OMEGA Module¶
GCE OMEGA (One-zone Model for the Evolution of Galaxies) module
Functionality¶
This tool allows one to simulate the chemical evolution of single-zone galaxies. Having the star formation history as one of the input parameters, OMEGA can target local galaxies by using observational data found in the literature.
Made by¶
FEB2015: C. Ritter, B. Cote
MAY2015: B. Cote
The code inherits the chem_evol class, which contains common functions shared by SYGMA and OMEGA. The code in chem_evol has been developed 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 MAR2015: B. Cote
v0.6 OCT2016: B. Cote
Usage¶
Import the module:
>>> import omega as o
Get help:
>>> help o
Get more information:
>>> o.omega?
Create a custom galaxy (closed box):
>>> o1 = o.omega(cte_sfr=1.0, mgal=1.5e10)
Simulate a known galaxy (open box):
>>> o2 = o.omega(galaxy='sculptor', in_out_control=True, mgal=1e6, mass_loading=8, in_out_ratio=1.5)
Analysis functions: See the Sphinx documentation
-
class
omega.omega(galaxy='none', in_out_control=False, SF_law=False, DM_evolution=False, Z_trans=1e-20, f_dyn=0.1, sfe=0.1, outflow_rate=-1.0, inflow_rate=-1.0, rand_sfh=0.0, cte_sfr=1.0, m_DM_0=100000000000.0, mass_loading=1.0, t_star=-1.0, sfh_file='none', in_out_ratio=1.0, stellar_mass_0=-1.0, z_dependent=True, exp_ml=2.0, nsmerger_bdys=[8, 100], imf_type='kroupa', alphaimf=2.35, imf_bdys=[0.1, 100], sn1a_rate='power_law', iniZ=0.0, dt=1000000.0, special_timesteps=30, tend=13000000000.0, mgal=10000000000.0, transitionmass=8, iolevel=0, ini_alpha=True, nb_nsm_per_m=-1.0, t_nsm_coal=-1.0, table='yield_tables/isotope_yield_table_MESA_only_fryer12_delay.txt', hardsetZ=-1, sn1a_on=True, nsm_dtd_power=[], sn1a_table='yield_tables/sn1a_t86.txt', ns_merger_on=True, f_binary=1.0, f_merger=0.0008, t_merger_max=10000000000.0, m_ej_nsm=0.025, nsmerger_table='yield_tables/r_process_rosswog_2014.txt', bhns_merger_on=False, m_ej_bhnsm=0.025, bhnsmerger_table='yield_tables/r_process_rosswog_2014.txt', iniabu_table='', extra_source_on=False, 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, f_arfo=1, t_merge=-1.0, imf_yields_range=[1, 30], exclude_masses=[], netyields_on=False, wiersmamod=False, skip_zero=False, redshift_f=0.0, print_off=False, long_range_ref=False, f_s_enhance=1.0, m_gas_f=-1.0, cl_SF_law=False, external_control=False, calc_SSP_ej=False, tau_ferrini=False, input_yields=False, popIII_on=True, t_sf_z_dep=1.0, m_crit_on=False, norm_crit_m=8000000000.0, mass_frac_SSP=0.5, sfh_array_norm=-1.0, imf_rnd_sampling=False, out_follows_E_rate=False, r_gas_star=-1.0, cte_m_gas=-1.0, t_dtd_poly_split=-1.0, stellar_param_on=False, bhnsmerger_dtd_array=array([], dtype=float64), DM_array=array([], dtype=float64), nsmerger_dtd_array=array([], dtype=float64), sfh_array=array([], dtype=float64), ism_ini=array([], dtype=float64), mdot_ini=array([], dtype=float64), mdot_ini_t=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), ytables_nsmerger_in=array([], dtype=float64), dt_in=array([], dtype=float64), dt_split_info=array([], dtype=float64), ej_massive=array([], dtype=float64), ej_agb=array([], dtype=float64), ej_sn1a=array([], dtype=float64), ej_massive_coef=array([], dtype=float64), ej_agb_coef=array([], dtype=float64), ej_sn1a_coef=array([], dtype=float64), dt_ssp=array([], dtype=float64), yield_interp='lin', mass_sampled=array([], dtype=float64), scale_cor=array([], dtype=float64), mass_sampled_ssp=array([], dtype=float64), scale_cor_ssp=array([], dtype=float64), poly_fit_dtd_5th=array([], dtype=float64), poly_fit_range=array([], dtype=float64), m_tot_ISM_t_in=array([], dtype=float64))[source]¶ Bases:
chem_evol.chem_evolImportant : By default, a closed box model is always assumed.
