BlackBody1D

class astropy.modeling.blackbody.BlackBody1D(temperature=<Quantity 5000.0 K>, bolometric_flux=<Quantity 1.0 erg / (cm2 s)>, **kwargs)

Bases: astropy.modeling.Fittable1DModel

One dimensional blackbody model.

Parameters:

temperature : Quantity

Blackbody temperature.

bolometric_flux : Quantity

The bolometric flux of the blackbody (i.e., the integral over the spectral axis).

Notes

Model formula:

Examples

>>> from astropy.modeling import models
>>> from astropy import units as u
>>> bb = models.BlackBody1D()
>>> bb(6000 * u.AA)  
<Quantity 1.3585381201978953e-15 erg / (cm2 Hz s)>

import numpy as np
import matplotlib.pyplot as plt

from astropy.modeling.models import BlackBody1D
from astropy.modeling.blackbody import FLAM
from astropy import units as u
from astropy.visualization import quantity_support

bb = BlackBody1D(temperature=5778*u.K)
wav = np.arange(1000, 110000) * u.AA
flux = bb(wav).to(FLAM, u.spectral_density(wav))

with quantity_support():
    plt.figure()
    plt.semilogx(wav, flux)
    plt.axvline(bb.lambda_max.to(u.AA).value, ls='--')
    plt.show()

(png, svg, pdf)

Attributes Summary

bolometric_flux
input_units
input_units_allow_dimensionless
input_units_equivalencies
lambda_max	Peak wavelength when the curve is expressed as power density.
param_names
temperature

Methods Summary

evaluate(x, temperature, bolometric_flux)

Evaluate the model.

Attributes Documentation

bolometric_flux

input_units

input_units_allow_dimensionless = True

input_units_equivalencies = {'x': [(Unit("m"), Unit("Hz"), <function spectral.<locals>.<lambda>>), (Unit("m"), Unit("J"), <function spectral.<locals>.<lambda>>), (Unit("Hz"), Unit("J"), <function spectral.<locals>.<lambda>>, <function spectral.<locals>.<lambda>>), (Unit("m"), Unit("1 / m"), <function spectral.<locals>.<lambda>>), (Unit("Hz"), Unit("1 / m"), <function spectral.<locals>.<lambda>>, <function spectral.<locals>.<lambda>>), (Unit("J"), Unit("1 / m"), <function spectral.<locals>.<lambda>>, <function spectral.<locals>.<lambda>>), (Unit("1 / m"), Unit("rad / m"), <function spectral.<locals>.<lambda>>, <function spectral.<locals>.<lambda>>), (Unit("m"), Unit("rad / m"), <function spectral.<locals>.<lambda>>), (Unit("Hz"), Unit("rad / m"), <function spectral.<locals>.<lambda>>, <function spectral.<locals>.<lambda>>), (Unit("J"), Unit("rad / m"), <function spectral.<locals>.<lambda>>, <function spectral.<locals>.<lambda>>)]}

lambda_max

Peak wavelength when the curve is expressed as power density.

param_names = ('temperature', 'bolometric_flux')

temperature

Methods Documentation

evaluate(x, temperature, bolometric_flux)

Evaluate the model.

Parameters:

x : float, ndarray, or Quantity

Frequency at which to compute the blackbody. If no units are given, this defaults to Hz.

temperature : float, ndarray, or Quantity

Temperature of the blackbody. If no units are given, this defaults to Kelvin.

bolometric_flux : float, ndarray, or Quantity

Desired integral for the blackbody.

Returns:

y : number or ndarray

Blackbody spectrum. The units are determined from the units of bolometric_flux.