Fitter

class sed_analysis_tools.sed_analysis_tools.Fitter
static bb_Double(source: Star | Binary = None, p0: List[float] = [5000.0, -20, 5000, -20], threshold_primary_match: float | None = None) → ndarray

Fit a double blackbody model to the spectrum.

Parameters:

  • source (Union["Star", "Binary"]) – Source object containing spectrum and other properties (default is None).

  • p0 (List[float]) – Initial guess for fit parameters [T_1, logsf_1, T_2, logsf_2] (default is [5000.0, -20, 5000.0, -20]).

  • threshold_primary_match (Optional[float]) – Threshold for validating the primary blackbody fit match (default is None).

Returns:

Optimized fit parameters [T_1, logsf_1, T_2, logsf_2]. Returns NaNs if fit fails or is rejected.

Return type:

np.ndarray

static bb_Single(source: Star | Binary = None, p0: List[float] = [5000.0, -20]) → ndarray

Fit a single blackbody model to the spectrum.

Parameters:

  • source (Union["Star", "Binary"]) – Source object containing spectrum and other properties (default is None).

  • p0 (List[float]) – Initial guess for fit parameters [Temperature (K), Log Scaling Factor] (default is [5000.0, -20]).

Returns:

Optimized fit parameters [T, logsf]. Returns NaNs if fit fails or is rejected.

Return type:

np.ndarray

static get_logflux_bb_Double(*, T_1: float, logsf_1: float, T_2: float, logsf_2: float, filter_set: FilterSet = None, plot: bool = False) → float | ndarray

Calculate the flux for a double blackbody model with the given filter set.

Parameters:

  • T_1 (float) – Temperature of the first blackbody in Kelvin.

  • logsf_1 (float) – Logarithmic scaling factor for the first blackbody.

  • T_2 (float) – Temperature of the second blackbody in Kelvin.

  • logsf_2 (float) – Logarithmic scaling factor for the second blackbody.

  • filter_set (FilterSet, optional) – The filter set to convolve the blackbody spectra with. If mode is “no_filters”, fluxes are calculated directly for the wavelengths in filter_set.x.

  • plot (bool, optional) – Whether to generate a plot of the spectra and photometry (default is False).

Returns:

Logarithmic flux values corresponding to the filter set wavelengths or synthesized photometry.

Return type:

np.ndarray or float

static get_logflux_bb_Single(*, T: float, logsf: float, filter_set: FilterSet | None = None, plot: bool = False) → float | ndarray

Compute flux for a single blackbody model.

Parameters:

  • T (float) – Blackbody temperature in Kelvin.

  • logsf (float) – Logarithmic scaling factor.

  • filter_set (Optional[FilterSet]) – Set of filters to convolve the blackbody with (default is None).

  • plot (bool) – Whether to plot the result (default is False).

Returns:

Logarithmic flux for the blackbody model.

Return type:

float or np.ndarray

static synth_phot(wavelength: Unit('m'), flux: Unit('erg / (Angstrom s cm2)'), filter_response: ndarray) → Quantity

Compute synthetic photometry by integrating flux with a filter response.

Parameters:

  • wavelength (astropy.Quantity (u.m)) – Wavelength array.

  • flux (astropy.Quantity (u.erg / u.cm**2 / u.s / u.Angstrom)) – Flux density array.

  • filter_response (np.ndarray) – Filter transmission response.

Returns:

Integrated flux in units of ergs/cm^2/s/Å.

Return type:

astropy.Quantity

static x_T_logsf_to_logflux_bb(x: float | List[float] | ndarray, T: float, logsf: float) → float | ndarray

Compute the logarithmic flux for a blackbody given wavelength, temperature, and scaling factor.

Parameters:

  • x (float or array-like) – Logarithm of the wavelength in Angstroms.

  • T (float) – Temperature of the blackbody in Kelvin.

  • logsf (float) – Logarithmic scaling factor (related to radius and distance).

Returns:

Logarithmic blackbody flux in ergs/cm^2/s/Å.

Return type:

float or np.ndarray