- galaxy : string
Name of the target galaxy. By using a known galaxy, the code automatically selects the corresponding star formation history, stellar mass, and total mass (when available). By using ‘none’, the user has perfect control of these three last parameters.
Choices : ‘milky_way’, ‘milky_way_cte’, ‘sculptor’, ‘carina’, ‘fornax’, ‘none’
Default value : ‘none’
Special note : The ‘milky_way_cte’ option uses the Milky Way’s characteristics, but with a constant star formation history.
- cte_sfr : float
Constant star formation history in [Mo/yr].
Default value : 1.0
- rand_sfh : float
Maximum possible ratio between the maximum and the minimum values of a star formation history that is randomly generated.
Default value : 0.0 (deactivated)
Special note : A value greater than zero automatically generates a random star formation history, which pypasses the use of the cte_sfr parameter.
- sfh_file : string
Path to a file containing an input star formation history. The first and second columns must be the age of the galaxy in [yr] and the star formation rate in [Mo/yr].
Default value : ‘none’ (deactivated)
Special note : When a path is specified, it by passes the cte_sfr and the and_sfh parameters.
- stellar_mass_0 : float
Current stellar mass of the galaxy, in [Mo], at the end of the simulation.
Default value : -1.0 (you need to specify a value with unknown galaxies)
- in_out_control : boolean
The in_out_control implementation enables control of the outflow and the inflow rates independently by using constant values (see outflow_rate and inflow_rate) or by using a mass-loading factor that connects the rates to the star formation history (see mass_loading and in_out_ratio).
Default value : False (deactivated)
- mass_loading : float
Ratio between the outflow rate and the star formation rate.
Default value : 1.0
- outflow_rate : float
Constant outflow rate in [Mo/yr].
Default value : -1.0 (deactivated)
Special note : A value greater or equal to zero activates the constant utflow mode, which bypasses the use of the mass_loading parameter.
- in_out_ratio : float
Used in : in_out_control mode
Ratio between the inflow rate and the outflow rate. This parameter is used to calculate the inflow rate, not the outflow rate.
Default value : 1.0
- inflow_rate : float
Used in : in_out_control mode Constant inflow rate in [Mo/yr].
Default value : -1.0 (deactivated)
Special note : A value greater or equal to zero activates the constant inflow mode, which bypasses the use of the in_out_ratio parameter.
- SF_law : boolean
The SF_law inplementation assumes a Kennicutt-Schmidt star formation law and combines it to the known input star formation history in order to derive the mass of the gas reservoir at every timestep.
Default value : False (deactivated)
- sfe : float
Used in : SF_law and DM_evolution modes
Star formation efficiency present in the Kennicutt-Schmidt law.
Default value : 0.1
- f_dyn : float
Used in : SF_law and DM_evolution modes Scaling factor used to calculate the star formation timescale present in the Kennicutt-Schmidt law. We assume that this timescale is equal to a fraction of the dynamical timescale of the virialized system (dark and baryonic matter), t_star = f_dyn * t_dyn.
Default value : 0.1
- m_DM_0 : float
Used in : SF_law and DM_evolution modes Current dark matter halo mass of the galaxy, in [Mo], at the end of the simulations.
Default value : 1.0e+11
- t_star : float
Used in : SF_law and DM_evolution modes Star formation timescale, in [yr], used in the Kennicutt-Schmidt law. Default value = -1.0 (deactivated)
Special note : A positive value activates the use of this parameter, which bypasses the f_dyn parameter.
- DM_evolution : boolean
The DM_evolution implementation is an extension of the SF_law option. In addition to using a Kennicutt-Schmidt star formation law, it assumes an evolution in the total mass of the galaxy as function of time. With this prescription, the mass-loading factor has a mass dependency. The mass_loading parameter then only represents the final value at the end of the simulation.
Default value : False (deactivated)
- exp_ml : float
Used in : DM_evolution mode
Exponent of the mass dependency of the mass-loading factor. This last factor is proportional to M_vir**(-exp_ml/3), where M_vir is the sum of dark and baryonic matter.
