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Package cosmolopy :: Module luminosityfunction

Module luminosityfunction

source code

Galaxy luminosity functions (Schechter functions).

The LFHistory class implements a luminosity function history, encapsulating the changes in the galaxy luminosity distribution parameters as a function of redshift.

Classes
  LFHistory
Interpolate / extrapolate the Schechter parameters.
  BrokenPowerlawSED
Define an SED with a break at 912 Angstroms and different slopes above and below the break.
Functions
 
mass_from_sfr(sfr)
Use Labbe et al. (2009) relation between stellar mass and SFR.		 source code
 
sfr_from_mass(mass)
Use Labbe et al. (2009) relation between stellar mass and SFR.		 source code
 
sfr_from_L_nu(luminosity)
Use Kennicutt (1998) conversion from UV luminosity to star formation rate.		 source code
 
L_nu_from_sfr(sfr)
Use Kennicutt (1998) conversion from UV luminosity to star formation rate.		 source code
 
magnitudeAB_from_sfr(sfr)
Use Kennicutt (1998) conversion from UV luminosity to AB magnitude.		 source code
 
schechterL(luminosity, phiStar, alpha, LStar)
Schechter luminosity function.		 source code
 
schechterM(magnitude, phiStar, alpha, MStar)
Schechter luminosity function by magnitudes.		 source code
 
schechterCumuLL(luminosity, phiStar, alpha, LStar)
Integrate luminosity in galaxies above luminosity=L.		 source code
 
schechterCumuLM(magnitudeAB, phiStar, alpha, MStar)
Integrate luminosity in galaxies brighter than magnitudeAB.		 source code
 
schechterTotLL(phiStar, alpha, LStar)
Integrate total luminosity in galaxies.		 source code
 
schechterTotLM(phiStar, alpha, MStar)
Integrate total luminosity in galaxies.		 source code
 
iPhotonRateDensity(schechterParams, maglim=None, sedParams={}, wavelength=1500.0)
Ionizing photon rate density from a luminosity function.		 source code
 
plotLFevo(hist=None, params={'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6], 'alpha': [-1..., extrap_var='t', maglim=-19.252574989159953, z_max=20.0, skipIon=True)
Plot evolution of luminosity function params and total luminsity.		 source code
 
test_plot_schechter() source code
Variables
  B2007_z4 = {'MStar': -20.98, 'alpha': -1.73, 'phiStar': 0.0013...
  B2007_z5 = {'MStar': -20.64, 'alpha': -1.66, 'phiStar': 0.001,...
  B2007_z6 = {'MStar': -20.24, 'alpha': -1.74, 'phiStar': 0.0014...
  B2007_z7 = {'MStar': -19.3, 'alpha': -1.74, 'phiStar': 0.0014,...
  O2010_z7 = {'MStar': -19.9, 'alpha': -1.77, 'phiStar': 0.0014,...
  B2008 = {'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6], 'alp...
  B2008_fixed = {'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6]...
  zlinear = array([ 3.8, 5. , 5.9, 7.3, 9. ])
  B2008_linear_z5 = {'MStar': array([-21.072, -20.64 , -20.316, ...
  T2010ICLF = {'MStar': [-20.9, -20.55, -20.0, -19.7, -19.55], '...
  __package__ = 'cosmolopy'
Function Details

mass_from_sfr(sfr)

source code 

Use Labbe et al. (2009) relation between stellar mass and SFR.

See arXiv:0911.1356v4

Parameters

sfr:
the star formation rate in M_Sun / year.

Returns

mass:
stellar mass in units of M_Sun

sfr_from_mass(mass)

source code 

Use Labbe et al. (2009) relation between stellar mass and SFR.

See arXiv:0911.1356v4

Parameters

mass:
stellar mass in units of M_Sun

Returns

sfr:
the star formation rate in M_Sun / year.

sfr_from_L_nu(luminosity)

source code 

Use Kennicutt (1998) conversion from UV luminosity to star formation rate.

Parameters

luminosity:
the luminosity in units of ergs s^-1 Hz^-1 anywhere between 1500-2800 Angstroms.

Returns

The SFR in Msun/year.

Notes

Kennicutt (1998ARA&A..36..189K) says:

SFR/(MSun/year) = 1.4 * 10^-28 (L_nu/ergs s^-1 Hz^-1)

where L_nu is the UV luminosity anywhere between 1500-2800 Angstroms.

