The Large Synoptic Survey Telescope
... Gamma Ray Bursts and transients to high redshift Gravitational micro-lensing Strong galaxy & cluster lensing: physics of dark matter Multi-image lensed SN time delays: separate test of cosmology Variable stars/galaxies: black hole accretion QSO time delays vs z: independent test of dark energy Optic ...
... Gamma Ray Bursts and transients to high redshift Gravitational micro-lensing Strong galaxy & cluster lensing: physics of dark matter Multi-image lensed SN time delays: separate test of cosmology Variable stars/galaxies: black hole accretion QSO time delays vs z: independent test of dark energy Optic ...
Media Alert A new spin on star-forming galaxies
... A new spin on star-forming galaxies Australian researchers have discovered why some galaxies are “clumpy” rather than spiral in shape—and it appears low spin is to blame. The finding challenges an earlier theory that high levels of gas cause clumpy galaxies and sheds light on the conditions that bro ...
... A new spin on star-forming galaxies Australian researchers have discovered why some galaxies are “clumpy” rather than spiral in shape—and it appears low spin is to blame. The finding challenges an earlier theory that high levels of gas cause clumpy galaxies and sheds light on the conditions that bro ...
Weighing Ultracompact Dwarf Galaxies in the Fornax Cluster
... 2006). Results for the dwarf elliptical nucleus (FCC303) and a fifth UCD in Fornax (Drinkwater et al. 2003) are also shown in this figure. The difference between assuming a Kroupa or Salpeter IMF is that a Salpeter IMF implies that two of five Fornax UCDs would be dominated by intermediate-age popul ...
... 2006). Results for the dwarf elliptical nucleus (FCC303) and a fifth UCD in Fornax (Drinkwater et al. 2003) are also shown in this figure. The difference between assuming a Kroupa or Salpeter IMF is that a Salpeter IMF implies that two of five Fornax UCDs would be dominated by intermediate-age popul ...
PPT
... * HOD modeling helps to study galaxy evolution. * It is useful to separate central and satellite galaxies. * HODs inferred from the data have a general agreement with those predicted by galaxy formation models. ...
... * HOD modeling helps to study galaxy evolution. * It is useful to separate central and satellite galaxies. * HODs inferred from the data have a general agreement with those predicted by galaxy formation models. ...
Mobasher
... Post-starburst galaxies (age 0.2–1.0 Gyr) Elliptical (age > 3 Gyr) Dusty starburst galaxies ...
... Post-starburst galaxies (age 0.2–1.0 Gyr) Elliptical (age > 3 Gyr) Dusty starburst galaxies ...
Astronomy HOMEWORK Chapter 15 1. Where in the Galaxy is the
... Shapley noted that most globular clusters were in just a few contellations around Sagittarius. He obtained distances by the apparent brightness of RR Lyrae variables (similar to Cepheid variables) and plotted the positions of these globular clusters. They formed a spherical distribution about a poin ...
... Shapley noted that most globular clusters were in just a few contellations around Sagittarius. He obtained distances by the apparent brightness of RR Lyrae variables (similar to Cepheid variables) and plotted the positions of these globular clusters. They formed a spherical distribution about a poin ...
27DarkMatter
... • Since there are lots of stars in a galaxy, we can measure the orbital speed at lots of different distances from the center of the galaxy: you can actually measure speed of gas even farther out, beyond the stars • A given object is pulled by all of the mass that exists inside of its orbit • Since m ...
... • Since there are lots of stars in a galaxy, we can measure the orbital speed at lots of different distances from the center of the galaxy: you can actually measure speed of gas even farther out, beyond the stars • A given object is pulled by all of the mass that exists inside of its orbit • Since m ...
The Milky Way Galaxy
... Your book gives estimates of the mass of the Galaxy from 1 to 4 X 1011 solar masses. A more recent determination of the mass of the Galaxy is even larger, 1.5-4.0 X 1012 solar masses. This is on the basis of stars of known absolute magnitude called horizontal branch stars. An analysis of 1000 of th ...
... Your book gives estimates of the mass of the Galaxy from 1 to 4 X 1011 solar masses. A more recent determination of the mass of the Galaxy is even larger, 1.5-4.0 X 1012 solar masses. This is on the basis of stars of known absolute magnitude called horizontal branch stars. An analysis of 1000 of th ...
Supermassive black hole activity in local field early
... 6/100 show both a nuclear X-ray source and a star cluster After accounting for LMXB contamination: 24-34% of the galaxies host an active super- massive black hole (95% C.L.) Next: ACTIVE FRACTION as a function of host stellar mass and ...
... 6/100 show both a nuclear X-ray source and a star cluster After accounting for LMXB contamination: 24-34% of the galaxies host an active super- massive black hole (95% C.L.) Next: ACTIVE FRACTION as a function of host stellar mass and ...
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.