Short wavelength astronomy
Short wavelength astronomy looks at the highest energy (and shortest wavelength) forms of electromagnetic radiation. The bands looked at range from ultraviolet (UV) to gamma rays.
To make things hard for astronomers, the majority of these forms of radiation are some of the more difficult to observe from Earth, as the gasses in our atmosphere prevents these from reaching the ground. As such, these telescopes are almost exclusively in space-based observatories.
Gamma-rays have the shortest wavelengths of the observed wavelengths, and also have the most energy. Because of this, gamma-rays are only emitted by the most energetic object in our universe: Black Holes, Neutron stars, Pulsars, Supernovae, and also the centre of young galaxies.
As Gamma-rays are only emitted under the most extreme conditions, and only a small number of gamma-rays are emitted at a time. This isn’t as bad as it sounds though; it just means gamma-ray observatories spend more time looking at fewer objects.
As we cannot see these objects in many of the other bands Gamma-ray observing is important for understanding the interaction of matter and radiation where temperatures are hundreds of millions of degrees, matter is very dense, or magnetic fields are very strong.
After Gamma-rays, X-rays are the next most energetic radiation observed. This means that we can use these to see what happens to the previous objects when they loose energy, as well as regular objects like stars and other galaxies.
The next most energetic form of electromagnetic radiation is ultraviolet (UV), and as we know, the gasses in the Earth’s atmosphere block out the majority of the UV light before it gets to the ground. For this reason UV observing is done almost exclusively in space-based observatories.
UV radiation is emitted by stars and galaxies when they are hot, at the beginning and end of their lifetimes. As the majority of stars and galaxies spend their time in stable cool states, UV astronomy gives a unique insight into the extreme stages of an object's lifetime.
Unfortunately, the gasses contained in interstellar dust clouds absorb at UV wavelengths, so we are not able to obtain all the information a star or galaxy sends our way. It is still worth doing the observations though, as we will get very useful information about both the object and the dust. If we know about the dust, then we can remove the effects of it and find out more information about the objects. Because of reasons like this, it is always important to couple observing with theoretical simulations.
To make things hard for astronomers, the majority of these forms of radiation are some of the more difficult to observe from Earth, as the gasses in our atmosphere prevents these from reaching the ground. As such, these telescopes are almost exclusively in space-based observatories.
Gamma-rays have the shortest wavelengths of the observed wavelengths, and also have the most energy. Because of this, gamma-rays are only emitted by the most energetic object in our universe: Black Holes, Neutron stars, Pulsars, Supernovae, and also the centre of young galaxies.
As Gamma-rays are only emitted under the most extreme conditions, and only a small number of gamma-rays are emitted at a time. This isn’t as bad as it sounds though; it just means gamma-ray observatories spend more time looking at fewer objects.
As we cannot see these objects in many of the other bands Gamma-ray observing is important for understanding the interaction of matter and radiation where temperatures are hundreds of millions of degrees, matter is very dense, or magnetic fields are very strong.
After Gamma-rays, X-rays are the next most energetic radiation observed. This means that we can use these to see what happens to the previous objects when they loose energy, as well as regular objects like stars and other galaxies.
The next most energetic form of electromagnetic radiation is ultraviolet (UV), and as we know, the gasses in the Earth’s atmosphere block out the majority of the UV light before it gets to the ground. For this reason UV observing is done almost exclusively in space-based observatories.
UV radiation is emitted by stars and galaxies when they are hot, at the beginning and end of their lifetimes. As the majority of stars and galaxies spend their time in stable cool states, UV astronomy gives a unique insight into the extreme stages of an object's lifetime.
Unfortunately, the gasses contained in interstellar dust clouds absorb at UV wavelengths, so we are not able to obtain all the information a star or galaxy sends our way. It is still worth doing the observations though, as we will get very useful information about both the object and the dust. If we know about the dust, then we can remove the effects of it and find out more information about the objects. Because of reasons like this, it is always important to couple observing with theoretical simulations.