Pandeia Configuration Dictionaries

This page describes the keywords in the JWST Pandeia configuration dictionary, provides valid keyword values (when applicable), and provides examples of adjusting Pandeia configuration dictionaries to produce particular outputs.

On this page

Pandeia configuration dictionaries are python dictionaries, and may be created or edited as such. Whilst it is possible to create a Pandeia configuration dictionary from scratch, it is generally preferable to modify an existing dictionary.



Creating Pandeia configuration dictionaries

Pandeia configuration dictionaries may be created entirely from scratch, imported from JSON files, or created by using Pandeia's "build_default_calc" function. Instructions on importing pandeia configuration information from JSON files can be found on the quickstart page.



Configuration dictionary structure

The Pandeia configuration dictionary has the following structure:

  • calculation: dictionary, contains flags to turn on and off the various calculation parameters

    • noise: dictionary, contains flags to turn on and off the available noise parameters

      • crs: boolean, flag to turn on and off the cosmic ray contribution to the noise value

      • darkcurrent: boolean, flag to turn on and off the dark current contribution to the noise value

      • ffnoise: boolean, flag to turn on and off the flat field contribution to the noise

      • readnoise: boolean, flag to turn on and off readout noise

      • rn_correlation: boolean, flag to turn on and off correlated readnoise

    • effects: dictionary, contains flags to turn on and off detector and sky effects

      • background: boolean, flag to turn on and off whether the background count rate is included. Note that in order to apply a background, this value and the background_subtraction key in the strategy dictionary must be set to True.

      • ipc: boolean, flag to turn on and off inter-pixel capacitance

      • saturation: boolean, flag to turn on and off checks for saturation, and the effects of saturation and signal-to-noise

  • configuration: dictionary, contains parameters related to the scene being observed and the instrument configuration.

    • scene_size: floating point value, the default size of the scene in arc seconds (the scene will always be a square, with size values referring to the length of a single side)

    • max_scene_size: floating point value, the maximum size to which the scene can grow in order to include all sources.

    • dynamic_scene: boolean, whether the scene should dynamically grow to include all sources (up to a maximum of max_scene_size)

    • instrument: dictionary, contains the instrument configuration parameters

      • aperture: string, the aperture to be used.

      • disperser: string, the disperser to be used (if any)

      • filter: string, the filter to be used (if any)

      • instrument: string, the instrument to be used (if using build_default_calc, the value provided for instrument will be set here)

      • mode: string, the mode to be used (if using build_default_calc, the value provided for mode will be set here)

    • detector: dictionary, contains the detector configuration

      • ngroup: integer, the number of groups in each ramp

      • nint: integer, the number of ramps in each exposure

      • nexp: integer, the number of exposures

      • subarray: string, which subset of the detector to use (or 'full' to use the entire detector)

      • readmode: string, which readout mode to use

  • strategy: dictionary, what observing strategy to use. The exact contents vary by strategy, but a typical strategy contains:

    • aperture_size: floating point, the size of the exposure aperture

    • sky_annulus: list of 2 floating point values. The inner and outer radius of the annulus in which the sky countrate will be measured

    • units: string, the units of the aperture size and sky annulus

    • background_subtraction: boolean, flag to turn background subtraction on and off. Note that in order to apply a background this value and the background key in the calculation:effects dictionary must be set to True

    • target_type: string, optional: the type of target being observed.

    • target_source: integer, which source to include in the observation. Only checked if 'target_type' is 'source'.

    • display_string: string, for information, the name of the observing method being used.

    • method: string, the internal function name of the observing method being used.

    • target_xy: list of 2 floating point values: the pixel location of the target

  • background: the background value. Either a string with value 'none', 'minzodi', or 'ecliptic', or a list of 2 arrays containing the wavelength (microns) and background flux (MJy/sr).

  • background_level: the background level. A string with the value 'low', 'medium', or 'high'; if background is 'minzodi', the value 'benchmark' is also allowed.

