van der Wel et al., 2004, ApJ, 602, L5 - ST-ECF
... selection effects. The last authors found that galaxies with residuals from the r 1/4 profile had young ages. However, we find no such relation in our sample. Stellar population models indicate that the low M/L of the blue z ≈ 1 galaxies may be due to an age difference of a factor of 3. Alternativel ...
... selection effects. The last authors found that galaxies with residuals from the r 1/4 profile had young ages. However, we find no such relation in our sample. Stellar population models indicate that the low M/L of the blue z ≈ 1 galaxies may be due to an age difference of a factor of 3. Alternativel ...
The age of elliptical galaxies and bulges in a merger model The age
... 3 illustrates the epoch at which elliptical galaxies typically underwent their last major merging event. As can be seen, most ellipticals were formed by a merger that occurred between 5 and 10 Gyr ago. It is also apparent from this diagram that a substantial fraction of the stars in an elliptical ga ...
... 3 illustrates the epoch at which elliptical galaxies typically underwent their last major merging event. As can be seen, most ellipticals were formed by a merger that occurred between 5 and 10 Gyr ago. It is also apparent from this diagram that a substantial fraction of the stars in an elliptical ga ...
REVIEW Early star-forming galaxies and the reionization of the Universe
... medium (IGM), into an ionized state. Neutral hydrogen first formed 370,000 years after the Big Bang and released the radiation presently observed as the cosmic microwave background (CMB)1. Initially devoid of sources of light, the Universe then entered a period termed the ‘Dark Ages’2, which lasted ...
... medium (IGM), into an ionized state. Neutral hydrogen first formed 370,000 years after the Big Bang and released the radiation presently observed as the cosmic microwave background (CMB)1. Initially devoid of sources of light, the Universe then entered a period termed the ‘Dark Ages’2, which lasted ...
On Wave Dark Matter, Shells in Elliptical Galaxies, and the Axioms
... harmonic perturbations from spherically symmetric scalar field solutions to the Klein-Gordon equation. It is more typical for the Klein-Gordon equation to describe a complex scalar field f . If one is willing to allow the connection coefficients Γijk to be complex valued, then complex valued f are n ...
... harmonic perturbations from spherically symmetric scalar field solutions to the Klein-Gordon equation. It is more typical for the Klein-Gordon equation to describe a complex scalar field f . If one is willing to allow the connection coefficients Γijk to be complex valued, then complex valued f are n ...
Cosmic Sculpture: A new way to visualise the Cosmic Microwave
... internal grid making the final plastic printed models less breakable. The eventual result of this process is a GCode file which can be input to the Ultimaker. Figure 3 shows an Ultimaker printer in the process of printing our 3D representation of the CMB, complete with Cura-generated support structu ...
... internal grid making the final plastic printed models less breakable. The eventual result of this process is a GCode file which can be input to the Ultimaker. Figure 3 shows an Ultimaker printer in the process of printing our 3D representation of the CMB, complete with Cura-generated support structu ...
Inflationary Cosmology
... wall collisions make the universe extremely inhomogeneous. If they are formed far away from each other, which is the case if the probability of their formation is small and inflation is long, each of these bubbles represents a separate open universe with a vanishingly small Ω. Both options are unac ...
... wall collisions make the universe extremely inhomogeneous. If they are formed far away from each other, which is the case if the probability of their formation is small and inflation is long, each of these bubbles represents a separate open universe with a vanishingly small Ω. Both options are unac ...
Direct Detection of Classically Undetectable Dark
... many dark matter models (e.g. WIMPs) Dark matter particle was in thermal equilibrium with rest of universe at early cosmological times As universe expands, density of dark matter drops low enough that interactions become rare Dark matter streams around and clumps into galaxies today ...
... many dark matter models (e.g. WIMPs) Dark matter particle was in thermal equilibrium with rest of universe at early cosmological times As universe expands, density of dark matter drops low enough that interactions become rare Dark matter streams around and clumps into galaxies today ...
The Interstellar Medium in High Redshift Galaxies Comes of Age
... molecular interstellar medium in high redshift galaxies, the past years have brought great advances in our understanding of the actual physical properties of the gas, which set the conditions for star formation. Observations of the ground-state CO J = 1−0 line have furnished crucial information on t ...
