Power Point
... telescope (nearby this not the case – one has to target individual galaxies in clusters one by one) • around a cluster there are many more galaxies that lie within a single telescope pointing than for a typical field pointing ...
... telescope (nearby this not the case – one has to target individual galaxies in clusters one by one) • around a cluster there are many more galaxies that lie within a single telescope pointing than for a typical field pointing ...
The End of the Dark Ages
... structure formation based on CDM scenarios predict that the first objects in principle able to make stars should form at redshift z ≈ 30 and have a total mass M ≈ 106 M¯ or baryonic mass Mb ≈ 105 M¯ (usually referred to as minihalos. This conclusion is reached by requiring that the cooling time, tc ...
... structure formation based on CDM scenarios predict that the first objects in principle able to make stars should form at redshift z ≈ 30 and have a total mass M ≈ 106 M¯ or baryonic mass Mb ≈ 105 M¯ (usually referred to as minihalos. This conclusion is reached by requiring that the cooling time, tc ...
PoS(AASKA14)174 - Proceeding of science
... fields on the largest scales. Current theories fall short of explaining the observed field strengths by factors of a million or more. The only way to solve this puzzle is with a much better sampling of our magnetic environment, so that the sources of magnetic enrichment become apparent as well as th ...
... fields on the largest scales. Current theories fall short of explaining the observed field strengths by factors of a million or more. The only way to solve this puzzle is with a much better sampling of our magnetic environment, so that the sources of magnetic enrichment become apparent as well as th ...
PowerPoint Presentation - 21. Galaxy Evolution
... • What do we mean by galaxy evolution and how do we study it? ...
... • What do we mean by galaxy evolution and how do we study it? ...
Red Supergiants as Cosmic Abundance Probes
... that one must attempt to derive abundances based on only the strong emission lines (e.g., [O III] 500.7 nm), which contain no temperature information on their own, by calibrating against either results from the direct method or from photoionisation models. The limitation of these strongline methods ...
... that one must attempt to derive abundances based on only the strong emission lines (e.g., [O III] 500.7 nm), which contain no temperature information on their own, by calibrating against either results from the direct method or from photoionisation models. The limitation of these strongline methods ...
Chapter15 (with interactive links)
... Composition & Age: Heavy Elements in Stars We observe younger stars to have more heavy elements than older stars. Residing in the disk of our galaxy, the Sun has about a 2% concentration of heavy elements, a relatively high amount. Even globular cluster stars have a small amount of heavy elem ...
... Composition & Age: Heavy Elements in Stars We observe younger stars to have more heavy elements than older stars. Residing in the disk of our galaxy, the Sun has about a 2% concentration of heavy elements, a relatively high amount. Even globular cluster stars have a small amount of heavy elem ...
Probing Gravity with Observations of the Cosmic Microwave Background Sarah Church Stanford University
... ∆T large (maximal compression) ∆T intermediate ∆T small (maximal rarefaction ...
... ∆T large (maximal compression) ∆T intermediate ∆T small (maximal rarefaction ...
Weak gravitational lensing
While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.