  • scene: list of dictionaries, one for each source in the scene. Each source dictionary includes:

    • position: dictionary, containing information about the source position. By default, all parameters should always be present in the position dictionary, but Pandeia will interpret any missing parameter as having the value 0.

      • position_parameters: list of strings, one for each parameter present. Possible parameters are:

        • x_offset: float, the offset of the source in the x direction from the centre of the scene, in arcseconds

        • y_offset: float, the offset of the source in the y direction from the centre of the scene, in arcseconds

        • orientation: float, the angle of the source with respect to the positive scene x axis, in degrees

      • Each parameter named in the position parameters list must be present in the position dictionary as a separate key of the defined type.

    • shape: dictionary, containing information about the source shape

      • geometry: string, one of 'point', 'flat', 'gaussian2d', 'sersic', 'sersic_scale', or 'power'. Different shapes require different shape parameters, as follows:

        • point: Does not require any other parameters. Parameters present will be ignored.

        • flat: Requires the parameters 'major' and 'minor' to be present.

        • gaussian2d: Requires the parameters 'major' and 'minor' to be present.

        • sersic: Requires the parameters 'major', 'minor', and 'sersic_index' to be present.

        • sersic_scale: Requires the parameters 'major', 'minor', and 'sersic_index' to be present.
        • power: Requires the parameters 'r_core' and 'power_index' to be present.
      • shape_parameters: list of strings, one for each parameter present. Possible parameters are:

        • major: float, length of the major axis, in arcseconds.

        • minor: float, length of the minor axis, in arcseconds.

        • sersic_index: float, index of the sersic profile. An index of 1.0 yields an exponential profile, 0.5 a gaussian profile, and 4.0 a de Vaucouleurs profile.

        • power_index: float, index of the power law spatial profile.
      • norm_method: string, defines where the profile is to be normalized. Possible values are "integ_infinity", "surf_center", and "surf_scale". For flat profiles, "surf_scale" is not valid; for power law profiles, neither "surf_scale" nor "integ_infinity" are valid.
      • surf_area_units: string, defines the area unit of the surface brightness normalization. Possible values are "null" (for integ_infinity only), "arcsec^2", or "sr".
      • Each parameter named in the shape parameters list must be present in the shape dictionary as a separate key of the defined type.

    • spectrum: dictionary, containing information about the source SED.

      • name: string, name of the source. Provided for information, not referenced by the engine during the calculation.

      • spectrum_parameters: list of strings, one for each parameter present. Possible parameters are:

        • redshift: float, redshift of the source. Redshift is applied after the spectrum has been created, but before extinction has been added, before continuum normalization, and before any emission lines have been added.

        • lines: list of dictionaries, giving information on each line to be added to the SED. NOTE that redshift, extinction, and normalization will not be applied to any lines specified here. Each line dictionary has the following parameters:

          • id: string or integer. Identifier given to the line. Not used internally.

          • name: string. Name of the line. Not used internally.

          • emission_or_absorption: string, line type. Currently, all lines are treated as emission lines.

          • center: float, central wavelength of the line, in microns.

          • width: float, FWHM of the line in km/s.

          • strength: float, line strength, definition depends on line type:

            • Emission Lines: line strength in erg/cm^2/s

            • Absorption Lines: central optical depth (once they are implemented).

          • profile: string, line profile, currently the only supported value is 'gaussian'

        • sed: dictionary, provides the parameters of the source continuum SED. Contains the following keys:

          • sed_type: string, defines the type of SED. Possible values are 'no_continuum', 'flat', 'powerlaw', 'blackbody', 'phoenix', 'hst_calspec', 'brown', and 'input'. Depending on the SED type chosen, other parameters may be needed.

            • no_continuum: takes no parameters1

            • flat: takes 'unit'1

            • powerlaw: takes 'unit' and 'index'1

            • blackbody: takes 'temp'1

            • phoenix: takes 'key' (if perform_calculation is run with webapp=True) or takes 'teff', 'log_g', and 'metallicity' (if perform_calculation is run with webapp=False)

            • hst_calspec: takes 'key'

            • brown: takes 'key', galaxy models based on Brown et al. (2014).

