The Gravitational Microlensing Planet Search Technique from
... background imply significantly poorer photometric accuracy even for relatively uncrowded stars such as the example shown above. Nevertheless, there are some events for which the signals of Earth-mass planets are large enough to be detected. Our simulations of a survey from a 2.5m wide-field imaging ...
... background imply significantly poorer photometric accuracy even for relatively uncrowded stars such as the example shown above. Nevertheless, there are some events for which the signals of Earth-mass planets are large enough to be detected. Our simulations of a survey from a 2.5m wide-field imaging ...
ppt
... is shown through the form “body – field”, the content “interaction” and the dynamic characteristics “mass” with two different types, but it has the causality relation together: “gravitational mass” (M), or “interaction mass”, and “inertial mass” (m). • - Electron and positron are the fundamental par ...
... is shown through the form “body – field”, the content “interaction” and the dynamic characteristics “mass” with two different types, but it has the causality relation together: “gravitational mass” (M), or “interaction mass”, and “inertial mass” (m). • - Electron and positron are the fundamental par ...
Rich Clusters of Galaxies
... evolution. We can compare galaxy evolution in rich clusters with that in lowdensity environments. They provide constraints on the distribution and the amount of dark matter which is needed to bind the clusters. They also are important as gravitational telescopes because of their lensing effect on mu ...
... evolution. We can compare galaxy evolution in rich clusters with that in lowdensity environments. They provide constraints on the distribution and the amount of dark matter which is needed to bind the clusters. They also are important as gravitational telescopes because of their lensing effect on mu ...
Ten Years Of XMM-Newton: Scientific Achievements And Future Prospects Norbert Schartel
... galaxy evolution Targets an unexplored discovery space Pathfinder for future X-ray missions. ...
... galaxy evolution Targets an unexplored discovery space Pathfinder for future X-ray missions. ...
First Light: Physical Characterization of Early Star Formation in the
... We will use JWST, which excels at stable, deep near-infrared imaging, to measure photometric ages and abundances of stars in the low surface brightness halos of spiral and elliptical galaxies and in dwarfs. Such halos are thought to harbor some of the earliest stellar generations, yet also contain t ...
... We will use JWST, which excels at stable, deep near-infrared imaging, to measure photometric ages and abundances of stars in the low surface brightness halos of spiral and elliptical galaxies and in dwarfs. Such halos are thought to harbor some of the earliest stellar generations, yet also contain t ...
UMich w/s
... (Diemand et al. 04) Need different technique at large radii, e.g. full velocity distribution function modelling.. And understand tides. ...
... (Diemand et al. 04) Need different technique at large radii, e.g. full velocity distribution function modelling.. And understand tides. ...
Large-scale, Optical/Near-IR Galaxy Surveys with a 4
... distribution of an L* galaxy (Re~2-4 kpc) can be mapped in detail. The spectrograph will consists of ~10 multi-object spectrographs each having a digital micro-mirror device (DMD) to isolate galaxies for spectroscopy, and each DMD consisting of a 2Kx1K array of 0.25x0.25 micromirrors. The spectr ...
... distribution of an L* galaxy (Re~2-4 kpc) can be mapped in detail. The spectrograph will consists of ~10 multi-object spectrographs each having a digital micro-mirror device (DMD) to isolate galaxies for spectroscopy, and each DMD consisting of a 2Kx1K array of 0.25x0.25 micromirrors. The spectr ...
v1 - ESO
... In 1936 Edwin Hubble presented his tuning fork diagram classifying the different types of galaxy to be found in the Universe. This was the first attempt to find a pattern in the properties of different systems and thus search for a common evolutionary link. Elliptical galaxies appear to be shaped pr ...
... In 1936 Edwin Hubble presented his tuning fork diagram classifying the different types of galaxy to be found in the Universe. This was the first attempt to find a pattern in the properties of different systems and thus search for a common evolutionary link. Elliptical galaxies appear to be shaped pr ...
Evidence for strong evolution in galaxy environmental quenching
... blue. At all redshifts, the passive fraction in clusters is higher than in the field. The passive fraction nearly doubles from z ∼ 1.6 to z ∼ 1.3, jumping from 42% to over 80%, but changes little between z ∼ 1.3 and z . 1. The lower two redshift ranges have passive fractions consistent with the z = ...
... blue. At all redshifts, the passive fraction in clusters is higher than in the field. The passive fraction nearly doubles from z ∼ 1.6 to z ∼ 1.3, jumping from 42% to over 80%, but changes little between z ∼ 1.3 and z . 1. The lower two redshift ranges have passive fractions consistent with the z = ...
Other galaxies, the expansion of the universe
... the Coma cluster must contain much more mass than could be identified in stars and gas. He attributed this to some form of mysterious dark matter. Other astronomers ignored these findings until the 1970's when Vera Rubin found evidence for dark matter in many individual galaxies. ...
... the Coma cluster must contain much more mass than could be identified in stars and gas. He attributed this to some form of mysterious dark matter. Other astronomers ignored these findings until the 1970's when Vera Rubin found evidence for dark matter in many individual galaxies. ...
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.