Defines the conversion between Jy/beam and “brightness temperature”, T_B, in Kelvins. The brightness temperature is a unit very commonly used in radio astronomy. See, e.g., “Tools of Radio Astronomy” (Wilson 2009) eqn 8.16 and eqn 8.19 (these pages are available on google books).
T_B \equiv S_\nu / \left(2 k \nu^2 / c^2 \right)
However, the beam area is essential for this computation: the brightness temperature is inversely proportional to the beam area
Parameters: | beam_area : Beam Area equivalent
disp : Quantity with spectral units |
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Examples
Arecibo C-band beam:
>>> import numpy as np
>>> from astropy import units as u
>>> beam_sigma = 50*u.arcsec
>>> beam_area = 2*np.pi*(beam_sigma)**2
>>> freq = 5*u.GHz
>>> equiv = u.brightness_temperature(beam_area, freq)
>>> u.Jy.to(u.K, equivalencies=equiv)
3.526294429423223
>>> (1*u.Jy).to(u.K, equivalencies=equiv)
<Quantity 3.526294429423223 K>
VLA synthetic beam:
>>> bmaj = 15*u.arcsec
>>> bmin = 15*u.arcsec
>>> fwhm_to_sigma = 1./(8*np.log(2))**0.5
>>> beam_area = 2.*np.pi*(bmaj*bmin/fwhm_to_sigma**2)
>>> freq = 5*u.GHz
>>> equiv = u.brightness_temperature(beam_area, freq)
>>> u.Jy.to(u.K, equivalencies=equiv)
7.065788175060084