Cosmology
... expected that the night sky is bright, since one would always see a star in any direction • The resolution: the universe we can see is finite ...
... expected that the night sky is bright, since one would always see a star in any direction • The resolution: the universe we can see is finite ...
Galaxies
... • The motion of stars near the galactic center gives the mass of the galactic nucleus. • Infrared images of the stars show the motion. • The mass is 2.6 million (106) M. ...
... • The motion of stars near the galactic center gives the mass of the galactic nucleus. • Infrared images of the stars show the motion. • The mass is 2.6 million (106) M. ...
Answer Key: Big Bang Balloon Analysis Questions
... examples using the actual numbers from your data and explaining what they mean. 2. The dots farthest from the home dot appeared to move greater distances away from the home dot than the dots nearer to the home dot. ONCE AGAIN: CITE ACTUAL DATA! You should give several examples using the actual numbe ...
... examples using the actual numbers from your data and explaining what they mean. 2. The dots farthest from the home dot appeared to move greater distances away from the home dot than the dots nearer to the home dot. ONCE AGAIN: CITE ACTUAL DATA! You should give several examples using the actual numbe ...
Cosmology with objects from the Hamburg Quasar Surveys
... which accurate abundances can be obtained only with knowledge of the spectral energy distribution (SED) of the ionizing background. Consequently, one has to admit that the metallicity of the largest part of the baryons is at present not known. The direct measurement of the SED is possible only in ab ...
... which accurate abundances can be obtained only with knowledge of the spectral energy distribution (SED) of the ionizing background. Consequently, one has to admit that the metallicity of the largest part of the baryons is at present not known. The direct measurement of the SED is possible only in ab ...
Large-scale, Optical/Near-IR Galaxy Surveys with a 4
... From Asteroids to Cosmology” suggests, the SDSS has made important discoveries in nearly all fields of astrophysics. We expect that this survey/exoplanet telescope will too. Obvious applications besides galaxy evolution include: dark energy; the largescale structure of the universe; quasars, absorpt ...
... From Asteroids to Cosmology” suggests, the SDSS has made important discoveries in nearly all fields of astrophysics. We expect that this survey/exoplanet telescope will too. Obvious applications besides galaxy evolution include: dark energy; the largescale structure of the universe; quasars, absorpt ...
An introduce of the spectrograph of the GALEX
... imaging and grism surveys in two bands (1350-1750 and 1750-2750 Å). The surveys include an all-sky imaging survey (mAB~=20.5), a medium imaging survey of 1000 deg2 (mAB~=23), a deep imaging survey of 100 deg2 (mAB~=25), and a nearby galaxy survey. Spectroscopic (slitless) grism surveys (R=100-200) a ...
... imaging and grism surveys in two bands (1350-1750 and 1750-2750 Å). The surveys include an all-sky imaging survey (mAB~=20.5), a medium imaging survey of 1000 deg2 (mAB~=23), a deep imaging survey of 100 deg2 (mAB~=25), and a nearby galaxy survey. Spectroscopic (slitless) grism surveys (R=100-200) a ...
Electromagnetic Spectrum
... (numbered 1–4 in this diagram). Each observer experiences these light waves differently. ...
... (numbered 1–4 in this diagram). Each observer experiences these light waves differently. ...
Section 6 The Expanding Universe The Doppler Effect
... At the end of World War I the number of known galaxies in the universe totalled one: our own Milky Way. Everything that was observable was believed to be part of the Milky Way or unimportant puffs of gas at the periphery of the universe. Hubble was to demonstrate that there are many more galaxies. C ...
... At the end of World War I the number of known galaxies in the universe totalled one: our own Milky Way. Everything that was observable was believed to be part of the Milky Way or unimportant puffs of gas at the periphery of the universe. Hubble was to demonstrate that there are many more galaxies. C ...
Module 6
... emits a plane light wave along a path that forms an angle ’ with respect to the x’-axis. For an observer in frame S, the light source is moving at speed v as shown in Figure 6-1(b). The observer sees the light traveling in a direction that forms angle with respect to the x-axis. The two angles ar ...
... emits a plane light wave along a path that forms an angle ’ with respect to the x’-axis. For an observer in frame S, the light source is moving at speed v as shown in Figure 6-1(b). The observer sees the light traveling in a direction that forms angle with respect to the x-axis. The two angles ar ...
HST FRONTIER FIELDS PRELIMINARY MAP MODELING CATs
... Producing a magnification map involves solving the lens equation for light rays originating from distant sources and deflected by the massive foreground cluster. This is ultimately an inversion problem for which several sets of codes and approaches have been developed independently (see recent revie ...
... Producing a magnification map involves solving the lens equation for light rays originating from distant sources and deflected by the massive foreground cluster. This is ultimately an inversion problem for which several sets of codes and approaches have been developed independently (see recent revie ...
Observational Overview
... DISK – thin compared to the diameter, thickness = 0.3 kpc and diameter = 25 kpc. Contains all raw material for making stars (huge clouds of molecular hydrogen and dust (tiny particles made of carbon and silicate)) and all the young stars, including Sun which is 8 kpc from centre. BULGE – contains o ...
... DISK – thin compared to the diameter, thickness = 0.3 kpc and diameter = 25 kpc. Contains all raw material for making stars (huge clouds of molecular hydrogen and dust (tiny particles made of carbon and silicate)) and all the young stars, including Sun which is 8 kpc from centre. BULGE – contains o ...
10.1
... compressed. They are shifted more toward the violet end of the spectrum. If the star is moving away from you, there is a red shift, which means its wavelengths get longer. They are stretched out and shifted toward the red end of the spectrum. This red-shifting of wavelengths has been observed with m ...
... compressed. They are shifted more toward the violet end of the spectrum. If the star is moving away from you, there is a red shift, which means its wavelengths get longer. They are stretched out and shifted toward the red end of the spectrum. This red-shifting of wavelengths has been observed with m ...
Cosmology with the shear
... tures along the line of sight. Making use of the periodic boundary conditions of the simulation volume, we applied random rotations, translations, and parity flips to the matter distribution of each snapshot prior to the projection. For the ray-tracing, we assumed that light rays are only deflected ...
... tures along the line of sight. Making use of the periodic boundary conditions of the simulation volume, we applied random rotations, translations, and parity flips to the matter distribution of each snapshot prior to the projection. For the ray-tracing, we assumed that light rays are only deflected ...
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).