BlackBody1D¶
-
class
astropy.modeling.blackbody.
BlackBody1D
(temperature=<Quantity 5000. K>, bolometric_flux=<Quantity 1. erg / (cm2 s)>, **kwargs)[source] [edit on github]¶ Bases:
astropy.modeling.Fittable1DModel
One dimensional blackbody model.
Parameters: Notes
Model formula:
\[f(x) = \pi B_{\nu} f_{\text{bolometric}} / (\sigma T^{4})\]Examples
>>> from astropy.modeling import models >>> from astropy import units as u >>> bb = models.BlackBody1D() >>> bb(6000 * u.AA) # doctest: +FLOAT_CMP <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()
()
Attributes Summary
bolometric_flux
input_units
This property is used to indicate what units or sets of units the evaluate method expects, and returns a dictionary mapping inputs to units (or None
if any units are accepted).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
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bolometric_flux
¶
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input_units
¶ This property is used to indicate what units or sets of units the evaluate method expects, and returns a dictionary mapping inputs to units (or
None
if any units are accepted).Model sub-classes can also use function annotations in evaluate to indicate valid input units, in which case this property should not be overridden since it will return the input units based on the annotations.
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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>>)]}¶
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lambda_max
¶ Peak wavelength when the curve is expressed as power density.
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param_names
= ('temperature', 'bolometric_flux')¶
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temperature
¶
Methods Documentation
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evaluate
(x, temperature, bolometric_flux)[source] [edit on github]¶ Evaluate the model.
Parameters: - x : float,
ndarray
, orQuantity
Frequency at which to compute the blackbody. If no units are given, this defaults to Hz.
- temperature : float,
ndarray
, orQuantity
Temperature of the blackbody. If no units are given, this defaults to Kelvin.
- bolometric_flux : float,
ndarray
, orQuantity
Desired integral for the blackbody.
Returns: - y : number or ndarray
Blackbody spectrum. The units are determined from the units of
bolometric_flux
.
- x : float,
-