utils

class cosmic.utils.ConfigParser(defaults=None, dict_type=<class 'dict'>, allow_no_value=False, *, delimiters=('=', ':'), comment_prefixes=('#', ';'), inline_comment_prefixes=None, strict=True, empty_lines_in_values=True, default_section='DEFAULT', interpolation=<object object>, converters=<object object>)

Bases: RawConfigParser

ConfigParser implementing interpolation.

_DEFAULT_INTERPOLATION = <configparser.BasicInterpolation object>

__abstractmethods__ = frozenset({})

__doc__ = 'ConfigParser implementing interpolation.'

__module__ = 'configparser'

_abc_impl = <_abc._abc_data object>

_read_defaults(defaults)

Reads the defaults passed in the initializer, implicitly converting values to strings like the rest of the API.

Does not perform interpolation for backwards compatibility.

add_section(section)

Create a new section in the configuration. Extends RawConfigParser.add_section by validating if the section name is a string.

set(section, option, value=None)

Set an option. Extends RawConfigParser.set by validating type and interpolation syntax on the value.

class cosmic.utils.VariableKey(item)

Bases: object

A dictionary key which is a variable. @ivar item: The variable AST object.

__dict__ = mappingproxy({'__module__': 'cosmic.utils', '__doc__': '\n    A dictionary key which is a variable.\n    @ivar item: The variable AST object.\n    ', '__init__': <function VariableKey.__init__>, '__eq__': <function VariableKey.__eq__>, '__hash__': <function VariableKey.__hash__>, '__dict__': <attribute '__dict__' of 'VariableKey' objects>, '__weakref__': <attribute '__weakref__' of 'VariableKey' objects>, '__annotations__': {}})

__doc__ = '\n    A dictionary key which is a variable.\n    @ivar item: The variable AST object.\n    '

__eq__(compare)

Return self==value.

__hash__()

Return hash(self).

__init__(item)

__module__ = 'cosmic.utils'

__weakref__

list of weak references to the object (if defined)

cosmic.utils.a_from_p(p, m1, m2)

Computes the separation from orbital period with KEPLER III

Parameters:

pfloat/array

orbital period [day]

m1float/array

primary mass [msun]

m2float/array

secondary mass [msun]

Returns:

sepfloat/array

separation [rsun]

cosmic.utils.calc_Roche_radius(M1, M2, A)

Get Roche lobe radius (Eggleton 1983)

Parameters:

M1float

Primary mass [any unit]

M2float

Secondary mass [any unit]

Afloat

Orbital separation [any unit]

Returns:

Roche radiusfloat

in units of input ‘A’

cosmic.utils.check_initial_conditions(full_initial_binary_table)

Checks initial conditions and reports warnings

Only warning provided right now is if star begins in Roche lobe overflow

cosmic.utils.conv_select(bcm_save, bpp_save, final_kstar_1, final_kstar_2, method, conv_lims)

Select bcm data for special convergence cases

Parameters:

bcm_savepandas.DataFrame

bcm dataframe containing all saved bcm data

bpp_savepandas.DataFrame

bpp dataframe containing all saved bpp data

final_kstar_1list

contains list of final primary kstars specified by user

final_kstar_2list

contains list of final primary kstars specified by user

methodstr

stage in binary evolution to check convergence for only one method may be supplied and they are specified in the inifile

conv_limsdict

dictionary where keys are convergence params and the values are lists containing a [lo, hi] value to filter the convergence param between any non-specified convergence params will not be filtered

Returns:

conv_savepandas.DataFrame

filtered dataframe containing binaries that fulfill user-specified convergence criteria

cosmic.utils.convert_kstar_evol_type(bpp)

Provides way to convert integer values to their string counterpart

The underlying fortran code relies on integers to indicate things like the evoltuionary stage of the star as well as key moments in its evolutionary track. If you pass the data frame returned from running

`Evolve.evolve`

you can convert the columns with these integer proxies to their true astrophysical meaning.

cosmic.utils.dat_transform(dat, dat_list)

Transform a data set to have limits between zero and one using param_transform, then transform to log space

Parameters:

dat ” DataFrame

Data to transform to eventually perform KDE

dat_listlist

List of DataFrame columns to include in transformation

Returns:

dat_transarray

Transformed data for columns in dat_list

cosmic.utils.dat_un_transform(dat_sample, dat_set, dat_list)

Un-transform data that was transformed in dat_transform

Parameters:

dat_samplearray

Data sampled from kde generated with transformed data

dat_setDataFrame

Un-transformed data (same as dat in dat_transform)

dat_listlist

List of DataFrame columns to include in transformation

Returns:

datarray

Array of data sampled from kde that is transformed back to bounds of the un-transformed data set the kde is generated from

cosmic.utils.error_check(BSEDict, filters=None, convergence=None, sampling=None)

Checks that values in BSEDict, filters, and convergence are viable

cosmic.utils.filter_bin_state(bcm, bpp, method, kstar1_range, kstar2_range)

Filter the output of bpp and bcm, where the kstar ranges have already been selected by the conv_select module

Parameters:

bcmpandas.DataFrame

bcm dataframe

bpppandas.DataFrame

bpp dataframe

methoddict,

one or more methods by which to filter the bpp or bcm table, e.g. {'binary_state' : [0,1]}; This means you do not want to select the final state of the binaries in the bcm array

kstar1_rangelist

list containing all kstar1 values to retain

kstar2_rangelist

list containing all kstar2 values to retain

Returns:

bcmpandas.DataFrame

filtered bcm dataframe

cosmic.utils.get_FeH_from_Z(Z, Z_sun=0.02)

Converts from Z to FeH under the assumption that all stars have the same abundance as the sun

Parameters:

Zarray

metallicities to convert to Fe/H

Z_sunfloat

solar metallicity

Returns:

