Abell 1656: the Coma Cluster of galaxies - Euro-VO
... We can clearly see two lines: one around 1250 Å and one around 1350 Å. We will now check that these are consistent one with the hydrogen line Ly-α at rest, and the other at a velocity beyond that of the Coma cluster. Select the tab. Choose the Full NIST database in the Template section. Unselect al ...
... We can clearly see two lines: one around 1250 Å and one around 1350 Å. We will now check that these are consistent one with the hydrogen line Ly-α at rest, and the other at a velocity beyond that of the Coma cluster. Select the tab. Choose the Full NIST database in the Template section. Unselect al ...
Jeans Length
... N molecules of mass m in box of size L at temp T. • Gravitational Energy: EG ~ G M M L ...
... N molecules of mass m in box of size L at temp T. • Gravitational Energy: EG ~ G M M L ...
MACHOs
... magnification was just starting to show a change but using the value for the maximum magnification A – that’s not true because the max magnification is the peak, not at the bottom of the curve where the magnification is just starting – therefore the value for magnification does not correspond to the ...
... magnification was just starting to show a change but using the value for the maximum magnification A – that’s not true because the max magnification is the peak, not at the bottom of the curve where the magnification is just starting – therefore the value for magnification does not correspond to the ...
Manuscript - Kapteyn Astronomical Institute
... galaxies are thicker than those of larger systems, we have compiled measurements of the thickness of stellar disks (quantified by the apparent axis ratio, b/a) for a wide range of galaxy masses. Although the observed b/a is not a measurement of the intrinsic shape of the disk, if one assumes random ...
... galaxies are thicker than those of larger systems, we have compiled measurements of the thickness of stellar disks (quantified by the apparent axis ratio, b/a) for a wide range of galaxy masses. Although the observed b/a is not a measurement of the intrinsic shape of the disk, if one assumes random ...
spiral galaxies
... much empty space between stars that it’s unlikely two stars would smash together. And though the sun and all its orbiting planets, including Earth, will probably end up in a new position, they won’t be destroyed. Eventually the galactic centers, each of which likely contains a super massive black ho ...
... much empty space between stars that it’s unlikely two stars would smash together. And though the sun and all its orbiting planets, including Earth, will probably end up in a new position, they won’t be destroyed. Eventually the galactic centers, each of which likely contains a super massive black ho ...
HEIC0007 Photo release: Stephan`s Quintet
... observations revealed that all but one of the galaxies are receding from Earth at about the same velocity (~6000 km/s). The discordant galaxy (NGC 7320 seen in the bottom of the Hubble image) is receding much less rapidly (~800 km/s). Some astronomers saw this as evidence that redshift is unrelated ...
... observations revealed that all but one of the galaxies are receding from Earth at about the same velocity (~6000 km/s). The discordant galaxy (NGC 7320 seen in the bottom of the Hubble image) is receding much less rapidly (~800 km/s). Some astronomers saw this as evidence that redshift is unrelated ...
Cluster Analysis of Massive Datasets in Astronomy 1 Introduction
... where t(i) ’s are equally spaced grid points which belong to Sbc , km is the total number of the grid points belonging to Sbc and m is the grid size. For the choice of the number of grid points, Wand (1994) provided some guideline for the multivariate case. For two dimensional case, table 1 in Wand ...
... where t(i) ’s are equally spaced grid points which belong to Sbc , km is the total number of the grid points belonging to Sbc and m is the grid size. For the choice of the number of grid points, Wand (1994) provided some guideline for the multivariate case. For two dimensional case, table 1 in Wand ...
The Universe
... older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) that indicates the degree of tightness of the spiral arms and the size of the central bulge. An Sa galaxy has tightly ...
... older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) that indicates the degree of tightness of the spiral arms and the size of the central bulge. An Sa galaxy has tightly ...
The Universe
... older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) that indicates the degree of tightness of the spiral arms and the size of the central bulge. An Sa galaxy has tightly ...
... older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) that indicates the degree of tightness of the spiral arms and the size of the central bulge. An Sa galaxy has tightly ...
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.