table_MESA_only_fryer12_delay.txt', hardsetZ=-1, sn1a_on=True, sn1a_table='yield_tables/sn1a_t86.txt', sn1a_energy=1e+51, ns_merger_on=True, bhns_merger_on=False, f_binary=1.0, f_merger=0.0008, t_merger_max=10000000000.0, m_ej_nsm=0.025, nsm_dtd_power=[], m_ej_bhnsm=0.025, bhnsmerger_table='yield_tables/r_process_rosswog_2014.txt', nsmerger_table='yield_tables/r_process_rosswog_2014.txt', iniabu_table='', extra_source_on=False, nb_nsm_per_m=-1.0, t_nsm_coal=-1.0, extra_source_table='yield_tables/extra_source.txt', f_extra_source=1.0, pop3_table='yield_tables/popIII_heger10.txt', imf_bdys_pop3=[0.1, 100], imf_yields_range_pop3=[10, 30], starbursts=[], beta_pow=-1.0, gauss_dtd=[1000000000.0, 660000000.0], exp_dtd=2000000000.0, nb_1a_per_m=0.001, direct_norm_1a=-1, Z_trans=0.0, f_arfo=1.0, imf_yields_range=[1, 30], exclude_masses=[], netyields_on=False, wiersmamod=False, yield_interp='lin', stellar_param_on=False, t_dtd_poly_split=-1.0, stellar_param_table='yield_tables/isotope_yield_table_MESA_only_param.txt', tau_ferrini=False, dt_in=array([], dtype=float64), nsmerger_dtd_array=array([], dtype=float64), bhnsmerger_dtd_array=array([], dtype=float64), ytables_in=array([], dtype=float64), zm_lifetime_grid_nugrid_in=array([], dtype=float64), isotopes_in=array([], dtype=float64), ytables_pop3_in=array([], dtype=float64), zm_lifetime_grid_pop3_in=array([], dtype=float64), ytables_1a_in=array([], dtype=float64), mass_sampled=array([], dtype=float64), scale_cor=array([], dtype=float64), poly_fit_dtd_5th=array([], dtype=float64), poly_fit_range=array([], dtype=float64), ytables_nsmerger_in=array([], dtype=float64))

Bases: chem_evol.chem_evol

sfr : string

Description of the star formation, usually an instantaneous burst.

Choices :

‘input’ - read and use the sfr_input file to set the percentage

of gas that is converted into stars at each timestep.

‘schmidt’ - use an adapted Schmidt law (see Timmes95)

Default value : ‘input’

special_timesteps : integer

Number of special timesteps. This option (already activated by default) is activated when special_timesteps > 0. It uses a logarithm timestep scheme which increases the duration of timesteps throughout the simulation.

Default value : 30

dt : float

Duration of the first timestep [yr] if special_timesteps is activated. Duration of each timestep if special_timesteps is desactivated.

Default value : 1.0e6

tend : float

Total duration of the simulation [yr].

Default value : 13.0e9

imf_bdys : list

Upper and lower mass limits of the initial mass function (IMF) [Mo].

Default value : [0.1,100]

imf_yields_range : list

Initial mass of stars that contribute to stellar ejecta [Mo].

Default value : [1,30]

imf_type : string

Choices : ‘salpeter’, ‘chabrier’, ‘kroupa’, ‘alphaimf’ ‘alphaimf’ creates a custom IMF with a single power-law covering imf_bdys.

Default value : ‘kroupa’

alphaimf : float

Aplha index of the custom IMF, dN/dM = Constant * M^-alphaimf

Default value : 2.35

imf_bdys_pop3 : list

Upper and lower mass limits of the IMF of PopIII stars [Mo].

Default value : [0.1,100]

imf_yields_range_pop3 : list

Initial mass of stars that contribute to PopIII stellar ejecta [Mo]. PopIII stars ejecta taken from Heger et al. (2010)

Default value : [10,30]

iniZ : float

Initial metallicity of the gas in mass fraction (e.g. Solar Z = 0.02).

Choices : 0.0, 0.0001, 0.001, 0.006, 0.01, 0.02

(-1.0 to use non-default yield tables)

Default value : 0.0

Z_trans : float

Variable used when interpolating stellar yields as a function of Z. Transition Z below which PopIII yields are used, and above which default yields are used.

Default value : -1 (not active)

mgal : float

Initial mass of gas in the simulation [Mo].

Default value : 1.6e11

sn1a_on : boolean

True or False to include or exclude the contribution of SNe Ia.

