The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... lected from Steidel et al. (2003, 2004). For this paper, 41 BM/BX galaxies to KAB = 23 are selected from their sample with spectroscopic redshift z > 1.4. Galaxies analogous to the LBGs at 0.6 ≤ z ≤ 1.4 (hereafter GALEX/LBGs) are selected with the GALEX/HST (F U V − N U V )AB versus (N U V − F 435W ...
... lected from Steidel et al. (2003, 2004). For this paper, 41 BM/BX galaxies to KAB = 23 are selected from their sample with spectroscopic redshift z > 1.4. Galaxies analogous to the LBGs at 0.6 ≤ z ≤ 1.4 (hereafter GALEX/LBGs) are selected with the GALEX/HST (F U V − N U V )AB versus (N U V − F 435W ...
A new view of galaxy evolution
... a filter just a bit bluer. This is the These galaxies are very bright and thus traditional way to find distant galaxies easy to see because they are undergoing intense and is being used today to find the most distant star formation, a common process in the early galaxies in the universe. universe. H ...
... a filter just a bit bluer. This is the These galaxies are very bright and thus traditional way to find distant galaxies easy to see because they are undergoing intense and is being used today to find the most distant star formation, a common process in the early galaxies in the universe. universe. H ...
Chapter 24
... many millions of galaxies. We begin our study of these enormous accumulations of matter simply by considering their appearance on the sky. Seen through even a small telescope, images of galaxies look distinctly nonstellar. They have fuzzy edges, and many are quite elongated—not at all like the sharp ...
... many millions of galaxies. We begin our study of these enormous accumulations of matter simply by considering their appearance on the sky. Seen through even a small telescope, images of galaxies look distinctly nonstellar. They have fuzzy edges, and many are quite elongated—not at all like the sharp ...
Galaxies
... However, at a fundamental level we still lack a solid understanding of the basic physics of galaxy evolution. We do not know for certain that all galaxies form at peaks in the dark matter density distribution. There is considerable debate about cold versus hot accretion of gas onto dark matter halos ...
... However, at a fundamental level we still lack a solid understanding of the basic physics of galaxy evolution. We do not know for certain that all galaxies form at peaks in the dark matter density distribution. There is considerable debate about cold versus hot accretion of gas onto dark matter halos ...
Dust in the Circumgalactic Medium of Low
... of reddening due to dust in the circumgalactic medium of galaxies. We detect the mean change in the colors of “standard crayons” correlated with the presence of foreground galaxies at z ∼ 0.05 as a function of angular separation. Following Peek & Graves (2010), we create standard crayons using passi ...
... of reddening due to dust in the circumgalactic medium of galaxies. We detect the mean change in the colors of “standard crayons” correlated with the presence of foreground galaxies at z ∼ 0.05 as a function of angular separation. Following Peek & Graves (2010), we create standard crayons using passi ...
The type Ia supernova 1994D in NGC 4526: the early phases The
... of opportunity at ESO. In this paper, we present and discuss the UBVRI photometry and the spectra collected during this campaign from 11 days before maximum to about two months afterwards. Several absorption components of the Na I D lines arising in our Galaxy, in NGC 4526 and in high-velocity cloud ...
... of opportunity at ESO. In this paper, we present and discuss the UBVRI photometry and the spectra collected during this campaign from 11 days before maximum to about two months afterwards. Several absorption components of the Na I D lines arising in our Galaxy, in NGC 4526 and in high-velocity cloud ...
The science case for - Astrophysics
... ever formed? By discovering and analysing distant galaxies, gas clouds, and supernovae, the history of star formation, and the creation history of the chemical elements can be quantified. What were the first objects? Were stars the first objects to form? Were the first stars the source of the ultrav ...
... ever formed? By discovering and analysing distant galaxies, gas clouds, and supernovae, the history of star formation, and the creation history of the chemical elements can be quantified. What were the first objects? Were stars the first objects to form? Were the first stars the source of the ultrav ...
Clusters as laboratories for the study of galaxy evolution
... “On the evolutionary status of early-type galaxies in clusters at z ~ 0.2 I. The Fundamental Plane” – Fritz et al. 2005 MNRAS, 358, 233 Photometry, morphology, and spectra for galaxies in A2390 & A2218 “For the total sample of 34 E+S0 cluster galaxies which enter the FP we deduce only a mild evolut ...
... “On the evolutionary status of early-type galaxies in clusters at z ~ 0.2 I. The Fundamental Plane” – Fritz et al. 2005 MNRAS, 358, 233 Photometry, morphology, and spectra for galaxies in A2390 & A2218 “For the total sample of 34 E+S0 cluster galaxies which enter the FP we deduce only a mild evolut ...
3 science case - Giant Magellan Telescope Organization
... study, astronomers can rarely carry out the controlled experiments that are the hallmark of the scientific method. Progress in our understanding of the cosmos often proceeds from the discovery of new classes of objects or phenomena to the painstaking confrontation between observation and theory. Ast ...
... study, astronomers can rarely carry out the controlled experiments that are the hallmark of the scientific method. Progress in our understanding of the cosmos often proceeds from the discovery of new classes of objects or phenomena to the painstaking confrontation between observation and theory. Ast ...
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).