MultiFilterASTs

class beast.observationmodel.noisemodel.toothpick.MultiFilterASTs(astfile, filters, vega_fname=None, *args, **kwargs)

Bases: NoiseModel

A noise model for based Artificial Star Tests (ASTs) that are provided as one single table.

The noise model is computed in equally spaced bins in log flux space to avoid injecting noise when the ASTs grossly oversample the model space. This is the case for single band ASTs - this is always the case for the BEAST toothpick noise model.

astfile

file containing the ASTs

Type:

str

filters

sequence of filter names

Type:

list

filter_aliases

alias of filter names between internal and external names

Type:

dict

Parameters:

• astfile (str) – file containing the ASTs

• filters (list) – filters using the internal namings (obs_inst_band)

• vega_fname (str, optional) – filename of the vega database

Methods Summary

__call__(sedgrid, **kwargs)	Call self as a function.
fit([nbins, progress])	Alias of fit_bins
fit_bins([nbins, ast_nonrecovered_ratio, ...])	Compute the necessary statistics before evaluating the noise model
interpolate(sedgrid[, progress])	Interpolate the results of the ASTs on a model grid
setFilters(filters[, vega_fname])	Set the filters and update the vega reference for the conversions
set_data_mappings(colnames)	Map the user-defined AST column names with the BEAST-required name formats User-defined names are set in settings.obs_colnames AST file has input vega magnitudes listed as F###W_IN and output flux/vegamag listed as F###W_RATE.

Methods Documentation

__call__(sedgrid, **kwargs)

Call self as a function.

fit(nbins=50, progress=True)

Alias of fit_bins

fit_bins(nbins=50, ast_nonrecovered_ratio=2.0, min_flux=None, max_flux=None, progress=True)

Compute the necessary statistics before evaluating the noise model

Parameters:

• nbins (int) – number of bins between the min/max values

• ast_nonrecovered_ratio (float) – mark any ASTs with a an output/input flux ratio larger than this value as nonrecovered

• min_flux (float) – min flux value in physical units for model bins default = None which means calculated from ast input fluxes

• max_flux (float) – max flux value in physical units for model bins default = None which means calculated from ast input fluxes

• progress (bool, optional) – if set, display a progress bar

• also (.. see)

interpolate(sedgrid, progress=True)

Interpolate the results of the ASTs on a model grid

Parameters:

• sedgrid (beast.core.grid type) – model grid to interpolate AST results on

• progress (bool, optional) – if set, display a progress bar

Returns:

• bias (ndarray) – bias table of the models

• sigma (ndarray) – dispersion table of the models

• comp (ndarray) – completeness table per model

setFilters(filters, vega_fname=None)

Set the filters and update the vega reference for the conversions

Parameters:

• filters (list) – filters using the internally normalized namings

• vega_fname (str, optional) – filename of the vega database

set_data_mappings(colnames)

Map the user-defined AST column names with the BEAST-required name formats User-defined names are set in settings.obs_colnames AST file has input vega magnitudes listed as F###W_IN and output flux/vegamag listed as F###W_RATE. The BEAST calls these things <TELESCOPE>_<DETECTOR>_F###W_in and <TELESCOPE>_<DETECTOR>_F###W_out, respectively. Example: F###W_IN -> HST_WFC3_F###W_in & F###W_RATE -> HST_WFC3_F###W_out

Parameters:

colnames (list) – list of column names in the photometry file indicating the flux/vegamag for each filter same thing as settings.obs_colnames, should end in _RATE if coming from DOLPHOT Example: [“F475W_RATE”, “F814W_RATE”] or [“WFC3_F475W_RATE, “ACS_F814W_RATE”], depending on the user’s combination of instrument and filter for their observed photometry file.