NIRCam for JWST: Your Next Near
... • NIRCam has been designed to be efficient for surveying through the use of dichroics • The requirement for NIRCam to be fully redundant for its wavefront sensing role means that twice the area can be observed at once • NIRCam’s expanded wavelength range as compared to HST’s combined with HST-like a ...
... • NIRCam has been designed to be efficient for surveying through the use of dichroics • The requirement for NIRCam to be fully redundant for its wavefront sensing role means that twice the area can be observed at once • NIRCam’s expanded wavelength range as compared to HST’s combined with HST-like a ...
Zinc and chromium abundances in a third
... The finding that the only two abundance measurements available at z < 1 are both well below solar – and quite typical of the sample at z > 1.5 – has caused concerns as to whether DLAs are really unbiased tracers of the chemical evolution history of the universe. Here we report measurements of the ab ...
... The finding that the only two abundance measurements available at z < 1 are both well below solar – and quite typical of the sample at z > 1.5 – has caused concerns as to whether DLAs are really unbiased tracers of the chemical evolution history of the universe. Here we report measurements of the ab ...
Evolutionary properties of galaxies and mass assembly up
... the LF shape at high redshift appears to be different from what is seen at low redshift. Is this difference due to an increase with cosmic time of the number of faint red galaxies, developing a steep slope of LF of early type galaxies in over-dense regions as in 2dF ? But : a) We do not see any chan ...
... the LF shape at high redshift appears to be different from what is seen at low redshift. Is this difference due to an increase with cosmic time of the number of faint red galaxies, developing a steep slope of LF of early type galaxies in over-dense regions as in 2dF ? But : a) We do not see any chan ...
Type Ia supernovae and the ESSENCE supernova survey
... equal to , indicating that Einstein (1917) might have been right after all. ...
... equal to , indicating that Einstein (1917) might have been right after all. ...
The Nature of Light
... determined by how many atoms have electrons at certain orbits, which is further determined by temperature, density, and abundance of the atoms and can be calculated in statistical physics. • Therefore, a given spectral line is formed at a certain temperature/density structure. • Spectral lines are ...
... determined by how many atoms have electrons at certain orbits, which is further determined by temperature, density, and abundance of the atoms and can be calculated in statistical physics. • Therefore, a given spectral line is formed at a certain temperature/density structure. • Spectral lines are ...
Discovery of radio afterglow from most distant cosmic explosion
... • We have detected the radio afterglow of GRB 090324 at z=8.3 • The best-fit broad-band afterglow model is a quasi-spherical (θj>12o), hyper-energetic (1052 erg) explosion in a constant, low density (n=1 cm-3) medium. • GRB 050904 (z=6.26) was also hyper-energetic but it exploded into a high density ...
... • We have detected the radio afterglow of GRB 090324 at z=8.3 • The best-fit broad-band afterglow model is a quasi-spherical (θj>12o), hyper-energetic (1052 erg) explosion in a constant, low density (n=1 cm-3) medium. • GRB 050904 (z=6.26) was also hyper-energetic but it exploded into a high density ...
Quasars - Ann Arbor Earth Science
... must be enormously bright to be visible at such a great distance Quasi-stellar object QSO or Quasar ...
... must be enormously bright to be visible at such a great distance Quasi-stellar object QSO or Quasar ...
slides - CAASTRO
... Distance to the Sun › The distance to the Sun can be measured using the transit of Venus › A transit is where the planet moves across the Sun › We can measure this at different places on Earth ...
... Distance to the Sun › The distance to the Sun can be measured using the transit of Venus › A transit is where the planet moves across the Sun › We can measure this at different places on Earth ...
Black Holes
... gravitationally redshifted to infinitely long wavelengths. Each photon would use all its energy trying to escape from the edge of the black hole. • What was once light would have no energy left by the time it reached the spaceship. • Theoretically, this radiation would still reach it, still moving a ...
... gravitationally redshifted to infinitely long wavelengths. Each photon would use all its energy trying to escape from the edge of the black hole. • What was once light would have no energy left by the time it reached the spaceship. • Theoretically, this radiation would still reach it, still moving a ...
WORD - UWL faculty websites
... Physical Science Workshop: Astronomy Applications of Light & Color ...
... Physical Science Workshop: Astronomy Applications of Light & Color ...
General relativistic cosmology
... motions, the expansion has no effect on comoving coordinate values, and the coordinate distances between particles are forever fixed. In other words, the coordinate system expands with space itself. Proper distance: The instantaneous (dt = 0) distance between any two points. The distance between any ...
... motions, the expansion has no effect on comoving coordinate values, and the coordinate distances between particles are forever fixed. In other words, the coordinate system expands with space itself. Proper distance: The instantaneous (dt = 0) distance between any two points. The distance between any ...
Herschel-ATLAS: SDSS cross-correlation induced by weak lensing
... We report a highly significant spatial correlation between galaxies with S350μm ≥30 mJy detected in the equatorial fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) with estimated redshift >1.5 and SDSS galaxies at 0.2 ≤ z ≤ 0.6. The significance of the cross-correlation is ...
... We report a highly significant spatial correlation between galaxies with S350μm ≥30 mJy detected in the equatorial fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) with estimated redshift >1.5 and SDSS galaxies at 0.2 ≤ z ≤ 0.6. The significance of the cross-correlation is ...
Spectroscopy PPT
... element has its own unique line spectrum, like a fingerprint) 2. Tells us if galaxies and stars are moving away from us or toward us (called?) ...
... element has its own unique line spectrum, like a fingerprint) 2. Tells us if galaxies and stars are moving away from us or toward us (called?) ...
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).