Title: What do we know about Dark Matter and Dark Energy
1What do we know about Dark Matter and Dark Energy?
- CAS Meeting, 14 January 2006
- Dr. Uwe Trittmann
- Otterbein College
2Starting Point
- Before we can say anything about the dark side,
we have to answer the following questions - What is bright matter?
- What do we know about bright matter?
3Bright Matter
- All normal or bright matter can be seen in
some way - Stars emit light, or other forms of
electromagnetic radiation - All macroscopic matter emits EM radiation
characteristic for its temperature - Microscopic matter (particles) interact via the
Standard Model forces and can be detected this way
4The Structure of Matter
Atom Nucleus and Electrons
Nucleus Protons and Neutrons (Nucleons)
Nucleon 3 Quarks
? 10-10m ?
? 10-14m ?
?10-15m?
5Elementary Particles
- All ordinary nuclear matter is made out of
quarks - Up-Quark Down-Quark
- (charge 2/3)
(charge -1/3) - In particular
- Proton uud ? charge 1
- Nucleons
- Neutron
udd ? charge 0
(composite particles)
6The Forces of the Standard Model
- Force (wave)
- Gravity couples to mass
- Electromagnetic force
- couples to charge
- Weak force
- responsible for radioactive decay
- Strong force
- couples to quarks
- Carrier (particle)
- graviton (?)
- photon
- W, W-, Z0
- 8 gluons
massless carriers ? long ranged
massive carriers ? short ranged
7The particles of the Standard Model
Matter particles have half-integer spin (fermions)
Force carriers have integer spin (bosons)
8Conclusion
- We know a lot about the structure of matter!
- We know a lot about the forces between matter
particles - We know al lot about the theory that describes
all of this (the Standard Model) - ? Great News !
9Pie in the Sky Content of the Universe
5
Dark Energy Dark Matter SM Matter
25
70
- ?We know almost everything about almost nothing!
10What is the dark stuff?
- Dark Matter is the stuff we know nothing about
(but we have some ideas)
Dark Energy is the stuff we have absolutely
no idea about
11Conclusion
- If we dont know anything about it, it is boring,
and there is nothing to talk about. - ? End of lecture!
12Alternate Conclusion
- If we dont know anything about it, it is
interesting because there is a lot to be
discovered, learned, explored, - ? beginning of lecture!
13So what do we know? Is it real?
- It is real in the sense that it has specific
properties - The universe as a whole and its parts behave
differently when different amounts of the dark
stuff is in it - Lets have a look!
14First evidence for dark matter The missing mass
problem
- Showed up when measuring rotation curves of
galaxies
15The Mass of the Galaxy
- Can be determined using Keplers 3rd Law
- Solar System the orbital velocities of planets
determined by mass of Sun - Galaxy orbital velocities of stars are
determined by total mass of the galaxy contained
within that stars orbit - Two key results
- large mass contained in a very small volume at
center of our Galaxy - Much of the mass of the Galaxy is not observed
- consists neither of stars, nor of gas or dust
- extends far beyond visible part of our galaxy
(dark halo)
16Properties of Dark Matter
- Dark Matter is dark at all wavelengths, not just
visible light - We cant see it (cant detect it)
- Only effect is has it acts gravitationally like
an additional mass - Found in galaxies, galaxies clusters, large scale
structure of the universe - Necessary to explain structure formation in the
universe at large scales
17What is Dark Matter?
- More precise What does Dark matter consist of?
- Brown dwarfs?
- Black dwarfs?
- Black holes?
- Neutrinos?
- Other exotic subatomic particles?
18Classification of Dark Matter
- Classify the possibilities
- Hot Dark Matter
- Warm Dark Matter
- Cold Dark Matter
- Baryonic Dark Matter
You could have come up with this, huh?!
19Hot Dark Matter
- Fast, relativistic matter
- Example neutrino
- Pro
- interact very weakly, hard to detect ? dark!
