brightness_temperature¶

astropy.units.
brightness_temperature
(beam_area, disp)[source] [edit on github]¶ 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
Beam area in angular units, i.e. steradian equivalent
disp :
Quantity
with spectral unitsExamples
Arecibo Cband 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) 217.2658703625732