| Home | Trees | Indices | Help |
|---|
object --+ | BrokenPowerlawSED
Inherited from object:
__delattr__,
__format__,
__getattribute__,
__hash__,
__new__,
__reduce__,
__reduce_ex__,
__repr__,
__setattr__,
__sizeof__,
__str__,
__subclasshook__
6.6260755e-27
Inherited from object:
__class__
Normalized luminosity in the defined band.
wavelength0 and wavelength1 in Angstroms.
This is the fraction of total luminosity in the band. Multiply the result by the total luminosity (energy per second) to get physical units.
Normalized photon emission rate in the band between wavelength0 and wavelength1.
Units are erg^-1 (which could also be expressed as s^-1 per (erg/s)).
Multiply the result by the total luminosity (in ergs per unit time), to get the actual photon emission rate.
To get the ionizing photon emission rate (per unit luminosity): >>> BrokenPowerlawSED().photonRate_wavelength(0., 912.) 3272819078.0292048
Return a model SED for a galaxy.
Bolton and Haehnelt (2007MNRAS.382..325B) use an SED with
- eps_nu ~ v^0 for 912 < lambda < 3000 Ang.
- ~ v^-3 for labmda < 912 Ang.
'with an additional break in the spectrum at the Lyman limit'
eps_L = eps(1500)/6
The spectrum at the given frequency/frequencies.
Multiply by the total luminosity to get the luminosity per unit frequency.
Units are (fraction of total luminosity) per Hz.
The ratio of ionizing photon emission rate to luminosity.
The ratio of ionizing photon emission rate to luminosity at the given wavelength Q/L_nu(lambda) in units of photons s^-1 (erg s^-1 Hz^-1)^-1.
While this function takes an argument in angstroms, the ratio is calculated using the luminosity per unit frequence, so as to be easily comensurate with luminosities inferred from AB magnitudes.
| Home | Trees | Indices | Help |
|---|