ExtendedFsps

class eazy.sps.ExtendedFsps

Bases: object

Extended functionality for the fsps.StellarPopulation object

Attributes Summary

FFT_SMOOTH
cosmology
fsps_ages	(linear) ages of the FSPS SSP age grid, Gyr
is_lognorm_sfh
izmet	Get zmet index for nearest self.zlegend value to loggzsol.
line_av_func
lognorm_center
lognorm_fburst
lognorm_logwidth
lsf_func
meta	Full metadata, including line properties
param_dict	dict version of self.params
scale_lines
scale_lyman_series
sfr10	SFR averaged over last MAXIMUM(tage, 10 Myr) from sfr_avg
sfr100	SFR averaged over maximum(tage, 100 Myr) from sfr_avg

Methods Summary

as_template(wave, flux[, label, meta])	Return a eazy.templates.Template object with metadata
continuum_to_obsframe([zred, cosmology, ...])	Compute a normalization factor to scale input FSPS model flux density units of (L_sun / Hz) or (L_sun / AA) to observed-frame unit.
fit_grism(mb[, plist, func_kwargs, verbose, ...])	Fit models to grism spectrum
fit_phot(phot_dict[, filters, flux_unit, ...])	Fit models to observed spectrum
fit_spec(wave_obs, flux_obs, err_obs[, ...])	Fit models to observed spectrum
get_full_spectrum([tage, Av, get_template, ...])	Get full spectrum with reprocessed emission lines and dust emission
light_age_band([bands, flat])	Get light-weighted age of current model
line_to_obsframe([zred, cosmology, verbose, ...])	Scale factor to convert internal line luminosities (L_sun) to observed frame
lognorm_avg_sfr([tage, dt])	Analytic average SFR for lognorm SFH
lognormal_integral([tage])	Integral of lognormal SFH up to t=tage
narrow_emission_lines([tage, emwave, ...])	Replace broad FSPS lines with specified line widths
objfun_fitgrism(theta, self, plist, mb, TEF, ...)	Objective function for fitting spectra
objfun_fitphot(theta, self, plist, flux_fnu, ...)	Objective function for fitting spectra
objfun_fitspec(theta, self, plist, wave_obs, ...)	Objective function for fitting spectra
param_floats([params])	Return a list of parameter values.
parameter_bounds(params[, limit_age])	Parameter bounds for scipy.optimize.least_squares
pset(params)	Return a subset dictionary of self.meta
redden(wave)
set_dust([Av, dust_obj_type, wg00_kwargs])	Set dust_obj attribute
set_fir_template([arrays, file, verbose, ...])	Set the far-IR template for reprocessed dust emission
set_lognormal_sfh([min_sigma, verbose])	Set lognormal tabular SFH

Attributes Documentation

FFT_SMOOTH = False

cosmology = FlatLambdaCDM(name='WMAP9', H0=<Quantity 69.32 km / (Mpc s)>, Om0=0.2865, Tcmb0=<Quantity 2.725 K>, Neff=3.04, m_nu=<Quantity [0., 0., 0.] eV>, Ob0=0.04628)

fsps_ages

(linear) ages of the FSPS SSP age grid, Gyr

is_lognorm_sfh = False

izmet

Get zmet index for nearest self.zlegend value to loggzsol.

line_av_func = None

lognorm_center = 0.0

lognorm_fburst = -30

lognorm_logwidth = 0.05

lsf_func = None

meta

Full metadata, including line properties

param_dict

dict version of self.params

scale_lines = {}

scale_lyman_series = 0.1

sfr10

SFR averaged over last MAXIMUM(tage, 10 Myr) from sfr_avg

sfr100

SFR averaged over maximum(tage, 100 Myr) from sfr_avg

Methods Documentation

as_template(wave, flux, label='fsps_tau{tau:3.1f}_logz{logzsol:4.2f}_tage{tage:4.2f}_av{Av:4.2f}', meta=None)

Return a eazy.templates.Template object with metadata

continuum_to_obsframe(zred=None, cosmology=None, unit=Unit('uJy'), verbose=False, target_stellar_mass=None, target_sfr=None, target_lir=None)

Compute a normalization factor to scale input FSPS model flux density units of (L_sun / Hz) or (L_sun / AA) to observed-frame unit.