            • input: takes 'spectrum',

          • unit: string, either 'fnu' or 'flam'. Used by flat and power law spectra.

          • index: float, exponent of the power law. Used by power law spectra.

          • temp: float, temperature of the blackbody. Used by blackbody spectra.

          • key: string, the type of source to model. Used by phoenix, hst_calspec, and galaxies spectra. Valid values are shown below in the appendix.

          • t_eff: float, effective temperature of the phoenix model star, in K. Allowed range is 2000 to 70,000.

          • log_g: float, logarithm of the surface gravity of the phoenix model star, in cgs units. Allowed range is 0.0 to 5.5.

          • metallicity: float, logarithm of the metallicity of the phoenix model star, relative to solar metallicity. Allowed range is -4.0 to 0.5.

          • spectrum: list of 2 arrays, or ndarray. The wavelength (micron) and flux (mJy) arrays of the SED to use. In an ndarray, wavelength is the 0th index, and flux the 1st index.

        • normalization: dictionary defining the source brightness. Contains the following keys:

          • type: string, defines the type of normalization. Possible values are 'at_lambda', 'hst', 'jwst' 'photsys', and 'none'. Depending on the normalization type chosen, other parameters may be needed.

            • none takes no parameters.

            • hsttakes 'bandpass', 'norm_flux', and 'norm_fluxunit'

            • jwst takes 'bandpass', 'norm_flux', and 'norm_fluxunit'

            • photsys takes 'bandpass', 'norm_flux', and 'norm_fluxunit'

            • at_lambda takes 'norm_wave', 'norm_waveunit', 'norm_flux', and 'norm_fluxunit'

          • norm_wave: float, reference wavelength in units of 'norm_waveunit', used by 'at_lambda'.

          • norm_waveunit: string, specifies the wavelength units used for normalization, used by 'at_lambda'. Available values are 'm', 'nm', 'um' (micron), 'mm', 'micron', 'microns', 'angstrom'

          • norm_flux: float, reference flux value in units of 'norm_fluxunit', used by all normalization methods other than 'none'.

          • norm_fluxunit: string, specifies the flux units used for normalization. Used by all methods other than 'none'. Available values are 'flam', 'fnu', 'vegamag', 'abmag', 'mjy', 'ujy' (micro-Jansky), 'njy', 'jy'

          • bandpass: string, specifies the bandpass for 'hst', 'jwst', and 'photsys' normalizations. Possible values are shown in the appendix

        • extinction: dictionary defining the wavelength-dependent extinction between the source and the observer. Contains the following keys:

          • law: string, the extinction law being used. Values include seven models from Weingartner & Draine (2001) (3 generic Milky Way models: 'mw_rv_31', 'mw_rv_40', 'mw_rv_55'; 2 LMC models: 'lmc_avg' and 'lmc_2'; one SMC model: 'smc_bar', and the 'hd210121' model), and one Chapman (2009) model: 'chapman09'.

          • value: float, the extinction value, in units of 'unit'

          • unit: string, the units of the extinction value, either 'nh' for hydrogen column density or 'mag' for magnitudes.

          • bandpass: the bandpass in which the extinction is measured, only used if the unit is 'mag'.



Sample code creating a background spectrum using the JWST Background Tool (JBT)

jbt_background
# The following section is only needed if the PYSYN_CDBS environment variable is not already set. 
# The PYSYN_CDBS environment variable should point to the path of the CDBS data files 
import os 
location_of_cdbs = "/path/to/cdbs/files" 
os.environ['PYSYN_CDBS'] = location_of_cdbs 
# End section 

# The following section is only needed if the pandeia_refdata environment variable is not already set 
# The pandeia_refdata environment variable should point to the path of the pandeia reference data 
import os 
location_of_pandeia_refdata = "/path/to/pandeia/refdata" 
os.environ['pandeia_refdata'] = location_of_pandeia_refdata 
# End section 

from pandeia.engine.calc_utils import build_default_calc 
from jwst_backgrounds import jbt   

