IFU observations of the high-z Universe
... • The correlation of Ly-alpha emitters with the distribution of intergalactic gas provides another route to observationally constrain feedback • Based on Adelberger et al (2003) who find that the mean transmission increases close to a QSO – This result is derived from 3 Ly- sources only ...
... • The correlation of Ly-alpha emitters with the distribution of intergalactic gas provides another route to observationally constrain feedback • Based on Adelberger et al (2003) who find that the mean transmission increases close to a QSO – This result is derived from 3 Ly- sources only ...
HST Observations of the
... because it did not become obstructed during orbit by the Earth or Moon and it is also relatively free of foreground stars and other galaxy clusters images of the region were taken using ultraviolet, optical and infrared ...
... because it did not become obstructed during orbit by the Earth or Moon and it is also relatively free of foreground stars and other galaxy clusters images of the region were taken using ultraviolet, optical and infrared ...
Dark Matter Mathematics
... BUT . . . Velocities do not drop off Result: Dark Matter mass is about 10x Luminous Matter mass ...
... BUT . . . Velocities do not drop off Result: Dark Matter mass is about 10x Luminous Matter mass ...
ppt
... Ho / Da comparison vs cosmology Use the joint data sets to get insights into the evolution of the ICM physics • S-Z integrated pressure along the line of sight • X L-T (z) relation ...
... Ho / Da comparison vs cosmology Use the joint data sets to get insights into the evolution of the ICM physics • S-Z integrated pressure along the line of sight • X L-T (z) relation ...
pdf format
... distant parts of the Milky Way and we find that they are moving faster than the Sun, so that their orbital periods are all about the same as the Sun, what does this tell us about the total mass of the Galaxy? Hint in the solar system the more distant planets orbit much more slowly. MGalaxy + Msun = ...
... distant parts of the Milky Way and we find that they are moving faster than the Sun, so that their orbital periods are all about the same as the Sun, what does this tell us about the total mass of the Galaxy? Hint in the solar system the more distant planets orbit much more slowly. MGalaxy + Msun = ...
AY5 Homework for Quiz 3: Spring 2015
... The flat rotation curve for orbits of stars at the Sun and beyond (in radius from the center of the Galaxy) requires much more mass in the galaxy than can be accounted for in identified stars ...
... The flat rotation curve for orbits of stars at the Sun and beyond (in radius from the center of the Galaxy) requires much more mass in the galaxy than can be accounted for in identified stars ...
DM in the Galaxy - University of Oxford
... • Need also dº/dr for population • Wilkinson & Evans (99): ...
... • Need also dº/dr for population • Wilkinson & Evans (99): ...
The initial conditions and the large
... Gaussian vs Non-Gaussian information The two distributions can be distinguished easily by higher-order correlations! ...
... Gaussian vs Non-Gaussian information The two distributions can be distinguished easily by higher-order correlations! ...
A dearth of dark matter in strong gravitational lenses
... An unavoidable prediction of MOND is that in high surface brightness systems, such as luminous elliptical galaxies, there should be little discrepancy between the detectable baryonic mass and the Newtonian dynamical mass within the bright luminous object. In other words, with the traditional Newtoni ...
... An unavoidable prediction of MOND is that in high surface brightness systems, such as luminous elliptical galaxies, there should be little discrepancy between the detectable baryonic mass and the Newtonian dynamical mass within the bright luminous object. In other words, with the traditional Newtoni ...
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.