Recent Developments in Cosmology
... From our vantage point 13 billion years after the Big Bang, we are now trying to unravel what happened in the earliest tiny fraction of a second, when the Universe was 0.000000000000000000000000000000000001 seconds old! We can test our ideas about the Very Early Universe by observing the distributio ...
... From our vantage point 13 billion years after the Big Bang, we are now trying to unravel what happened in the earliest tiny fraction of a second, when the Universe was 0.000000000000000000000000000000000001 seconds old! We can test our ideas about the Very Early Universe by observing the distributio ...
Confronting predictions of the galaxy stellar mass function with
... overview) is a smaller volume but the mass and spatial resolution are better than MassiveBlack by a factor of 25 and 2.7, respectively. The smaller volume means that a smaller part of the high-mass function can be sampled and that in the mass range where it overlaps with MassiveBlack it can be used ...
... overview) is a smaller volume but the mass and spatial resolution are better than MassiveBlack by a factor of 25 and 2.7, respectively. The smaller volume means that a smaller part of the high-mass function can be sampled and that in the mass range where it overlaps with MassiveBlack it can be used ...
SPECTROSCOPY OF HIGH-REDSHIFT TYPE Ia SUPERNOVAE
... indeed be “normalised” in the same way as their local counterparts, which is exactly the effect one is trying to measure! The issue of the SN Ia environment is easier to get a handle on, since SNe Ia (unlike any other type of SN) occur in early as well as late-type galaxies, and so meaningful compar ...
... indeed be “normalised” in the same way as their local counterparts, which is exactly the effect one is trying to measure! The issue of the SN Ia environment is easier to get a handle on, since SNe Ia (unlike any other type of SN) occur in early as well as late-type galaxies, and so meaningful compar ...
spiral galaxies
... much empty space between stars that it’s unlikely two stars would smash together. And though the sun and all its orbiting planets, including Earth, will probably end up in a new position, they won’t be destroyed. Eventually the galactic centers, each of which likely contains a super massive black ho ...
... much empty space between stars that it’s unlikely two stars would smash together. And though the sun and all its orbiting planets, including Earth, will probably end up in a new position, they won’t be destroyed. Eventually the galactic centers, each of which likely contains a super massive black ho ...
Quasars- The Brightest Black Holes
... In 1962 an opportunity arose for a much clearer determination of the position of one of these powerful but as yet unidentified sources, 3C273, when it would be eclipsed by the Moon three times - in May, August and October. The advantage of such an event is that we always know the position of the Mo ...
... In 1962 an opportunity arose for a much clearer determination of the position of one of these powerful but as yet unidentified sources, 3C273, when it would be eclipsed by the Moon three times - in May, August and October. The advantage of such an event is that we always know the position of the Mo ...
File
... structures called filaments. These filaments are the largest known structures in the universe. ...
... structures called filaments. These filaments are the largest known structures in the universe. ...
Redshift
In physics, redshift happens when light or other electromagnetic radiation from an object is increased in wavelength, or shifted to the red end of the spectrum. In general, whether or not the radiation is within the visible spectrum, ""redder"" means an increase in wavelength – equivalent to a lower frequency and a lower photon energy, in accordance with, respectively, the wave and quantum theories of light.Some redshifts are an example of the Doppler effect, familiar in the change of apparent pitches of sirens and frequency of the sound waves emitted by speeding vehicles. A redshift occurs whenever a light source moves away from an observer. Another kind of redshift is cosmological redshift, which is due to the expansion of the universe, and sufficiently distant light sources (generally more than a few million light years away) show redshift corresponding to the rate of increase in their distance from Earth. Finally, gravitational redshift is a relativistic effect observed in electromagnetic radiation moving out of gravitational fields. Conversely, a decrease in wavelength is called blueshift and is generally seen when a light-emitting object moves toward an observer or when electromagnetic radiation moves into a gravitational field. However, redshift is a more common term and sometimes blueshift is referred to as negative redshift.Knowledge of redshifts and blueshifts has been applied to develop several terrestrial technologies such as Doppler radar and radar guns. Redshifts are also seen in the spectroscopic observations of astronomical objects. Its value is represented by the letter z.A special relativistic redshift formula (and its classical approximation) can be used to calculate the redshift of a nearby object when spacetime is flat. However, in many contexts, such as black holes and Big Bang cosmology, redshifts must be calculated using general relativity. Special relativistic, gravitational, and cosmological redshifts can be understood under the umbrella of frame transformation laws. There exist other physical processes that can lead to a shift in the frequency of electromagnetic radiation, including scattering and optical effects; however, the resulting changes are distinguishable from true redshift and are not generally referred to as such (see section on physical optics and radiative transfer).