If target_stellar_mass, target_sfr, or target_lir specified, then scale the output to the desired value using the intrinsic properties. Units are linear Msun, Msun/yr, and Lsun, respectively.

fit_grism(mb, plist=['tage', 'zred'], func_kwargs={'lorentz': False}, verbose=True, lsq_kwargs={'loss': 'huber', 'max_nfev': 200, 'method': 'trf', 'verbose': True, 'x_scale': 1.0}, show=False, TEF=None, photoz_obj=None, flux_unit=Unit('erg / (Angstrom s cm2)'))

Fit models to grism spectrum

fit_phot(phot_dict, filters=None, flux_unit=Unit('uJy'), plist=['tage', 'Av', 'gas_logu', 'sigma_smooth'], func_kwargs={'lorentz': False}, verbose=True, lsq_kwargs={'loss': 'huber', 'max_nfev': 200, 'method': 'trf', 'verbose': True, 'x_scale': 1.0}, show=False, TEF=None, photoz_obj=None)

Fit models to observed spectrum

fit_spec(wave_obs, flux_obs, err_obs, mask=None, plist=['tage', 'Av', 'gas_logu', 'sigma_smooth'], func_kwargs={'lorentz': False}, verbose=True, bspl_kwargs=None, cheb_kwargs=None, lsq_kwargs={'loss': 'huber', 'max_nfev': 200, 'method': 'trf', 'verbose': True, 'x_scale': 1.0}, show=False)

Fit models to observed spectrum

get_full_spectrum(tage=1.0, Av=0.0, get_template=True, set_all_templates=False, z=None, tie_metallicity=True, **kwargs)

Get full spectrum with reprocessed emission lines and dust emission

dust_fraction: Fraction of the SED that sees the specified Av

light_age_band(bands=['v'], flat=True)

Get light-weighted age of current model

line_to_obsframe(zred=None, cosmology=None, verbose=False, unit=<Quantity 1.e-17 erg / (s cm2)>, target_stellar_mass=None, target_sfr=None, target_lir=None)

Scale factor to convert internal line luminosities (L_sun) to observed frame

If target_stellar_mass, target_sfr, or target_lir specified, then scale the output to the desired value using the intrinsic properties. Units are linear Msun, Msun/yr, and Lsun, respectively.

lognorm_avg_sfr(tage=None, dt=0.1)

Analytic average SFR for lognorm SFH

lognormal_integral(tage=0.1, **kwargs)

Integral of lognormal SFH up to t=tage

narrow_emission_lines(tage=0.1, emwave=[], line_sigma=100, oversample=5, clip_sigma=10, verbose=False, get_eqw=True, scale_lyman_series=None, scale_lines={}, force_recompute=False, use_sigma_smooth=True, lorentz=False, **kwargs)

Replace broad FSPS lines with specified line widths

tage : age in Gyr of FSPS model FSPS sigma: line width in A in FSPS models emwave : (approx) wavelength of line to replace line_sigma : line width in km/s of new line oversample : factor by which to sample the Gaussian profiles clip_sigma : sigmas from line center to use for the line scale_lyman_series : scaling to apply to Lyman-series emission lines scale_lines : scaling to apply to other emission lines, by name

Returns: dict with keys

wave_full, flux_full, line_full = wave and flux with fine lines wave, flux_line, flux_clean = original model + removed lines ymin, ymax = range of new line useful for plotting

static objfun_fitgrism(theta, self, plist, mb, TEF, kwargs, ret_type)

Objective function for fitting spectra

static objfun_fitphot(theta, self, plist, flux_fnu, err_fnu, is_flam, filters, TEF, kwargs, ret_type)

Objective function for fitting spectra

static objfun_fitspec(theta, self, plist, wave_obs, flux_obs, err_obs, mask, bspl, kwargs, ret_type)

Objective function for fitting spectra

param_floats(params=None)

Return a list of parameter values. If params is None, then use full list in self.params.all_params.

parameter_bounds(params, limit_age=False)

Parameter bounds for scipy.optimize.least_squares

pset(params)

Return a subset dictionary of self.meta

redden(wave)

set_dust(Av=0.0, dust_obj_type='WG00x', wg00_kwargs={'dust_distribution': 'homogeneous', 'dust_type': 'mw', 'geometry': 'shell'})

Set dust_obj attribute

dust_obj_type:

‘WG00’ = dust_attenuation.radiative_transfer.WG00 ‘C00’ = dust_attenuation.averages.C00 ‘WG00x’ = ParameterizedWG00 ‘KC13’ = Kriek & Conroy (2013) with dust_index parameter ‘R15’ = Reddy et al. (2015) with dust bump parameter

ir_template: (wave, flux)

Template to use for re-emitted IR light

set_fir_template(arrays=None, file='templates/magdis/magdis_09.txt', verbose=True, unset=False, scale_pah3=0.5)

Set the far-IR template for reprocessed dust emission

set_lognormal_sfh(min_sigma=3, verbose=False, **kwargs)

Set lognormal tabular SFH