# The following are parameters which can easily be changed 
ra = 27.5 
dec = -12.7 
background_primary_wavelength = 4.0 # in microns, doesn't actually matter as we want the full spectrum. 
day_of_interest = 0 # the first day of visibility for the target sky co-ordinates in the current cycle 
telescope = 'jwst' 
instrument = 'nircam' 
mode = 'sw_imaging' 
configuration = build_default_calc(telescope, instrument, mode)

bg = jbt.background(ra, dec, background_primary_wavelength) 
wave_array = bg.bkg_data['wave_array'] 
flux_array = bg.bkg_data['total_bg'][day_of_interest] 
configuration['background'] = [] 
configuration['background'].append(wave_array) 
configuration['background'].append(flux_array)

Note that, in order to use the JWST backgrounds tool (JBT), it must be installed in your conda environment (i.e. by typing "pip install jwst_backgrounds" at the command line). For more information on the JBT, see the JBT documentation page.

Creating a scene with a custom galaxy spectrum and a foreground star

custom_background_scene
from copy import deepcopy   
# The following section is only needed if the PYSYN_CDBS environment variable is not already set. 
# The PYSYN_CDBS environment variable should point to the path of the CDBS data files 
import os 
location_of_cdbs = "/path/to/cdbs/files" 
os.environ['PYSYN_CDBS'] = location_of_cdbs 
# End section 

# The following section is only needed if the pandeia_refdata environment variable is not already set 
# The pandeia_refdata environment variable should point to the path of the pandeia reference data 
import os 
location_of_pandeia_refdata = "/path/to/pandeia/refdata" 
os.environ['pandeia_refdata'] = location_of_pandeia_refdata 
# End section 


import pysynphot 
from pandeia.engine.calc_utils import build_default_calc 

# The following are parameters which can easily be changed 
telescope = 'jwst' 
instrument = 'nircam' 
mode = 'sw_imaging' 
configuration = build_default_calc(telescope, instrument, mode) 

# The following are values that can be set to anything desired. 
custom_galaxy_name = 'My Background Galaxy' 
custom_galaxy_spectrum_file = '/path/to/galaxy/spectrum/gal_spec.fits' 
custom_galaxy_orientation = 27.1 #degrees 
custom_galaxy_major_axis = 18.0 
custom_galaxy_minor_axis = 2.5 
custom_galaxy_sersic_index = 1.5 
custom_galaxy_norm_method = 'surf_scale'
custom_galaxy_surf_area_units = 'arcsec^2'
custom_galaxy_redshift = 0.1 
custom_galaxy_extinction = 0.6 # magnitudes 
custom_galaxy_brightness = 19.9 
custom_galaxy_bandpass = 'johnson,v' 
custom_galaxy_fluxunit = 'abmag'

spec = pysynphot.FileSpectrum(custom_galaxy_spectrum_file) 
spec.convert('microns')
spec.convert('mjy')

source_gal = deepcopy(configuration['scene'][0])
source_gal['position']['orientation'] = custom_galaxy_orientation 
source_gal['shape']['geometry'] = 'sersic' 
source_gal['shape']['shape_parameters'] = ['major', 'minor', 'sersic_index', 'norm_method', 'surf_area_units'] 
source_gal['shape']['major'] = custom_galaxy_major_axis 
source_gal['shape']['minor'] = custom_galaxy_minor_axis 
source_gal['shape']['sersic_index'] = custom_galaxy_sersic_index 
source_gal['shape']['norm_method'] = custom_galaxy_norm_method
source_gal['shape']['surf_area_units'] = custom_galaxy_surf_area_units
source_gal['spectrum']['name'] = custom_galaxy_name 
source_gal['spectrum']['redshift'] = custom_galaxy_redshift 
source_gal['spectrum']['extinction']['value'] = custom_galaxy_extinction 
source_gal['spectrum']['sed'] = {'sed_type': 'input', 'spectrum': [spec.wave, spec.flux]} 
source_gal['spectrum']['normalization'] = {} 
source_gal['spectrum']['normalization']['type'] = 'photsys' 
source_gal['spectrum']['normalization']['bandpass'] = custom_galaxy_bandpass 
source_gal['spectrum']['normalization']['norm_flux'] = custom_galaxy_brightness 
source_gal['spectrum']['normalization']['norm_fluxunit'] = custom_galaxy_fluxunit 

