phot_class.classification

The classification module tabulates light-curve fits for a given survey and determines the corresponding classification coordinates:

\[x = \chi^2_{blue}(Ia) - \chi^2_{blue}(91bg)\]
\[y = \chi^2_{red}(Ia) - \chi^2_{red}(91bg)\]

Function Documentation

phot_class.classification.classify_targets(fits_table, band_names=None, lambda_eff=None, out_path=None)[source]

Tabulate fitting coordinates for SNe based on their fit results

See the create_empty_table function for the assumed input table format. If band_names or lambda_eff are not given, they are taken from fits_table.meta. Any targets having one or more fits with the string ‘failed’ in the message are skipped (case insensitive).

Parameters:
  • fits_table (Table) – A table of fit results
  • band_names (list) – List of band names used when fitting
  • lambda_eff (list) – The effective wavelength of each band in angstroms
  • out_path (str) – Optionally write results to file
Returns:

An astropy table of fitting coordinates
phot_class.classification.tabulate_fit_results(data_iter, band_names, lambda_eff, fit_func, fitting_method='band', config=None, out_path=None)[source]

Tabulate fit results for a collection of data tables

Results already written to out_path are skipped.

Parameters:
  • data_iter (iter) – Iterable of photometric data for different SN
  • band_names (list) – Name of bands included in data_iter
  • lambda_eff (list) – Effective wavelength for bands in band_names
  • fit_func (func) – Function to use to run fits
  • config (dict) – Specifies priors / kwargs for fitting each model
  • out_path (str) – Optionally cache results to file
Returns:

An astropy table with fit results