By Mike F.
A
little background: Radio astronomers use temperature to describe the strength
of detected radiation. Any body with a temperature above -273 deg C (approximately
absolute 0) emits electromagnetic radiation (EM).This
thermal radiation isn't just in the infrared but is exhibited across the
entire electromagnetic spectrum. (Note: it will have a greater intensity
(peak) at a specific area of the EM spectrum depending on its temperature).
For example, bodies at 2000 K (Kelvin), the radiation is primarily in the
infrared region and at 10000 K, the radiation is primarily in the visible
light region. There is also a direct correlation between temperature and
the amount of energy emitted, which is described by Planck's law.
When
the temperature of a body is lowered, two things happen. First, the peak
shifts in the direction towards the longer wavelengths and second, it emits
less radiation at all wavelengths.
This
turns out to be extremely useful. When a radio astronomer looks at a particular
point of the sky and says that it has a noise temperature of 1500 K, he/she
isn't declaring how hot the body (nebulae, etc) really is, but is providing
a measurement of the strength of the radiation from the source at the observed
frequency. For example, radiation from an extra solar body may be heated
from a nearby source such as a star.If
this body is radiating at a temperature of 500 K, it exhibits the same
emissions across all frequencies that a local test source does. The calculated
noise figure will be the same across all frequencies. (Note: this does
not take into account other sources of radiation such as synchrotron radiation).
So, here's the rub. Not only does the source that is of interest to the radio astronomer emit thermal radiation but also both the local environment (ground, atmosphere, etc) and the equipment (antenna, amplifiers, cables, receiver, etc) being used to make the measurements. To accurately observe and measure the distant sources, the radio astronomer must subtract all of the local environment and detection equipment noise additions.
where the constant is calculated from
1/[9.4608x10 15(4pik) 1/2]. Here the constant is
the number of meters per one light year, and k is the boltzmann constant.
"
What
makes you think you can discover anything? Who are you? Nobody.
Nobody at all. But the secrets of the universe don't mind. They reveal
themselves to nobodies who care. Isaac Newton was a nobody. Michael Faraday
was a bookbinder's apprentice....The big laboratories spend millions of
dollars, and they work slowly and surely, and they get results. But not
the big steps. Those come from the human mind. Not from the laboratory.
Call the inspiration, call them intuition, maybe blind luck, Maybe it's
God, saying, "Now's the time".
The
planet earth is a speck of dust, remote and alone in the void. There are
powers in the universe inscrutable and profound. Fear cannot save u. Rage
cannot help us. We must see the stranger in a new light-the light of understanding.
And to achieve this, we must begin to understand ourselves, and each other.
.
"Given an effective radiated power
of the transmitter (in watts), the effective area of the receiving antenna
(in square meters), the excess receiver noise temperature of the receiver
used (in K), the averaging time of the receiver (in seconds), and the accepted
band-width of the signal (in Hz), the range at which we can detect a signal
transmitted by an intelligent civilization, is