# The following are values that can be set to anything desired 
star_type = 'g2v' 
star_position_x = 0.35 # arcseconds 
star_position_y = -0.14 # arcseconds 
star_norm_bandpass = 'johnson,v' 
star_norm_flux = 22.2 
star_norm_fluxunit = 'abmag' 
source_star = deepcopy(configuration['scene'][0]) 
source_star['position']['x_offset'] = star_position_x 
source_star['position']['y_offset'] = star_position_y 
source_star['shape'] = {'geometry': 'point', 'shape_parameters': []} 
source_star['spectrum']['name'] = 'G2V Star' 
source_star['spectrum']['redshift'] = 0. 
source_star['spectrum']['extinction']['value'] = 0. 
source_star['spectrum']['normalization'] = {} 
source_star['spectrum']['normalization']['type'] = 'photsys' 
source_star['spectrum']['normalization']['bandpass'] = star_norm_bandpass 
source_star['spectrum']['normalization']['norm_flux'] = star_norm_flux 
source_star['spectrum']['normalization']['norm_fluxunit'] = star_norm_fluxunit 
source_star['spectrum']['sed'] = {'sed_type': 'phoenix', 'key': star_type} 

configuration['scene'] = [source_gal, source_star]

If the scene above is run through Pandeia, the resulting output image will be generated:

Creating a sample slitless spectrograph observation of a superimposed star and galaxy


sample_slitless_spectrograph
from copy import deepcopy 
# The following section is only needed if the PYSYN_CDBS environment variable is not already set. 
# The PYSYN_CDBS environment variable should point to the path of the CDBS data files 
import os 
location_of_cdbs = "/path/to/cdbs/files" 
os.environ['PYSYN_CDBS'] = location_of_cdbs 
# End section 
# The following section is only needed if the pandeia_refdata environment variable is not already set 
# The pandeia_refdata environment variable should point to the path of the pandeia reference data 
import os
location_of_pandeia_refdata = "/path/to/pandeia/refdata" 
os.environ['pandeia_refdata'] = location_of_pandeia_refdata 
# End section 

from pandeia.engine.calc_utils import build_default_calc 

# The following are parameters which can easily be changed 
telescope = 'jwst' 
instrument = 'miri' 
mode = 'lrsslitless' 
configuration = build_default_calc(telescope, instrument, mode) 

# The following are values that can be set to anything desired. 
galaxy_name = 'NGC 3521-type Galaxy' 
galaxy_orientation = 77.3 #degrees 
galaxy_y_offset = -0.13 # arcseconds 
galaxy_major_axis = 22.0 #arcseconds 
galaxy_minor_axis = 4.5 #arcseconds 
galaxy_sersic_index = 3.7
galaxy_norm_method = 'integ_infinity'
galaxy_surf_area_unit = None
galaxy_redshift = 0.1 
galaxy_extinction = 0.3 
# magnitudes 
galaxy_sed = 'ngc_3521' 
galaxy_brightness = -2.0 
galaxy_bandpass = 'miri,imaging,f560w' 
galaxy_fluxunit = 'abmag' 
source_gal = deepcopy(configuration['scene'][0]) 
source_gal['position']['orientation'] = galaxy_orientation 
source_gal['position']['y_offset'] = galaxy_y_offset 
source_gal['shape']['geometry'] = 'sersic_scale' 
source_gal['shape']['shape_parameters'] = ['major', 'minor', 'sersic_index', 'norm_method', 'surf_area_unit']
source_gal['shape']['major'] = galaxy_major_axis 
source_gal['shape']['minor'] = galaxy_minor_axis 
source_gal['shape']['sersic_index'] = galaxy_sersic_index 
source_gal['shape']['norm_method'] = galaxy_norm_method
source_gal['shape']['surf_area_unit'] = galaxy_surf_area_unit
source_gal['spectrum']['name'] = galaxy_name 
source_gal['spectrum']['redshift'] = galaxy_redshift 
source_gal['spectrum']['extinction']['value'] = galaxy_extinction 
source_gal['spectrum']['sed'] = {'sed_type': 'brown', 'key': galaxy_sed} 
source_gal['spectrum']['normalization'] = {} 
source_gal['spectrum']['normalization']['type'] = 'jwst' 
source_gal['spectrum']['normalization']['bandpass'] = galaxy_bandpass 
source_gal['spectrum']['normalization']['norm_flux'] = galaxy_brightness 
source_gal['spectrum']['normalization']['norm_fluxunit'] = galaxy_fluxunit 