... molecular interstellar medium in high redshift galaxies, the past years have brought great advances in our understanding of the actual physical properties of the gas, which set the conditions for star formation. Observations of the ground-state CO J = 1−0 line have furnished crucial information on t ...
Lecture 12: Galaxy Evolution
... Dwarf galaxies • Dwarf galaxies are a crucial part of the galaxy evolution puzzle but we know very little about them. • Main theory (see later) proposes that galaxies built-up from smaller units through repeated merging. • Numerical simulations typically predict several thousand dark matter haloe ...
... Dwarf galaxies • Dwarf galaxies are a crucial part of the galaxy evolution puzzle but we know very little about them. • Main theory (see later) proposes that galaxies built-up from smaller units through repeated merging. • Numerical simulations typically predict several thousand dark matter haloe ...
Teaching Tips Table of Contents - Hubble Deep Field
... Grade levels / Target audience........................................................................................ 1 Subjects ........................................................................................................................... 1 Concepts ................................... ...
... Grade levels / Target audience........................................................................................ 1 Subjects ........................................................................................................................... 1 Concepts ................................... ...
The nature of the ultraluminous X-ray sources inside galaxies and
... In the cases in which QSOs have been found to be clustered about active galaxies the scale of the clustering is ∼50 −500 . Thus it is clear that there will be an effect that must be taken into account, associated with the fact that since there is a considerable range in the distances of the parent g ...
... In the cases in which QSOs have been found to be clustered about active galaxies the scale of the clustering is ∼50 −500 . Thus it is clear that there will be an effect that must be taken into account, associated with the fact that since there is a considerable range in the distances of the parent g ...
the origin of the hubble sequence - Yale Astronomy
... 4. The Cosmological Context of Galaxy Formation Most of the calculations mentioned above have adopted simple and idealized initial conditions for protogalaxies, but there has been much progress in recent years in understanding the structure and evolution of the universe and the likely initial condit ...
... 4. The Cosmological Context of Galaxy Formation Most of the calculations mentioned above have adopted simple and idealized initial conditions for protogalaxies, but there has been much progress in recent years in understanding the structure and evolution of the universe and the likely initial condit ...
OLIMPO
... • We have selected 40 nearby rich clusters to be measured in a single long duration flight. • For all these clusters high quality data are available from XMM/Chandra ...
... • We have selected 40 nearby rich clusters to be measured in a single long duration flight. • For all these clusters high quality data are available from XMM/Chandra ...
Galaxies
... The galaxies within a typical cluster are bunched together fairly tightly. The distance between adjacent galaxies in a given cluster averages a few hundred thousand parsecs, which is only about 10 times greater than the size of a typical galaxy. Galaxies simply do not have that much room to roam a ...
... The galaxies within a typical cluster are bunched together fairly tightly. The distance between adjacent galaxies in a given cluster averages a few hundred thousand parsecs, which is only about 10 times greater than the size of a typical galaxy. Galaxies simply do not have that much room to roam a ...
13 Galaxies - Journigan-wiki
... number of faint, diffuse patches of light. To avoid confusing them with comets in the future he began to assign them numbers. Galaxies are still referred to by their “M” or Messier number. ...
... number of faint, diffuse patches of light. To avoid confusing them with comets in the future he began to assign them numbers. Galaxies are still referred to by their “M” or Messier number. ...
Sunday, March 24, 2013
... an accurate understanding of the distance scale from which many other cosmic parameters depend. The amount of energy we detect at the Earth emitted by an object is dependent on its intrinsic luminosity and the distance. This is critical to understanding other aspects of the phenomenon. While the Hub ...
... an accurate understanding of the distance scale from which many other cosmic parameters depend. The amount of energy we detect at the Earth emitted by an object is dependent on its intrinsic luminosity and the distance. This is critical to understanding other aspects of the phenomenon. While the Hub ...
1 - Philosophy, Theology, History, Science, Big Questions
... background information includes the information that there is only one universe, the claim that this universe is life-permitting, where this is an indexical that picks out the one universe that actually exists. When I speak of the “fine-tuning evidence (data),”or “the evidence (data) of finetuning,” ...
... background information includes the information that there is only one universe, the claim that this universe is life-permitting, where this is an indexical that picks out the one universe that actually exists. When I speak of the “fine-tuning evidence (data),”or “the evidence (data) of finetuning,” ...