Default value : True

sn1a_rate : string

SN Ia delay-time distribution function used to calculate the SN Ia rate.

Choices :

‘power_law’ - custom power law, set parameter with beta_pow (similar to Maoz & Mannucci 2012)

‘gauss’ - gaussian DTD, set parameter with gauss_dtd

‘exp’ - exponential DTD, set parameter with exp_dtd

‘maoz’ - specific power law from Maoz & Mannucci (2012)

Default value : ‘power_law’

sn1a_energy : float

Energy ejected by single SNIa event. Units in erg.

Default value : 1e51

ns_merger_on : boolean

True or False to include or exclude the contribution of neutron star mergers.

Default value: True

beta_pow : float

Slope of the power law for custom SN Ia rate, R = Constant * t^-beta_pow.

Default value : -1.0

gauss_dtd : list

Contains parameter for the gaussian DTD: first the characteristic time [yrs] (gaussian center) and then the width of the distribution [yrs].

Default value : [3.3e9,6.6e8]

exp_dtd : float

Characteristic delay time [yrs] for the e-folding DTD.

nb_1a_per_m : float

Number of SNe Ia per stellar mass formed in a simple stellar population.

Default value : 1.0e-03

direct_norm_1a : float

Normalization coefficient for SNIa rate integral.

Default: deactived but replaces the usage of teh nb_1a_per_m when its value is larger than zero.

transitionmass : float

Initial mass which marks the transition from AGB to massive stars [Mo].

Default value : 8.0

exclude_masses : list

Contains initial masses in yield tables to be excluded from the simulation;

Default value : []

table : string

Path pointing toward the stellar yield tables for massive and AGB stars.

Default value : ‘yield_tables/isotope_yield_table_MESA_only_fryer12_delay.txt’ (NuGrid)

sn1a_table : string

Path pointing toward the stellar yield table for SNe Ia.

Default value : ‘yield_tables/sn1a_t86.txt’ (Tielemann et al. 1986)

nsmerger_table : string

Path pointing toward the r-process yield tables for neutron star mergers

Default value : ‘yield_tables/r_process_rosswog_2014.txt’ (Rosswog et al. 2013)

iniabu_table : string

Path pointing toward the table of initial abuncances in mass fraction.

Default value : ‘yield_tables/iniabu/iniab2.0E-02GN93.ppn’

yield_interp : string

if ‘None’ : no yield interpolation, no interpolation of total ejecta

if ‘lin’ - Simple linear yield interpolation.

if ‘wiersma’ - Interpolation method which makes use of net yields as used e.g. in Wiersma+ (2009); Does not require net yields.

if netyields_on is true than makes use of given net yields

else calculates net yields from given X0 in yield table.

Default : ‘lin’

netyields_on : boolean

if true assumes that yields (input from table parameter) are net yields.

Default : false.

total_ejecta_interp : boolean

if true then interpolates total ejecta given in yield tables

over initial mass range.

Default : True

stellar_param_on : boolean

if true reads in additional stellar parameter given in table stellar_param_table.

Default : true in sygma and false in omega

stellar_param_table: string

Path pointoing toward the table hosting the evolution of stellar parameter derived from stellar evolution calculations.

Default table : ‘yield_tables/isotope_yield_table_MESA_only_param.txt’

iolevel : int

Specifies the amount of output for testing purposes (up to 3).

Default value : 0

poly_fit_dtd : list

Array of polynomial coefficients of a customized delay-time distribution function for SNe Ia. The polynome can be of any order. Example : [0.2, 0.3, 0.1] for rate_snIa(t) = 0.2*t**2 + 0.3*t + 0.1 Note : Must be used with the poly_fit_range parameter (see below)

Default value : np.array([]) –> Desactivated

poly_fit_range : list –> [t_min,t_max]

Time range where the customized delay-time distribution function for SNe Ia will be applied for a simple stellar population.

Default value : np.array([]) –> Desactivated

mass_sampled : list

Stellar masses that are sampled to eject yields in a stellar population. Warning : The use of this parameter bypasses the IMF calculation and do not ensure a correlation with the star formation rate. Each sampled mass will eject the exact amount of mass give in the stellar yields.

