1. Dark Energy & Dark Matter
Shamit Kachru (Stanford and SLAC)
LASER, Stanford, August 2012
Tuesday, August 7, 2012

2. Introduction
It was the burden of Newton to teach us that the same
laws that we can infer from terrestrial experiments, also
apply in the heavens:
Tuesday, August 7, 2012

3. Fast foward 250+ years:
We have learned a lot about the constitution and
interactions of terrestrial matter!
Tuesday, August 7, 2012

4. But, starting with Newton’s observation, we can infer that
what we know about constitutes only a small fraction of
what exists:
In fact, Newtonian logic suffices to understand 1/4 of this.
The other 3/4 requires Einstein.
Tuesday, August 7, 2012

5. Dark Matter
Galaxies are massive, gravitationally bound systems that
consist of stars and stellar remnants, gas and dust, and, as
it happens, a bit more.
There are in excess of 170 billion galaxies in the observable
Universe. Telescopes capable of imaging distant galaxies
came online in the first quarter of the 20th century.
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6. Fritz Zwicky and Vera Rubin were the first two to argue
that there is more to typical galaxies than meets the eye:
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7. The flatness of the curve indicates that there is more
matter present outside the luminous core of the galaxy.
Quantitative estimates, based by now on a bewildering
variety of independent probes, indicate that there is five
times more of this “dark matter” than there is stuff we
know about!
From indirect tests, as well as e.g. the Bullet Cluster event,
Tuesday, August 7, 2012

8. we know the dark matter interacts with “our” stuff very
weakly. (Its self-interactions are also bounded).
Many candidates have been proposed for the composition
of this stuff (and maybe more than contributes some
Dark Matter Candidates -
fraction):
A Terribly Incomplete Survey
Thermal Relics ! equilibrium This list is by no means
at early times complete ! I will focus on
SUSY ! neutralino several classes
SUSY ! gravitino SUSY is perhaps the favored
source of dark matter
Neutrino candidates
standard model + "sterile#
Axions are the favored solution
right-handed to the strong CP problem
Non-thermal Relics ! Neutrinos are the least good
everything else candidate, but are known to
actually exist
Axion
Primordial black holes are a
Primordial Black Holes
possibility ! difficult to form
Planck mass and larger
There is a dirty little secret !
???
if it's relevant it's more
interesting than dark matter
Tuesday, August 7, 2012 Edward A. Baltz (KIPAC) XXXII SLAC Summer Institute ! Nature's Greatest Puzzles 8/2/04

9. We aim to learn about it using either astrophysical “dark
matter annihilation” events (e.g. in the center of
the galaxy):
or via production or direct detection here on Earth:
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10. Given that “our” 4% of the stuff gives rise to such diverse
structures and consequences, it is perhaps reasonable to
think that many things could be afoot in the dark sector.
Dark Energy
This still leaves us with a missing 75%. First of all, how do
we know that? It is already perhaps surprising that we
could infer the existence of the dark matter, which
interacts so very weakly with us.
The key to the discovery of dark energy lies back in the
original observations of Einstein and Hubble.
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11. Einstein:
Gravitation is geometry. The geometry of space is fixed by
the matter within it.
Hubble:
Space-time at the largest scales illustrates this!
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12. Expanding Universe encoded in “redshifts”:
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13. In a simple equation, the spatial slices are expanding in time
in a way governed by a(t), the “scale factor”:
ds = −dt + a (t)(dx + dy + dz )
2 2 2 2 2 2
The dynamics of the Universe at large scales is then
determined by how the various matter sources “tell” a(t)
to behave:
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14. * Very little mass leads to a Universe which expands
forever, with the expansion slowed slightly by the
gravitational pull of matter.
* In contrast, above a critical amount, there is enough
matter that its gravitational pull causes recollapse of the
spatial slices -- a “big crunch”.
What was completely unexpected in 1998, when the
verdict came in, was the third possibility: a Universe that
not only continues to expand, but whose expansion
accelerates!
Tuesday, August 7, 2012

15. But this is what was found by a detailed study of the
properties of distant Type IA supernovae.
Because of the way they arise, such supernovae are thought
to be ~ “standard candles”.
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16. Old supernovae are brighter than they should be -
because the expansion is accelerating!
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17. “Normal” matter -- stuff that behaves like dust particles --
and even photons, cannot make the Universe do this.
In fact, as nearly as we can tell, the accelerated expansion is
caused by a small and positive “cosmological constant”
modifying Einstein’s theory -- an energy density of empty
space.
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18. On the one hand, such a cosmological constant should not
have been unexpected (though it was).
“Virtual” quantum particles, if nothing else, would be
expected to generate a cosmological term in our best
theories.
This would be on top of any “classical” vacuum energy
present in our vacuum.
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19. The best estimates we get from such quantum loops would
suggest a “natural” size for the vacuum energy roughly
1060 − 10120 times larger than what we see!
How are we to understand this? We’re not sure yet.
Amazingly, the most conservative answer today (still
untested) relies on vacuum selection occurring in a
complicated potential landscape:
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20. Such a potential landscape seems to arise naturally in string
theory, one promising candidate for a theory unifying
gravity with other interactions:
But to do justice to this subject would require further
discussion of eternal inflation, string theory, and even
anthropic arguments; all would take us far afield, and we
have no more time!
Tuesday, August 7, 2012

21. Thanks for your attention!
Shamit Kachru
Department of Physics
Stanford University and SLAC
http://www.stanford.edu/dept/physics/people/faculty/
kachru_shamit.html
Tuesday, August 7, 2012