L_nu_from_sfr(sfr)

source code 

Use Kennicutt (1998) conversion from UV luminosity to star formation rate.

Parameters

sfr:
The SFR in Msun/year.

Returns

luminosity:
the luminosity in units of ergs s^-1 Hz^-1 anywhere between 1500-2800 Angstroms.

Notes

Kennicutt (1998ARA&A..36..189K) says:

SFR/(MSun/year) = 1.4 * 10^-28 (L_nu/ergs s^-1 Hz^-1)

where L_nu is the UV luminosity anywhere between 1500-2800 Angstroms.

magnitudeAB_from_sfr(sfr)

source code 

Use Kennicutt (1998) conversion from UV luminosity to AB magnitude.

Convenience function: uses L_nu_from_sfr and magnitudes.magnitude_AB_from_L_nu.

schechterCumuLL(luminosity, phiStar, alpha, LStar)

source code 

Integrate luminosity in galaxies above luminosity=L.

Uses an analytical formula.

schechterCumuLM(magnitudeAB, phiStar, alpha, MStar)

source code 

Integrate luminosity in galaxies brighter than magnitudeAB.

Uses an analytical formula.

schechterTotLL(phiStar, alpha, LStar)

source code 

Integrate total luminosity in galaxies.

Uses an analytical formula.

schechterTotLM(phiStar, alpha, MStar)

source code 

Integrate total luminosity in galaxies.

Uses an analytical formula.

iPhotonRateDensity(schechterParams, maglim=None, sedParams={}, wavelength=1500.0)

source code 

Ionizing photon rate density from a luminosity function.

in units of photons s^-1.

Given schecterParams, the parameters of a Schechter luminosity function (in terms of AB Magnitudes), sedParams, the parameters of the galactic Spectral Energy Distribution, and the wavelength of the AB Magnitudes, calculate the emission rate density of ionizing photons.

See Also

BrokenPowerlawSED

schechterTotLM

plotLFevo(hist=None, params={'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6], 'alpha': [-1..., extrap_var='t', maglim=-19.252574989159953, z_max=20.0, skipIon=True)

source code 

Plot evolution of luminosity function params and total luminsity.

Schechter function at each redshift is integrated up to maglim to find total luminsity.


Variables Details

B2007_z4

Value:
{'MStar': -20.98, 'alpha': -1.73, 'phiStar': 0.0013, 'z': 3.8}

B2007_z5

Value:
{'MStar': -20.64, 'alpha': -1.66, 'phiStar': 0.001, 'z': 5.0}

B2007_z6

Value:
{'MStar': -20.24, 'alpha': -1.74, 'phiStar': 0.0014, 'z': 5.9}

B2007_z7

Value:
{'MStar': -19.3, 'alpha': -1.74, 'phiStar': 0.0014, 'z': 7.4}

O2010_z7

Value:
{'MStar': -19.9, 'alpha': -1.77, 'phiStar': 0.0014, 'z': 6.8}

B2008

Value:
{'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6],
 'alpha': [-1.73, -1.66, -1.74, -1.74, -1.74],
 'phiStar': [0.0013, 0.001, 0.0014, 0.0011, 0.0011],
 'z': [3.8, 5.0, 5.9, 7.3, 9.0]}

B2008_fixed

Value:
{'MStar': [-20.98, -20.64, -20.24, -19.8, -19.6],
 'alpha': [-1.74, -1.74, -1.74, -1.74, -1.74],
 'phiStar': [0.0011, 0.0011, 0.0011, 0.0011, 0.0011],
 'z': [3.8, 5.0, 5.9, 7.3, 9.0]}

B2008_linear_z5

Value:
{'MStar': array([-21.072, -20.64 , -20.316, -19.812, -19.2  ]),
 'alpha': [-1.74, -1.74, -1.74, -1.74, -1.74],
 'phiStar': [0.0011, 0.0011, 0.0011, 0.0011, 0.0011],
 'z': array([ 3.8,  5. ,  5.9,  7.3,  9. ])}

T2010ICLF

Value:
{'MStar': [-20.9, -20.55, -20.0, -19.7, -19.55],
 'alpha': [-1.57, -1.63, -1.84, -1.9, -1.999],
 'phiStar': [0.0013, 0.0015, 0.001, 0.0006, 0.00022],
 'z': [4.0, 5.0, 7.0, 8.0, 9.0]}

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