Default value : np.array([]) –> Desactivated

scale_cor : 2D list

Determine the fraction of yields ejected for any given stellar mass bin. Example : [ [1.0,8], [0.5,100] ] means that stars with initial mass between 0 and 8 Msu will eject 100% of their yields, and stars with initial mass between 8 and 100 will eject 50% of their yields. There is no limit for the number of [%,M_upper_limit] arrays used. Default value : np.array([]) –> Desactivated

Methods

plot_iso_ratio(fig=18, source='all', marker='', shape='', color='', label='', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, return_x_y=False, xaxis='age', yaxis='C-12/C-13', markevery=500, solar_ab='yield_tables/iniabu/iniab2.0E-02GN93.ppn', solar_iso='solar_normalization/Asplund_et_al_2009_iso.txt')

Plots ratios of isotopes.

Parameters:

yaxis: string

Ratio of isotopes, e.g. C-12/C-13

Examples

>>> s.plot_iso_ratio(yaxis='C-12/C-13')         

plot_mass(fig=0, specie='C', source='all', norm='no', label='', shape='', marker='', color='', markevery=20, multiplot=False, return_x_y=False, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, linewidth=2)

mass evolution (in Msun) of an element or isotope vs time. Note: Used in WENDI.

Parameters:

specie : string

1. isotope or element name, in the form ‘C’ or ‘C-12’
2. ratio of element or isotope, e.g. ‘C/O’, ‘C-12/O-12’

source : string

Specifies if yields come from all sources (‘all’), including AGB+SN1a, massive stars. Or from distinctive sources: only agb stars (‘agb’), only SN1a (‘SN1a’), or only massive stars (‘massive’)

norm : string

if ‘no’, no normalization If ‘current’, normalize to current total amount of specie

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

Examples

>>> s.plot_mass(specie='C')

plot_mass_range_contributions(fig=7, specie='C', prodfac=False, rebin=1, time=-1, label='', shape='-', marker='o', color='r', markevery=20, extralabel=False, log=False, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots yield contribution (Msun) of a certain mass range versus initial mass. Each stellar ejecta in one mass range is represented by the same yields, yields from certain stellar simulation. Be aware that a larger mass range means also a larger amount of yield for that range. Note: Used in WENDI.

Parameters:

specie : string

Element or isotope name in the form ‘C’ or ‘C-12’

prodfac : boolean

if true, calculate stellar production factor for each mass range. It is the final stellar yield divided by the initial (IMF-weighted) total mass (ISM+stars) in that region.

rebin : change the bin size to uniform mass intervals of size ‘rebin’

default 0, bin size is defined by ranges of (stellar) yield inputs

log : boolean

if true, use log yaxis

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

Examples

>>> s.plot_mass_range_contribution(element='C')

plot_mass_ratio(fig=0, species_ratio='C/N', source='all', norm=False, label='', shape='', marker='', color='', markevery=20, multiplot=False, return_x_y=False, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, logy=True)

Mass ratio of two species indicated by species_ratio over time. Choice can either be elemental ratio or isotopic ratios. Masses of species are in solar masses. Note: Similar to plot_mass but with ratios of masses.

Parameters:

specie : string

ratio of element or isotope, e.g. ‘C/O’, ‘C-12/O-12’

source : string

Specifies if yields come from all sources (‘all’), including AGB+SN1a, massive stars. Or from distinctive sources: only agb stars (‘agb’), only SN1a (‘SN1a’), or only massive stars (‘massive’)

norm : boolean

If True, normalize to current total ISM mass

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

logy : bool

if yes, choose yaxis in log scale

Examples

>>> s.plot_mass_ratio('C-12')

plot_massfrac(fig=2, xaxis='age', yaxis='O-16', source='all', norm='no', label='', shape='', marker='', color='', markevery=20, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots mass fraction of isotope or element vs either time or other isotope or element.

Parameters:

xaxis : string

either ‘age’ for time or isotope name, in the form e.g. ‘C-12’

yaxis : string

isotope name, in the same form as for xaxis

source : string

Specifies if yields come from all sources (‘all’), including AGB+SN1a, massive stars. Or from distinctive sources: only agb stars (‘agb’), only SN1a (‘SN1a’), or only massive stars (‘massive’)

norm : string

if ‘no’, no normalization of mass fraction if ‘ini’, normalization ot initial abundance

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

Examples

>>> s.plot_massfrac('age','C-12')

plot_metallicity(source='all', label='', marker='o', color='r', shape='-', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots the metal fraction defined as the sum of all isotopes except H1, H2, H3, He3, He4, Li6, Li7.