Default value : 2.0
- 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
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plot_abu_distr(species, source='all', norm='', 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)[source]¶ - Plot abundance distribution at point in time normalized to solar system distribution.
Parameters: species : array
isotopes or element names, in the form [‘C’] or [‘C-12’]
time : float
Time in yrs telling when to extract abundances, e.g. birth SS 9.2Gyr
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
Choose the solar abundances, e.g. ‘Grevesse_Noels_1993’, same notation as in stellab?
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_abu_distr(species=['C-12','O-16'],time=9.2e9,norm='Asplund_et_al_2009')
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plot_abun(fig=20, age=9200000000.0, solar_norm=False, iso_on=False, list_elem=[], list_iso=[], return_x_y=False, over_plot_solar=False, solar_ab_m='yield_tables/iniabu/iniab2.0E-02GN93.ppn', f_y_annotate=0.9, marker='o', marker_s='^', shape='', shape_s='-', color='b', color_s='r', label='Prediction', label_s='solar', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, markersize=5)[source]¶ This function plots the abundance distribution in mass fraction at any given point in time or at any given metallicity.
Parameters: age : float
Time passed since the beginning of the simulation at which abundance distribution is taken. Default: Time until the formation of the pre-solar cloud.
solar_norm: boolean
If True, the abundances will be divide by the solar abundances. If False, there is no normalization. Default: False
iso_on : boolean
If True, the abundances will be in terms of isotopes. If False, the abundances will be in terms of elements.
list_elem : array of strings
Contain the list of elements included in the abundances distribution. Default: [], all elements will be included. Example: list_elem=[‘H’,’He’,’C’,’N’,’O’,’Fe’]
list_iso : array of strings
Contain the list of isotopes included in the abundances distribution. Default: [], all isotopes will be included. Example: list_iso=[‘H-1’,’C-12’,’C-13’,’N-14’,’N-15’] Note: list_iso dominates over list_elem is both are used.
return_x_y : boolean
If False, show the plot. If True, return two arrays containing the X and Y axis data, respectively. If True and iso_list=True, return a multi-D array [i][j][:] where j=0 -> list of mass numbers A for the isotopes associated with the element i, j=1 -> list of abundances
over_plot_solar : boolean
If True, plot the solar abundances distribution along with the predictions Note: This option is desactivated if solar_norm=True
solar_ab_m : string
Path of the solar normalization containing the mass fraction of each isotope Default: solar_ab_m=’yield_tables/iniabu/iniab2.0E-02GN93.ppn’
f_y_annotate : float (between 0 and 1)
Fraction of the Y axis where the name of the element will be shown Default: f_y_annotate=0.9
fig : string, float
Figure name.
marker : string
Figure marker.
marker_s : string
Marker of the solar abundance distribution.
shape : string
Line style.
shape_s : string
Line style of the solar abundance distribution.
color : string
Line color.
color_s : string
Line color of the solar abundances pattern.
label : string
Figure label.
label_s : string
Label of the solar abundance distribution.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
markersize : float
Size of the markers Default: markersize=5
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plot_dark_matter(fig=11, marker='', shape='', color='', label='Dark matter', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the dark matter halo mass of the galaxy as a function of time.
Parameters: fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_dark_matter(label='Dark Matter')
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plot_inflow_rate(fig=10, marker='', shape='', color='', label='Inflow', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the mass inflow rate as a function of time in units of [Mo/yr].
Parameters: fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_inflow_rate(label='Inflow Rate')
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plot_iso_ratio(return_x_y=False, xaxis='age', yaxis='C-12/C-13', solar_ab='yield_tables/iniabu/iniab2.0E-02GN93.ppn', solar_iso='solar_normalization/Asplund_et_al_2009_iso.txt', 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)[source]¶ This function plots the evolution of an isotopic ratio as a function of time, as a function of an abundance ratio, or as a function of another isotopic ratio. Isotopic ratios are given in the delta notation and abundances ratios are given in spectroscopic notation.