# The following are values that can be set to anything desired 
star_type = 'f5v' 
star_position_y = 0.25 # arcseconds 
star_norm_bandpass = 'miri,imaging,f560w' 
star_norm_flux = 18.0 
star_norm_fluxunit = 'abmag' 
emission_line_center = 11. #microns 
emission_line_width = 1500. #km/s 
emission_line_strength = 1.e-15 
source_star = deepcopy(configuration['scene'][0]) 
source_star['position']['y_offset'] = star_position_y 
source_star['shape'] = {'geometry': 'point', 'shape_parameters': []} 
source_star['spectrum']['name'] = 'F5V Star' 
source_star['spectrum']['redshift'] = 0. 
source_star['spectrum']['extinction']['value'] = 0. 
source_star['spectrum']['normalization'] = {} 
source_star['spectrum']['normalization']['type'] = 'jwst' 
source_star['spectrum']['normalization']['bandpass'] = star_norm_bandpass 
source_star['spectrum']['normalization']['norm_flux'] = star_norm_flux 
source_star['spectrum']['normalization']['norm_fluxunit'] = star_norm_fluxunit 
emission_line = {} 
emission_line['id'] = 0 
emission_line['name'] = 'Sample Emission Line' 
emission_line['emission_or_absorption'] = 'emission' 
emission_line['center'] = emission_line_center 
emission_line['width'] = emission_line_width 
emission_line['strength'] = emission_line_strength 
emission_line['profile'] = 'gaussian' 
source_star['spectrum']['lines'] = [emission_line] 
source_star['spectrum']['sed'] = {'sed_type': 'phoenix', 'key': star_type}

configuration['scene'] = [source_gal, source_star]

Two figures are shown below. The first is a MIRI F560W image of the scene resulting from the above commands. The second is a set of three slitless spectra created with the MIRI P750L slitless spectrograph, one of each scene source individually, and a final observation of the combined scene. Note that the three separate spectra result from three separate Pandeia observations with the same instrument and detector settings, but different source lists. Note: The F560W image is partially saturated, and included mostly to provide an indication of the relative source locations on the detector.



Sample code

Creating a source galaxy with a redshifted emission line

galaxy_redshifted_emission
from copy import deepcopy
 
# The following section is only needed if the PYSYN_CDBS environment variable is not already set.
# The PYSYN_CDBS environment variable should point to the path of the CDBS data files
import os
location_of_cdbs = "/path/to/cdbs/files"
os.environ['PYSYN_CDBS'] = location_of_cdbs
# End section
 
# The following section is only needed if the pandeia_refdata environment variable is not already set
# The pandeia_refdata environment variable should point to the path of the pandeia reference data
import os
location_of_pandeia_refdata = "/path/to/pandeia/refdata"
os.environ['pandeia_refdata'] = location_of_pandeia_refdata
# End section
from pandeia.engine.calc_utils import build_default_calc
 
# The following are parameters which can easily be changed
telescope = 'jwst'
instrument = 'miri'
mode = 'imaging'
 
configuration = build_default_calc(telescope, instrument, mode)
 
