Download Where is the rest of the universe?

Where is the rest of the Universe?
If we can only “see” 4.9% of the universe, where is the other 95%?
Dark matter
Dark matter does not give off observable energy in any EM wavelength, but can be
detected by watching the behavior of space objects. A few examples are:
• The stars in the outer reaches of a spiral galaxy orbit with the same speed as
those much closer in. This implies that the galaxy is surrounded by a massive
spherical distribution of unseen matter, which adds to its total mass.
• The gravitational centers of galaxy clusters do not lie at their expected place,
but are offset. This implies that there is much more unseen matter present.
• Gravitational lenses are often found with no apparent visible matter in the
foreground to act as the lens. The lensing agent is usually a very large
concentration of dark matter.
• Our Local Group of galaxies and some other nearby clusters are streaming off in
the same direction in space towards an unknown and unseen super massive object
or complex nicknamed “The Great Attractor”.
Flavors of Dark Matter: WIMPs vs. MACHOs
WIMPs: Weakly-Interacting Massive Particles. Dark, tiny particles fill the
universe, but they are so tiny and weakly interacting that they are difficult to
detect by gravity studies. This is currently the favored idea.
MACHOs: Massive Compact Halo Objects. Dark, ultra dense matter surrounds
galaxies and resides within and beyond their observed halos. It also may exist
between galaxies in a cluster or even in the “voids” of the bubble structure of the
universe. This dark matter could take the form of neutron stars and black holes, or
other types of objects yet unknown.