astLib.astSED.StellarPopulation

Package astLib :: Module astSED :: Class StellarPopulation |
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# Class StellarPopulation

source code

Known Subclasses:
  - BC03Model
  - , M05Model
  - , P09Model

This class describes a stellar population model, either a Simple Stellar Population (SSP) or a Composite Stellar Population (CSP), such as the models of Bruzual & Charlot 2003 or Maraston 2005.

The constructor for this class can be used for generic SSPs or CSPs stored in white space delimited text files, containing columns for age, wavelength, and flux. Columns are counted from 0 ... n. Lines starting with # are ignored.

The classes M05Model (for Maraston 2005 models), BC03Model (for Bruzual & Charlot 2003 models), and P09Model (for Percival et al. 2009 models) are derived from this class. The only difference between them is the code used to load in the model data.

Instance Methods | [hide private]
__init__(self, fileName, ageColumn=0, wavelengthColumn=1, fluxColumn=2) | source code
SED object |
getSED(self, ageGyr, z=0.0, normalise=False, label=None) Extract a SED for given age. | source code
dictionary |
getColourEvolution(self, passband1, passband2, zFormation, zStepSize=0.05, magType=`'``Vega``'`) Calculates the evolution of the colour observed through passband1 - passband2 for the StellarPopulation with redshift, from z = 0 to z = zFormation. | source code
dictionary |
getMagEvolution(self, passband, magNormalisation, zNormalisation, zFormation, zStepSize=0.05, onePlusZSteps=False, magType=`'``Vega``'`) Calculates the evolution with redshift (from z = 0 to z = zFormation) of apparent magnitude in the observed frame through the passband for the StellarPopulation, normalised to magNormalisation (apparent) at z = zNormalisation. | source code
float |
calcEvolutionCorrection(self, zFrom, zTo, zFormation, passband, magType=`'``Vega``'`) Calculates the evolution correction in magnitudes in the rest frame through the passband from redshift zFrom to redshift zTo, where the stellarPopulation is assumed to be formed at redshift zFormation. | source code

Method Details | [hide private]

### getSED(self, ageGyr, z=0.0, normalise=False, label=None) | source code
Extract a SED for given age. Do linear interpolation between models if necessary. Parameters: `ageGyr` (float) - age of the SED in Gyr `z` (float) - redshift the SED from z = 0 to z = z `normalise` (bool) - normalise the SED to have area 1 Returns: SED object SED

### getColourEvolution(self, passband1, passband2, zFormation, zStepSize=0.05, magType=`'``Vega``'`) | source code
Calculates the evolution of the colour observed through passband1 - passband2 for the StellarPopulation with redshift, from z = 0 to z = zFormation. Parameters: `passband1` (Passband object) - filter passband through which to calculate the first magnitude `passband2` (Passband object) - filter passband through which to calculate the second magnitude `zFormation` (float) - formation redshift of the StellarPopulation `zStepSize` (float) - size of interval in z at which to calculate model colours `magType` (string) - either "Vega" or "AB" Returns: dictionary dictionary of numpy.arrays in format {'z', 'colour'}

### getMagEvolution(self, passband, magNormalisation, zNormalisation, zFormation, zStepSize=0.05, onePlusZSteps=False, magType=`'``Vega``'`) | source code
Calculates the evolution with redshift (from z = 0 to z = zFormation) of apparent magnitude in the observed frame through the passband for the StellarPopulation, normalised to magNormalisation (apparent) at z = zNormalisation. Parameters: `passband` (Passband object) - filter passband through which to calculate the magnitude `magNormalisation` (float) - sets the apparent magnitude of the SED at zNormalisation `zNormalisation` (float) - the redshift at which the magnitude normalisation is carried out `zFormation` (float) - formation redshift of the StellarPopulation `zStepSize` (float) - size of interval in z at which to calculate model magnitudes `onePlusZSteps` (bool) - if True, zSteps are (1+z)*zStepSize, otherwise zSteps are linear `magType` (string) - either "Vega" or "AB" Returns: dictionary dictionary of numpy.arrays in format {'z', 'mag'}

### calcEvolutionCorrection(self, zFrom, zTo, zFormation, passband, magType=`'``Vega``'`) | source code
Calculates the evolution correction in magnitudes in the rest frame through the passband from redshift zFrom to redshift zTo, where the stellarPopulation is assumed to be formed at redshift zFormation. Parameters: `zFormation` (float) - redshift to evolution correct from `zTo` (float) - redshift to evolution correct to `zFormation` (float) - formation redshift of the StellarPopulation `passband` (Passband object) - filter passband through which to calculate magnitude `magType` (string) - either "Vega" or "AB" `zFrom` (float) Returns: float evolution correction in magnitudes in the rest frame