Chapter 1
... ratios are higher than a cooler nebula. This is because to produce [O iii] λ4363 an electron needs to be excited to 5.3 eV, which requires more energy than for 4959/5007 which result from decay from 1 D2 level, 2.5 eV above the ground-state (see Figure 2.2). Therefore, these ratios can be used to co ...
... ratios are higher than a cooler nebula. This is because to produce [O iii] λ4363 an electron needs to be excited to 5.3 eV, which requires more energy than for 4959/5007 which result from decay from 1 D2 level, 2.5 eV above the ground-state (see Figure 2.2). Therefore, these ratios can be used to co ...
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 ...
Background Information on Galaxy Classification
... probably so many dwarf galaxies that their combined mass probably exceeds that of all the larger galaxies taken together. But their small size and dimness make them hard to detect and we have only been able to discover them when they are relatively nearby. Hubble based his classification scheme sole ...
... probably so many dwarf galaxies that their combined mass probably exceeds that of all the larger galaxies taken together. But their small size and dimness make them hard to detect and we have only been able to discover them when they are relatively nearby. Hubble based his classification scheme sole ...
PPT
... •The distance to NGC is 80 million light years, which Mkn 205 is 14 times farther away at a distance of 1 billion light year. •The very distant quasar is nearly as bright as the much closer galaxy. The extraordinary brightness of quasars, which is a blending of the term quasi-stellar radio source, i ...
... •The distance to NGC is 80 million light years, which Mkn 205 is 14 times farther away at a distance of 1 billion light year. •The very distant quasar is nearly as bright as the much closer galaxy. The extraordinary brightness of quasars, which is a blending of the term quasi-stellar radio source, i ...
POLITECNICO DI TORINO Invariance Principles and Extended
... n-dimensional manifold is given in the Chapter 4. We show that such deformations can be regarded as extended conformal transformations. In particular, their features can be related to the perturbation theory giving a natural picture by which gravitational waves are described by small deformations of ...
... n-dimensional manifold is given in the Chapter 4. We show that such deformations can be regarded as extended conformal transformations. In particular, their features can be related to the perturbation theory giving a natural picture by which gravitational waves are described by small deformations of ...
150 Million ly - Northern Michigan University
... http://www.nasa.gov/press/2014/january/nasa-and-esa-space-telescopeshelp-solve-mystery-of-ultra-compact-burned-out/#.U0fwLFcXKSo ...
... http://www.nasa.gov/press/2014/january/nasa-and-esa-space-telescopeshelp-solve-mystery-of-ultra-compact-burned-out/#.U0fwLFcXKSo ...
Big Bang
The Big Bang theory is the prevailing cosmological model for the universe from the earliest known periods through its subsequent large-scale evolution. The model accounts for the fact that the universe expanded from a very high density and high temperature state, and offers a comprehensive explanation for a broad range of observed phenomena, including the abundance of light elements, the cosmic microwave background, large scale structure, and Hubble's Law. If the known laws of physics are extrapolated beyond where they are valid, there is a singularity. Modern measurements place this moment at approximately 13.8 billion years ago, which is thus considered the age of the universe. After the initial expansion, the universe cooled sufficiently to allow the formation of subatomic particles, and later simple atoms. Giant clouds of these primordial elements later coalesced through gravity to form stars and galaxies.Since Georges Lemaître first noted, in 1927, that an expanding universe might be traced back in time to an originating single point, scientists have built on his idea of cosmic expansion. While the scientific community was once divided between supporters of two different expanding universe theories, the Big Bang and the Steady State theory, accumulated empirical evidence provides strong support for the former. In 1929, from analysis of galactic redshifts, Edwin Hubble concluded that galaxies are drifting apart, important observational evidence consistent with the hypothesis of an expanding universe. In 1965, the cosmic microwave background radiation was discovered, which was crucial evidence in favor of the Big Bang model, since that theory predicted the existence of background radiation throughout the universe before it was discovered. More recently, measurements of the redshifts of supernovae indicate that the expansion of the universe is accelerating, an observation attributed to dark energy's existence. The known physical laws of nature can be used to calculate the characteristics of the universe in detail back in time to an initial state of extreme density and temperature.