- Con
- Existing boundaries limit contribution to missing
mass - Hot Dark matter cannot explain how galaxies
formed - Microwave background (WMAP) indicates that
mastter clumped early on - Hot dark matter does not clump (its simply too
fast)
20Baryonic Dark Matter
- Normal matter
- Brown Dwarfs
- Dense regions of heavy elements
- MACHOs massive compact halo objects
- Big Bang nucleosynthesis limits contribution
21Cold Dark Matter
- Slow, non-relativistic particles
- Most attractive possibility
- Large masses (BH, etc) ruled out by grav. lensing
data - Major candidates
- Axions
- Sterile neutrinos
- SIMPs (strongly interacting massive particles)
- WIMPs (weakly ), e.g. neutralinos
- All of the above are exotic, i.e. outside the
SM
22Alternatives
- Maybe missing mass, etc. can be explained by
something else? - Incomplete understanding of gravitation
- Modified Newtonian Dynamics (MOND)
- Nonsymmetric gravity
- General relativity
23The silent majority Dark Energy
70
24Aside Standard Cosmology
- Based on Einsteins theory of Gravity, aka
General Relativity - Assumes isotropic, homogeneous universe
- This smeared out mass property is approximately
valid if we average over large distances in the
universe
25General Relativity ?! Thats easy!
Rµ? -1/2 gµ? R 8pG/c4 Tµ?
OK, fine, but what does that mean?
- (Actually, it took Prof. Einstein 10 years to
come up with that!)
26The Idea behind General Relativity
- In modern physics, we view space and time as a
whole, we call it four-dimensional space-time. - Space-time is warped by the presence of masses
like the sun, so Mass tells space how to bend - Objects (like planets) travel in straight lines
through this curved space (we see this as
orbits), so - Space tells matter how to move
27Still too complicated?
- Here is a picture Sun
- Planets orbit
28Effects of General Relativity
- Bending of starlight by the Sun's gravitational
field (and other gravitational lensing effects)
29What General Relativity tells us
- The more mass there is in the universe, the more
braking of expansion there is - So the game is
- Mass vs. Expansion
- And we can even calculate who wins!
30The size of the Universe depends on time!
Expansion wins!
Its a tie!
Mass wins!
Time
31The Universe expands!
- Where was the origin of the expansion?
- ?Everywhere!
- Every galaxy sees the others receding from it
there is no center
32Big Bang
- The universe expands now, so looking back in time
it actually shrinks until? - ?Big Bang model The universe is born out of a
hot dense medium - 13.7 billion years ago.
33The Fate of the Universe determined by a single
number!
- Critical density is the density required to just
barely stop the expansion - Well use ?0 actual density/critical density
- ?0 1 means its a tie
- ?0 gt 1 means the universe will recollapse (Big
Crunch) ? Mass wins! - ?0 lt 1 means gravity not strong enough to halt
the expansion ? Expansion wins! - And the number is ?0 1 (probably)
34The Shape of the Universe
- In the basic scenario there is a simple relation
between the density and the shape of space-time - Density Curvature 2-D example Universe
Time Space - ?0gt1 positive sphere closed,
bound finite - ?01 zero (flat) plane open, marginal
infinite - ?0lt1 negative saddle open, unbound
infinite
35Expansion of the Universe
- Either it grows forever
- Or it comes to a standstill
- Or it falls back and collapses (Big crunch)
- In any case Expansion slows down!
Surprise of the year 1998 (Birthday of Dark
Energy) All wrong! It accelerates!
36Enter The Cosmological Constant
- Usually denoted ?0, it represents a uniform
pressure which either helps or retards the
expansion (depending on its sign)
- Physical origin of ?0 is unclear
- Einsteins biggest blunder or not !
- Appears to be small but not quite zero!