Parameters:

source : string

Specifies if yields come from

all sources (‘all’), including AGB+SN1a, massive stars. Or from

distinctive sources:

only agb stars (‘agb’),

only SN1a (‘SN1a’)

only massive stars (‘massive’)

Examples

>>> s.plot_metallicity(source='all')

plot_net_yields(fig=91, species='[C-12/Fe-56]', netyields_iniabu='yield_tables/iniabu/iniab_solar_Wiersma.ppn')

Plots net yields as calculated in the code when using netyields_on=True.

To be used only with net yield input.

Parameters:

species : string

Isotope ratio in spectroscopic notation.

Examples

>>> s.plot_net_yields(species='[C-12/Fe-56]')

plot_sn_distr(fig=5, rate=True, rate_only='', xaxis='time', fraction=False, label1='SNIa', label2='SN2', shape1=':', shape2='--', marker1='o', marker2='s', color1='k', color2='b', markevery=20, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots the SN1a distribution:

The evolution of the number of SN1a and SN2

Parameters:

rate : boolean

if true, calculate rate [1/century] else calculate numbers

fraction ; boolean

if true, ignorate rate and calculate number fraction of SNIa per WD

rate_only : string

if empty string, plot both rates (default)

if ‘sn1a’, plot only SN1a rate

if ‘sn2’, plot only SN2 rate

xaxis: string

if ‘time’ : time evolution if ‘redshift’: experimental! use with caution; redshift evolution

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

Examples

>>> s.plot_sn_distr()

plot_spectro(fig=3, xaxis='age', yaxis='[Fe/H]', source='all', label='', shape='-', marker='o', color='k', markevery=100, show_data=False, show_sculptor=False, show_legend=True, return_x_y=False, sub_plot=False, linewidth=3, sub=1, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, solar_ab='')

Plots elements in spectroscopic notation. Note: Used in WENDI.

Parameters:

xaxis : string

Spectroscopic notation of elements e.g. [Fe/H] if ‘age’: time evolution in years

yaxis : string

Elements in spectroscopic notation, e.g. [C/Fe]

source : string

If yields come from all sources use ‘all’ (include AGB+SN1a, massive stars.)

If yields come from distinctive source: only agb stars use ‘agb’, only SN1a (‘SN1a’), or only massive stars (‘massive’)

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

Examples

>>> plt.plot_spectro('[Fe/H]','[C/Fe]')

plot_star_formation_rate(fig=6, fraction=True, source='all', marker='', shape='', color='', label='', abs_unit=True, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots the star formation rate over time. Shows fraction of ISM mass which transforms into stars.

Parameters:

fraction : boolean

if true: fraction of ISM which transforms into stars; else: mass of ISM which goes into stars

source : string

either ‘all’ for total star formation rate; ‘agb’ for AGB and ‘massive’ for massive stars

marker : string

marker type

shape : string

line shape type

fig: figure id

Examples

>>> s.star_formation_rate()

plot_stellar_param(fig=8, quantity='Ekindot_wind', label='', marker='o', color='r', shape='-', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, markevery=1)

Plots the evolution of stellar parameter as provided as input in stellar parameter table (stellar_param_table variable).

Parameters:

quantity: string

Name of stellar parameter of interest. Check for available parameter via <sygma instance>.stellar_param_attrs

Examples

>>> s.plot_stellar_param(quantity='Ekin_wind')

plot_table_param(fig=8, ax='', xaxis='mini', quantity='Lifetime', iniZ=0.02, masses=[], label='', marker='o', color='r', shape='-', table='yield_tables/isotope_yield_table.txt', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots the yield table quantities such as lifetimes versus initial mass as given in yield input tables.

Parameters:

xaxis : string

if ‘mini’: use initial mass if ‘time’: use lifetime

iniZ : float

Metallicity of interest

masses: list

List of initial masses to be plotted

table: string

Yield table

Examples

>>> s.plot_table_param(quantity='Lifetiem')

plot_table_remnant(fig=8, xaxis='mini', iniZ=0.02, masses=[], label='', marker='o', color='r', shape='-', table='yield_tables/isotope_yield_table.txt', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots the remnant masses versus initial mass given in yield tables.

Parameters:

xaxis : string

if ‘mini’: use initial mass; if of the form [specie1/specie2] use spec. notation of

yaxis : string

iniZ : float

Metallicity to choose.

Examples

>>> s.plot_table_remnant(iniZ=0.02)

plot_table_yield(fig=8, xaxis='mini', yaxis='C-12', iniZ=0.0001, netyields=False, masses=[], label='', marker='o', color='r', shape='-', table='yield_tables/isotope_yield_table.txt', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, solar_ab='', netyields_iniabu='')

Plots the yields of the yield input grid versus initial mass or Z or [Fe/H]. Yield can be plotted in solar masses or in spectroscopic notation.