# The following are values that can be set to anything desired.
galaxy_name = 'NGC 3521-type Galaxy'
galaxy_major_axis = 12.5 #arcseconds
galaxy_minor_axis = 4.0 #arcseconds
galaxy_sersic_index = 1.0
galaxy_norm_method = 'integ_infinity'
galaxy_surf_area_unit = None
galaxy_redshift = 1.5
galaxy_extinction = 0.3 # magnitudes
galaxy_sed = 'ngc_3521'
galaxy_brightness = 9.0
galaxy_bandpass = 'miri,imaging,f560w'
galaxy_fluxunit = 'abmag'
emission_line_center = 0.65628 #H alpha, microns
emission_line_width = 150. #km/s
emission_line_strength = 1.e-15

source_gal = deepcopy(configuration['scene'][0])
source_gal['shape']['geometry'] = 'sersic_scale'
source_gal['shape']['shape_parameters'] = ['major', 'minor', 'sersic_index', 'norm_method', 'surf_area_unit']
source_gal['shape']['major'] = galaxy_major_axis
source_gal['shape']['minor'] = galaxy_minor_axis
source_gal['shape']['sersic_index'] = galaxy_sersic_index
source_gal['shape']['norm_method'] = galaxy_norm_method
source_gal['shape']['surf_area_unit'] = galaxy_surf_area_unit
source_gal['spectrum']['name'] = galaxy_name
source_gal['spectrum']['redshift'] = galaxy_redshift
source_gal['spectrum']['extinction']['value'] = galaxy_extinction
source_gal['spectrum']['sed'] = {'sed_type': 'brown', 'key': galaxy_sed}
source_gal['spectrum']['normalization'] = {}
source_gal['spectrum']['normalization']['type'] = 'jwst'
source_gal['spectrum']['normalization']['bandpass'] = galaxy_bandpass
source_gal['spectrum']['normalization']['norm_flux'] = galaxy_brightness
source_gal['spectrum']['normalization']['norm_fluxunit'] = galaxy_fluxunit
emission_line = {}
emission_line['id'] = 0
emission_line['name'] = 'Redshifted H-alpha emission'
emission_line['emission_or_absorption'] = 'emission'
emission_line['center'] = emission_line_center * (1 + galaxy_redshift)
emission_line['width'] = emission_line_width * (1 + galaxy_redshift)
emission_line['strength'] = emission_line_strength
emission_line['profile'] = 'gaussian'
source_gal['spectrum']['lines'] = [emission_line]
  
configuration['scene'] = [source_gal]



Appendices valid values for configuration dictionary

The following are valid values for configuration dictionaries:

config['spectrum']['sed']

  • sed_type = 'phoenix'

    • key may have the following values:

      • o3v

      • o5v

      • o6i

      • o7v

      • o8i

      • o9v

      • b0v

      • b0iii

      • b0i

      • b1v

      • b3v

      • b5iii

      • b5v

      • b5i

      • b8v

      • a0i

      • a0v

      • a1v

      • a5i

      • a3v

      • a5v

      • f0i

      • f0v

      • f5i

      • f2v

      • f5v

      • f8v

      • g0v

      • g0iii

      • g2v

      • g5v

      • g0i

      • g8v

      • g5iii

      • g5i

      • k0v

      • k0iii

      • k2v

      • k0i

      • k5v

      • k5iii

      • k7v

      • k5i

      • m0i

      • m0iii

      • m0v

      • m2i

      • m2v

      • m5v

  • sed_type = 'hst_calspec'

    • key may have the following values:

      • gd71

      • gd153

      • g191b2b

      • hz43

      • p330e

      • sirius

      • vega

      • wd0308-565

      • wd1057+719

  • sed_type = 'brown'

    • key may have the following values:

