Radio Astronomy Fundamentals
We started on Chapter 2.
Particular websites of interest are:
of radio astronomy)
(Discovery of the Cosmic Microwave Background Radiation)
for the latest satellite results to measure the 3K background
(Discovery of Pulsars)
(Indirect detection of gravitational waves)
learned about power, spectral power, brightness, brightness
distribution, and flux density. Do you recall the units?
We considered an antenna looking at part of a
source brightness distribution and figured out what we would
An antenna is, in most cases, a one-pixel camera. We went
in more detail through the differences and similarities between the
convolution integral as a mathematical description of the output of
a linear filter and the convolution integral as a mathematical
description of what is measured by an antenna when scanning a
source. The difference is that the source function is convolved with
the mirror image
of the beam pattern.
We looked at different combinations of source brightness
distributions and beam patterns.
20 - 22 February
focused on blackbody characteristics, antenna temperature, spectral
power and noise.
We learned how to compute the minimum detectable antenna temperature
and flux density. We looked at applications, particularly, we
learned how to determine the surface temperature of a solar system
body, like a planet, a moon or an asteroid. We also learned how to
measure the radius of such a body by measuring the antenna