Parameters:

xaxis : string

if ‘mini’: use initial mass; if of the form [specie1/specie2] use spec. notation

yaxis : string

specifies isotopes or elements with ‘C-12’ or ‘C’: plot yield of isotope; if chosen spectros: use form [specie3/specie4]

iniZ : float

specifies the metallicity to be plotted

masses : list

if empty plot all available masses for metallicity iniZ; else choose only masses in list masses

netyields : bool

if true assume net yields in table and add corresponding initial contribution to get total yields

table : string

table to plot data from; default sygma input table

Examples

>>> s.plot_iso_ratio(yaxis='C-12')

plot_table_yield_mass(fig=8, xaxis='mini', yaxis='C-12', iniZ=0.0001, netyields=False, masses=[], label='', marker='o', color='r', shape='-', table='yield_tables/isotope_yield_table.txt', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots yields for isotopes given in yield tables.

Parameters:

xaxis : string

if ‘mini’ use initial mass on x axis

yaxis : string

isotope to plot.

Examples

>>> s.plot_iso_ratio(yaxis='C-12')

plot_totmasses(fig=4, mass='gas', source='all', norm='no', label='', shape='', marker='', color='', markevery=20, log=True, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots either gas or star mass as fraction of total mass vs time. Note: Used in WENDI.

Parameters:

mass : string

either ‘gas’ for ISM gas mass or ‘stars’ for gas locked away in stars (total gas - ISM gas)

norm : string

normalization, either ‘no’ for no normalization (total gas mass in solar masses),

for normalization to the initial gas mass (mgal) with ‘ini’,

for normalization to the current total gas mass ‘current’. The latter case makes sense when comparing different sources (see below)

source : string

specifies if yields come from all sources (‘all’), including AGB+SN1a, massive stars. Or from distinctive sources: only agb stars (‘agb’), only SN1a (‘sn1a’), or only massive stars (‘massive’)

log : boolean

if true plot logarithmic y axis

label : string

figure label

marker : string

figure marker

shape : string

line style

color : string

color of line

fig : string,float

to name the plot figure

Examples

>>> s.plot_totmasses()

plot_yield_mtot(fig=8, plot_imf_mass_ranges=True, fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)

Plots total mass ejected by stars (!). To distinguish between the total mass of yields from the table and fitted total mass

Parameters:

plot_imf_mass_ranges : boolean

If true plots the initial mass ranges for which yields are consider.

Examples

>>> s.plot_yield_mtot()

write_evol_table(elements=['H'], isotopes=['H-1'], table_name='gce_table.txt', path='', interact=False)

Writes out evolution of the SSP accummulated ejecta in fraction of total mass of the SSP in the following format (each timestep in a line):

&Age &H-1 &H-2 ....

&0.000E+00 &1.000E+00 &7.600E+08 & ...

&1.000E+07 &1.000E+00 &7.600E+08 & ...

This method has a notebook and normal version. If you are using a python notebook the function will open a link to a page containing the table.

Parameters:

table_name : string,optional

Name of table. If you use a notebook version, setting a name is not necessary.

elements : array

Containing the elements with the name scheme ‘H’,’C’

isotopes : array

If elements list empty, ignore elements input and use isotopes input; Containing the isotopes with the name scheme ‘H-1’, ‘C-12’

interact: bool

If true, saves file in current directory (notebook dir) and creates HTML link useful in ipython notebook environment

Examples

>>> s.write_evol_table(elements=['H','C','O'],table_name='testoutput.txt')

write_stellar_param_table(table_name='gce_stellar_param_table.txt', path='evol_tables', interact=False)

Writes out evolution of stellar parameter such as luminosity and kinetic energy. Stellar parameter quantities are available via <sygma instance>.stellar_param_attrs.

Table structure:

&Age &Quantity1 &Quantity2 ...

&0.000E+00 &0.000E+00 &0.000E+00

&0.000E+00 &0.000E+00 &0.000E+00

Parameters:

table_name : string,optional

Name of table. If you use a notebook version, setting a name is not necessary.

path : string

directory where to save table.

interact: bool

If true, saves file in current directory (notebook dir) and creates HTML link useful in ipython notebook environment

Examples

>>> s.write_evol_table(table_name='testoutput.txt')