      • Values present in the web UI

        • ngc_3690

        • ngc_6240

        • ngc_5953

        • ic_4553

        • ngc_5256

        • ngc_3521

        • ngc_4125

        • ngc_4552

        • cgcg_049-057

        • ngc_0337

        • ngc_4138

        • ii_zw_096

        • ngc_0695

        • ngc_4725

        • ugca_219

        • ngc_3079

        • ngc_6090

        • mrk_33

      • Values that will work, but are not present in the web UI

        • ngc_4579

        • ngc_4670

        • ugc_05101

        • ngc_4860

        • ugc_04881

        • cgcg_436-030

        • ngc_0520

        • ngc_1144

        • ngc_7673

        • ngc_7674

        • ngc_7679

        • ngc_7771

        • ngc_3627

        • mrk_0475

        • ngc_0584

        • ic_5298

        • ngc_0628

        • ngc_4385

        • ngc_5653

        • ngc_4387

        • ngc_4660

        • iras_08572+3915

        • ngc_2388

        • ic_0691

        • ngc_4473

        • ngc_4889

        • mrk_0930

        • ngc_5257

        • ugc_12150

        • ngc_3938

        • ngc_0750

        • ngc_4551

        • ngc_4550

        • ngc_4559

        • ngc_4926

        • arp_118

        • ngc_1614

        • ngc_7591

        • ngc_7592

        • ngc_5258

        • ugc_08335_nw

        • arp_256_s

        • iii_zw_035

        • arp_256_n

        • ngc_4486

        • iras_17208-0014

        • ugca_166

        • ugc_09618_n

        • ngc_2537

        • ngc_6052

        • ngc_2623

        • mrk_1490

        • ngc_1275

        • ngc_0855

        • ngc_3265

        • ngc_4254

        • ngc_5992

        • ngc_4536

        • ngc_4826

        • ngc_4631

        • ngc_2798

        • ugc_06850

        • ugc_06665

        • ngc_4321

        • ugc_09618_s

        • ngc_5033

        • ngc_7585

        • ngc_1068

        • ic_0860

        • ngc_3379

        • ngc_5055

        • ngc_0660

        • ngc_5194

        • ngc_5195

        • ngc_4621

        • ngc_3310

        • ngc_4625

        • ngc_5713

        • ugca_410

        • haro_06

        • ngc_4088

        • ngc_7331

        • ngc_0474

        • ngc_5866

        • mrk_0331

        • cgcg_453-062

        • ngc_4168

        • ic_0883

        • ngc_3870

        • ngc_4676_a

        • mrk_1450

        • ugc_08696

        • ic_4051

        • ngc_5104

        • ngc_4194

        • ngc_7714

        • ngc_2403

        • ugc_08335_se

        • ngc_4365

        • ngc_3190

        • um_461

        • ugca_208

        • ngc_3198

        • ngc_3351

        • ngc_4569

        • ugc_09618

        • ngc_3049

        • ngc_4594

        • ngc_4458

        • ngc_4450

        • ngc_3773

config['spectrum']['normalization']

  • type = 'hst'

    • bandpass may have the following values:

      • wfc3,ir,f098m

      • wfc3,ir,f105w

      • wfc3,ir,f110w

      • wfc3,ir,f125w

      • wfc3,ir,f140w

      • wfc3,ir,f160w

  • type = 'jwst'

    • bandpass may have the following values:

      • nircam,sw_imaging,f070w

      • nircam,sw_imaging,f090w

      • nircam,sw_imaging,f115w

      • nircam,sw_imaging,f150w

      • nircam,sw_imaging,f200w

      • nircam,sw_imaging,f212n

      • nircam,lw_imaging,f277w

      • nircam,lw_imaging,f356w

      • nircam,lw_imaging,f444w

      • miri,imaging,f560w

      • miri,imaging,f770w

      • miri,imaging,f1000w

      • miri,imaging,f1280w

      • miri,imaging,f1500w

      • miri,imaging,f1800w

      • miri,imaging,f2100w

      • miri,imaging,f2550w

  • type = 'photsys'

    • bandpass may have the following values:

      • bessell,j

      • bessell,h

      • bessell,k

      • cousins,i

      • johnson,v

      • johnson,i

      • johnson,j

      • johnson,k

      • sdss,u

      • sdss,g

      • sdss,r

      • sdss,i

      • sdss,z

      • spitzer,irac3.6

      • spitzer,irac4.5

      • spitzer,irac5.8

      • spitzer,irac8.0

      • spitzer,mips24




Published

 

Latest updates

  • Updated for ETC v1.3