- Particle Physics biggest failure
37Effects of the Cosmological Constant
- Introduced by Einstein, not necessary
- Repulsive ? accelerates expansion of universe
Hard to distinguish today
38Triple evidence for Dark Energy
- Supernova data
- Large scale structure of the cosmos
- Microwave background
39Microwave Background Signal from the Big Bang
- Heat from the Big Bang should still be around,
although red-shifted by the subsequent expansion - Predicted to be a blackbody spectrum with a
characteristic temperature of 3Kelvin by George
Gamow (1948) - ? Cosmic Microwave Background Radiation (CMB)
40Discovery of Cosmic Microwave Background
Radiation (CMB)
- Penzias and Wilson (1964)
- Tried to debug their horn antenna
- Couldnt get rid of background noise
- ? Signal from Big Bang
- Very, very isotropic (1 part in 100,000)
41CMB Heres how it looks like!
Peak as expected from 3 Kelvin warm object
Shape as expected from black body
42Maybe pigeons?
- Proposed error pigeon crap in antenna
- Real reason a signal from the Big Bang
Pigeon trap
? Horn antenna
43Latest Results WMAP(Wilkinson Microwave
Anisotropy Probe)
- Measure fluctuations in microwave background
- Expect typical size of fluctuation of one degree
if universe is flat - Result
- Universe is flat !
44Experiment and Theory
Expect accoustic peak at l200 ? There it is!
45Supernova Data
- Type Ia Supernovae are
- standard candles
- Can calculate distance
- from brightness
- Can measure redshift
- General relativity gives us distance as a
- function of redshift for a given universe
- Supernovae are further away than
- expected for any decelerating (standard)
- universe
46Supernova Data
magnitude
redshift
47Redshift Everything is moving away from us!
- Measure spectrum of galaxies and compare to
laboratory measurement - lines are shifted towards red
- This is the Doppler effect Red-shifted objects
are moving away from us
48Example Spectrum of a Quasar
Highly redshifted spectrum
? the quasar is very far away and
keeps going!
Quasar
Lab
49Large Scale Structure of the Cosmos
- Large scale structure of the universe can be
explained only by models which include Dark
Matter and Dark Energy
Experiments 2dF GRS, SDSS
50Properties of Dark Energy
- Should be able to explain acceleration of cosmic
expansion ? acts like a negative pressure - Must not mess up structure formation or
nucleosynthesis - Should not dilute as the universe expands ? will
be different of content of universe as time
goes by
51The Pie changes - As time goes by
-11.5
-7.5
¼ size ½
Now
2 size 4
24.5
11.5
52Why does the Pie change?
- Dark energy density stays constant
- Matter density falls of like volume
- Volume grows, mass stays constant
- Big Question why do we live in an era where the
content is rather democratic? - Because we are here to observe!
(Dangerous answer)
53What is Dark Energy?
- We have a few ideas what it could be
- Unfortunately none of these makes fits our job
description - Wanted Dark Energy Candidate
54Dark Energy Candidates
- Global Vacuum Energy
- Local Vacuum Energy
- Dynamical Dark Energy
- Modified Gravity
55Global Vacuum Energy
- Cosmological constant
- Constant in space and time
- Same across the universe
- Pro
- Could be explainable from first principles
- Con
- No known explanation yet
56Local Vacuum Energy
- Constant in the observable universe, but
different in very distant parts of cosmos - Pro
- Maybe explains why cosmological const. is so
small here - Con
- Requires different domains
57Dynamical Dark Energy
- Quintessence
- Slowly varying energy source
- Pro
- Testable
- Can gradually go to zero energy
- Con
- Has not been detected
58Modified Gravity
- Modification of general relativity on large
scales - Pro
- Does not need dark energy
- Con
- Hard to modify and still explain existing data
59Threefold Evidence
- Three independent measurements agree
- Universe is flat
- 30 Matter
- 70 dark energy
60Measuring Dark Energy
Dark energy acts like negative pressure, and is
characterized by its equation of state, w
p/? ? We can measure w!
61Conclusion
- Need more ideas
- No problem! Thats what theorists produce every
day - Need more data
- Some space missions (Planck, etc) are on the way
- LHC probing SUSY will start operation in 2007