Parameters: return_x_y : boolean
If False, show the plot. If True, return two arrays containing the X and Y axis data, respectively.
xaxis : string
X axis, either ‘age’, an abundance ratio such as ‘[Fe/H]’, or an isotopic ratio such as ‘C-12/C-13’.
yaxis : string
Y axis, isotopic ratio such as ‘C-12/C-13’.
solar_ab : string
Path to the solar abundances used to normalize abundance ratios.
solar_iso : string
Path to the solar isotopes used to normalize the isotopic ratios.
fig : string, float
Figure name.
source : string
Specificies if yields come from all sources (‘all’) or from distinctive sources: only AGB stars (‘agb’), only SN Ia (‘sn1a’), or only massive stars (‘massive’)
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_iso_ratio(xaxis='[Fe/H]', yaxis='C-12/C-13')
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plot_mass(fig=0, specie='C', 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, show_legend=True)[source]¶ - mass evolution (in Msun) of an element or isotope vs time.
Parameters: specie : string
isotope or element name, in the form ‘C’ or ‘C-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
show_legend : boolean
Default True. Show or not the legend
Examples
>>> s.plot('C-12')
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plot_mass_loading(fig=8, marker='', shape='', color='', label='Mass-loading', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the mass-loading factor, which is the ratio between the mass outflow rate and the star formation rate, as a function of time.
Parameters: fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_mass_loading(label='Mass-Loading Factor')
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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)[source]¶ 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')
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plot_mdf(fig=19, return_x_y=False, axis_mdf='[Fe/H]', dx=0.05, solar_ab='yield_tables/iniabu/iniab2.0E-02GN93.ppn', sigma_gauss=0.0, nb_sigma=3.0, marker='', shape='', norm=True, color='', label='', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the stellar metallicity distribution function (MDF), or the distribution function of any other abundance ratio.
Parameters: return_x_y : boolean
If False, show the plot. If True, return two arrays containing the X and Y axis data, respectively.
axis_mdf : string
Abundance ratio for the distribution such as ‘[Fe/H]’ or ‘[Mg/H]’.
dx : float
Bin resolution of the distribution.
solar_ab : string
Path to the solar abundances used to normalize abundance ratios.
sigma_gauss : float
Each point in the MDF can be associated with a gaussian. This implies that in reality, the metallicity should have a certain dispersion when stars form at each timestep (instead of using only a single average value). The sigma_guass parameter sets the sigma value eac gaussian function.
nb_sigma : float
When sigma_gauss is greater than zero, nb_sigma is the number of sigma by which the X axis range is expanded.
norm : boolean
Normalize the MDF is True Default : True
fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_mdf(axis_mdf='[Fe/H]', sigma_gauss=0.2)
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plot_outflow_rate(fig=9, marker='', shape='', color='', label='Outflow', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the mass outflow rate as a function of time in units of [Mo/yr].
Parameters: fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_outflow_rate(label='Outflow Rate')
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plot_redshift(fig=16, marker='', shape='', color='', label='Redshift', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the redshift a function of time.
Parameters: fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_redshift(label='Redshift')
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plot_sf_timescale(fig=15, marker='', shape='', color='', label='', fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14)[source]¶ This function plots the star formation timescale as a function of time in units of [yr].
Parameters: fig : string, float
Figure name.
marker : string
Figure marker.
shape : string
Line style.
color : string
Line color.
label : string
Figure label.
fsize : 2D float array
Figure dimension/size.
fontsize : integer
Font size of the numbers on the X and Y axis.
rspace : float
Extra space on the right for the legend.
bspace : float
Extra space at the bottom for the Y axis label.
labelsize : integer
Font size of the X and Y axis labels.
legend_fontsize : integer
Font size of the legend.
Examples
>>> o1.plot_sf_timescale(label='Star Formation Timescale')
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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)[source]¶ Plots the SN1a distribution: The evolution of the number of SN1a and SN2 #Add numbers/dt numbers/year...
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()
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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, plot_data=False, fsize=[10, 4.5], fontsize=14, rspace=0.6, bspace=0.15, labelsize=15, legend_fontsize=14, only_one_iso=False, solar_ab='', sfr_thresh=0.0, m_formed_thresh=1.0, solar_norm='')[source]¶ Plots elements in spectroscopic notation:
Parameters: xaxis : string
Elements spectroscopic notation 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]')
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plot_star_formation_rate(fig=6, fraction=False, 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)[source]¶ 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()
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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)[source]¶ Plots either gas or star mass in fraction of total mass vs time.
Parameters: mass : string
either ‘gas’ for ISM gas mass or ‘stars’ for gas locked away in stars (totalgas - ISM gas)
norm : string
normalization, either ‘no’ for no normalization (total gass 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
specificies 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()