Radio Astronomy Fundamentals
We started on Chapter 2.
websites of interest are:
of radio astronomy)
(Discovery of the Cosmic Microwave Background Radiation)
the latest satellite results to measure the 3K background
(Discovery of Pulsars)
(Indirect detection of gravitational waves)
8 - 15 February
learned about power, spectral power,
brightness, brightness distribution, and flux density. Do you
We considered an antenna looking at part of a source brightness
distribution and figured out what we would measure.
An antenna is, in most cases, a one-pixel camera. We went
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. Difference is that the source function is
convolved with the mirror
image of the beam pattern whereas the mirror image is not
of the impulse response.
We looked at different combinations of source brightness
and beam patterns.
17 - 24
on blackbody characteristics, antenna temperature, spectral
power and noise.
finished Chapter 2.