FeHarray

Fe/H corresponding to metallicities

cosmic.utils.get_Z_from_FeH(FeH, Z_sun=0.02)

Converts from FeH to Z under the assumption that all stars have the same abundance as the sun

Parameters:

FeHarray

Fe/H values to convert

Z_sunfloat

solar metallicity

Returns:

Zarray

metallicities corresponding to Fe/H

cosmic.utils.get_binfrac_of_Z(Z)

Calculates the theoretical binary fraction as a function of metallicity. Following Moe+2019

Parameters:

Zarray

metallicity Z values

Returns:

binfracarray

binary fraction values

cosmic.utils.get_met_dep_binfrac(met)

Returns a population-wide binary fraction consistent with Moe+19 based on the supplied metallicity

Parameters:

metfloat

metallicity of the population

Returns:

binfracfloat

binary fraction of the population based on metallicity

cosmic.utils.get_porb_norm(Z, close_logP=4.0, wide_logP=6.0, binfrac_tot_solar=0.66, Z_sun=0.02)

Returns normalization constants to produce log normals consistent with Fig 19 of Moe+19 for the orbital period distribution

Parameters:

Zarray

metallicity values

close_logPfloat

divding line beween close and intermediate orbits

wide_logPfloat

dividing line between intermediate and wide orbits

binfrac_totfloat

integrated total binary fraction at solar metallicity

Returns:

norm_widefloat

normalization factor for kde for wide binaries

norm_closefloat

normalization factor for kde for wide binaries

cosmic.utils.idl_tabulate(x, f, p=5)

Function that replicates the IDL int_tabulated function which performs a p-point integration on a tabulated set of data

Parameters:

xarray

tabulated x-value data

farray

tabulated f-value data, same size as x

pint

number of chunks to divide tabulated data into Default: 5

Returns:

retfloat

Integration result

cosmic.utils.knuth_bw_selector(dat_list)

Selects the kde bandwidth using Knuth’s rule implemented in Astropy If Knuth’s rule raises error, Scott’s rule is used

Parameters:

dat_listlist

List of data arrays that will be used to generate a kde

Returns:

bw_minfloat

Minimum of bandwidths for all of the data arrays in dat_list

cosmic.utils.mass_min_max_select(kstar_1, kstar_2, **kwargs)

Select a minimum and maximum mass to filter out binaries in the initial parameter sample to reduce the number of unneccessary binaries evolved in BSE

Parameters:

kstar_1int, list

BSE stellar type for the primary or minimum and maximum stellar types for the primary

kstar_2int, list

BSE stellar type for the secondary or minimum and maximum stellar types for the secondary

Returns:

min_mass[0]float

minimum primary mass for initial sample

max_mass[0]float

maximum primary mass for initial sample

min_mass[1]float

minimum secondary mass for initial sample

max_mass[1]float

maximum secondary mass for initial sample

cosmic.utils.p_from_a(sep, m1, m2)

Computes separation from orbital period with kepler III

Parameters:

sepfloat/array

separation [rsun]

m1float/array

primary mass [msun]

m2float/array

secondary mass [msun]

Returns:

pfloat/array

orbital period [day]

cosmic.utils.param_transform(dat)

Transforms a data set to limits between zero and one Leaves some wiggle room on the edges of the data set

Parameters:

datarray

array of data to transform between 0 and 1

Returns:

datTransformedarray

array of data with limits between 0 and 1

cosmic.utils.parse_inifile(inifile)

Provides a method for parsing the inifile and returning dicts of each section

cosmic.utils.pop_write(dat_store, log_file, mass_list, number_list, bcm, bpp, initC, conv, kick_info, bin_state_nums, match, idx)

Writes all the good stuff that you want to save from runFixedPop in a

single function

Parameters:

dat_storepandas HDFStore

H5 file to write to

log_filefile write

log file to write to

mass_listlist

list containing the mass of the singles, mass of the binaries, and mass of the stars

n_listlist

list containing the number of singles, number of binaries, and number of stars

bcmpandas.DataFrame

bcm array to write

bpppandas.DataFrame

bpp array to write

initCondpandas.DataFrame

initCond array to write

convpandas.DataFrame

conv array to write

kick_infopandas.DataFrame

kick_info array to write

bin_state_numslist

contains the count of binstates 0,1,2

matchpandas.DataFrame

contains the match values for each conv_param

idxint

contains the index of the bcm so we can pick up where we left off if runFixedPop hits a wall time

Returns:

Nothing!

cosmic.utils.rndm(a, b, g, size)

Power-law generator for pdf(x)propto x^{g} for a<=x<=b

Parameters:

afloat

Minimum of range for power law

bfloat

Maximum of range for power law

gfloat

Index for power law

sizeint

Number of data points to draw

Returns:

powerarray

Array of data sampled from power law distribution with params fixed by inputs

cosmic.utils.zcnsts(z)

Calculate constants based on the metallicty * zpars: 1; M below which hook doesn’t appear on MS, Mhook. * 2; M above which He ignition occurs non-degenerately, Mhef. * 3; M above which He ignition occurs on the HG, Mfgb. * 4; M below which C/O ignition doesn’t occur, Mup. * 5; M above which C ignites in the centre, Mec. * 6; value of log D for M<= zpars[2] * 7; value of x for Rgb propto M^(-x) * 8; value of x for tMS = numpy.maximum(tHOOK,x*tBGB) * 9; constant for McHeIf when computing Mc,BGB, mchefl. * 10; constant for McHeIf when computing Mc,HeI, mchefl. * 11; hydrogen abundance. * 12; helium abundance. * 13; constant x in rnumpy.minimum = rgb*x**y used by LM CHeB. * 14; z**0.4 to be used for WD L formula.